Psi2 Lupi

Psi2 Lupi (ψ2 Lup) is a triple star system in the constellation Lupus. It is visible to the naked eye with an apparent magnitude of 4.75. Based upon an annual parallax shift of 8.97 mas as seen from Earth, it is located around 360 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of due to interstellar dust. This system is a member of the Upper Centaurus-Lupus subgroup of the Scorpius–Centaurus Association.
The inner pair of stars in this system form a double-lined spectroscopic binary with an orbital period of 12.26 days and an eccentricity of 0.19. The two components are described as similar in appearance. They have the spectrum of a B-type main sequence star with a stellar classification of B5 V. The luminosity has a micro-variability with a frequency of 0.94483 cycles per day and an amplitude of 0.0067 in magnitude. The third component is a magnitude 10 star at an angular separation of 0.51 arc seconds.


Alpha Sagittarii

Alpha Sagittarii (α Sagittarii, abbreviated Alpha Sgr, α Sgr), also named Rukbat , is a star in the constellation of Sagittarius.
Properties.
Alpha Sagittarii is a blue, class B dwarf star. It does not appear particularly bright in the sky to the naked eye, with a visual apparent magnitude of +3.97.
The star has an effective temperature about twice that of the Sun and is nearly three times as massive, with a luminosity in visible wavelengths about 117 times that of the Sun. Based on an excess emission of infrared radiation, it may have a debris disk, much like Vega. It is a single-lined spectroscopic binary system. The ROSAT All Sky Survey discovered that Alpha Sagittarii is emitting an excess flux of X-rays, which is not expected to originate from a star of this spectral class. The most likely explanation is that the companion is an active pre-main sequence star or else a star that has just reached the main sequence.
Nomenclature.
"α Sagittarii" (Latinised to "Alpha Sagittarii") is the star's Bayer designation. It is unclear why Bayer designated this star as the alpha, rather than Epsilon Sagittarii or Sigma Sagittarii. This led some old star charts to occasionally depict Alpha and Beta Sagittarii as much brighter than they are in reality, as they are invisible from northern Europe, being too far south to see there.
The star bore the traditional names "Rukbat" and "Alrami", derived from the Arabic "rukbat al-rāmī" 'the knee of the archer'. The star Delta Cassiopeiae also bore the traditional names "Ruchbah" or "Rukbat", from the Arabic word ركبة "rukbah" meaning "knee". In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included "Rukbat" for this star (Delta Cassiopeiae was later given the name "Ruchbah").
In Chinese, (), meaning "Celestial Spring", refers to an asterism consisting of Alpha Sagittarii, Beta¹ Sagittarii and Beta² Sagittarii. Consequently, the Chinese name for Alpha Sagittarii itself is (, .)
This star, together with Beta¹ Sagittarii and Beta² Sagittarii, were "Al Ṣuradain" (ألسردين), the two Surad, desert birds.


V4650 Sagittarii

V4650 Sagittarii (qF362) is a luminous blue variable star (LBV) in the constellation of Sagittarius. Located some 25,000 light years away, the star is positioned on the edge of a starburst cluster known as the Quintuplet cluster.
Discovery.
V4650 Sgr was first catalogued in 1996 as star 362 in a list of stars in the galactic centre region near the Quintuplet Cluster. The acronym qF is used for stars in the list and so the star name is qF 362. The acronym FMM is also used, hence FMM 362. The LBV nature of qF 362 was not recognised until 1999. It is one of three LBVs close to the Quintuplet Cluster, all highly luminous stars.
V4650 was discovered using infrared telescopes. It is extremely faint at optical wavelengths due to interstellar extinction. The 2MASS survey recorded it at 17th magnitude in red light and 19th magnitude in blue light, while it is a 7th magnitude object in K band infrared.
Properties.
V4650 Sgr is calculated to be one of the most luminous stars known, at to . It is considered to be a bona-fide luminous blue variable, although it has not been observed to change temperature from the S Doradus minimum strip to a cooler outburst state. The infrared brightness has varied between magnitude 7.0 and 7.9. It is calculated to have a temperature of 11,300 K and a radius of . Unlike both the two nearby LBVs, V4650 Sgr has no detectable associated nebulosity.


L Carinae

The Bayer designations l Carinae and L Carinae are distinct.


HR 5256

HR 5256 is a star located thirty-three light-years away from the Sun in the northern circumpolar constellation of Ursa Major. It has an orange hue and is a challenge to view with the naked eye, having an apparent visual magnitude of 6.52 The distance to this star is very nearly 10 parsecs, so the absolute magnitude of 6.51 is nearly the same as the star's apparent magnitude. HR 5256 is drifting nearer to the Sun with a radial velocity of −26.4 km/s, and will make its closest approach to the Sun in about , when it will be at a distance of .
This object is an ordinary K-type main-sequence star with a stellar classification of K3 V, which indicates it is undergoing core hydrogen fusion. It is over five billion years of age and is spinning slowly with a projected rotational velocity of 4.6 km/s. The star has an estimated 82% of the Sun's mass and 78% of the Sun's radius. It is radiating just 28% of the luminosity of the Sun from its photosphere at an effective temperature of 4,811 K.


H Velorum

The Bayer designations h Velorum and H Velorum are distinct. Due to , both designations link here. For the star


38 Arietis

38 Arietis (abbreviated 38 Ari) is a variable star in the northern constellation of Aries. "38 Arietis" is the Flamsteed designation. It was once designated 88 Ceti, forming part of the neighboring constellation of Cetus. With an apparent visual magnitude of +5.18, it is bright enough to be viewed with the naked eye. The measured annual parallax shift of 27.52 mas is equivalent to a distance of approximately from Earth.
The spectrum of this star matches a stellar classification of A7 III-IV, with the luminosity class of III-IV indicating it shows traits part way between the subgiant and giant star stages of its evolution. It is a Delta Scuti variable with a period of 0.0355 days (51 minutes) and a magnitude change of 0.040. This star is larger than the Sun, with more than double the Sun's radius and 11 times the luminosity. This energy is being radiated into outer space from the atmosphere at an effective temperature of 7,638 K, giving it the white-hued glow of an A-type star.


V448 Carinae

V448 Carinae is a single star in the constellation Carina. It has the Bayer designation O Carinae, while "V448 Carinae" is the variable star designation. This object has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.60. It is located at a distance of approximately 680 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +26 km/s.
This is an aging giant star with a stellar classification of K5III. Having exhausted the supply of hydrogen at its core, it has cooled and expanded off the main sequence and now has 51 times the girth of the Sun. It is classified as a probable semiregular variable star with a sub-type of SRd and a brightness that varies from visual magnitude 5.66 down to 5.86 over a period of 56.5 days. The star is an estimated 2.85 billion years old with 1.73 times the mass of the Sun. It is radiating 582 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,974 K.


57 Cancri

57 Cancri is a double star in the zodiac constellation of Cancer, located around 460 light years away from the Sun. They are visible to the naked eye as a faint star with a combined apparent visual magnitude of +5.40. The brighter member, designated component A. is a yellow-hued giant star with a stellar classification of G7 III and an apparent magnitude of +6.09. Its companion, component B, is an orange-hued giant with a class of K0 III and an apparent magnitude of +6.37. As of 2017, the pair had an angular separation of along a position angle of 310°.


Epsilon Delphini

Epsilon Delphini (ε Delphini, abbreviated Eps Del, ε Del), officially named Aldulfin , is a solitary, blue-white hued star in the northern constellation of Delphinus. It is visible to the naked eye with an apparent visual magnitude of 4.03. Based upon an annual parallax shift of 9.87 mas as seen from the Earth, the system is located about 330 light-years from the Sun. At Epsilon Delphini's distance, the visual magnitude is diminished by an extinction factor of 0.11 due to interstellar dust. The star is moving closer to the Sun with a radial velocity of −19 km/s.
This is a B-type giant star with a stellar classification of B6 III. It has 4.6 times the Sun's radius and is radiating 676 times the solar luminosity from its photosphere at an effective temperature of 13,614 K. The star may be slightly variable, occasionally brightening to magnitude 3.95. It is spinning with a projected rotational velocity of 52 km/s.
Proper names.
"ε Delphini" (Latinised to "Epsilon Delphini") is the star's Bayer designation.
The star bore the traditional Arabic name "ðanab ad-dulfīn" or Dzaneb al Delphin, which appeared in the catalogue of stars in the "Calendarium of Al Achsasi Al Mouakket" and which was translated into Latin as "Cauda Delphini", meaning 'the dolphin's tail'. In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the name "Aldulfin" for this star on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.
In Chinese, (), meaning "Rotten Gourd", refers to an asterism consisting of Epsilon Delphini, Eta Delphini, Theta Delphini, Iota Delphini and Kappa Delphini. Consequently, the Chinese name for Epsilon Delphini itself is (, .). From this Chinese name, the name "Pae Chaou" was formed.


Alpha Serpentis

Alpha Serpentis (α Serpentis, abbreviated Alpha Ser, α Ser), formally named Unukalhai , is a double star in the head (Serpens Caput) of the equatorial constellation of Serpens. With an apparent visual magnitude of 2.6, this star is the brightest in the constellation and it can be viewed with the naked eye from most of the Earth. Parallax measurements yield an estimated distance of about from the Sun.
Properties.
Alpha Serpentis is a giant star with a stellar classification of K2 III, having consumed the hydrogen at its core and evolved away from the main sequence. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 12 times the radius of the Sun. The effective temperature of the outer envelope is 4,498 K, giving it an orange hue that is characteristic of a K-type star. It has been classified as a strong CN star, showing a higher than expected strength in the cyanogen bands.
This star is radiating about 38 times the luminosity of the Sun, while a further 32 times the Sun's luminosity is being emitted in the infrared, for 70-fold total. A magnitude +11.8 companion is at an angular separation of 58 arcseconds from Alpha Serpentis, while a 13th magnitude star lies 2.3 arcminutes distant.
Nomenclature.
"α Serpentis" (Latinised to "Alpha Serpentis") is the system's Bayer designation.
It bore the traditional names "Unukalhai" (alternatively spelt "Unuk al Hay" or "Unuk Elhaija") from the Arabic عنق الحيّة "ʽunuq al-ḥayyah" "the serpent's neck", and "Cor Serpentis" from the Latin "the Heart of the Serpent". In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name "Unukalhai" for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
Alpha Serpentis is a member of the indigenous Arabic asterism "al-Nasaq al-Yamānī" "the Southern Line" of "al-Nasaqān" "the Two Lines", along with Delta Serpentis, Epsilon Serpentis, Delta Ophiuchi, Epsilon Ophiuchi, Zeta Ophiuchi and Gamma Ophiuchi. According to a 1971 NASA catalogue, "al-Nasaq al-Yamānī" or "Nasak Yamani" was the name for two stars: Delta Serpentis as "Nasak Yamani I" and Epsilon Serpentis as "Nasak Yamani II".
In Chinese, (), meaning "Right Wall of Heavenly Market Enclosure", refers to an asterism which represents eleven old states in China and which is marking the right borderline of the enclosure, consisting of Alpha Serpentis, Beta Herculis, Gamma Herculis, Kappa Herculis, Gamma Serpentis, Beta Serpentis, Delta Serpentis, Epsilon Serpentis, Delta Ophiuchi, Epsilon Ophiuchi and Zeta Ophiuchi. Consequently, the Chinese name for Alpha Serpentis itself is (, ), and represents the state Shu (蜀) (or Shuh) (together with Lambda Serpentis in R.H.Allen's works).
References.
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24 Lyncis

24 Lyncis is a single star in the northern constellation of Lynx. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 4.96. The distance to this star, as determined from its parallax measurements, is around 274 light years. It is moving further away from the Earth with a heliocentric radial velocity of about +9 km/s.
This object has a stellar classification of A3 IVn, matching an A-type star with a subgiant luminosity class. The 'n' suffix indicates "nebulous" absorption lines due to rapid rotation. The star is spinning with a projected rotational velocity of 233 km/s, giving it an equatorial bulge that is 17% larger than the polar radius. Zorec et al. (2012) estimate the star is actually 88% of the way through its main sequence lifetime. It is 262 million years old with 1.89 times the mass of the Sun. 24 Lyncis is radiating 61 times the luminosity of the Sun from its photosphere at an effective temperature of 8,786 K.
There is a magnitude 11.15 visual companion at an angular separation of along a position angle of 324°, as of 2010.


HD 290327

HD 290327 is a single star in the equatorial constellation of Orion. It has a yellow hue with an apparent visual magnitude of 8.99, which is too faint to be viewed with the naked eye. Parallax measurements provide a distance estimate of 184 light years from the Sun. It is drifting away with a radial velocity of +29.5 km/s, having come to within around a million years ago.
Kazanasmas (1973) found a stellar classification of G5IV for this object, matching a G-type star that is evolving along the subgiant branch. It was later given a class of G8V, suggesting it is instead a G-type main-sequence star. This object is nearly twelve billion years old and is spinning slowly with a projected rotational velocity of 1.4 km/s. The star has 86% of the mass of the Sun and 95% of the Sun's radius. It is radiating 75% of the luminosity of the Sun from its photosphere at an effective temperature of 5,525 K. The metallicity is sub-solar, meaning it has a lower abundance of elements other than hydrogen and helium compared to the Sun.
In 2009, a gas giant planet was found in orbit around the star. It is orbiting at a distance of around with a period of .


45 Cancri

45 Cancri is a binary star system in the zodiac constellation of Cancer, located 680 light years away from the Sun. It has the Bayer designation A1 Cancri; "45 Cancri" is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star at an apparent visual magnitude of 5.62. The pair form a double-lined spectroscopic binary with an orbital period of and an eccentricity of 0.46. They are drifting closer to the Earth with a heliocentric radial velocity of −6 km/s.
The primary, designated component A, is an aging giant star with a stellar classification of G8 III, but has most likely not yet made multiple ascents up the red giant branch. It has 3.11 times the mass of the Sun and has expanded to 14 times the Sun's radius. The star is radiating 210 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,058. The less evolved secondary, component B is likewise a giant star, having a class of A3 III. It has three times the mass of the Sun and shines with 191 times the Sun's luminosity.


Kappa Pictoris

κ Pictoris, Latinised as Kappa Pictoris, is a star in the constellation Pictor. It is close to the lower limit of stars that are visible to the naked eye having an apparent visual magnitude of +6.11. Based upon an annual parallax shift of 5.14 mas as seen from Earth, this star is located around 630 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.10 due to interstellar dust.
This is a B-type main sequence star with a stellar classification of B8/9 V. It is about 76.4% of the way through its main sequence lifespan. The star is spinning rapidly with a projected rotational velocity of 264 km/s. It has an estimated 3.4 times the mass of the Sun and is radiating 210 times the Sun's luminosity from its photosphere at an effective temperature of 11,641 K.


C Velorum

The Bayer designations c Velorum and C Velorum are distinct. Due to , both designations link here. For the star


Alpha Trianguli

Alpha Trianguli (α Trianguli, abbreviated Alpha Tri, α Tri) is a spectroscopic binary star in the constellation of Triangulum. Based on parallax measurements obtained during the Hipparcos mission, it is approximately distant from the Sun. The brighter or primary component is named Mothallah .
Nomenclature.
"α Trianguli" (Latinised to "Alpha Trianguli") is the system's Bayer designation.
The system bore the traditional names "Ras al Muthallah" or "Mothallah" and "Caput Trianguli" derived from the Arabic رأس المثلث' "raʼs al-muthallath" "the head of the triangle" and its Latin translation. The International Astronomical Union Working Group on Star Names (WGSN) has approved the name "Mothallah" for this star. For members of multiple star systems, and where a component letter (e.g. from the Washington Double Star Catalog) is not explicitly shown in the namelist, the WGSN says that the name should be understood to be attributed to the visually brightest component by visual brightness.
In combination with Beta Trianguli, these stars were called "Al Mīzān", which is Arabic for "The Scale Beam".
In Babylonian astronomy, Alpha Trianguli is listed as UR.BAR.RA "The Wolf", bearing the epithet "the seeder of the plough" in the MUL.APIN, listed after "The Plough", the name for a constellation formed of Triangulum plus Gamma Andromedae.
Properties.
Estimates of the combined stellar classification for this system range from F5III to F6IV, with the luminosity class of 'IV' or 'III' indicating the primary component is a subgiant or giant star, respectively. It is a member of a close binary system—a spectroscopic binary—whose components complete an orbit about their center of mass once every 1.736 days. Because the primary star is rotating rapidly, it has assumed the shape of an oblate spheroid. The ellipsoidal profile of the star, as viewed from Earth, varies over the course of an orbit causing the luminosity to vary in magnitude during the same period. Such stars are termed ellipsoidal variables. Within a few million years, as the primary continues to evolve into a red giant star, the system may become a semi-detached binary with the Roche lobe becoming filled to overflowing.
The mean apparent magnitude of +3.42 for this pair is bright enough to be readily seen with the naked eye. It forms the second brightest star or star system in this generally faint constellation, following Beta Trianguli. The effective temperature of the primary's outer envelope is 6,288 K, giving it a yellow-white hue typical of F-type stars. It has a mean radius about three times the radius of the Sun. The system is an estimated 1.6 billion years old.


NGC 468

NGC 468 is a spiral galaxy in the constellation Pisces. With its distance being approximately 209 million light-years from Earth, it was discovered by John Frederick William Herschel in 1827.


Beta Virginis

Beta Virginis, a name Latinized from β Virginis, is a star in the equatorial constellation of Virgo. It has the proper name Zavijava (), and, despite its designation 'beta', is the fifth-brightest star in Virgo with an apparent visual magnitude of 3.604. The distance to this star is 35.7 light years based on parallax, and it is drifting further away with a radial velocity of +4.1 km/s. It is 0.69 degrees north of the ecliptic, so it can be occulted by the Moon and (rarely) by planets. The next planetary occultation of Beta Virginis will take place on 11 August 2069, by Venus.
Properties.
This is an F-type main-sequence star with a stellar classification of F9 V, which means it is generating energy through core hydrogen fusion. Sun-like oscillations have been detected in Beta Virginis, allowing its internal structure to be modeled in more detail. It is around 2.9 billion years old with a projected rotational velocity of 4.3 km/s and appears to be near the end of its main sequence lifetime. Larger and more massive than the Sun, it is comparatively metal-rich (that is, it has a higher preponderance of elements heavier than helium). It is radiating 3.6 times the luminosity of the Sun from its photosphere at an effective temperature of 6,132 K.
According to Nelson & Angel (1998), Beta Virginis could host two or three jovian planets in wide orbits. The authors have set an upper limit of 1.9, 5 and 23 Jupiter masses for the putative planets with orbital periods of 15, 25 and 50 years respectively. Also Campbell et al. 1988 inferred the existence of planetary objects or even brown dwarfs around Beta Virginis. However more recent studies have not confirmed the existence of any substellar companion around Beta Virginis yet. McDonald Observatory team has set limits to the presence of one or more planets with masses between 0.16 and 4.2 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.
Nomenclature.
"β Virginis" (Latinised to "Beta Virginis") is the star's Bayer designation.
It bore the traditional names "Zavijava" (also "Zavijah", "Zavyava" and "Zawijah") and "Alaraph". "Zavijava" is from the Arabic "زاوية العواء" "zāwiyat al-cawwa’" 'corner of the barking (dog)'. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the name "Zavijava" for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
In Chinese, (), meaning "Right Wall of Supreme Palace Enclosure", refers to an asterism consisting of Beta Virginis, Sigma Leonis, Iota Leonis, Theta Leonis and Delta Leonis. Consequently, the Chinese name for Beta Virginis itself is (, .), representing (), meaning "The Right Law Administrator". 右執法 (Yòuzhífǎ), spelled "Yew Chi Fa" by R.H. Allen, means "the Right-hand Maintainer of Law".


Psi5 Aurigae

Psi5 Aurigae (ψ5 Aur, ψ5 Aurigae) is a star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25. Based upon parallax measurements made during the Hipparcos mission, this star is approximately distant from Earth. There is an optical companion which is 36 arcseconds away and has an apparent magnitude of +8.4.
The spectrum of this star shows it to be a G-type main sequence star with a stellar classification of G0 V. Thought to be around 4 billion years old, it is similar in size, mass, and composition to the Sun, making this a solar analog. It is radiating energy into space at an effective temperature of 5,989 K, giving it the golden-hued glow of a G-type star.
Observation in the infrared shows an excess emission that suggests the presence of a circumstellar disk of dust, known as a debris disk. This material has a mean temperature of 60 K, indicating that it is orbiting at a distance of about 29 astronomical units from the host star. The dust has about half the mass of the Moon and is around 600 million years old. The star is being examined for evidence of extrasolar planets, but none have been found so far.


HIP 57274 d

HIP 57274 d is an exoplanet orbiting the K-type main sequence star HIP 57274 about 84.5 light-years (26 parsecs, or nearly km) from Earth in the constellation Cetus. It orbits within the outer part of its star's habitable zone, at a distance of 1.01 AU. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star.
Characteristics.
Mass, radius and temperature.
HIP 57274 d is a gas giant, a planet that has a radius and mass close to that of the gas giants Jupiter and Saturn. It has a temperature of . It has an estimated mass of around 0.527 (167 ), and a potential radius of around 9 based on its mass, since it is slightly more massive than Saturn.
Host star.
The planet orbits a (K-type) star named HIP 57274, orbited by a total of three planets. The star has a mass of 0.73 and a radius of 0.68 . It has a surface temperature of 4640 K and is 7 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K.
The star's apparent magnitude, or how bright it appears from Earth's perspective, is 8.96. Therefore, HIP 57274 is too dim to be seen with the naked eye, but can be seen with good binoculars.
Orbit.
HIP 57274 d orbits its star every 432 days at a distance of 1.01 AU. This is very similar to that of Earth's orbital period and distance.
Habitability.
HIP 57274 d resides in the outer part of circumstellar habitable zone of the parent star. The exoplanet, with a mass of 0.527 , is too massive to be rocky, and because of this the planet itself may not be habitable. Hypothetically, large enough moons, with a sufficient atmosphere and pressure, may be able to support liquid water and potentially life.
For a stable orbit the ratio between the moon's orbital period "P"s around its primary and that of the primary around its star "P"p must be < 1/9, e.g. if a planet takes 90 days to orbit its star, the maximum stable orbit for a moon of that planet is less than 10 days. Simulations suggest that a moon with an orbital period less than about 45 to 60 days will remain safely bound to a massive giant planet or brown dwarf that orbits 1 AU from a Sun-like star. In the case of HIP 57274 d, the moon's orbit would have to be roughly 40 days to support a stable orbit.
Tidal effects could also allow the moon to sustain plate tectonics, which would cause volcanic activity to regulate the moon's temperature and create a geodynamo effect which would give the satellite a strong magnetic field.
To support an Earth-like atmosphere for about 4.6 billion years (the age of the Earth), the moon would have to have a Mars-like density and at least a mass of 0.07 . One way to decrease loss from sputtering is for the moon to have a strong magnetic field that can deflect stellar wind and radiation belts. NASA's Galileo's measurements hints large moons can have magnetic fields; it found that Jupiter's moon Ganymede has its own magnetosphere, even though its mass is only 0.025 .


WASP-80

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.
The star was named Petra in 2019 by Jordanian amateur astronomers as part of the "nameexoworlds" contest.
Three multiplicity surveys in 2015-2018 did not detect any stellar companions to WASP-80, but a survey in 2020 did detect a 0.07 companion candidate at an angular separation 2.132 arcseconds, with a false alarm probability of 3%.
Planetary system.
In 2013 a transiting hot Jupiter planet b was detected on a tight, circular orbit. The planet was named "Wadirum" by Jordanian astronomers in December 2019. Its equilibrium temperature is , slightly below the measured dayside temperature of .
Measurement of the Rossiter–McLaughlin effect in 2015 revealed WASP-80b's is orbit is well aligned with the equatorial plane of the star, with orbital obliquity equal to 14°.
Although one transmission spectrum of the planetary atmosphere showed signs of ionised potassium, another measurement in 2017 yielded a gray and featureless spectrum, probably due to a high cloud deck or haze in the atmosphere of WASP-80b.


Emptiness (Chinese constellation)

The Emptiness mansion () is one of the Twenty-eight mansions of the Chinese constellations. It is one of the northern mansions of the Black Tortoise.


NGC 740

NGC 740 is a barred spiral galaxy located in the Triangulum constellation. It is estimated to be 210 million light-years from the Milky Way and has a diameter of about 85,000 light-years. It was discovered by the Irish engineer Bindon Stoney, an assistant to William Parsons.


82 Cancri

82 Cancri is a solitary, orange-hued star in the zodiac constellation of Cancer. It has the Bayer designation Pi2 Cancri, which is Latinized from π2 Cancri; "82 Cancri" is the star's Flamsteed designation. The star lies just a degree to the south of the ecliptic. With an apparent visual magnitude of +5.33, it is dimly visible to the naked eye on a dark night. This star is located at a distance of approximately 540 light years from the Sun based on parallax. At that range, the visual magnitude is diminished by an extinction of 0.10 magnitudes due to interstellar dust. It is drifting further away with a radial velocity of +27 km/s.
This is an evolved K-type giant star with a stellar classification of K1 III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. The star currently has 31 times the girth of the Sun and is spinning slowly with a projected rotational velocity. It is radiating over 300 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,340 K. Based on its abundance of iron, the star has a lower abundances of heavier elements than the Sun.


List of stars in Pisces

This is the list of notable stars in the constellation Pisces, sorted by decreasing brightness.


Gliese 625

GJ 625 (AC 54 1646-56) is a red dwarf star of spectral type M2.0V, located in the constellation Draco, 21.1 light-years from Earth.
Planetary system.
On May 18, 2017, a planet was detected orbiting AC 54 1646-56 by the HARPS-N telescope. The planet, AC 54 1646-56b (GJ 625b), orbits on the inner edge of the optimistic circumstellar habitable zone of its star, and may support liquid water.


Epsilon Coronae Australis

Epsilon Coronae Australis (ε CrA), is a star system located in the constellation Corona Australis. Varying in brightness between apparent magnitudes of 4.74 to 5 over 14 hours, it is the brightest W Ursae Majoris variable (low mass contact binary) in the night sky.
Naming.
Nicolas Louis de Lacaille gave Epsilon Coronae Australis its Bayer designation. It is also known as HR 7152, and HD 175813.
Properties.
Epsilon Coronae Australis is an F4V dwarf star with an effective temperature of 6000 Kelvin. It ranges between apparent magnitudes of 4.74 to 5 over 14 hours, an absolute magnitude of +2.45, and a mass of 1.1 solar masses. Epsilon Coronae Australis is a W Ursae Majoris variable, indicating that it has a contact companion within the Roche Limit of the primary. The star is located at a distance of 30 pc (97 light years) from the Sun. Yildiz and colleagues estimated the age of the system at 2.83 ± 0.28 billion years based on study of the properties of the system and estimated rate of mass transfer. They found the current masses of the primary and secondary to be 1.72 ± 0.04 and 0.22 ± 0.02 solar masses respectively, from their original masses of 1.06 ± 0.03 and 2.18 ± 0.06 solar masses.


Upsilon Cancri

The Bayer designation Upsilon Cancri (υ Cnc / υ Cancri) is shared by two stars, in the constellation Cancer:
They are separated by 0.34° on the sky.


IU Aurigae

IU Aurigae is a triple star system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19. The eclipsing pair form a Beta Lyrae-type semidetached binary of two Bp stars with a period of 1.81147435 days. During the primary eclipse, the visual magnitude of the system drops to 8.89, while for the secondary it decreases to 8.74. The third component is a massive object with , and may actually be a binary – which would make this a quadruple star system.


Nu Microscopii

ν Microscopii, Latinised as Nu Microscopii, is a star in the constellation Microscopium. This is an orange hued star that is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.76. It was first catalogued as Nu Indi by the French explorer and astronomer Nicolas Louis de Lacaille in 1756, before being reclassified in Microscopium and given its current Bayer designation of Nu Microscopii by Gould. This object is located at a distance of around 252 light-years from the Sun, based on parallax, and is drifting further away with a radial velocity of about +9 km/s.
This is an aging giant star with a stellar classification of K0 III. It has expanded to 10.6 times the girth of the Sun after exhausting the supply of hydrogen at its core and evolving off the main sequence. The star has 2.46 times the mass of the Sun. It is radiating 59.5 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,925 K.


M Centauri

M Centauri (M Cen) is a binary star in the constellation Centaurus. It is approximately 260 light years from Earth.
M Centauri is a yellow G-type giant with an apparent magnitude of +4.64. It is a spectroscopic binary with an orbital period of 437 days.


HD 38858

HD 38858 is a G-type star, much like The Sun, with one detected planet. The planet, designated HD 38858 b, is about twice the mass of Uranus and orbits in the star's habitable zone.
The last observation of this system for a dust disc or comet belt was in 2009 by the Spitzer Space Telescope; a belt was inferred at 102 AU. It has an inclination of 48◦.
Exoplanet.
The exoplanet HD 38858 b was discovered in 2011 in orbit in its host star's habitable zone, a zone in which Earth-like conditions (namely the presence of liquid water) on a planet's surface are possible. The planet is likely a gas giant, a type of planet which astronomers believe is unlikely to support life as it is currently understood. However, the planet could have a rocky natural satellite capable of sustaining an Earth-like environment. In 2020, the issue of habitability was explored by the popular YouTube channel "Fire of Learning", in which the planet was referred to as "Kynigos", and its hypothetical satellite was compared to the Jovian Moons of Europa and Io. Potential obstacles to habitability of any natural satellite, including the eccentricity of the planet's orbit, likelihood of the moon being tidally locked, and probable prevalence of geothermic activity owed to its orbit around the gas giant, were highlighted.


Omicron Ophiuchi

ο Ophiuchi, Latinized as Omicron Ophiuchi, is a wide double star in the equatorial constellation of Ophiuchus. The co-moving pair are visible to the naked eye as a dim point of light, with the two components having apparent visual magnitudes of 5.14 and 6.59. As of 2015, they had an angular separation of along a position angle of 354°. The distance to both stars is approximately 281 light years based on parallax, and they are drifting closer to the Sun with a radial velocity of around −29 km/s.
The brighter member of the pair, designated component A, is an aging giant star with a stellar classification of G8III. With the supply of hydrogen at its core exhausted, it has expanded to 12 times the radius of the Sun. The star is radiating 75 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,849 K. The secondary star, component B, has a class of F6IV-V, matching an F-type star with a luminosity class that is a blend of traits from a main sequence and a subgiant star. It has three times the Sun's radius and is radiating 12.6 times the Sun's luminosity at 6,296 K.


NGC 3302

NGC 3302 is an unbarred lenticular galaxy in the constellation Antlia. It was discovered by the astronomer John Herschel on January 28, 1835.


NGC 5752

NGC 5752 is a spiral galaxy in the constellation Boötes, member of Arp 297 interacting galaxies group of four galaxies: NGC 5752, NGC 5753, NGC 5754, NGC 5755.


NGC 6820 and NGC 6823

NGC 6820 is a small reflection nebula near the open cluster NGC 6823 in Vulpecula. The reflection nebula and cluster are embedded in a large faint emission nebula called Sh 2-86. The whole area of nebulosity is often referred to as NGC 6820.
M27, the Dumbbell Nebula, is found three degrees to the east, and α Vulpeculae three degrees to the west.
Open star cluster NGC 6823 is about 50 light-years across and lies about 6,000 light-years away. The center of the cluster formed about two million years ago and is dominated in brightness by a host of bright young blue stars. Outer parts of the cluster contain even younger stars. It forms the core of the Vulpecula OB1 stellar association.


Beta Sagittae

Beta Sagittae, Latinized from β Sagittae, is a single star in the northern constellation of Sagitta. It is a faint star but visible to the naked eye with an apparent visual magnitude of 4.38. Based upon an annual parallax shift of 7.7237 mas as seen from the Gaia satellite, it is located 420 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −22 km/s.
This is an evolved red giant with a stellar classification of . The suffix notation indicates a mild overabundance of the cyanogen molecule in the spectrum. Beta Sagittae is an estimated 129 million years old with 4.33 times the mass of the Sun, and has expanded to roughly 27 times the Sun's radius. The star is radiating 392 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,850 K.
Naming.
In Chinese, (), meaning "Left Flag", refers to an asterism consisting of β Sagittae, α Sagittae, δ Sagittae, ζ Sagittae, γ Sagittae, 13 Sagittae, 11 Sagittae, 14 Sagittae and ρ Aquilae. Consequently, the Chinese name for β Sagittae itself is (, .)


NGC 6027d

NGC 6027d is a barred spiral galaxy that is strictly a visual member of Seyfert's Sextet, a compact group of galaxies, which is located in the constellation Serpens. NGC 6027d is not interacting with the other galaxies in the cluster, but is in the background and just happens to be in the same line of sight. The galaxy is nearly 700 million light years away from the interacting group and is believed to be extremely large in size.


WR 7

WR 7 (HD 56925) is a Wolf–Rayet star in the constellation of Canis Major. It lies at the centre of a complex bubble of gas which is shocked and partially ionised by the star's radiation and winds.
The distance is uncertain, with estimates between 3.5 kiloparsecs (11,410 light-years) and 6.9 kiloparsecs (22,500 light-years). Assuming a distance of 4.8 kiloparsecs (15,600 light-years), this star is calculated to be 280,000 times brighter than our Sun] 16 times more massive, and 1.41 times larger with a surface temperature of 112,000 K.
Stars of its kind are characterised by a rapid loss of stellar mass, driven by chemically enriched high-speed stellar winds. It is estimated that it loses mass at the rate of 7x10−5 solar masses each year through winds of 1,545 km/s.
The ring nebula NGC 2359 is excited by the ionising radiation of WR7. It is also known as Thor's Helmet or the Duck Nebula. The ring is approximately 4pc across and prominent at wavelengths from radio to X-ray.


Psalterium Georgii

Psalterium Georgii (also Harpa Georgii) (Latin for "George's harp") was a constellation created by Maximilian Hell in 1789 to honor George III of Great Britain. It was created from northern stars in Eridanus and was next to the constellation Taurus, and included 10 Tauri. It is no longer in use.


Beta Pavonis

Beta Pavonis, Latinized from β Pavonis, is a single, white-hued star in the southern constellation of Pavo. It can be seen with the naked eye, having an apparent visual magnitude of 3.42. Based upon an annual parallax shift of 24.14 mas as seen from Earth, it is located 135 light years from the Sun. It is moving away from the Sun with a radial velocity of +4 km/s. Beta Pavonis is a member of the Ursa Major Moving Group, a set of stars that share a similar motion through space.
Zorec and Royer (2012) list a stellar classification for this star of A5 IV, indicating it is an evolving subgiant star that has consumed the hydrogen at its core and has begun to expand onto the red giant branch. However, Houk (1979) listed a more evolved class of A7 III, suggesting it is already a giant star. It has about 2.3 times the Sun's radius and 2.51 times the mass of the Sun. At the estimated age of 305 million years, the star still has a relatively high rate of spin, having a projected rotational velocity of 75 km/s. Beta Pavonis is radiating 66 times the Sun's luminosity from its photosphere at an effective temperature of about 8,184.


HD 70555

HD 70555 (w Puppis) is a class K2.5II-III (orange giant) star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.


NGC 2509

NGC 2509 is an open cluster in the constellation of Puppis. It was discovered on 3 December 1783 by William Herschel. It was described as "bright, pretty rich, slightly compressed" by John Louis Emil Dreyer, the compiler of the New General Catalogue.
The cluster is about 14 light-years (4.2 parsecs) wide, but the cluster's other parameters remain poorly known. Some studies have estimated a distance of about 9,500 light-years (2,900 parsecs) away from the Solar System, while older estimates put it at only 2980 light-years (912 parsecs) away. Estimates of the cluster's age have also varied significantly, from 1.2 billion years old to 8 billion years old. The latest analysis based on the parallaxes measured by the Gaia spacecraft confirms that it is a relatively distant object, with a distance between 2500 and 3000 parsecs.


List of stars in Argo Navis


NGC 2202

NGC 2202 is an open cluster in the constellation Orion. The object was discovered in 1825 by the German-Russian astronomer Friedrich Georg Wilhelm von Struve.


HR 6384

HR 6384 is a binary star system in the southern constellation of Ara, the Altar. The system is faintly visible to the naked eye with a combined apparent visual magnitude that fluctuates around 6.153, and it is located at a distance of approximately from the Sun. It is drifting closer with a radial velocity of around −34 km/s.
The system appears to be a close, interacting binary with a hot secondary component of class A or hotter. It forms a suspected ellipsoidal variable with a period of 80 days and an amplitude variation of 0.08 in magnitude. The primary component is an aging red giant/bright giant with a stellar classification of M1/M2II/III, currently on the asymptotic giant branch. With the supply of hydrogen at its core exhausted, it has expanded to 160 times the girth of the Sun. It is radiating 3,562 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,562 K.


List of stars in Piscis Austrinus

This is the list of notable stars in the constellation Piscis Austrinus, sorted by decreasing brightness.


Delta Coronae Australis

Delta Coronae Australis is a single star located in the southern constellation of Corona Australis. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.57. The star is located about 174 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +21 km/s.
This object is an evolved giant star with a stellar classification of K1III. After exhausting the supply of hydrogen at its core, the star expanded off the main sequence and now has 11 times the radius of the Sun. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through core helium fusion. The star is 2.8 billion years old with 1.5 times the mass of the Sun. It is radiating 55 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,654 K.


Beta Fornacis

Beta Fornacis (Beta For, β Fornacis, β For) is the Bayer designation for a solitary star in the southern constellation of Fornax. It is visible to the naked eye with an apparent visual magnitude of 4.46. Based upon an annual parallax shift of 18.89 mas, it is located around 173 light years away from the Sun. At that distance, the visual magnitude is reduced by an interstellar extinction factor of 0.1.
This is an evolved, G-type giant star with a stellar classification of G8 III. It is a red clump giant, which means it has undergone helium flash and is currently generating energy through the fusion of helium at its core. The star has an estimated 1.53 times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating over 55 times the solar luminosity from its outer atmosphere at an effective temperature of 4,820 K.
Beta Fornacis has a visual companion, CCDM J02491-3224B, which has an apparent visual magnitude of approximately 14.0. As of 1928, it lay at an angular separation of 4.80 arc seconds along a position angle of 67°. Located around three degrees to the southwest is the globular cluster NGC 1049.


Delta Telescopii

The Bayer designation Delta Telescopii (δ Tel, δ Telescopii) is shared by two stars in the southern constellation Telescopium. They are separated by 0.16° on the sky.


R Aurigae

R Aurigae (R Aur) is a Mira variable, a pulsating red giant star in the constellation of Auriga, at a distance of .
R Aurigae has an apparent visual magnitude which varies between 6.7 and 13.9 with a period of 450 days. The light curve varies strongly from cycle to cycle, sometimes having a pronounced hump on the ascending branch and usually having rise and fall times approximately equal. The cycle period has oscillated slowly between about 450 and 465 days. The discoverer of R Aurigae's variability is not known, but it was widely observed in the late 19th century and its spectrum was described in 1890.
R Aurigae is catalogued as a component of a double star, with the 10th magnitude HD 233095, although the two stars are unrelated.


Kepler-28b

Kepler-28b is an extrasolar planet orbiting the star Kepler-28. It is a transiting planet that is smaller than Jupiter that orbits very closely to Kepler-28.
Host star.
Kepler-28 is the host star of Kepler-28b, and is alternatively known as KOI-870 and KIC 6949607. The star is smaller, less massive, and cooler than the Sun, with (respectively) a radius 0.7 times of the Sun; a mass 0.75 times of the Sun; and an effective temperature of 4590 K. The star has a high metallicity with relation to the Sun, as it has a metallicity of [M/H] = 0.34. With an apparent magnitude of 15.05, Kepler-28 is effectively invisible to the naked eye from Earth.
Characteristics.
Kepler-28b is a gas giant. Upon discovery, it was poorly characterized, with only upper mass limit of 1.51 times the mass of Jupiter can be ascertained from dynamical simulations. The planet, which transits its host star, completely passes across the face of Kepler-28 in 2.77 hours. The ratio of its orbital period with that of Kepler-28c is 1.52. In 2016, improved radial velocity data has allowed to classify Kepler-28b as a small (sub-Neptune) gas giant.


HD 207832

HD 207832 is a G-type main-sequence star. Its surface temperature is 5764 K. HD 207832 is slightly enriched compared to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.17 and is much younger at an age of 0.74 billion years. Kinematically, it belongs to the thin disk of the Milky Way.
A multiplicity study in 2014 detected a candidate comoving stellar companion - a red dwarf star or brown dwarf with a spectral class M6.5, at a very wide projected separation of 38.57′ (2.0 light years)
Planetary system.
In 2012, two planets, named HD 207832b and HD 207832c, were discovered by the radial velocity method on wide, eccentric orbits. The planetary system would remain stable even if the planetary orbits are coplanar.
Although discovery of the inner planet was confirmed in 2018, the discovery of both planets was suspected to be a false positive in 2020, as newer radial velocity data do not support the existence of the planets.


Beta Leonis Minoris

Beta Leonis Minoris (Beta LMi, β Leonis Minoris, β LMi) is a binary star in the constellation of Leo Minor. It has an overall apparent visual magnitude of approximately 4.2. Although it is the only star in Leo Minor with a Bayer designation, it is only the second brightest star in the constellation (the brightest is 46 Leonis Minoris).
Binary system.
β Leonis Minoris is a binary that can be resolved for a portion of each orbit. When the two components are too close to resolve, it appears as a single G9 giant star with some indications of a second set of spectral lines. The orbit derived as a double-lined spectroscopic binary is poor, and a better orbit has been calculated using only the spectral lines of the primary, plus input from the known visual observations. The orbital period is nearly 39 years and the eccentricity is high at 0.683. The semi-major axis of the orbit is , but the separation varies from to .
The primary star is a late G-class red clump giant, a star that is fusing helium in its core and lies at the cool end of the horizontal branch. The properties of the secondary star can only be estimated from its relative brightness and its spectral class. It is an F8 subgiant, hotter than the sun and starting to evolve away from the main sequence.


Theta Microscopii

The Bayer designation Theta Microscopii (θ Mic / θ Microscopii) is shared by two star systems, in the constellation Microscopium:


Iota Coronae Borealis

Iota Coronae Borealis, Latinized from ι Coronae Borealis, is a binary star system in the constellation Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of is 4.96. Based upon an annual parallax shift of 10.46 mas as seen from the Earth, it is located about 312 light years from the Sun.
This is a single-lined spectroscopic binary with an orbital period of 35.5 days and an eccentricity of 0.56. The visible member, component A, has a stellar classification of , indicating it is a chemically peculiar mercury-manganese star with narrow absorption lines. The secondary member, component B, appears to be an A-type star.


NGC 7600

NGC 7600 is an elliptical galaxy about 160 million light-years in the constellation Aquarius classified as a lenticular galaxy, or, more formally, an S0 galaxy.


WW Aurigae

WW Aurigae is an eclipsing binary star system in the northern constellation of Auriga. It has a combined maximum apparent visual magnitude of 5.86, which is bright enough to be dimly visible to the naked eye. Based upon an annual parallax shift of , it is located 297 light years from the Earth. The system is moving further away with a heliocentric radial velocity of −9 km/s, having come to within some 3.12 million years ago.
This is a double-lined spectroscopic binary system, having a circular orbit with a period of 2.5 days. It was discovered to be variable independently by Friedrich Schwab and Heinrich Van Solowiew in 1913. Both components are metallic-lined, or Am stars, with a spectrum showing a deficiency of calcium and scandium, and an overabundance of heavier elements. Together they form an EA, or Algol-type, eclipsing binary with the primary occultation reducing the net magnitude to a minimum of 6.54 and the secondary eclipse lowering it to 6.43, over a cycle time of 2.52501936 days.


Taurus Molecular Cloud

The Taurus Molecular Cloud is a molecular cloud in the constellations Taurus and Auriga. This cloud hosts a stellar nursery containing hundreds of newly formed stars. The Taurus Molecular Cloud is only 140 pc (430 ly) away from earth, making it the nearest large star formation region. It also reveals characteristics that make it ideal for detailed physical studies. It has been important in star formation studies at all wavelengths.
The cloud is notable for containing many complex molecules, including cyanopolyynes HC"n"N for "n"=3,5,7,9.
The Taurus Molecular Cloud was identified in the past as a part of the Gould Belt, a large structure surrounding the solar system. More recently (January 2020) the Taurus Molecular Cloud was identified as being part of the much larger Radcliffe wave, a wave-shaped structure in the local arm of the Milky Way.
The newly formed stars in this cloud have an age of 1-2 million years. The Taurus-Auriga association, which is the stellar association of the cloud, contains the variable star T Tauri, which is the prototype of T Tauri stars. The many young stars and the close proximity to earth is an ideal condition to search for protoplanetary disks around members of the association, to search for exoplanets around these stars or to identify brown dwarfs that are part of the association. Members of this region are suited for direct imaging of exoplanets, because young planets glow brightly in infrared wavelengths.
Members of the Taurus-Auriga association with a circumstellar disk or exoplanet:


Kepler-56

Kepler-56 is a red giant roughly 3,060 light years away with slightly more mass than the Sun. It has two confirmed planets, one slightly smaller than Neptune, and another slightly smaller than Saturn. Both planets were discovered in 2012.
Planetary system.
In 2012, a planetary system was discovered around Kepler-56 via transit method. Planets were subsequently confirmed through transit timing variation method.
Asteroseismological studies revealed that the orbits of Kepler-56b and Kepler-56c are about 45° misaligned to the host star's equator. Follow-up radial velocity measurements revealed the evidence of a gravitational perturbator but currently it is not clear if it is a nearby star or a third planet.
Both Kepler-56b and Kepler-56c will be devoured by their parent star in 130 and 155 million years, respectively.


Lambda Ursae Majoris

Lambda Ursae Majoris (λ Ursae Majoris, abbreviated Lambda UMa, λ UMa), formally named Tania Borealis , is a star in the northern circumpolar constellation of Ursa Major.
Properties.
This star has an apparent visual magnitude of +3.45, making it one of the brighter members of the constellation. The distance to this star has been measured directly using the parallax technique, which yields a value of roughly with a 4% margin of error. The stellar classification of Lambda Ursae Majoris is A2 IV, with the luminosity class of 'IV' indicating that, after 410 million years on the main sequence, this star is in the process of evolving into a giant star as the supply of hydrogen at its core becomes exhausted. Compared to the Sun it has 240% of the mass and 230% of the Sun's radius, but is radiating 37 times as much luminosity. This energy is being emitted from the star's outer atmosphere at an effective temperature of 9,280 K, giving it the characteristic white-hot glow of an A-type star.
Nomenclature.
"λ Ursae Majoris" (Latinised to "Lambda Ursae Majoris") is the star's Bayer designation.
It bore the traditional names "Tania" (shared with Mu Ursae Majoris) and "Tania Borealis". "Tania" comes from the Arabic phrase 'the Second Spring (of the Gazelle)'. and "Borealis" (originally "borealis") is Latin for 'the north side'. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included "Tania Borealis" for this star.
In Chinese, (), meaning "Three Steps", refers to an asterism consisting of Lambda Ursae Majoris, Iota Ursae Majoris, Kappa Ursae Majoris, Mu Ursae Majoris, Nu Ursae Majoris and Xi Ursae Majoris. Consequently, the Chinese name for Lambda Ursae Majoris itself is (, ).


NGC 4305

NGC 4305 is a dwarf spiral galaxy located about 100 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer John Herschel on May 2, 1829.
The galaxy has a nearby major companion; NGC 4306.
Physical characteristics.
NGC 4305 exhibits well-defined, smooth spiral arms which terminate well outside its central bulge. This spiral structure appears to have been induced by a tidal interaction with NGC 4306. Such a tidal interaction would also explain its deficiency in neutral hydrogen gas (HI).
Virgo Cluster membership.
Although considered to be a member of the Virgo Cluster, its high radial velocity and blue luminosity suggest it is in fact a background galaxy.


NW Puppis

NW Puppis, also known as υ2 Puppis, is a star in the constellation Puppis. Located around 910 light-years distant, it shines with a luminosity approximately 1108 times that of the Sun and has a surface temperature of 15,000 K. Anamarija Stankov ruled this star out as a Beta Cephei variable.
Neither component of this double is given a letter in Lacaille's catalogue or the British Association star catalogue. Gould gave them the designations (Latin letter) v1 and v2 Puppis, but these are rarely used. Lacaille applied the Greek letter υ to the star now called υ Carinae. The designation υ2 first appeared in several catalogues at the end of the 19th century.


Zeta Lyrae

The Bayer designation ζ Lyrae (Zeta Lyrae, ζ Lyr) is shared by two stars in the constellation Lyra:


Upsilon Eridani

The Bayer designation Upsilon Eridani (υ Eri / υ Eridani) is shared by four stars, in the constellation Eridanus:
This series of stars bore the traditional proper names "Theemim" (also "Theemin") and "Beemin" (also "Beemim"). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the names "Theemin" for υ2 Eridani on 1 February 2017 and "Beemim" for υ3 Eridani on 30 June 2017; both are now so included in the List of IAU-approved Star Names.


PV Cephei

PV Cephei is variable star of Orion type located in the constellation of Cepheus at a distance of over 1600 light-years from Earth. Although the terms 'Orion variable/Orion type' are now no longer used by most astronomers. The term 'Young Stellar Object' or YSO is preferred, since 'Orion Variable' is a term which was given at a time when these objects were thought to be more homogeneous than is now known to be the case. It has been used by the CGVS compilers but astronomers generally do not use these terms any more.


Beta Draconis

Beta Draconis, a name Latinized from β Draconis, is a binary star system and the third-brightest star in the northern circumpolar constellation of Draco. The two components are designated Beta Draconis A (officially named Rastaban , the traditional name of the system) and B respectively. With a combined apparent visual magnitude of 2.79, it is bright enough to be easily seen with the naked eye. Based upon parallax measurements from the Hipparcos astrometry satellite, it lies at a distance of about from the Sun. The system is drifting closer with a radial velocity of −21 km/s.
The binary system consists of a bright giant orbited by a dwarf companion once every four millennia or so. The companion is about 11 magnitudes fainter than the primary star, and the two are separated by .
The spectrum of the primary, Beta Draconis A, matches a stellar classification of G2Ib-IIa, showing mixed features of a bright giant and a supergiant star, and is listed as a standard star for that spectral class. It is about 65 million years old and is currently undergoing its first convective dredge-up. Compared to the Sun, Beta Draconis A is an enormous star with six times the mass and roughly 40 times the radius. At this size, it is emitting about 950 times the luminosity of the Sun from its outer envelope at an effective temperature of 5,160 K, giving it the yellow hue of a G-type star. The star has a particularly strong chromospheric emission that is generating X-ray and far-UV radiation. There is a detectable magnetic field with a longitudinal field strength of .
Beta Draconis lies on or near the cepheid instability strip, yet only appears to be a microvariable with a range of about 1/100th of a magnitude. It was confirmed as a variable star with a range of about 1/100th of a magnitude by Gabriel Cristian Neagu using data from the TESS and Hipparcos missions. The variability was reported to the AAVSO (American Association of Variable Star Observers), in the Variable Star Index.
Nomenclature.
"β Draconis" (Latinised to "Beta Draconis") is the system's Bayer designation. The designations of the two components as "Beta Draconis A" and "B" derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
It bore the traditional name "Rastaban", which has also been used for Gamma Draconis. This name, less commonly written "Rastaben", derives from the Arabic phrase "ra's ath-thu'ban" "head of the serpent/dragon". It was also known as "Asuia" and "Alwaid" , the latter from the Arabic "al-ʽawāʼidh" "the old mother camels". In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name "Rastaban" for the component Beta Draconis A on 21 August 2016 and it is now so included in the List of IAU-approved Star Names.
Beta Draconis is part of the asterism of the Mother Camels (Arabic "al'awa'id"), along with Gamma Draconis (Eltanin), Mu Draconis (Erakis), Nu Draconis (Kuma) and Xi Draconis (Grumium), which was later known as the "Quinque Dromedarii".
In Chinese, (), meaning "Celestial Flail", refers to an asterism consisting of Beta Draconis, Xi Draconis, Nu Draconis, Gamma Draconis and Iota Herculis. Consequently, the Chinese name for Beta Draconis itself is known as (, ).


Zeta Canis Minoris

Zeta Canis Minoris (ζ Canis Minoris) is a solitary, blue-white hued star in the equatorial constellation of Canis Minor. It is a dim star but visible to the naked eye with an apparent visual magnitude of 5.13. Based upon an annual parallax shift of 5.23 mas as seen from Earth, this star is located around 410 light years from the Sun. It is moving away from the Sun with a radial velocity of +32.3 km/s.
This is a B-type bright giant star with a stellar classification of B8 II. It is a Mercury-Manganese star, showing an overabundance of these elements in its spectrum. The mean longitudinal magnetic field strength is . The star has about four times the mass of the Sun and is radiating 490 times the Sun's luminosity from its photosphere at an effective temperature of 13,500 K.


NGC 5965

NGC 5965 is a spiral galaxy located in the constellation Draco. It is located at a distance of circa 150 million light years from Earth, which, given its apparent dimensions, means that NGC 5965 is about 260,000 light years across. It was discovered by William Herschel on May 5, 1788. Two supernovae have been observed in NGC 5965, SN 2001 cm (type II, mag 17.5) and SN 2018cyg (type II, mag 17.0).
NGC 5965 is seen nearly edge-on, with an inclination of 80 degrees. Dust is seen across the galactic disk, while there is also a red dust lane at the nucleus. The bulge is X-shaped, that suggests that the galaxy is actually barred. NGC 5965 along with another edge-on galaxy, NGC 5746, were the galaxies used to confirm that peanut shaped bulge are associated with the presence of a bar, by spectrographically observing the disturbance caused at the velocity distributions of the galaxies.
The galaxy features some level of disk disturbance, like a warp, as the outer part of the disk along with a ring-like dust lane appear to be on a different plane from the bulge, but it could also be a projection effect. When observed in K band, the galaxy features a stellar ring.
NGC 5965 lies in a galaxy filament which also includes NGC 5987 and its loose group, which includes NGC 5981, NGC 5982, NGC 5985, three galaxies known as the Sampler.
The Lancashire Watch Company of Prescot was founded in 1889 by Thomas P. Hewitt as a rival to the large American and Swiss watch companies. It failed in 1910.
History.
Until the late 19th century, Prescot had been the centre of the watchmaking trade in England. The workers produced watch parts in small workshops attached to their cottages and were paid by piece work. By 1889 the "American System of Watch Manufacturing" meant that the Waltham Watch Company and others could produce watches at a much lower price and the town fell into decline.
In 1889 a company was formed and eventually a large factory was built to create complete watches under one roof. The products produced had more in common with earlier American designs than traditional English fusee watches. Because of economies of scale the Lancashire Watch Company struggled to compete with the larger American and Swiss factories. It could not make a profit and went bankrupt in 1910. Thomas P Hewitt's watch was sold at Christies Auction in 1995 fetching $215,000, purchased by Robbie Dickson; a well-known historical watch collector.


HMS Aimwell

HMS "Aimwell" (W 113) was a of the Royal Navy during the Second World War.
Service history.
"Aimwell" was laid down on 15 November 1941 at the Defoe Shipbuilding Company in Bay City, Michigan, as BAT-7. She was delivered to the United States Navy and was transferred to the Royal Navy under the Lend-Lease Act on 6 June 1942. HMRT "Aimwell" was visited by Franklin D. Roosevelt on 26 January 1943, when Roosevelt was returning from the Casablanca Conference. The tug was stationed with West Africa Command between 1942 and 1943. She returned to American custody postwar on 30 March 1946. BAT-7 was struck on 1 May 1946 and sold to Moller on 6 January 1948. Renamed "Patricia Moller", she was again renamed "Golden Cape" in 1952 and finally sold in 1971 to the Luzon Stevedoring Corporation. She was renamed "Hawkeye" and was mined and sunk in the Mekong on 3 February 1975.


Toebox

The toebox is the section of footwear that surrounds the toes on closed-toe shoes. Toeboxes that do not fit can cause injuries and foot deformities. Toeboxes come in a variety of shapes and styles of construction, some of which are a matter of fashion, and some of which are designed for specialized functions.
Fitting.
A simple way to test if a toe box is too tight is to take out the insole and stand on it. If the toes overhang the insole, the toebox is too small.
A toe box also needs enough extra room to accommodate movements of the foot, such as lengthening arches and toe splay. With each step, ankles and feet bend, toes spread and flex, and the arches of the foot flatten and rebound. Because the arches flatten, the foot lengthens and widens as it takes weight. Weight-bearing causes the foot to widen across the ball by up to . A foot with a higher longitudinal arch will lengthen more in use, and more room in front of the toes may be needed.
When running, weight is shifted onto the ball and toes of the foot; the heel barely touches. A narrow toebox therefore hinders function more. High heels also shift weigh onto the toes.
Problems.
Generally, toes should not touch toeboxes. Toeboxes that put pressure on the foot slowly produce permanent deformities; toe boxes that strike the toes cause bruising; and toeboxes that rub hurt the skin.
Joint deformities.
Too-tight toeboxes can permanently deform the foot, weakening it enough to significantly impair function. Tight socks can have similar effects, especially if the foot is already fairly deformed.
Roomy toeboxes which permit free movement help; the improvement depends on the amount and duration of the deformity, and the age of the patient.
If too-narrow and too-short toeboxes have previously been worn, the muscles of the arches will be weaker; the foot may expand more, and the muscles may feel tired and painful until they strengthen. Foot exercize and broader shoes tend to thicken and widen the foot; a re-fitting after six months may be needed, although after that the shoe size of adults generally stabilizes.
Bunions.
Shoes which put pressure on the outside edge of the big toe cause bunion (bending of the big toe sideways towards the other toes). Bunion prevention requires a shoe with a sole which does not taper on that side, so that the big toe can point in its natural direction. Any material bunion deformity appreciably weakens the foot; the sideways shift in the big toe decreases leverage and shifts weight-bearing. However, this deformity is very common. A bunionette, a similar bending of the little toe, is caused by a too-narrow toebox which puts pressure on the other side of the toes; it is not uncommon, but generally causes less impairment, as the little toe is less mechanically important. Women over 50 who remember wearing narrow toeboxes in their 20s and 30s are more likely to have foot pain and bunions.
Hammertoes.
Tight toeboxes are the most common cause of hammertoes, mallet toes and claw toes. A too-small toebox forces the toes to bend; eventually, the ligaments in the top of the foot shorten, and the toes no longer relax to a straight position when taken out of the shoes. If the ligaments continue to tighten, it may become impossible to straighten the toes.
Wearing wide, roomy toeboxes which are longer than the longest toe, and are not tight or painful anywhere, prevents and treats hammertoes. High heels can force the toes forwards against the ends of the toebox, so they should also be avoided. Shoes should fasten such that the toes do not slide into a collision with the end of the toebox, especially when going downhill.
Skin and nail problems.
Blisters and calluses.
Ill-fitting toeboxes can rub against the foot, causing blisters, and eventually calluses and corns. These often occur on the toes and the balls of the foot. Foot deformation and dysfunction can encourage calluses to form.
Jogger's toes.
If the toebox does not have enough room around the toes, or the foot can slide forwards far enough to jam the toes into the end of the toebox, it can also cause black toenail (jogger's toe). The toes also need vertical space; a toe cap which is low enough to press on the top of the toe may also cause bruising under the nail, especially if the toe cap is stiff. If the toebox is pointed, the toes may be wedged forwards into the area with inadequate height.
Ingrown toenails.
Narrow pointed shoes (or tight socks) can be a factor in causing ingrown toenails.
Vertical profile.
Toes boxes are either structured (with a three-dimensional shape, often produced with a thermoplastic interlayer) or unstructured. Structuring mostly affects the depth of the toebox. Some moccasins have wide, unstructured toeboxes, somewhat loose on the foot, which allow toe splay. Many toe boxes also include toe spring, where the sole curves up towards the toes. When the shoe is flexible enough to bend with the foot, at the ball of the foot, this is not needed. Most toeboxes, at a point 5 cm from the tip, are ~44 mm deep, regardless of style. Especially wide and deep toeboxes may be used to provide space for foot deformities and foot orthotics.
Horizontal profile.
Toe boxes also come in various widths and horizontal-plane shapes. Foot-shaped toeboxes are rare. Most toe boxes are widest at the ball of the foot, then taper towards the toes, although the foot widens from the base of the toes forwards. Toe boxes often taper symmetrically, from both sides; feet do not. If toebox taper is wide enough that it is outside the space needed by the foot, a tapered toebox can be comfortable. Many shoes have a toebox which is excessively narrow in relation to heel width; if a sufficiently wide toebox can be picked out, the shoe will often be loose on the heel. Some shoe manufacturers make "split sizes", where the toe and heel size are varied independently, on a combination last.
Split toeboxes.
Some toeboxes are split. Some are split into two pockets, like those of jika-tabi; others are split into more pockets. Five-pockets toeboxes can be difficult to fit, as each pocket may be too long, too short, too wide, or too narrow. Splitting the toebox helps allow toe splay and gripping.
Applications.
Military.
An early-20th-century survey by the United States Army Medical Corps's Army Shoe Board found that less than five percent of the enlisted men had good feet, and attributed most of the problems to poor shoe fit (including civilian shoes). The toeboxes of the new military-issue shoes were therefore designed to fit mildly deformed rather than underformed feet. The Shoe Board recognized that fit would be imperfect, and recommended breaking in new shoes rapidly by standing in them in three inches of water for ~5 minutes, to soak the leather through, and then walking on a level surface outdoors for ~1 hour, or until the shoes have dried. Failing this, they suggested breaking them in by wearing them for initially short periods, progressively lengthened, to break in the shoe rather than the foot. They also recommended using special shoe stretchers with removable pegs to stretch the toeboxes wider, and stretch bumps over blisters, corns, and bunions.
Ballet.
Ballet pointe shoes have highly specialized toeboxes, as the end of the toeboxes, called the platform, must bear a dancer's entire weight when dancing "en pointe". This is a pressure of about 220 psi or 1.5 MPa. When a dancer leaps and lands "en pointe", the higher transient load, acting on the same area, briefly creates a much higher pressure. The toebox is a rigid socket, built from layers of paper, glue, and fabric (usually burlap), and covered with a satin fabric. They sometimes contain plastic, but this tends to produce a stiff shoe and is not popular. The toe boxes start out too stiff to dance in, and must be broken in; after a certain amount of dancing, depending on technique and conditions, the toeboxes become too soft to support the foot. Reinforcement with fresh glue may postpone the date when the shoes must be replaced.
The toebox must be carefully fitted. The width of the toe box must accord with the dancer's toe shape. When the dancer stand with the feet pointing straight ahead and parallel (sixth position), and bends their knees deeply without raising their heels from the floor (a demi-plié), the feet lengthen; the toes should just touch the platform when in this position. The top of the toebox should be long enough that the throat (edge) falls a bit beyond the far end of the third phalanx, covering it entirely. Dancers often wear specialized padding around and between their toes.
Creasing.
A stiff, multipiece shoe with toe caps, which has been left on the last a long time, will crease less across the toebox. Leather quality has little effect. Using a shoe tree and a shoehorn will reduce creasing. Creasing is a cosmetic concern, but generally does not impair function.


Dostyq (Almaty Metro)

Dostyk () is a planned Line 1 station of Almaty Metro that is currently under construction. It was originally planned to be opened in 2018, however the completion date was moved to 2021 which will be opened near the intersection of Abay Avenue and Momyshuly Street.


William Henry Wilkinson (trade unionist)

William Henry Wilkinson (1850 – 25 April 1906) was a British trade unionist.
Born in Haslingden, Wilkinson became a cotton weaver in 1864. He was a founder member of the Haslingden Weavers' Association, and was appointed as its general secretary in 1879. At the time, the Blackburn Weavers' Association were on strike, opposing wage reductions of 10%. Realising that, if the Blackburn Weavers lost, the cuts would be likely to be applied in Haslingden too, Wilkinson raised large sums - around £140 per week - to support the Blackburn Weavers. Thanks to this, the strike was won, and Wilkinson came to prominence in textile trade unionism.
The secretaryship was a part-time post, and Wilkinson continued to work as a weaver and, occasionally, as an overlooker, until 1880 when he became clerk of the North East Lancashire Amalgamated Weavers' Association. Its secretary, Thomas Birtwistle, founded the broader Northern Counties Amalgamated Association of Weavers, and in 1885, Wilkinson became secretary of this Second Amalgamation.
Wilkinson undertook various other roles, including membership of the executive of the Labour Representation Committee, and serving as secretary of the International Association of Textile Workers. He continued as secretary of the Haslingden Weavers until 1904. His health then worsened, and he stood down from the International Association at its conference in 1906, then took leave of absence from his remaining posts, dying soon after.


Arion (software)

Arion is a physically based, unbiased render engine developed by RandomControl.
Versions.
Arion standalone is a general purpose rendering tool with a visual UI. There are also versions that integrate into 3ds Max and Rhinoceros.


Red Wilson (musician)

Oscar O. "Red" Wilson (February 20, 1920 – June 6, 2005) was an American musician and fiddle-maker who played old-time and bluegrass music in North Carolina. He is also the founder of Mayland Recording Studios.
Biography.
Wilson grew up in Avery County where he learned traditional fiddle and banjo tunes of western North Carolina. In 1941, he was drafted into the army and served in North Africa and Sicily during World War II. He was honored with the Purple Heart by the end of his military service.
In the 1950s, Wilson joined the local band Toe River Valley Boys as a fiddler. The group played at many square dances in Little Switzerland. During his time with the band, Wilson composed tunes that combined traditional elements with more commercial bluegrass elements.
After retiring, Wilson performed at local festivals and music workshops. He was also the operator of the Mayfield Recording Studios in Spruce Pine. He was honored with the North Carolina Heritage Award in 2003 before dying two years later in Bakersville.


4th Combat Engineer Battalion

The 4th Combat Engineer Battalion (4th CEB) is a combat engineer battalion of the United States Marine Corps Reserve. The headquarters is in Baltimore, Maryland and the Battalion has units in West Virginia, Alabama, Virginia, and Tennessee. They belong to the 4th Marine Division of the Marine Forces Reserve.
History.
World War II.
Activated 25 August 1943 at Camp Pendleton, California, as Headquarters Company, 1st Battalion, 20th Marines, 4th Marine Division, Fleet Marine Force. Deployed during February 1944 to the Pacific Theater. Redesignated 31 August, as Headquarters and Service Company, 4th Engineer Battalion, 4th Marine Division. Participated in the Battle of Kwajalein, Battle of Saipan, Battle of Tinian and the Battle of Iwo Jima. Redeployed during October 1945 to Maui, Hawaii. Relocated during November 1945 to Camp Pendleton, California, where it was deactivated on 15 November 1945.
1951–2000.
Reactivated on 1 November 1951 at Baltimore, Maryland, as Headquarters Company, 1st Engineer Battalion. Redesignated 1 July 1962 as 4th Engineer Battalion, 4th Marine Division.
Redesignated 1 June 1976 as 4th Combat Engineer Battalion, 4th Marine Division. Participated in numerous training exercises throughout the 1970s and 1980s. Called to Active Duty December 1990 to participate in the Persian Gulf War. Released from Active Duty May 1991.
Global War on Terror.
In January 2003 the Battalion activated and deployed personnel in support of Operation Iraqi Freedom. December 2004 activated and deployed personnel to serve as members of the 5th Civil Affairs Group and continue to support Operation Iraqi Freedom and Operation Enduring Freedom. 8 members of the battalion were killed supporting operations in Iraq.


Reuben Bosworth

Reuben Bosworth (ca.1797 – 26 July 1883) was a watch and clockmaker in Nottingham.
Life.
He was born around 1797 in Smisby, Derbyshire. He married late in life in 1856 to Sarah.
He was a watchmaker and clockmaker in Nottingham. He was apprenticed John Whitehurst in Derby, and then moved to Nottingham and succeeded William Hall, taking over his duties in regulating and winding the Nottingham Town Hall clock in 1833. In the financial year 1 September 1842 to 1 September 1843 it was reported that he received the annual salary of £18 18s. 0d (equivalent to £ in ) for winding up and regulating the Exchange and Town-hall clocks. In 1842 he was employed by the Leicester corporation to illuminate the Exchange clock at Leicester with a single plate of glass, which would be the largest in the East Midlands.
In the "Nottingham Review" of 15 March 1844, an article appeared praising his work. The Exchange Clock. We beg to draw the attention of our readers to the superior performance of this time keeper. The clock was made by Mr. Reuben Bosworth….and to such great accuracy has Mr. Bosworth regulated its rate of going, that, from the second of November last to the present time [March 1844] a period of four months, it has not varied half a minute.
He made turret clocks, some of which are still found in Nottinghamshire and Derbyshire, wall clocks which he sold to the Midland Railway which were used in railway offices and signal boxes, and longcase clocks and watches.
It is suggested that some of his turret clock business was taken over in 1845 by G. & F. Cope.
He died on 26 July 1883 leaving £7,861 3s 9d. (equivalent to £ in ) to his wife.
Works.
He produced turret clocks for the following buildings:


Maxwell Render

Maxwell Render is an unbiased 3D render engine, developed by Next Limit Technologies in Madrid, Spain. This stand-alone software is used in the film, animation, and VFX industry, as well as in architectural and product design visualization. It offers various plug-ins for 3D/CAD and post production applications.
Overview.
Maxwell Render was released to the public as an early alpha in December 2004 (after two years of internal development) utilizing a global illumination (GI) algorithm based on a metropolis light transport variation. Next Limit Technologies released its latest version of Maxwell Render V4.2 in February 2018.
The physically correct rendering engine was originally used as a tool for animation and visual effects. Maxwell Render's trademark Multilight feature, which permits the changing of light intensities and colors in real time, was used in the feature film "The Curious Case of Benjamin Button".
General features.
Physically-based advantages
Multilight™
FIRE: Fast Interactive Rendering
Materials
Realistic Camera Model
Memory Saving Instances
Accurate 3D Motion Blur
Hair, Grass and Fur
Volumetrics
Particle Rendering
Industry standard support
Network Rendering
Post Production
Interaction with other software.
Maxwell Render for SketchUp is a simplified version of Maxwell Render, fully integrated into the SketchUp software application. Users can set the camera, lighting and environment, apply SketchUp or Maxwell MXM materials, and render and save image files. It is widely used in product design, architectural and engineering visualization.
Plug-ins.
3D application plug-ins
Postproduction application plug-ins
Third party supported plug-ins


CESMM3

The Civil Engineering Standard Method of Measurement (commonly known as CESMM3) sets out a procedure for the preparation of a bill of quantities for civil engineering works, for pricing and for expression and measurement of quantities of work.
CESMM3 includes 26 main clauses of work:


Non-circular gear

A non-circular gear (NCG) is a special gear design with special characteristics and purpose. While a regular gear is optimized to transmit torque to another engaged member with minimum noise and wear and with maximum efficiency, a non-circular gear's main objective might be ratio variations, axle displacement oscillations and more. Common applications include textile machines, potentiometers, CVTs (continuously variable transmissions), window shade panel drives, mechanical presses and high torque hydraulic engines.
A regular gear pair can be represented as two circles rolling together without slip. In the case of non-circular gears, those circles are replaced with anything different from a circle. For this reason NCGs in most cases are not round, but round NCGs looking like regular gears are also possible (small ratio variations result from meshing area modifications).
Generally NCG should meet all the requirements of regular gearing, but in some cases, for example variable axle distance, could prove impossible to support and such gears require very tight manufacturing tolerances and assembling problems arise. Because of complicated geometry, NCGs are most likely spur gears and molding or electrical discharge machining technology is used instead of generation.
Mathematical description.
Ignoring the gear teeth for the moment (i.e. assuming the gear teeth are very small), let formula_1 be the radius of the first gear wheel as a function of angle from the axis of rotation formula_2, and let formula_3 be the radius of the second gear wheel as a function of angle from its axis of rotation formula_4. If the axles remain fixed, the distance between the axles is also fixed:
Assuming that the point of contact lies on the line connecting the axles, in order for the gears to touch without slipping, the velocity of each wheel must be equal at the point of contact and perpendicular to the line connecting the axles, which implies that:
Each wheel must be cyclic in its angular coordinates. If the shape of the first wheel is known, the shape of the second can often be found using the above equations. If the relationship between the angles is specified, the shapes of both wheels can often be determined analytically as well.
It is more convenient to use the circular variable formula_7 when analyzing this problem. Assuming the radius of the first gear wheel is known as a function of "z", and using the relationship formula_8, the above two equations can be combined to yield the differential equation:
where formula_10 and formula_11 describe the rotation of the first and second gears respectively. This equation can be formally solved as:
where formula_13 is a constant of integration.


Wilkanowski

Władysław William "Willy" Wilkanowski (November 15, 1886 in Działyń, Poland – December 8, 1954, Long Island, USA) was a Polish-American violin-maker, guitar-maker and violinist. He was a very productive luthier, known for making over 5000 violins and 100 violas with his staff at his workshop. He also created 30 unique, high-end archtop guitars, one of which, the Wilkanowski Airway W-4, was famously owned by Johnny Cash since the 1980s, when it also was featured as the centerfold in the Guitar World magazine.
Wilkanowski was also known to be a family man, doting on his wife Amelia (1886 – May 6, 1952), with whom he had raised 9 surviving children. When Amelia got sick, in 1950 he moved his workshop to their Long Island home to be close to her and look after her. After she died of the illness in 1952, he became very depressed and despondent without her. William stopped making instruments altogether and lost his source of income, which negatively affected his finances, adding to his depressive state. In early December 1954, he finally committed suicide and was laid to rest next to Amelia on December 13, 1954.
Early life.
Wilkanowski was born on November 15, 1886 as listed on his grave and on his draft card, and the year 1886 indicated as estimated in several census records of New York. His obituary states his age to be 69 in December 1954, which would then indicate the birth year as 1885. The draft card of 1942 reveals his birth place to be Działyń, but it is unclear, which of the 4 places of this name in Poland it could have been.
According to Fairfield's book, William built his first violin already at age 9 (in 1895), which would indicate that he came from a luthier or a musical family. In 1903, by the age of 17, he was a trained violin maker.
As many Poles of the time would leave the poverty and the Russian and German nationalist oppression of partitioned Poland, he joined his family in the United States. The year 1904, when he would be 17–18 years old, is listed as year of his immigration in the 1920 New York census, where his name is misspelled William Wikanoski and mistranscribed as Wikanski.

As countless Poles would do to assimilate in the United States, he changed his Polish first name Wladyslaw to the English name with the same initial, William, which would not be given as a child name in Poland, unless as the German form Wilhelm in the German speaking partitions of Poland. In the New York census records, there are several people listed with the last name Wilkanowski. At least one male relative of Wilkanowski already resided in New York – the father of his cousin Maximilian, born in New York. In 1905, William and his wife Amelia had their daughter Helen; several children followed, listed as 7 children, all born in New York and speaking Polish and English, as listed in the census of 1920.
Initially, William worked in the shop of Oliver Ditson of Boston. In the 1930s, he worked for Fred Gretsch (New York City), out of his own workshop and store in 58 Nassau Street, Brooklyn, New York. William was also a violinist himself and was a member of a polka band in the 1920s.
Career in the United States.
He was listed as a violin maker in Brooklyn by 1933, and at least one violin made in Brooklyn dates to 1924. From 1937 to 1941, he worked in both an era and a location renowned for the jazz guitar. Gretsch offered Wilkanowski's violins in a 1940 flyer with the text "his own personal work…no other hand touches them." His violins were offered from $50–150.
Wilkanowski is thought to have produced 5,000 violins and 100 violas by 1942. Some of the higher quality violins were marked with an inlayed logo of the stylized letter "W"; these instruments are thought to be entirely of his own making, while many of the others were made in the shops with assistants. The Gretsch Company released the Synchromatic line during the early '40s also, which were also archtop guitars, but shared no other similarities with Wilkanowski guitars. His role in the Synchromatic is not known.
Although known for his violins, Wilkanowski also produced a limited number of archtop guitars. The guitars were never catalogued. By 1942 he had sold 30 of these instruments, each unique in appointments and features, at $400 each, except for two deluxe Airway guitars, sold for $600. This price was in line with what was being charged for a D’Angelico New Yorker, or a Gibson Guitar Corporation Super 400. There is no evidence of guitars made by Wilkanowski after 1943, instead he continued making and successfully selling violins until 1952.
Features of his guitars.
Most of the Wilkanowski guitars would look not like regular jazz guitars, but very much like oversized and slightly squished violins or small cellos with an added guitar neck. Some of his guitars did not have the cello shape, but rather a more conventional archtop shape, without the cello-like points above the waist. The Wilkanowski headstock is thought to have been the main influence in the headstock for the current Ovation Guitar. Many of his guitars have the unique flattened oval Wilkanowski headstock, although some featured a violin like scroll of aluminium, and some of his headstocks would just be like conventional guitar headstock. The backs of most of his guitars were one piece of flamed maple, with no center joint. The wood William used would often be the Po Valley Poplar, a figured cello tonewood that can resemble maple. The finishing techniques included very light stain, or a violin color finish, and light sealer. The multiple layer binding was wooden, something fairly innovative at the time, and was raised above the level of the top and back plates. The f holes varied by instrument, standard shape, segmented, and later more modern cutouts appeared. Some of the Instruments displayed the name AIRWAY, some had a W on the headstock, and some remained unbranded. Some of the guitars carry serial numbers, a signature, or a label. Several of the guitars are labeled Wilkanowski and Son, although nothing is known of the son's responsibility. One of these guitars, the Airway W-4 model with abalone shell inlayed rim around the entire body front and abalone ornaments on the neck, was given as a gift to Johnny Cash by his wife June in the 1980s. Johnny kept this guitar until his death, and the instrument was subsequently sold at the Johnny Cash estate auction by Sotheby's in 2004, for 30,000 dollars, to appear again on auctions later.
Personal life, family and death.
Researching Wilkanowski's registered family data, it must be noted, that nearly all records until his death in 1954 were filled in cursive handwriting with ink pens by English speaking clerks. These handwritten records are full of spelling mistakes and very vague age and event estimates. None of the census records, marriage certs etc. provide exact dates of birth for any of the family members, typically only registering a loose estimate of age at the time of the census and a variety of misspelled Polish names. This makes exact date estimation of many life events for Wilkanowski quite difficult.
William married a fellow Polish immigrant, Michalina Amelia, who came to New York in about 1901. Their wedding photo was provided by family to the biography article. Their marriage was registered twice in May and June of the year 1911, but according to later census records, the couple already had children from around the year 1904. This would mean that Wilkanowski and Amelia either had their first children out of wedlock, or got married any time around 1904, perhaps only registering in a church, as many Catholic Poles would view a church wedding as sufficient for their daily life. She would go by the name Amelia, also registered as Emily or as Emilia (1930 Census). Her maiden name was also listed and misspelled as Glowinska, Growdanska and Grobinska. in New York. Together they seem to have registered 11 children in total, 8 daughters and 3 sons. 9 of their children would survive them – the 7 daughters Helene, Genowefa/Genevieve (1907–1977), Carolyne, Florence, Irene, Viola and Natalie (1924–2009), and the 2 sons Henry (1922–1965) and Theodore Joseph (1919–1969). In the 1940 New York census, Amelia is listed as Emily and 53 years old, 1 year older than William listed as "Wm", 52 years old. Five of their youngest children – the 3 girls and 2 sons – are listed living with the parents in the same 1940 census, which indicates their 5 oldest daughters already moved out and married. The name Joseph seems to have been significant to Wilkanowski, who would also label some of his violins with the name "Juzek", which is the slightly misspelled Polish diminutive of Joseph.
The Wilkanowski couple had a daughter, Isabella (1912–1945, married Reges), who worked as a waitress and unfortunately died by accident in Sept. 1945, aged 32. William provided herthe cause of death as carbon monoxide poisoning. In the 1920 census, a 15-year-old boy named Benjamin was listed as the oldest son of the family "Wilkanoski", with little Theodore being 8 months old. This Benjamin is missing from all later census records and documents.
In the 1940s, both of Wilkanowski's sons were drafted for the World War II, and William himself was also registered for draft.
Henry was registered in 1942 and started service in 1943 with his infantry battalion, which earned him a military grave at the Long Island National cemetery. On his draft card, Henry listed his father William as his employer and Edward Wilkanowski as a relative to contact.

Theodore was drafted in 1940 in the Young Man Draft and he listed his father as contact and his employer as Wilkanowski + Son (which was the label on the archtop guitars). Theodore later became a corporal in WWII.

William's own registration card from April 1942 has a small but detailed description of him, providing the date and place of his birth, misspelled as the non-existing place "Dziatyn" (as the Polish small letter ł looks very much like the Latin t), his age as 56 which was then crossed over and corrected to the factual 55, as he had his birthday in November; his height as 5'4, his weight as 155 pounds, his eye color as brown, hair as gray and complexion as ruddy. In the occupation field, William did not disclose himself as a luthier, but as self employed. Like Henry, William also listed the Edward Wilkanowski of Russau Street in Brooklyn as a contact. This Edward was most likely the brother of Maximilian J. Wilkanowski, who worked in William's violin shop.
The obituary in The Brooklyn Eagle of Saturday, December 11, 1954 describes in detail the death of William as suicide by hanging and that his body was found Wednesday December 8 in his home by Henry, who stopped by to pick his father up for a family dinner. William was interred on Monday December 13, 1954 in the Cemetery of the Holy Rood in Westbury, Nassau County NY, next to his wife.
After his death, a number of unfinished and dusty violins were found in his home. It seems as some of them were then finished by his coworkers or family members, as some Wilkanowski violins have labels dated later than 1952.