36 Capricorni

36 Capricorni is a single, yellow-hued star in the southern constellation of Capricornus. It is visible to the naked eye with an apparent visual magnitude of +4.50. The distance to this star, as determined from an annual parallax shift of , is around 171 light years. It is currently moving closer with a heliocentric radial velocity of −21 km/s, and will come within in about 685,000 years ago.
This is an evolved G-type giant star with a stellar classification of G7IIIb Fe–1, where the suffix notation indicates an underabundance of iron found in the spectrum. At the age of 2.4 billion years it has become a red clump giant, meaning it is generating energy through helium fusion at its core. It has an estimated 1.94 times the mass of the Sun and is radiating 44.7 times the Sun's luminosity from its photosphere at an effective temperature of 5,017 K.
Chinese Name.
In Chinese, (), meaning "Twelve States", refers to an asterism which is represent twelve ancient states in the Spring and Autumn period and the Warring States period, consisting of 36 Capricorni, φ Capricorni, ι Capricorni, 37 Capricorni, 35 Capricorni, χ Capricorni, θ Capricorni, 30 Capricorni, 33 Capricorni, ζ Capricorni, 19 Capricorni, 26 Capricorni, 27 Capricorni, 20 Capricorni, η Capricorni and 21 Capricorni. Consequently, 36 Capricorni itself is represent the state Jin ()(or Tsin), together with κ Herculis in "Right Wall of Heavenly Market Enclosure" (asterism)


Calabash Nebula

The Calabash Nebula, also known as the Rotten Egg Nebula or by its technical name OH 231.84 +4.22, is a protoplanetary nebula (PPN) 1.4 light years (13 Pm) long and located some 5,000 light years (47 Em) from Earth in the constellation Puppis. The name "Calabash Nebula" was first proposed in 1989 in an early paper on the expected nebular dynamics, based on the nebula's appearance
The Calabash is an almost certain member of the open cluster Messier 46, as it has the same distance, radial velocity, and proper motion.
Description.
Violent gas collisions that produced supersonic shock fronts in a dying star are seen in a detailed image from NASA's Hubble Space Telescope.
The object is sometimes called the Rotten Egg Nebula as it contains a relatively large amount of sulphur. The densest parts of the nebula are composed of material ejected recently by the central star and accelerated in opposite directions. This material, shown as yellow in the image, is zooming away at speeds up to one and a half million kilometers per hour (one million miles per hour). Most of the star's original mass is now contained in these bipolar gas structures.
A team of Spanish and US astronomers used NASA's Hubble Space Telescope to study how the gas stream rams into the surrounding material, shown in blue. They believe that such interactions dominate the formation process in planetary nebulae. Due to the high speed of the gas, shock-fronts are formed on impact and heat the surrounding gases. Although computer calculations had predicted the existence and structure of such shocks for some time, previous observations had not been able to prove the theory.
This new Hubble image used filters that only let through light from ionized hydrogen and nitrogen atoms. Astronomers were able to distinguish the warmest parts of the gas heated by the violent shocks and found that they form a complex double-bubble shape. The bright yellow-orange colors in the picture show how dense, high-speed gas is flowing from the star, like supersonic speeding bullets ripping through a medium in opposite directions. The central star itself is hidden in the dusty band at the center.
Much of the gas flow observed today seems to stem from a sudden acceleration that took place about 800 years ago. Astronomers believe that 1,000 years from now, the Calabash Nebula will become a fully developed planetary nebula.
Ground-based imagery.
In wide field images, the Calabash nebula is visible near the bright planetary nebula NGC 2438 in deep photographs. Although the Calabash Nebula is at the same distance as M46, NGC 2438 is a larger object in the foreground.


Nu Leonis

ν Leonis, Latinised as Nu Leonis, is a binary star system in the zodiac constellation of Leo. It is faintly visible to the naked eye with an apparent visual magnitude of 5.15; parallax measurements indicate it is around 500 light years away. At this distance, the visual extinction from interstellar dust is 0.33 magnitudes.
It is 0.05 degree north of the ecliptic, so it can be occulted by the moon or planets.
This is a single-lined spectroscopic binary system with an orbital period of 137.3 days and an eccentricity of 0.7. The primary component is a B-type subgiant star with a stellar classification of B6 IV. It has about 3.37 times the mass of the Sun, 2.3 times the Sun's radius, and radiates 244 times the luminosity of the Sun from an outer atmosphere with an effective temperature of 9,552 K. The rotation rate is moderate with a projected rotational velocity of 100 km/s. Little is known about the companion.


Nu Ursae Majoris

Nu Ursae Majoris (ν Ursae Majoris, abbreviated Nu UMa, ν UMa), formally named Alula Borealis , is a double star in the northern circumpolar constellation of Ursa Major. At an apparent visual magnitude of +3.490, it is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to ν Ursae Majoris is about .
This is a giant star with a stellar classification of K3 III. It has expanded to about 57 times the radius of the Sun and is radiating 775 times the Sun's luminosity. The effective temperature of the outer envelope is 4,070 K; cool enough to give it an orange hue typical of a K-type star. It has a 10th-magnitude optical companion at an angular separation of 7.1 arcseconds.
Nomenclature.
"ν Ursae Majoris" (Latinised to "Nu Ursae Majoris") is the star's Bayer designation.
It also bore the traditional name of "Alula Borealis". "Alula" (shared with Xi Ursae Majoris) comes from the Arabic phrase 'the First Spring'. and "Borealis" is Latin for 'northern'. 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 "Alula Borealis" for this star.
In Chinese, (), meaning "Three Steps", refers to an asterism consisting of Nu Ursae Majoris, Iota Ursae Majoris, Kappa Ursae Majoris, Lambda Ursae Majoris, Mu Ursae Majoris, and Xi Ursae Majoris. Consequently, the Chinese name for Nu Ursae Majoris itself is (, ).


NGC 6509

NGC 6509 is a galaxy in the New General Catalogue. It is located in the constellation Ophiuchus. It is a Sc type spiral galaxy.


23 Vulpeculae

23 Vulpeculae is a triple star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.52 and it is located approximately 327 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +1.47 km/s.
Component A forms a binary system with an orbital period of 25.33 years, an eccentricity of 0.40, and a semimajor axis of . The 4.80 magnitude member of this pair, component Aa is an aging giant star with a stellar classification of , where the suffix indicates an underabundance of iron in the spectrum. This star has 2.4 times the mass of the Sun and is radiating 146 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,429 K. Its companion, component Ab, has magnitude 6.5. The tertiary member, component B, has a separation of 0.26" and a magnitude of 6.94.


Omicron Canis Majoris

The Bayer designation Omicron Canis Majoris (ο CMa / ο Canis Majoris) is shared by two stars, in the constellation Canis Major:
They are separated by 2.06° on the sky.
ο¹ Canis Majoris was member of asterism 軍市 (Jūn Shì), "Market for Soldiers", "Well" mansion. ο² Canis Majoris was not any member of asterism.


Gliese 638

Gliese 638 is a main sequence star in the constellation of Hercules. It is located about 31.9 light years from the Earth. This is a suspected variable star with a measured apparent magnitude that ranges from 8.09–8.11. As a K-class star, it has a lower mass than the Sun, and consequently is less luminous.


RZ Pyxidis

RZ Pyxidis is eclipsing binary system in the constellation Pyxis, made up of two young stars less than 200,000 years old. Both are hot blue-white stars of spectral type B7V and are around 2.5 times the size of the Sun. One is around five times as luminous as the sun and the other around four times as luminous. The system is classified as a Beta Lyrae variable, he apparent magnitude ranging from 8.83 to 9.72 over 0.66 days.


Gamma Equulei

Gamma Equulei, Latinized from γ Equulei, is a double star in the northern constellation of Equuleus. It is located at a distance of around from Earth and is visible to the naked eye with a slightly variable apparent visual magnitude of around 4.7. The star is drifting closer to the Sun with a radial velocity of −16.5 km/s.
Properties.
The primary component of γ Equulei is a chemically peculiar star with a stellar classification of . It has a spectrum corresponding to an A9 main sequence star, but with unusual abundances of strontium, chromium, and europium. Stars with this type of spectral peculiarity are called Ap stars. The abundances of some metals are believed to be due to chemical stratification in the slowly-rotating star, unusual for hot main sequence stars. A fairly wide range of spectral types have been published for γ Equulei, ranging from A5 to F1, some of them also indicating unusual abundances of iron in the spectrum. γ Equulei has particularly sharp absorption lines in its spectrum, a sign of very slow rotation.
γ Equulei undergoes rapid periodic variations in brightness, which places it among the rapidly oscillating Ap (roAp) stars. The apparent magnitude varies between extremes of +4.58 and +4.77. It shows pulsations in several periods near 12 minutes. The strongest pulsation is at 11.7 minutes; others are found at 11.9, 12.2, and 12.4 minutes. These are identified as a series of even and odd p-mode (pressure-induced) pulsations.
The surface magnetic field of γ Equulei undergoes slow variation, ranging from +577 G to –1,101 G. Although only 67 years of magnetic field measurements are available, a period of has been fit to the data. This is thought to be the rotation period of γ Equulei.
γ Equulei has a magnitude 8.69 companion at an angular separation of 1.26 arcseconds.


Kepler-63

Kepler-63 is a G-type main-sequence star about 638 light-years away. The star is much younger than the Sun, at . Kepler-63 is similar to the Sun in its concentration of heavy elements.
The star is exhibiting strong starspot activity, with relatively cold (4700 K) starspots concentrated in two mid-latitude bands similar to the Sun, changing their position in a cycle with a period of 1.27 years. Due to high magnetic activity associated with its young age, Kepler-63 has a very hot corona heated to 8 million degrees, and produces over ten times the solar amount of x-rays than the Sun.
Multiplicity surveys did not detect any stellar companions to Kepler-63 by 2016.
Planetary system.
In 2013 a transiting hot Jupiter planet b was detected on a tight orbit. The orbit is nearly polar to the equatorial plane of the star.


Psi Eridani

Psi Eridani, Latinized from ψ Eridani, is a star in the constellation Eridanus. With an apparent visual magnitude is 4.81, it can be seen with the naked eye on a clear, dark night. Based upon an annual parallax shift of 4.41 milliarcseconds, it is located roughly 740 light years away from the Sun.
This is a B-type main sequence star with a stellar classification of B3 V. However, Houk and Swift (1999) classed it as a more evolved subgiant star. It is about 32 million years old and has a projected rotational velocity of 52 km/s. The estimated mass is seven times that of the Sun, and it has around 4.5 times the Sun's radius. Psi Eridani shines with 2,878 times the solar luminosity from its outer atmosphere at an effective temperature of 18,700 K.


Pi Ursae Majoris

The Bayer designation Pi Ursae Majoris (π UMa, π Ursae Majoris) is shared by two stars in the constellation Ursa Major:
They are separated by 0.70° in the sky. They are sometimes given the name Muscida, which can also refer to ο Ursae Majoris.
The two stars, Pi¹ and Pi² together, are considered an optical double star. They are not a binary star, in that they are not gravitationally linked, but they are close to each other as seen in the sky, and so are optically associated.


NGC 375

NGC 375 is an elliptical galaxy located in the constellation Pisces. It was discovered on September 12, 1784 by William Herschel. It was described by Dreyer as "pretty faint, small, round, brighter middle." Along with galaxies NGC 379, NGC 380, NGC 382, NGC 383, NGC 384, NGC 385, NGC 386, NGC 387 and NGC 388, NGC 375 forms a galaxy cluster called Arp 331.


HD 79498

HD 79498 is a primary of the star system located approximately 160 light years away in the constellation Cancer. This G5 spectral class star has an apparent magnitude of 8.03 and is about the same size and mass as the Sun. It has a higher than solar abundance of elements other than hydrogen and helium; what astronomers term a metal-rich star.
The secondary star of the star system is the BD+23 2063 B located on the projected separation of the 2900 AU from the primary. It is a red dwarf of spectral class M0.
Planetary system.
The McDonald Observatory planet search program discovered planet orbiting primary in 2011 using radial velocity method.


70 Ophiuchi

70 Ophiuchi is a binary star system located 16.6 light years away from the Earth. It is in the constellation Ophiuchus. At magnitude 4 it appears as a dim star visible to the unaided eye away from city lights.
History.
This star system was first catalogued as a binary star by William Herschel in the late 18th century in his study of binary stars. Herschel proved that this system is a gravitationally bound binary system where the two stars orbit around a common center of mass. This was an important contribution to the proof that Newton's law of universal gravitation applied to objects beyond the solar system. He commented at the time that there was a possible third "unseen companion" affecting the orbit of the two visible stars.
Variability.
70 Ophiuchi is a variable star with a magnitude range for the two stars combined of 4.00 to 4.03. The type of variability is uncertain and it is not clear which of the two components causes the variations. It has been suspected of being either a BY Draconis variable or an RS Canum Venaticorum variable, and a period of 1.92396 days has been measured.
Binary star.
The primary star is a yellow-orange main sequence dwarf of spectral type K0, while the secondary is an orange dwarf of spectral type K4. The two stars orbit each other at an average distance of 23.2 AU. But since the orbit is highly elliptical (at "e"=0.499), the separation between the two varies from 11.4 to 34.8 AU, with one orbit taking 88.38 years to complete.
Claims of a planetary system.
In 1855, William Stephen Jacob of the Madras Observatory claimed that the orbit of the binary showed an anomaly, and it was "highly probable" that there was a "planetary body in connection with this system". This is the first known attempt to use astrometric methods to detect an exoplanet, although Friedrich Bessel had applied similar methods 10 years earlier to deduce the existence of Sirius B.
T. J. J. See made a stronger claim for the existence of a dark companion in this system in 1899, but Forest Ray Moulton soon published a paper proving that a three-body system with the specified orbital parameters would be highly unstable. The claims by Jacob and See have both been shown to be erroneous.
Discovery of a "third dark companion" was announced by Louis Berman in 1932. This "dark body" around 70 Oph A was thought to have an 18-year period and a mass of 0.1 to 0.2 the Sun's mass. A claim of a planetary system was again made, this time by Dirk Reuyl and Erik Holberg in 1943. The companion was estimated to have a mass 0.008 to 0.012 that of the Sun and a 17-year period. This caused quite a sensation at the time but later observations have gradually discredited this claim.
The negative results of past studies does not completely rule out the possibility of planets. In 2006 a McDonald Observatory team set limits to the presence of one or more planets around 70 Ophiuchi with masses between 0.46 and 12.8 Jupiter masses and average separations spanning between 0.05 and 5.2 AU.


HD 205765

HD 205765 is a star in the equatorial constellation of Aquarius. It is an A-type main sequence star with an apparent magnitude of 6.2, which, according to the Bortle scale, makes it faintly visible to the naked eye from dark rural skies. This star is spinning rapidly with a projected rotational velocity of 172 km/s.


Dipper (Chinese constellation)

The Dipper mansion (斗宿, pinyin: Dǒu Xiù) is one of the Twenty-eight mansions of the Chinese constellations. It is one of the northern mansions of the Black Tortoise. In Taoism, it is known as the "Six Stars of the Southern Dipper" (南斗六星, Nándǒu liù xīng), in contrast to the Big Dipper north to this mansion.


NGC 7457

NGC 7457 is an unbarred lenticular galaxy in the constellation Pegasus. NGC 7457 is its New General Catalogue designation. It was discovered by the astronomer William Herschel on 12 September 1784.
NGC 7457 is estimated to be about 43 million light-years (13.2 megaparsecs) away from the Sun. There are about 201 globular clusters in the galaxy. The core of NGC 7457 is surprisingly bright and compact, with many stars.


Alnilam

Alnilam , designation ε Orionis, (Latinized to Epsilon Orionis, abbreviated Epsilon Ori, ε Ori) and 46 Orionis (46 Ori), is a large blue supergiant star some 2,000 light-years distant in the constellation of Orion. It is estimated to be 275,000 to 832,000 times as luminous as the Sun, and 30–64.5 times as massive.
Observation.
It is the 29th-brightest star in the sky (the 4th-brightest in Orion) and is a blue supergiant. Together with Mintaka and Alnitak, the three stars make up Orion's belt, known by many names across many ancient cultures. Alnilam is the middle star. It is slightly variable, from magnitude 1.64 to 1.74. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It is also one of the 58 stars used in celestial navigation. It is at its highest point in the sky around midnight on December 15.
Physical characteristics.
Estimates of Alnilam's properties vary. Crowther and colleagues, using stellar wind and atmospheric modelling in 2006, came up with a luminosity 275,000 times that of the Sun (), and effective temperature of 27,000 K and a radius 24 times that of the Sun (). Searle and colleagues, using CMFGEN code to analyse the spectrum in 2008, calculated a luminosity of , an effective temperature of 27,500 ± 100 K and a radius of . Analysis of the spectra and age of the members of the Orion OB1 association yields a mass 34.6 times that of the Sun ( on the main sequence) and an age of 5.7 million years.
A more recent detailed analysis of Alnilam across multiple wavelength bands produced very high luminosity, radius, and mass estimates, assuming the distance of 606 parsecs suggested by the Hipparcos new reduction. Adopting the larger parallax from the original Hipparcos reduction gives a distance of 412 parsecs and physical parameters more consistent with earlier publications. The luminosity of at 606 parsecs is the highest ever derived for this star.
Alnilam's relatively simple spectrum has made it useful for studying the interstellar medium. Within the next million years, this star may turn into a red supergiant and explode as a supernova. It is surrounded by a molecular cloud, NGC 1990, which it illuminates to make a reflection nebula. Its stellar winds may reach up to 2000 km/s, causing it to lose mass about 20 million times more rapidly than the Sun.
Nomenclature and history.
"ε Orionis" is the star's Bayer designation and "46 Orionis" its Flamsteed designation.
The traditional name "Alnilam" derives from the Arabic النظام "al-niẓām" 'arrangement/string (of pearls)'. Related spellings are "Alnihan" and "Alnitam": all three variants are evidently mistakes in transliteration or copy errors, the first perhaps due to confusion with النيلم "al-nilam" 'sapphire'. 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 "Alnilam" for this star. It is now so entered in the IAU Catalog of Star Names.
Orion's Belt.
The three belt stars were collectively known by many names in many cultures. Arabic terms include "Al Nijād" 'the Belt', "Al Nasak" 'the Line', "Al Alkāt" 'the Golden Grains or Nuts', and, in modern Arabic, "Al Mīzān al H•akk" 'the Accurate Scale Beam'. In Chinese mythology, they were also known as The Weighing Beam.
In Chinese, (), meaning "Three Stars (asterism)", refers to an asterism consisting of Alnilam, Alnitak, and Mintaka (Orion's Belt), with Betelgeuse, Bellatrix, Saiph, and Rigel later added. Consequently, the Chinese name for Alnilam is (, ). It is one of the western mansions of the White Tiger.


HD 202628

HD 202628 is a single star in the southern constellation of Microscopium. It has an apparent visual magnitude of +6.7, which makes it too faint to be readily visible to the naked eye. The star is located at a distance of 77.7 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12.1 km/s. The absolute magnitude of this star is 4.86.
The stellar classification of HD 202628 is G1.5V, matching a yellow-hued G-type main-sequence star similar to the Sun. The chromospheric activity level and amount of X-ray emission is consistent with a star that is younger that the Sun. It is spinning with a projected rotational velocity of 2.6 km/s. The star has 107% of the mass of the Sun and 95% of the Sun's radius. The metallicity, or abundance of heavier elements, appears to be about the same as in the Sun. It is radiating 95% of the luminosity of the Sun from its photosphere at an effective temperature of 5,843 K.
In 2010, an infrared excess from a circumstellar disk of dust was detected around this star by the Spitzer Space Telescope. The net emission at 70 microns (70 μm) is almost 20 times as high as the star's flux at this wavelength. The disk has been directly imaged by the Hubble Space Telescope. It is oval-shaped with an orbital eccentricity of 0.18, and is inclined at 64° to the line of sight from the Earth. The inner edge of the ring, which lies at around 158 AU from the star, is sharply defined. This suggests that there is an exoplanet responsible for this defined edge, and it has been calculated as orbiting between 86 and 158 AU from HD 202628.


Mu Centauri

Mu Centauri, Latinized from μ Centauri, is a third-magnitude star in the southern constellation of Centaurus. With the stars ν and φ Centauri, it marks what has been traditionally portrayed as "dextro Latere" (the right side) of the Centaur. The apparent visual magnitude of this star is 3.42, making it one of the brighter members of the constellation. The distance to this star can be estimated directly using parallax measurements, which yield a value of roughly 510 light years (155 parsecs) from Earth.
The spectrum of Mu Centauri matches a stellar classification of B2 IV-Ve. The 'e' suffix is used to mark the presence of emission lines, which indicates this is a Be star surrounded by a circumstellar disk of hot gas that was formed from material ejected from the star. Mu Centauri is a pulsating variable star that has multiple non-radial cycles with a primary period of 0.503 days. Three other pulsation cycles have a similar period, while two have a shorter interval of about 0.28 days. It undergoes outburst events that result in the transfer of additional material to the surrounding disk. During these outbursts, the star can experience transient periodicities. Mu Centauri is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +2.75 to +3.25.
This star is spinning rapidly, with a projected rotational velocity of 194, km s−1 and is completing a full rotation in about 11.615 hours. The equatorial azimuthal velocity is around 85% of the critical velocity where the star would start to break up, resulting a pronounced equatorial bulge that is about 26% wider than the radius at the poles. Because of the oblate spheroidal shape of this star, the polar region is at a higher temperature than the equator—23,000 K versus 17,600 K respectively. Likewise, the gravitational force at the poles is greater than along the equator. The axis of rotation of the star is tilted by an angle of about (19 ± 3)° to the line of sight from the Earth.
At an estimated age of nearly 20 million years, this star is around 55–65% of the way through its evolutionary period on the main sequence of core hydrogen burning stars. It has around nine times the mass of the Sun and four times the Sun's radius, but emits over 2,000 times as much energy as the Sun. The outer atmosphere has a mean effective temperature of 22,410 K, giving the star a blue-white hue.
This star is a proper motion member of the Upper-Centaurus Lupus sub-group in the
Scorpius-Centaurus OB association,
the nearest such co-moving association of massive stars to the Sun.


Zeta Draconis

Zeta Draconis (ζ Draconis, abbreviated Zet Dra, ζ Dra) is a binary star in the northern circumpolar constellation of Draco. With an apparent visual magnitude of +3.17, it is the fifth-brightest member of this generally faint constellation. Its distance from the Sun has been measured using the parallax technique, yielding an estimate of roughly .
The two components are designated Zeta Draconis A (formally named Aldhibah , after the traditional name of the system) and B.
Nomenclature.
"ζ Draconis" (Latinised to "Zeta Draconis") is the system's Bayer designation. The designations of the two components as "Zeta Draconis A" and "B" derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
Zeta Draconis has the old Arabic name الذئب "al-dhiʼb" "the wolf", given in its feminine form "Al Dhiʼbah" (ذئبة) in Allen (1899) (though he mistranslated it as plural "hyenas", which would be الضباع "al-ḍibāʽ"). It shares the dual form of the name, الذئبين "al-dhiʼbayn", with Eta Draconis. It is also known as "Nodus III" (Third Knot, the knot being a loop in the tail of Draco).
In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Aldhibah" for the component Zeta Draconis A on 5 September 2017. It also approved the name "Athebyne" for Eta Draconis A on the same date. Both are now so included in the List of IAU-approved Star Names.
Zeta Draconis is mentioned in Hindu mythology as "Tara" who was a celestial goddess married to Lord Brhaspati. A divine epic was played out in the night sky when Lord Chandra, the moon, lusted after and abducted Tara, the blue pole star of Brhaspati, the planet Jupiter. By the completion of the epic Tara gives birth to Lord Budha, or Mercury.
In Chinese, (), meaning "Left Wall of Purple Forbidden Enclosure", refers to an asterism consisting of Zeta Draconis, Iota Draconis, Eta Draconis, Theta Draconis, Upsilon Draconis, 73 Draconis, Gamma Cephei and 23 Cassiopeiae. Consequently, the Chinese name for Zeta Draconis itself is (, ), representing (), meaning "The First Minister". 上弼 (Shǎngbì) is westernized into "Shang Pih" by R.H. Allen with meaning "the Higher Minister".
Properties.
Zeta Draconis A is a giant star with a stellar classification of B6 III. Compared to the Sun, this star is about 2.5 times larger, 3.5 times more massive, and is radiating 148 times as much luminosity. This energy is being emitted from the star's outer envelope at an effective temperature of nearly 13,400 K. The azimuthal rotation velocity along the equator is at least 55 km/s.
The north ecliptic pole is located at right ascension 18h and declination +66.5°. This is located roughly midway between Delta Draconis and Zeta Draconis. The north ecliptic pole almost coincides with the south celestial pole of Venus; Zeta Draconis is also the north pole star of Jupiter.


Xi Draconis

Xi Draconis (ξ Draconis, abbreviated Xi Dra, ξ Dra) is a double or binary star in the northern circumpolar constellation of Draco. It has an apparent visual magnitude of 3.75. Based upon parallax measurements, it is located at a distance of from the Sun. At this distance, the apparent magnitude is diminished by 0.03 from extinction caused by intervening gas and dust.
The two components are designated Xi Draconis A (officially named Grumium , a traditional name for the system) and B.
Nomenclature.
"ξ Draconis" (Latinised to "Xi Draconis") is the system's Bayer designation. The designations of the two components as "Xi 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 names "Grumium". This is a graphic corruption of the Latin "Grunnum" 'snout', as Ptolemy had described this star as being on the jawbone of the dragon. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Grumium" for the component Xi Draconis A on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.
This star was also known as "Nodus I" or "Nodus Primus". Along with Beta Draconis (Rastaban), Gamma Draconis (Eltanin), Mu Draconis (Erakis) and Nu Draconis (Kuma), it was one of "Al ʽAwāyd" "the Mother Camels", which were later known as the "Quinque Dromedarii".
In Chinese, (), meaning "Celestial Flail", refers to an asterism consisting of Xi Draconis, Nu Draconis, Beta Draconis, Gamma Draconis and Iota Herculis. Consequently, the Chinese name for Xi Draconis itself is (, ).
Namesake.
USS Grumium (AK-112) was a United States Navy Crater class cargo ship named after the star.
Properties.
Xi Draconis A is of spectral class K2-III. The possible companion, Xi Draconis B, is a 16th magnitude star 316 arcseconds away but, most likely, the pairing is just a line-of-sight coincidence.


Sh2-2

Sh 2-2, also known as Sharpless 2, is an emission nebula in the constellation of Scorpius. It appears as a mid-range brightness making it difficult to view. It is believed to currently host an X-ray binary star that originated and was ejected from the Scorpius OB1 association.
The nebulous area is fairly large with an irregular shape appearing as a H II region. The remnant has an apparent diameter that covers approximately 60'.


24 Vulpeculae

24 Vulpeculae is a single, yellow-hued star in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.30. The distance to this star can be estimated from its annual parallax shift of , which yields a separation of roughly 409 light years. It is moving further away with a heliocentric radial velocity of +15 km/s.
This is an evolved giant star with a stellar classification of G8III, having exhausted the hydrogen at its core and moved off the main sequence. It is a red clump giant, indicating it is presently on the horizontal branch and is generating energy through helium fusion in its core region. The interferometry-measured angular diameter of 24 Vul is , which, at its estimated distance, equates to a physical radius of about 16 times the radius of the Sun.
24 Vulpeculae is about 251 million years old and is spinning with a projected rotational velocity of 5.02 km/s. It has 3.41 times the mass of the Sun and is radiating 191 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,981 K. This is the probable (99.4% chance) source of X-ray emission coming from these coordinates.
References.
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52 Persei

52 Persei is a suspected triple star system in the northern constellation of Perseus. It has the Bayer designation f Persei, while "52 Persei" is the Flamsteed designation. The system is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.68. It is located around 600 light years away from the Sun based on parallax, and is drifting closer with a radial velocity of −4.5 km/s.
The variable velocity of this system was reported by W. W. Campbell in 1918. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.4. The components have a visual magnitude difference of 2.7 and are unresolved by speckle interferometry.
The primary component is an evolved bright giant star with a stellar classification of G5II. It has four times the mass of the Sun and has expanded to 32 times the Sun's radius. The star is radiating 531 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,868 K. The secondary is a suspected binary of unknown period, with its components having estimated masses equal to 2.4 and 1.0 times the mass of the Sun. The more massive member of the pair has an estimated spectral class of A2V, matching an A-type main-sequence star.


Kepler-60d

Kepler-60d is a planet discovered in 2012 that orbits the star Kepler-60. It was found by the Kepler Mission using the transit method.


NGC 7053

NGC 7053 is a spiral galaxy located about 200 million light-years away in the constellation of Pegasus. It was discovered by astronomer Albert Marth on September 2, 1863. It was then rediscovered by astronomer Heinrich d'Arrest on October 8, 1865.
On June 4, 2003 a type la supernova designated as SN 2003ep was discovered in NGC 7053.


Ursa Major Moving Group

The Ursa Major Moving Group, also known as Collinder 285 and the Ursa Major association, is the closest stellar moving group – a set of stars with common velocities in space and thought to have a common origin in space and time. In the case of the Ursa Major group, all the stars formed about 300 million years ago. Its core is located roughly 80 light years away and part of the Local Bubble. It is rich in bright stars including most of the stars of the Big Dipper.
Discovery and constituents.
All stars in the Ursa Major Moving Group are moving in roughly the same direction at similar velocities, and also have similar chemical compositions and estimated ages. This evidence suggests to astronomers that the stars in the group share a common origin.
Based on the numbers of its constituent stars, the Ursa Major Moving Group is believed to have once been an open cluster, having formed from a protostellar nebula approximately 500 million years ago. Since then, the sparse group has scattered over a region about 30 by 18 light-years, whose center is currently about 80 light-years away, making it the closest cluster-like object to Earth.
The Ursa Major Moving Group was discovered in 1869 by Richard A. Proctor, who noticed that, except for Dubhe and Alkaid (Eta Ursae Majoris), the stars of the Big Dipper asterism all have proper motions heading towards a common point in Sagittarius. Thus, the Big Dipper, unlike most constellations or asterisms, is largely composed of related stars.
Some of the brighter stream members include Alpha Coronae Borealis (α CrB or Alphecca or Gemma), Beta Aurigae (β Aur), Delta Aquarii (δ Aqr), Gamma Leporis (γ Lep) and Beta Serpentis (β Ser). More bright and moderately bright stars which are currently believed to be members of the group are listed below.
Group members.
Current criteria for membership in the moving group is based on the stars' motion in space. This motion can be determined from the proper motions and parallax (or distance) to the stars and radial velocities. A study published in 2003 using data gathered by the "Hipparcos" satellite (1989–1993) greatly improved both the proper motion and parallax estimates of nearby bright stars, refining the study of this and other moving groups.
Based on their distances (measured with "Hipparcos") and apparent magnitude, the absolute magnitude can be used to estimate the age of the stars. The stars in the moving group appear to have a common age of about 500 million years.
Core stars.
The core of the moving group consists of 14 stars, of which 13 are in the Ursa Major constellation and the other is in the neighboring constellation of Canes Venatici. The average apparent magnitude of all 14 core stars is approximately 4.42.
The following are members of the moving group closest to its center. These stars are all in Ursa Major except where indicated.
Stream stars.
There is also a "stream" of stars which are likely members of the Ursa Major Moving Group, scattered more widely across the sky (from Cepheus to Triangulum Australe).
Non-members.
The Big Dipper stars Dubhe (α UMa) and Alkaid (η UMa) are not members of the group, both being somewhat further away and moving in very different directions.
The bright, nearby star Sirius was long believed to be a member of the group, but may not be, according to research in 2003 by Jeremy King et al. at Clemson University. This research seems to indicate that it is too young to be a member, and is moving in the same direction as the group by mere coincidence.
Our Solar System is in the outskirts of this stream, but is not a member, being about 15 times older. Our Sun merely drifted in along its 250-million-year galactic orbit, and 40 million years ago was nowhere near the Ursa Major group.


Kepler-28

Kepler-28 is a star in the northern constellation of Cygnus., It is orbited by two exoplanets. It is located at the celestial coordinates: Right Ascension , Declination . With an apparent visual magnitude of 15.036, this star is too faint to be seen with the naked eye.
Planetary system.
The two warm sub-Neptune gas giant planets of Kepler-28 were discovered in 2011 and were confirmed in early 2012.


Iota Draconis

Iota Draconis (ι Draconis, abbreviated Iota Dra, ι Dra), also named Edasich , is a star in the northern circumpolar constellation of Draco. A visually unremarkable star of apparent magnitude 3.3, in 2002 it was discovered to have a planet orbiting it (designated Iota Draconis b, later named Hypatia). From parallax measurements, this star is located at a distance of about from the Sun.
Nomenclature.
"ι Draconis" (Latinised to "Iota Draconis") is the star's Bayer designation. On discovery the planet was designated Iota Draconis b (or Edasich b).
It bore the traditional name "Edasich", derived from the Arabic ' of Ulug Beg and the Dresden Globe, or 'Male hyena' by Kazwini, with "Eldsich" being recorded in the "Century Cyclopedia". 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 "Edasich" for this star.
In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Hypatia for this planet. The winning name was submitted by Hypatia, a student society of the Physics Faculty of the Universidad Complutense de Madrid, Spain. Hypatia was a famous Greek astronomer, mathematician, and philosopher.
In Chinese, (), meaning "Left Wall of Purple Forbidden Enclosure", refers to an asterism consisting of Iota Draconis, Theta Draconis, Eta Draconis, Zeta Draconis, Upsilon Draconis, 73 Draconis, Gamma Draconis and 23 Cassiopeiae. Consequently, the Chinese name for Iota Draconis itself is (, .), representing (), meaning "Left Pivot". 左樞 (Zuǒshū) is westernized into "Tsao Choo" by R.H. Allen with the same meaning
Properties.
Edasich is larger and more massive than the Sun, with 1.8 times the mass and nearly 12 times the radius. The spectrum matches a stellar classification of K2 III, indicating this is an evolved star that has exhausted the supply of hydrogen at its core and left the main sequence of stars like the Sun. With an expanded outer envelope, this giant star is radiating over 55 times the luminosity of the Sun at an effective temperature of 4,545 K. This temperature gives it an orange hue that is a characteristic of K-type stars. It is rotating at a leisurely rate, with a period of around 434 days. It is about 1.15 billion years old.
In the past Iota Draconis has been suspected of variability. However, the star has been found to have a constant luminosity to within about 0.004 magnitudes. Hence, as of 2010, the variability remains unconfirmed. An excess emission of infrared radiation at a wavelength of 70μm suggests the presence of a circumstellar disk of dust; what astronomers term a debris disk.
Planetary system.
The planetary companion discovered in 2002 was the first planet known to orbit a giant star. The habitable zone for this star lies in the range of 6.8–13.5 Astronomical Units, placing this planet well inside. The alignment of this planet's orbit may make it directly detectable via the transit method.


NGC 3552

NGC 3552 is a lenticular galaxy in the constellation Ursa Major. It was discovered on April 11, 1785 by William Herschel. It is a member of the galaxy cluster Abell 1185.


Epsilon Octantis

Epsilon Octantis, Latinized from ε Octantis, is a star in the southern circumpolar constellation of Octans. It is a faintly visible to the naked eye with an apparent visual magnitude of 5.09. The annual parallax shift of 11.22 mas yields a distance estimate of around 291 light years. It is moving further from the Sun with a radial velocity of +11.7 km/s.
This is an evolved, cool red giant star with a stellar classification of class M5III. It is a semiregular variable with a magnitude range of 4.58 to 5.3 and a (poorly defined) period around 55 days. The star has 1.34 times the mass of the Sun and has expanded to around 112 times the Sun's radius. It is radiating 1,819 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,560 K.


WASP-58

WASP-58 is a binary star system comprising a G-type main-sequence star and a red dwarf about 955 light-years away. WASP-58 is slightly depleted in heavy elements, having 80% of the solar abundance of iron. WASP-58 is much older than the Sun at 12.80 billion years.
Lithium was detected in the stellar spectrum of WASP-58A, making the star anomalous for its advanced age.
A multiplicity survey in 2015 did detect a red dwarf stellar companion at a projected separation of 1.281″ to WASP-58A, and it was confirmed to be gravitationally bound in 2016.
Planetary system.
In 2012 a transiting hot Jupiter planet b was detected on a tight, circular orbit around the primary star WASP-58A.
Planetary equilibrium temperature is .


List of stars in Lepus

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


NGC 5477

NGC 5477 is a dwarf galaxy located in the constellation of Ursa Major, 20 million light years away from Earth. It was discovered on April 14, 1789 by the astronomer William Herschel.


Zeta Hydrae

Zeta Hydrae (ζ Hya, ζ Hydrae) is a solitary star in the equatorial constellation of Hydra. This is a generally faint constellation, so, at an apparent visual magnitude of +3.10, this is the third-brightest member after Alphard and Gamma Hydrae.
Distance.
The distance to this star has been measured using the parallax technique, yielding a value of roughly . At this distance, the visual magnitude of the star is diminished by 0.03 as a result of extinction from intervening gas and dust. Delta Hydrae is about from Zeta Hydrae and may be a largely co-moving object. The star has one of the lower-error margin readings among those of the Gaia spacecraft which computes a parallax of 20.7182 ± 0.3925 mas and, if correct, a distance of 157 ± 3 light years.
Characteristics.
With a stellar classification of G9 II-III, this is an evolved giant star that is radiating 132 times the luminosity of the Sun from its outer envelope at an effective temperature of 4,925 K. At this heat, the star glows with the yellow hue of a G-type star. The radius of this star, as measured using interferometry, is about 18 times the Sun's radius. It has an estimated 4.2 times the mass of the Sun and is around old.
Name and etymology.
This star, along with δ Hya (Lisan al Sudja), ε Hya, η Hya, ρ Hya and σ Hya (Minchir), were Ulug Beg's "Min al Azʽal", "Belonging to the Uninhabited Spot". According to the catalogue of stars in the "Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars", "Min al Azʽal" or "Minazal" were the title for five stars:δ Hya as "Minazal I", η Hya as "Minazal II", ε Hya as "Minazal III", ρ Hya as "Minazal IV" and ζ Hya as "Minazal V" (exclude σ Hya).
In Chinese, (), meaning "Willow", refers to an asterism consisting of ζ Hydrae, δ Hydra, σ Hydrae, η Hydrae, ρ Hydrae, ε Hydrae, ω Hydrae and θ Hydrae Consequently, ζ Hydrae itself is known as (, ).
The people of Groote Eylandt called "Unwala", "The Crab", for the star cluster including this star, δ Hya (Lisan al Sudja), ε Hya, η Hya, ρ Hya and σ Hya (Minchir).


TW Horologii

TW Horologii is a variable star in the southern constellation of Horologium, near the eastern constellation border with Reticulum. It has a ruddy hue and is dimly visible to the naked eye with an apparent visual magnitude that ranges from 5.52 down to 5.95. Based on parallax measurements, it is located at a distance of approximately 1,370 light years from the Sun. It is drifting further away with a radial velocity of +14 km/s. In the past this star has been considered a member of the open cluster NGC 1252, but this now seems unlikely.
This is an aging red giant star on the asymptotic giant branch with a stellar classification of C-N4IIIb:. It is one of the brightest carbon stars and has a type of C2 3.5. The star is classified as a semiregular variable of type SRb and has a periodicity of 158 days. It has expanded to 164 times the radius of the Sun and, on average, is radiating 4,390 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,674 K. The short-lived element technetium has been observed in the spectrum, an indicator of thermal pulses during helium shell burning.
Based on the detection of excess ultraviolet excess, it is most likely a binary star system. An analysis of the motion of TW Horologii suggests a low-mass companion, although the UV excess suggests it is hot.
In 2013 the luminosity of Mira variables, based on Hipparcos parallaxes, was used to calibrate a Period-luminosity relationship for carbon stars. The absolute magnitude of TW Horologii was calculated to be −1.79.


Eta Capricorni

Eta Capricorni, Latinized from η Capricorni, is a binary star system in the southern constellation of Capricornus. It can be seen with the naked eye, having a combined apparent visual magnitude of +4.84. Based upon an annual parallax shift of 20.20 mas as seen from the Earth, the star is located about 161 light years from the Sun.
The pair orbit each other with a period of 27.85 years, a semimajor axis of 0.265 arc seconds, an eccentricity of 0.410. The primary member, component A, is a white-hued A-type main sequence star with an apparent magnitude of +5.02. Its companion, component B, has an apparent magnitude of +7.39.
Nomenclature.
"η Capricorni" (Latinised to "Eta Capricorni") is the system's Bayer designation. It also has the Flamsteed designation 22 Capricorni.
In Chinese, (), meaning "Twelve States", refers to an asterism which is represent twelve ancient states in the Spring and Autumn period and the Warring States period, consisting of η Capricorni, φ Capricorni, ι Capricorni, 38 Capricorni, 35 Capricorni, 36 Capricorni, χ Capricorni, θ Capricorni, 30 Capricorni, 33 Capricorni, ζ Capricorni, 19 Capricorni, 26 Capricorni, 27 Capricorni, 20 Capricorni and 21 Capricorni. Consequently, the Chinese name for η Capricorni itself is (, ), meaning that this star (together with 21 Capricorni and β Serpentis in "Right Wall of Heavenly Market Enclosure" (asterism)) represent "Zhou" () (possibly Chow, the dynasty in China).
Sometimes, this star is called by the name "Armus" in an astrological context.


NGC 6242

NGC 6242 is an open cluster in the constellation Scorpius.


56 Arietis

56 Arietis is a single, variable star in the northern zodiac constellation of Aries. It has the variable star designation SX Arietis, while "56 Arietis" is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued point of light with a baseline apparent visual magnitude of 5.79. The estimated distance to this star is approximately , based on parallax, and it is drifting further away with a radial velocity of +18 km/s.
This is a magnetic, chemically peculiar star of the silicon type with a stellar classification of B9pSi, and it has a rapid rotation period of 17.5 hours. This period is increasing by about two seconds every hundred years. The star displays evidence of a five year period for procession of its axis. 56 Arietis is the prototype of a class of variable stars known as SX Arietis variables, which are rotationally variable stars with strong magnetic fields. It ranges in brightness from 5.75 down to 5.81 with a cyclical period matching its rotation rate.


AV Microscopii

AV Microscopii is a variable star in the southern constellation of Microscopium. It is a dim, red-hued star near the lower limit of visibility to the naked eye with a baseline apparent visual magnitude of 6.28. The star is located approximately 740 light years away from the Sun, based on parallax, but is moving closer with a radial velocity of −23 km/s. It is a member of the Milky Way's old disk population.
Based upon a stellar classification of M4 III, this is an aging red giant star, having exhausted the supply of hydrogen at its core then expanded to around 78 times the Sun's radius. Earlier it had been classed as M3 II, with the luminosity class of a bright giant. Samus et al. (2017) have it tentatively classified as an irregular variable of subtype LC, suggesting this is a supergiant star. It is a pulsating variable with multiple periods discovered, ranging in apparent visual magnitude between 6.25 and 6.35. The star radiates 849 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,539 K.


HD 33203

HD 33203 is double star in the northern constellation of Auriga. It includes a bright giant star with a stellar classification of B2II. The two components have an angular separation of 1.617″ along a position angle of 222.1°.


UGC 9796

UGC 9796 is a lenticular and polar-ring galaxy in the constellation Boötes, and about 250 million light years distant from Earth. It is an object of great scientific interest as there have been very few polar ring galaxies discovered. UGC 9796 is a very gas-rich environment hosting as much solar masses of neutral hydrogen. DSS and SDSS images show that it is very similar to polar ring galaxy NGC 660, the best-known of all the polar ring galaxies.
This object is also known as "PGC 54461", "MCG+07-31-48", and "PRC A-06"


NGC 6309

NGC 6309, also known as the Box Nebula, is a planetary nebula located in the constellation Ophiuchus. It was discovered by the German astronomer Wilhelm Tempel in 1876. It has a luminosity of about 1800 times of the Sun. The distance to this nebula is not well known, but it is assumed to be about 6,500 light-years or 2,000 parsecs.
NGC 6309 is a quadrupolar nebula, with two pairs of lobes. Surrounding the pair is a spherical shell. The spherical shell formed before the four lobes.


Omega Hydrae

Omega Hydrae, Latinized from ω Hydrae, is a golden-hued star in the equatorial constellation of Hydra, located to the west-southwest of the brighter star Zeta Hydrae. Based upon an annual parallax shift of just 3.64 mas as seen from Earth, it is located roughly 900 light years from the Sun. It is faintly visible to the naked eye with an apparent visual magnitude of 5.00.
This is an evolved K-type star with a stellar classification of K2 II-III, which indicates a spectrum showing traits intermediate between the giant and bright giant stages. It is most likely (98% chance) on the horizontal branch, indicating that the star is generating energy through the thermonuclear fusion of helium at its core. With 4.32 times the Sun's mass, it has expanded to around 48 times the radius of the Sun. Omega Hydrae is about 180 million years old and spinning with a leisurely projected rotational velocity of 2.3 km/s. The star is radiating roughly 944 times the solar luminosity from its photosphere at an effective temperature of 4,789 K.


43 Persei

43 Persei is a binary star system in the northern constellation Perseus. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.28. The system is located around distant from the Sun, based on parallax.
This is a double-lined spectroscopic binary with an orbital period of 30.4 days and an eccentricity of 0.6. The primary component is an F-type main-sequence star with a stellar classification of F5V, a star that is fusing its core hydrogen. It has 1.54 times the mass of the Sun, 2.4 times the Sun's radius, and is spinning with a projected rotational velocity of . The star shines 10.8 times brighter than the Sun at an effective temperature of .
There are distant companions B (separation 75.5" and magnitude 10.66), C (separation 85.6" and magnitude 12.18), and D (separation 68" and magnitude 13.43).


List of stars in Aries

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


NGC 6328

NGC 6328 is an intermediate spiral galaxy located in the constellation Ara. It is classified as SAB(s)ab in the galaxy morphological classification scheme and was discovered by the British astronomer John Herschel on 2 May 1835. NGC 6328 is located at about 199 million light years away from earth.


Kepler-30

Kepler-30 is a star in the northern constellation of Lyra. It is located at the celestial coordinates:
Right Ascension Declination . With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye.
Kepler-30 is exhibiting a strong starspot activity.
Planetary system.
Three planets of Kepler-30 were detected by the transit method in 2011.
The planets are strongly interacting each other, with transit times variability exceeding one hour for each consecutive orbit. Due irregularity of orbits, confirmation of planetary system was delayed until 2012.
The planetary periods are close to 1:2:5 orbital resonance but are not resonant, producing an extremely complex orbital dynamics.


HU Delphini

HU Delphini, also known as Gliese 791.2, is a star system in the constellation of Delphinus. Its apparent magnitude is 13.07. With a trigonometric parallax of 113.4 ± 0.2 mas, it is about 28.76 light-years (8.82 parsecs) away from the Solar System.
HU Delphini is a binary star with a well-defined period of 538.6 days. The orbit has been derived from astrometry as well as through spectral observations, although that has been difficult because of the high projected rotational velocity. It is also fairly eccentric, at 0.558.
Both stars in the system are red dwarfs. The primary component of the system is only 23.7% as massive as the Sun, so it is fully convective. As a result, there are frequent starspots on its surface, especially near poles. While the normal surface temperature of the primary is 3000 K, the starspots themselves are cooler: only 2700 K. It is also a flare star, the first flare been detected in August 2000. The secondary star has a mass of 11.4% that of the Sun.


NGC 5460

NGC 5460 is an open cluster in the constellation Centaurus. It is a bright but loose cluster of intermediate age located approximately 2,300 light years away from Earth. It is located nearly 2 degrees east-southeast of Zeta Centauri.
Observation history.
NGC 5460 was discovered by James Dunlop in 1826. He described it on May 7, 1826 as "a curiously curved line of small stars, of nearly equal magnitudes; two stars of 7th magnitude to the east" and added it to his catalog as number 431. John Herschel described as "a region of large bright stars of 8, 9... etc. magnitude; a very coarse cluster" and added it to General Catalogue as No. 3555. In the New General Catalogue it is described as "very large, very little concentrated, stars 8th magnitude and fainter".
Characteristics.
NGC 5460 is a loose open cluster, of Trumpler type II3m. There are 272 probable member stars within the angular radius of the cluster and 96 within the central part of the cluster. The tidal radius of the cluster is 4.1 - 8.2 parsecs (13 - 26 light years) and represents the average outer limit of NGC 5460, beyond which a star is unlikely to remain gravitationally bound to the cluster core.
A photometric study by Barrado and Byrne in 1995 studied 353 stars near the core of the cluster and identified 25 members and 27 possible members. They estimated the age of the cluster to be 110 mys and its distance to be 740 pc and identified three stars, members and possible members, as variable. A spectrographic study of the cluster by Fossati et al. (2011) estimated the distance of the cluster to be 720 ± 50 pc, its age log t=8.2 ± 0.1 and the mean radial velocity −17.9 ± 5.2 km/s. The metallicity of the cluster is slightly higher than the solar one (Z = 0.013).
The brightest of the members is HD 123226 (mag. 8.98, B8), which is also the hottest star of the cluster. One more star, HD 122983, (mag. 9.77, B9.5IV/V) has been found to be variable, with period 3.4 days. It is a He-weak star. Other chemically peculiar stars within the cluster are HD 123182 (He-weak star of an unclear type, mag. 9.88, spectral type B9), and UCAC 11105038 (mag. 11.59, A8). Also, the hotter component of the HD 123225 system may be an HgMn star.


NGC 6384

NGC 6384 is an intermediate barred spiral galaxy located about 77 million light-years away in the northern part of the constellation Ophiuchus. It has a morphological classification of SAB(r)bc, indicating that it is a weakly barred galaxy (SAB) with an inner ring structure (r) orbiting the bar, and moderate to loosely wound spiral arms (bc). The galaxy is inclined by an angle of 47° to the line of sight, along a position angle of 40°. The estimated mass of the stars in this galaxy is 105 billion times the mass of the Sun.
At one time NGC 6384 was considered a normal galaxy with no activity in the nucleus. However, it is now classified as a transition object (T2), which is thought to be a LINER-type galaxy whose emission-line spectra is contaminated by H II regions in the nucleus.
On 24 June 1971, a type Ia supernova event was discovered in this galaxy at 27″ east and 20″ north of the nucleus. It reached a peak visual magnitude of 12.85 around the end of June. Designated SN 1971L, it was situated along a spiral arm, suggesting that the progenitor was not a member of the older, more evolved stellar population of the galaxy.


NGC 4707

NGC 4707 is an irregular galaxy in the constellation of Canes Venatici. It was discovered by John Herschel on 5 June 1834, and was described by John Louis Emil Dreyer, the compiler of the New General Catalogue, as a "small, stellar" galaxy.
NGC 4707 has a morphological type of Sm or Im, meaning that it is mostly irregular or has very weak spiral arms. The galaxy was imaged by the Hubble Space Telescope in 2016. The image showed the galaxy had little to no signs of a central bulge or any prominent structures (typical of Magellanic-type spirals). However, the telescope could resolve many stars, as well as several turquoise-colored star forming regions.


P Carinae

The Bayer designations p Carinae and P Carinae are distinct.


NGC 2608

NGC 2608 (also known as Arp 12) is a barred spiral galaxy located 93 million light-years away in the constellation Cancer (the Crab). It is 62,000 light-years across, and about 60% of the width of the Milky Way. It is considered a grand design spiral galaxy and is classified as SB(s)b, meaning that the galaxy's arms wind moderately (neither tightly nor loosely) around the prominent central bar.
It was classified by Halton Arp under "galaxies with split arms" in his 1966 Atlas of Peculiar Galaxies who noted that the "nucleus may be double or superposed star."
NGC 2608 is now considered to be a pair of interacting galaxies.


Mu2 Scorpii

Mu² Scorpii (μ² Scorpii, abbreviated Mu² Sco, μ² Sco), also named Pipirima , is a star in the zodiac constellation of Scorpius. It has an apparent visual magnitude of +3.56, which is bright enough to be seen with the naked eye. Its distance from the Sun is about 474 light-years, as determined by parallax measurements. It is a member of the Upper Centaurus-Lupus subgroup of the Scorpius–Centaurus Association.
Properties.
This is a blue-white, B-type subgiant star with a stellar classification of B2 IV. It has an estimated 7 times the radius of the Sun, almost 9 times the Sun's mass, and shines with 2,385 times the Sun's luminosity. The outer atmosphere has an effective temperature of 23,113 K. It is some 18.5 million years old and is spinning with a projected rotational velocity of 58 km/s.
Nomenclature.
"μ² Scorpii" (Latinised to "Mu² Scorpii") is the star's Bayer designation.
In Tahiti, a traditional story is told of a brother and sister, named "Pipiri" and "Rehua", who flee their parents into the sky and become stars. Their parents call them "Pipiri ma" while chasing them into the sky: "ma" "with, and" is used after names to mean "et al." In one account, the children become Shaula and Lesath in the tip of the tail of Scorpio, and in another they become Mu² and Mu¹ Scorpii. (In a similar version of the story told in the Cook Islands, they become Omega¹ and Omega² Scorpii).
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 "Pipirima" for this star on 5 September 2017 (along with Xamidimura for its partner) and it is now so included in the List of IAU-approved Star Names.
In Chinese astronomy, Mu² Scorpii is called 尾宿增二.


NGC 7046

NGC 7046 is a barred spiral galaxy located about 180 million light-years away in the constellation of Equuleus. NGC 7046 is also classified as a LINER-type galaxy. NGC 7046 has an estimated diameter of 106,990 light-years. NGC 7046 was discovered by astronomer William Herschel on October 10, 1790.


HD 23596

HD 23596 is a 7th magnitude star approximately 170 light years away in the constellation Perseus. The visual luminosity of the star is 2.63 times greater than our Sun. HD 23596 dwarfs the Sun is terms of physical properties; including mass, radius, age, metallicity, and temperature. The spectrum of the star is F8.
Planetary system.
In June 2002, a massive long-period planet orbiting the star was announced.


BX Circini

BX Circini is a star in the constellation Circinus. Its variability was discovered in 1995, with its apparent magnitude ranging from 12.57 to 12.62 over a period of 2 hours 33 minutes. It is currently classified as a PV Telescopii variable star, but has been put forward as the prototype of a new class of pulsating star—the BX Circini variables—along with the only other known example, V652 Herculis. This class of star is rare, possibly because this is a brief stage of stellar evolution. Its mass has been calculated to be around 40 percent that of the Sun and the average surface temperature has been measured at 23,390 ±90 K using optical spectra, but 1750 K cooler if analysing it in both the visual and ultraviolet. The temperature appears to vary by 3450 K.
This star has an extremely low proportion of hydrogen, which was first noticed in 1980. In fact, over 99% of its composition appears to be helium, qualifying it as an extreme helium star. Its origin is unclear, but thought to be a result of the merger of a helium white dwarf with a carbon/oxygen one. The two merge violently, with material from the lighter helium white dwarf forming the outer envelope. The resulting star expands and shines as a yellow giant, its outer helium shell igniting and undergoing fusion as material continues to be accreted from the lighter star. The size of the star is maintained by the weight upon the helium shell, and once that has become light enough and the helium is exhausted, the star begins heating and shrinking, becoming the smaller blue star now observed.


Theta Aurigae

Theta Aurigae (θ Aurigae, abbreviated Theta Aur, θ Aur) is a binary star in the constellation of Auriga. Based upon parallax measurements, the distance to this system is about .
The two components are designated Theta Aurigae A (also named Mahasim) and B.
Nomenclature.
"θ Aurigae" (Latinised to "Theta Aurigae") is the system's Bayer designation. The designations of the two components as "Theta Aurigae A" and "B" derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
Some authors state that Theta Aurigae had no traditional name, although Richard Hinckley Allen makes a passing reference about the name "Mahasim", as a name also used, with various spellings, for Eta Aurigae and Lambda Herculis, from the Arabic المِعْصَم "al-miʽşam" "the wrist" (of the charioteer). In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name "Mahasim" for the component Theta Aurigae A on 30 June 2017 and it is now so included in the List of IAU-approved Star Names.
It is known as 五車四 (the Fourth Star of the Five Chariots) in Chinese
Properties.
The primary component, Theta Aurigae A, is a large star with more than three times the mass of the Sun and over five times the Sun's radius. It is radiating 263 times the Sun's luminosity from its outer atmosphere at an effective temperature of 10,400 K, giving it the white hue of an A-type star. The star has a stellar classification of A0pSi, with the 'pSi' suffix indicating it is a chemically peculiar star with an abnormal abundance of silicon.
The primary is classified an Alpha2 Canum Venaticorum type variable star and has a surface magnetic field of about 1 kG. Its projected rotational velocity is , with the star completing a rotation in only 3.6 days. The axis of rotation is inclined by an angle of to the line of sight from the Earth.
The secondary, Theta Aurigae B, is a +7.2 magnitude companion, 4.5 magnitudes fainter than the primary, located at an angular separation of 3.91 arcseconds along a position angle of 304.9° as of 2002. This is an F-type main sequence star with a stellar classification in the range F2-5 V.
The mean combined apparent magnitude of the system is +2.65 but the variation of the primary causes the system's brightness to range from magnitude +2.62 to +2.70 with a period of 1.37 days. The system is an X-ray source with a luminosity of .


64 Serpentis

64 Serpentis is a single, blue-white hued star in Serpens Cauda, the eastern segment of the equatorial constellation of Serpens. With an apparent visual magnitude of 5.56, it is a dim star but visible to the naked eye in good seeing conditions. Based upon an annual parallax shift of , it is located roughly 1,100 light years away. It is moving closer to the Sun with a heliocentric radial velocity of about −10 km/s. It is one of the brightest stars in front of the Great Rift.
Over time this star has received a range of stellar classifications, which varied considerably in the determined luminosity class. Houk and Swift (1999) have it classified as B8/9 II, Slettebak (1982) listed a class of B8 IV, Cowley (1972) has , while Frémat et al. (2006) gave it a classification of B8 III. Despite these assignments, it is still considered to be in the main sequence phase. An overshoot of the convective core due to internal waves and rotational effects are believed to be mixing in fresh hydrogen and removing helium ashes, which is extending the duration of its stay on the main sequence. It may be chemically peculiar, displaying an overabundance of mercury (Hg) in its outer atmosphere.
64 Serpentis was observed extensively during the CoRoT mission, which allowed highly accurate monitoring of its brightness. This revealed that the star displays low-amplitude variations with the main frequency being 1.56 days long, while it has smaller variations with other frequencies. These variations may be due to rotational modulation of spots or clouds in the photosphere, or possibly from non-radial pulsations. It does not exhibit the signature of a significant magnetic field.
This is a classical Be star – a rapidly rotating B-type main sequence star that has formed an orbiting gaseous disk through a mass ejection process. The circling gas is heated by the star, creating the Balmer line emission that overlays the stellar spectrum. The rapid rotation gives the star an oblate shape with a prominent equatorial bulge. 64 Serpentis is about 170 million years old with roughly 4.4 times the mass of the Sun and is radiating 724 times the Sun's luminosity from its photosphere at an effective temperature of around 12,000 K.


E Centauri

E Centauri is a single star in the southern constellation of Centaurus. It is a white-hued star that is dimly visible to the naked eye with an apparent visual magnitude of +5.34. The distance to this object is approximately 560 light years based on parallax, and it has an absolute magnitude of −0.97. It is drifting closer to the Sun with a radial velocity of +7 km/s, and it is a candidate member of the Lower Centaurus Crux subgroup of the Sco OB2 association.
This is a late B- or early A-type main-sequence star with a stellar classification of B9.5/A0V, which indicates it is generating energy via core hydrogen fusion. It has 3.4 times the mass of the Sun and is spinning with a projected rotational velocity of 74 km/s. The star is radiating 302 times the luminosity of the Sun from its photosphere at an effective temperature of 9,886 K.


70 Pegasi

70 Pegasi is a binary star system in the northern constellation Pegasus. It is a faint star, visible to the naked eye under good seeing conditions, with an apparent visual magnitude of 4.56. The measured annual parallax shift measured from Earth's orbit is 18.65 mas, yielding a distance estimate of around 175 light years. The visual magnitude of the star is diminished by an extinction of due to interstellar dust. It is moving closer to the Sun with a radial velocity of −17 km/s.
This is a single-lined spectroscopic binary with an orbital period of and a high eccentricity of 0.713. The visible component has a stellar classification of G8 IIIa, indicating it is an evolved G-type giant star. It is a probable red clump star, which would mean it is generating energy through helium fusion at its core. The star has 2.5 times the mass of the Sun and has expanded to more than 8 times the Sun's radius. It is radiating about 48 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,032 K.
The secondary is most likely a low mass main sequence star with no more than 0.4 times the mass of the Sun.


HD 48265

HD 48265 is the Henry Draper Catalogue designation for a star in the southern constellation Puppis. It has an apparent visual magnitude of 8.07, which makes it too faint to be seen with the naked eye. Based upon parallax measurements made during the Hipparcos mission, it is located at a distance of roughly from Earth.
This star has a stellar classification of G5IV/V, suggesting that, at an age of 4.8 billion years, it has reached an intermediate evolutionary stage between a main sequence star and a subgiant. It has but 93% of the mass of the Sun, while its outer atmosphere has begun to expand, reaching about 2.3 times the Sun's radius. HD 48265 is radiating 62% of the Sun's luminosity from its atmosphere at an effective temperature of 5,508 K, giving it the cool orange glow of a K-type star. Measurement of the chemical abundances of this star indicate that, compared to the Sun, it has a 95% greater proportion of elements other than hydrogen and helium—what astronomers term the star's metallicity.
Planetary system.
In October 2008 the planet, HD 48265 b, was reported to be orbiting this star. This object was detected using the radial velocity method during an astronomical survey conducted by the Magellan Planet Search Program using the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope.
As part of the NameExoWorlds project of the IAU, HD 48265 b has been named Naqaỹa ("brother") and HD 48265 Nosaxa ("springtime") in the Moqoit language, as voted by Argentine voters in an online poll.


HAT-P-8

HAT-P-8 is a magnitude 10 star located 750 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of . The second is even less massive, at , and its spectral type is M6V.
Planetary system.
In 2008 the HATNet Project announced the discovery of extrasolar planet HAT-P-8b around this star. This planet is a hot Jupiter gas giant planet.


HD 37605

HD 37605 is a star in the equatorial constellation of Orion. It is orange in hue but is too faint to be visible to the naked eye, having an apparent visual magnitude of 8.67. Parallax measurements yield a distance estimate of 153 light years from the Sun. It has a high proper motion and is drifting closer with a radial velocity of −22 km/s.
This object is a K-type main-sequence star with a stellar classification of K0 V. It is an inactive, metal-rich star. Age estimates range from 1.8 up to 7 billion years old, and it is spinning with a projected rotational velocity of 4.5 km/s. The star has 98% of the mass of the Sun and 89% of the Sun's radius. It is radiating 60% of the luminosity of the Sun from its photosphere at an effective temperature of 5,380 K.
Planets.
There are two giant planets known in orbit. Planet b was discovered in 2004 and planet c was discovered eight years later. The planets do not transit relative to Earth; b's maximum inclination is 88.1%.
In a simulation, HD 37605 b's orbit "sweeps clean" most test particles within 0.5 AU; leaving only asteroids "in low-eccentricity orbits near the known planet’s apastron distance, near the 1:2 mean-motion resonance" with oscillating eccentricity up to 0.06, and also at 1:3 with oscillating eccentricity up to 0.4. Also, observation has ruled out planets heavier than 0.7 Jupiter mass with a period of one year or less; which still allows for planets at 0.8 AU or more.


Psi2 Aurigae

Psi2 Aurigae, Latinized from ψ2 Aurigae, is a star in the constellation Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 4.79. Based upon parallax measurements, this star is approximately away from the Earth. At that distance, the brightness of the star is diminished by 0.07 in magnitude from extinction caused by interstellar gas and dust.
Most studies categorized this as a K-type giant star with a stellar classification of K3 III. However, the results of a study published in 2003 list it with a classification of K3 Iab:, which would instead suggest it is a supergiant star. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 27 times the radius of the Sun. It is radiating 304 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,410 K.
It was also known to be part of a much bigger constellation named Telescopium Herschelii. It was also the constellation's brightest star before it was unrecognized by the International Astronomical Union (IAU).
References.
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NGC 2359

NGC 2359 (also known as Thor's Helmet) is an emission nebula in the constellation Canis Major. The nebula is approximately 3,670 parsecs (11.96 thousand light years) away and 30 light-years in size. The central star is the Wolf-Rayet star WR7, an extremely hot star thought to be in a brief pre-supernova stage of evolution. It is similar in nature to the Bubble Nebula, but interactions with a nearby large molecular cloud are thought to have contributed to the more complex shape and curved bow-shock structure of Thor's Helmet.
It is also catalogued as Sharpless 2-298 and Gum 4.
The nebula has an overall bubble shape, but with complex filamentary structures. The nebula contains several hundred solar masses of ionised material, plus several thousand more of unionised gas. It is largely interstellar material swept up by winds from the central star, although some material does appear to be enriched with the products of fusion and is likely to come directly from the star. The expansion rate of different portions of the nebula varies from 10 km/s to at least 30 km/s, leading to age estimates of 78,500 - 236,000 years. The nebula has been studied at radio and x-ray wavelengths, but it is still unclear whether it was produced at the class O main sequence stage of development, as a red supergiant, luminous blue variable, or mainly as a Wolf-Rayet star.
NGC 2361 is a bright knot of nebulosity on one edge of the central ring of NGC 2359.


T Carinae

T Carinae is a star in the southern constellation of Carina. Although given a variable star designation, it is now thought to be constant; the identifier "HD 94776" from the "Henry Draper catalogue" may be used instead. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.93. The distance to this object is approximately 285 light years based on parallax, and it has an absolute magnitude of 1.08. It is drifting closer to the Sun with a radial velocity of −26 km/s.
This is an aging giant star with a stellar classification of K0III, which indicates it has exhausted the supply of hydrogen at its core and expanded off the main sequence. It is a red clump giant, which means it is on the horizontal branch and is undergoing core helium fusion. At present it has nine times the Sun's radius and is radiating 39 times the luminosity of the Sun from its photosphere at an effective temperature of 4,729 K.
When used as a comparison star for AG Carinae in 1914 by H. E. Wood, this object was announced as a candidate variable star. A year later it was determined by R. Innis that it was AG Carinae that varied and this star is constant. Later, T Carinae became flagged as a low amplitude irregular variable. It is now catalogued as a probable constant star.


Turdus Solitarius

Turdus Solitarius (Latin for "solitary thrush") was a constellation created by French astronomer Pierre Charles Le Monnier in 1776 from stars of Hydra's tail. It was named after the Rodrigues solitaire, an extinct flightless bird that was endemic to the island of Rodrigues East of Madagascar in the Indian Ocean. It was replaced by another constellation, Noctua (the Owl), in "A Celestial Atlas" (1822) by the British amateur astronomer Alexander Jamieson. , neither constellation is in use.


HR 4072

HR 4072 is a binary star system in the northern circumpolar constellation of Ursa Major. It has the variable star designation ET Ursae Majoris, abbreviated ET Uma, while "HR 4072" is the system's designation from the "Bright Star Catalogue". It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.94. The system is located at a distance of approximately 339 light years from the Sun based on parallax measurements. The radial velocity measurement is poorly constrained, but it appears to be drifting closer to the Sun at the rate of around −3 km/s.
This is a double-lined spectroscopic binary star system with an orbital period of 11.6 days and an eccentricity of 0.26. The orbit for this star was first determined by R. H. Baker in 1912, then later revised.
The primary, designated component A, is an Ap type chemically-peculiar star with a stellar classification of A1:VpSiSrHg, although it has also been considered to be a mercury-manganese star. The suffix notation indicates abundance anomalies of silicon, strontium, and mercury in the spectrum. It is an α2 Canum Venaticorum variable with an amplitude of 0.05 magnitude in the B (blue) band. The star is rotating slowly with a projected rotational velocity of 4.5 km/s. It is radiating 139 times the luminosity of the Sun from its photosphere at an effective temperature of 10,307 K.
The secondary component has been reported to have characteristics of an Am star.


Alpha Equulei

Alpha Equulei (α Equulei, abbreviated Alpha Equ, α Equ), officially named Kitalpha , is a star in the constellation of Equuleus. It is a high proper motion star only 190 light years away.
Nomenclature.
"α Equulei" (Latinised to "Alpha Equulei") is the star's Bayer designation.
It bore the traditional name "Kitalpha" (rarely "Kitel Phard" or "Kitalphar)," a contraction of the Arabic name قطعة الفرس "qiṭ‘a(t) al-faras" "a piece of the horse". 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 "Kitalpha" for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
In Chinese, (), meaning Emptiness, is an asterism consisting of Alpha Equulei and Beta Aquarii. Consequently, the Chinese name for Alpha Equulei itself is (, .)
Properties.
The overall appearance of α Equulei is a G-type giant with an apparent magnitude of +3.92, but it is a spectroscopic binary consisting of two individual stars.
The primary star is a G7 giant about fifty times more luminous than the sun. It has an effective temperature of 5,100 K and a radius of 9.2 times greater than the sun.
The secondary is an A-type dwarf about 26 times as luminous as the sun. It has an effective temperature of 8,150 K and a radius 2.6 times greater than the sun. It is a chemically peculiar Am star.
The two stars revolve in a circular orbit every 98.8 days. Their respective orbital velocities allow their masses to be calculated at and respectively.


Omicron Cancri

The Bayer designation Omicron Cancri (ο Cnc / ο Cancri) is shared by two stars, in the constellation Cancer:
They are separated by 0.27° on the sky. With a physical separation of , the stars most likely form a co-moving pair.


Kappa Reticuli

Kappa Reticuli (κ Reticuli) is a binary star system in the southern constellation of Reticulum. It is visible to the naked eye, having a combined apparent visual magnitude of +4.71. Based upon an annual parallax shift of 46.12 mas as seen from Earth, it is located 71 light years from the Sun. Based upon its space velocity components, this star is a member of the Hyades supercluster of stars that share a common motion through space.
Houk and Cowley (1978) catalogued the yellow-hued primary, component A, with a stellar classification of F3 IV/V, indicating this is an F-type star that showing mixed traits of a main sequence and a more evolved subgiant star. Later, Grey et al. (2006) listed a class of F3 V, suggesting it is an F-type main-sequence star. It is emitting a statistically significant amount of infrared excess, suggesting the presence of an orbiting debris disk. The secondary, component B, is an orange-hued star with a visual magnitude of 10.4 at an angular separation of 54 arc seconds from the primary.


NGC 6090

NGC 6090 is a merging pair of spiral galaxies, 400 million light-years from the Earth, in the constellation of Draco. The cores of the two galaxies are around 10,000 light-years apart from each other, meaning that the merger is likely at its intermediate stage. Two large "tails", made of galactic material gravitationally ejected during the merger, have formed outside the main galaxies. Newly formed stars can be seen in the overlapping area.


T Normae

T Normae is a Mira variable star. It is located midway between Eta Normae and Gamma Circini. It ranges from magnitude 6.2 to 13.6 and a period of 244 days. Located around 900 light-years distant, it shines with a luminosity 760 times that of the Sun and has a surface temperature of 3234 K.


Mu Leonis

Mu Leonis (μ Leonis, abbreviated Mu Leo, μ Leo), also named Rasalas , is a star in the constellation of Leo. The apparent visual magnitude of this star is 3.88, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 0.02628 arc seconds as measured by the Hipparcos satellite, this system is from the Sun. In 2014, an exoplanet was discovered to be orbiting the star.
Nomenclature.
"μ Leonis" (Latinised to "Mu Leonis") is the star's Bayer designation.
It bore the traditional names "Rasalas" and "Alshemali", both abbreviations of "Ras al Asad al Shamaliyy". 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 "Rasalas" for this star on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.
Properties.
Mu Leonis is an evolved K-type giant star with a stellar classification of . The trailing notation indicates that, for a star of its type, it has stronger than normal absorption lines of cyanogen and calcium in its spectrum. It has around 1.5 times the Sun's mass, but has expanded to around 14 times the Sun's radius. Mu Leonis shines with 63 times the luminosity of the Sun from an outer atmosphere that has an effective temperature of 4,436 K. It is around 3.35 billion years old.
Planetary system.
In 2014 it was announced that Mu Leonis has a planetary companion that is at least 2.4 times as massive as Jupiter and orbits with a period of 358 days. This planet was detected by measuring radial velocity variations caused by gravitational displacement from the orbiting body.


Zeta Librae

The Bayer designation ζ Librae, Latinised as Zeta Librae (abbreviated ζ Lib / Zeta Lib) is shared by several star systems in the constellation Libra. Sources differ about the Flamsteed and Bayer designations that should be applied to four stars:
In light of the obvious confusion, the Bright Star Catalogue recommends the use of HR designations to unambiguously identify these four stars. HD 137949 does not have an HR number although it is included in the Bright Star Catalogue Supplement.


Psi8 Aurigae

Psi8 Aurigae (ψ8 Aur, ψ8 Aurigae) is a star in the northern constellation of Auriga. It has an apparent visual magnitude of 6.443 and, based upon parallax measurements, they are approximately distant from the Earth.
The spectrum of the star matches a stellar classification of B9.5p


Kepler-68

Kepler-68 is a Sun-like main sequence star. It is known to have at least three planets orbiting around it. The outermost planet has a mass similar to Jupiter but orbits within the habitable zone.
High resolution imaging observations of Kepler-68 carried out with the lucky imaging instrument AstraLux on the 2.2m telescope at Calar Alto Observatory detected a wide companion candidate approximately 11 arcseconds away. Comparing these observations to the 2MASS positions shows that the companions proper motion is consistent with it being bound to the Kepler-68 system, but further observations are needed to confirm this conclusion. Eleven arcseconds at the distance of Kepler-68 leads to a sky projected separation of approximately 1600 Astronomical units. A circular orbit at that distance would have a period of roughly 50,000 years.
Planetary system.
Currently, three planets have been discovered to orbit around Kepler-68. Two of the innermost planets were discovered by the planetary transit method. Follow-up Doppler measurements helped to determine the mass of Kepler-68b and helped to discover Kepler-68d. There is an additional signal present in the radial velocity measurements indicating another body in the system at a period of greater than 10 years. The mass of this object is unknown and it could be either another planet or a stellar companion.


Eta Normae

Eta Normae, Latinized from η Normae, is a single star in the southern constellation of Norma. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.65. The distance to this star is about 219 light years, based on parallax. The Gamma Normids radiate from a position near this star.
This is an aging giant star with a stellar classification of G8III, having exhausted the supply of hydrogen at its core then swollen and cooled off the main sequence. At present it has a diameter of 11 times that of the Sun. It is a red clump giant, meaning it is on the horizontal branch and is generating energy through core helium fusion. The star has 2.78 times the mass of the Sun and is radiating 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,052 K. It is a source for X-ray emission.


Upsilon Orionis

Upsilon Orionis (υ Ori, υ Orionis) is a star in the constellation Orion. It has the traditional name "Thabit" or "Tabit" (ﺛﺎﺑﺖ, Arabic for "the endurer"), a name shared with pi3 Orionis. It is a blue-white main sequence star of apparent magnitude 4.62 located over 3000 light-years distant from the Solar System. It is a suspected Beta Cephei variable.
Name.
Located south of Iota Orionis, Upsilon Orionis is one of two stars (the other is 29 Orionis) marking the top of Orion's right boot in Johann Bayer's "Uranometria" (1603). It was given the number 36 by John Flamsteed, while its proper name appears to be derived from the Arabic "Al Thabit" "the endurer". In his "" (1899), American amateur naturalist Richard Hinckley Allen noted that the name appeared on the star atlas "Geography of the Heavens", composed by Elijah Hinsdale Burritt, but its ultimate origin was unknown.
Properties.
Since 1943, this star has been consistently defined as a B0 main sequence star used as a reference for classifying the spectra of other stars on the MK scale, although in other studies it has been classified as O9V and O9.5V. The Galactic O-Star Spectroscopic Survey has defined it as the standard star for the O9.7 V spectral type.
In a 1981 paper, υ Orionis was observed to have nonradial pulsations over a period of around 12 hours, and has been classified as a Slowly pulsating B star. Subsequent review of Hipparcos catalog data indicated it was most likely a Beta Cephei variable, and is hence considered a candidate for that class. These are blue-white main sequence stars of around 10 to 20 times the mass of the Sun that pulsate with periods of 0.1 to 0.3 days; their changes in magnitude are much more pronounced in the ultraviolet than in the visual spectrum. It is classified as a Beta Cephei variable by the American Association of Variable Star Observers, and has an apparent magnitude of +4.62.
υ Orionis's parallax has been measured at 1.14 ±0.25, yielding a distance of approximately 3158 light years from Earth. A 1979 review of photometry of O and B stars found it to be around 1666 light-years distant, with a radius 7.2 times and luminosity 60,000 times that of the Sun, and surface temperature of 34347 K. and a mass 20 times that of the Sun. It is one of the most massive stars of the Orion OB1c Association (in Orion's Sword).


Theta Normae

θ Normae, Latinised as Theta Normae, is a binary star system in the constellation Norma. It has an apparent visual magnitude of 5.13 and is visible to the naked eye as a faint, blue-white hued point of light. Based upon an annual parallax shift of as seen from Earth, this system is located about 352 light years from the Sun. At that distance, the visual magnitude of these stars is diminished by an extinction of 0.45 due to interstellar dust.
Chini et al. (2012) identified this as a single-lined spectroscopic binary system. The visible component is a B-type main-sequence star with a stellar classification of B8 V. It is about 17 million tears old and is spinning rapidly with a projected rotational velocity of 251 km/s. The star has 3.6 times the mass of the Sun and 3.05 times the Sun's radius. It is radiating about 184 times the Sun's luminosity from its photosphere at an effective temperature of 12,341 K. This system displays an infrared excess, suggesting a debris disk is orbiting at a mean radius of with a temperature of 220 K.


Xi Herculis

Xi Herculis is a solitary star located within the northern constellation of Hercules. The star is visible to the naked eye with an apparent visual magnitude of 3.70. Based upon an annual parallax shift of 23.84 mas as seen from Earth, it is located 137 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.05 due to interstellar dust. It is a suspected member of the Sirius stream of co-moving stars.
This is an evolved G-type giant star with a stellar classification of G8 III. It is a red clump star, which means it is on the horizontal branch and generating energy through the thermonuclear fusion of hydrogen at its core. The star is emitting X-rays with a luminosity of in the 0.3–10 keV band. It has twice the mass of the Sun but, at the age of two and a half billion years, it has expanded to 10 times the Sun's radius. The star is radiating 51 times the solar luminosity from its photosphere at an effective temperature of 4,966 K.
Chinese name.
In R.H.Allen's , this star, together with ν Her and 99 Her (b Herculis) represent the state of Zhongshan (or Chung Shan' "the Middle Mountain"), but in Chinese literature, that names is applied to ο Her.


NGC 3003

NGC 3003 is a nearly edge-on barred spiral galaxy in the constellation of Leo Minor, discovered by William Herschel on December 7, 1785. It has an apparent visual magnitude of 11.78, at a distance of 19.5 Mpc from the Sun. It has a recessional velocity of 1474 km/s.
In 1961, a type II supernova with an apparent magnitude of 13.0 was detected within the galaxy, and was subsequently designated SN 1961F.


Kappa Ceti

The Bayer designation κ Ceti (Kappa Ceti) is shared by two stars in the constellation of Cetus:


Zeta Canis Majoris

Zeta Canis Majoris (ζ Canis Majoris, abbreviated Zeta CMa, ζ CMa), also named Furud , is a spectroscopic binary in the constellation of Canis Major.
Name.
"Zeta Canis Majoris" is the star's Bayer designation assigned by the German astronomer Johann Bayer in 1603.
The traditional name "Furud" or "Phurud" derives from the Arabic ألفرود "al-furūd" "the solitary ones". This was an appellation early Arab poets used for a number of anonymous stars. Later Arabian astronomers attempted to identify the name with particular stars, principally in the modern constellations Centaurus and Colomba. The stars of Colomba were assigned to Canis Majoris in the "Almagest", leading to more recent assignment of the name for Zeta Canis Majoris.
Al Sufi referred to these stars as ألأغربة "al-ʼaghribah" "the ravens".
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 "Furud" for this star.
Characteristics.
This star system has an apparent visual magnitude of +3.0, making it one of the brighter stars in the constellation and hence readily visible to the naked eye. Parallax measurements from the Hipparcos mission yield a distance estimate of around from the Sun. This is a single-lined spectroscopic binary system, which means that the pair have not been individually resolved with a telescope, but the gravitational perturbations of an unseen astrometric companion can be discerned by shifts in the spectrum of the primary caused by the Doppler effect. The pair orbit around their common center of mass once every 675 days with an eccentricity of 0.57.
The primary component is a large star with nearly four times the Sun's radius and almost eight times the mass of the Sun. It has a stellar classification of B2.5 V, which means it is a B-type main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. It is emitting 3,603 times the luminosity of the Sun and is a suspected Beta Cephei variable. This energy is being radiated from its outer envelope at an effective temperature of about 18,700 K, giving it the blue-white hue of a B-type star. It is relatively young for a star, with an estimated age of 32 million years.
Zeta Canis Majoris is located close to the solar antapex.