page_title: HD 28527
hierarchical_section_title: HD 28527
caption_attribution_description: English: This image shows the Hyades star cluster, the nearest cluster to us. The Hyades cluster is very well studied due to its location, but previous searches for planets have produced only one. A new study led by Jay Farihi of the University of Cambridge, UK, has now found the atmospheres of two burnt-out stars in this cluster — known as white dwarfs — to be “polluted” by rocky debris circling the star. Seeing evidence of asteroids points to the possibility of Earth-sized planets in the same system, as asteroids are the building blocks of major planets. Planet-forming processes are inefficient, and spawn many times more small bodies than large bodies — but once rocky embryos the size of asteroids are built, planets are sure to follow.
context_page_description: HD 28527 is a star in the constellation Taurus, and a member of the Hyades open cluster. It is faintly visible to the naked eye with an apparent visual magnitude of 4.78. The distance to this star, as determined from its parallax shift of 22 mas, is 148 light years. It is moving away from the Earth with a heliocentric radial velocity of +38 km/s.
  Based upon a stellar classification of A6 IV by Cowley et al., this is an A-type subgiant star that has consumed the hydrogen at its core and is evolving away from the main sequence. Older studies had it classed as an A-type main-sequence star with a class of A7 V. At the age of 307 million years, it has a high rate of spin, revolving upon its axis once every 1.278 days. It is a Delta Scuti variable with 1.75 times the mass of the Sun and 2.2 times the Sun's radius. The star is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,274 K.
  Due to its location near the ecliptic, this star is subject to lunar occultations. These events have provided occasional, but not definitive, evidence of a close secondary companion.
context_section_description: HD 28527 is a star in the constellation Taurus, and a member of the Hyades open cluster. It is faintly visible to the naked eye with an apparent visual magnitude of 4.78. The distance to this star, as determined from its parallax shift of 22 mas, is 148 light years. It is moving away from the Earth with a heliocentric radial velocity of +38 km/s.
  Based upon a stellar classification of A6 IV by Cowley et al. (1969), this is an A-type subgiant star that has consumed the hydrogen at its core and is evolving away from the main sequence. Older studies had it classed as an A-type main-sequence star with a class of A7 V. At the age of 307 million years, it has a high rate of spin, revolving upon its axis once every 1.278 days. It is a Delta Scuti variable with 1.75 times the mass of the Sun and 2.2 times the Sun's radius. The star is radiating 19 times the Sun's luminosity from its photosphere at an effective temperature of 8,274 K.
  Due to its location near the ecliptic, this star is subject to lunar occultations. These events have provided occasional, but not definitive, evidence of a close secondary companion. Eggleton and Tokovinin (2008) catalogue this as a possible triple star system, having the inner pair being similar stars with an angular separation of 0.02″, and the outer component a magnitude 6.7 star of class F2 at a much wider separation of 250″.
caption: Hyades cluster, with HD 28527 just NE of the θ Tauri pair (positions annotated in Commons)
exif: {"Image ImageDescription": "This image shows the Hyades star cluster, the nearest cluster to us. The Hyades cluster is very well studied due to its location, but previous searches for planets have produced only one. A new study led by Jay Farihi of the University of Cambridge, UK, has now found the atmospheres of two burnt-out stars in this cluster \u2014 known as white dwarfs \u2014 to be \u201cpolluted\u201d by rocky debris circling the star. Seeing  evidence of asteroids points to the possibility of Earth-sized planets  in the same system, as asteroids are the building blocks of major planets.  Planet-forming processes are inefficient, and spawn many times more  small bodies than large bodies \u2014 but once rocky embryos the size of  asteroids are built, planets are sure to follow."}