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BD+20°307 is a close binary star system approximately 300 light-years away in the constellation Aries. The system is surrounded by a dusty ring, and probably orbited by a 0.48M☉ white dwarf on a wide (980 AU) orbit. An exceptionally large amount of warm, small, silicate dust particles around the solar-type star BD+20°307 (HIP 8920, SAO 75016) has been reported. The composition, quantity and temperature of the dust may be explained by recent, frequent or huge collisions between asteroids or other planetesimals whose orbits are being perturbed by a nearby planet.

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  • BD+20°307 (en)
  • BD+20 307 (fr)
  • BD +20°307 (ja)
  • BD +20˚307 (ko)
  • BD +20 307 (pl)
  • BD+20°307 (ru)
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  • BD+20°307 est un système stellaire binaire de la constellation du Bélier entouré d'un disque de débris chaud supposé avoir été causé par la collision de deux corps de taille planétaire. Sa magnitude apparente visuelle est de 9,01. Il est distant de ∼391 a.l. (∼120 pc) de la Terre et il se rapproche du système solaire avec une vitesse radiale héliocentrique de −12 km/s. (fr)
  • BD +20°307は、おひつじ座の方向に地球から300光年離れた所にある恒星である。太陽と非常に良く似たG型主系列星の連星である。 (ja)
  • BD +20도 307은 양자리 방향으로 지구로부터 약 300광년 떨어진 곳에 있는 쌍성이다. 쌍성 구성원 각각은 태양과 거의 비슷하지만, 질량은 태양보다 약간 더 무겁다. 둘은 3.42일 주기로 질량 중심을 공전하고 있다. (ko)
  • BD +20 307 – gwiazda spektroskopowo podwójna znajdująca się w gwiazdozbiorze Barana, ok. 391 lat świetlnych od Słońca. (pl)
  • BD+20°307 is a close binary star system approximately 300 light-years away in the constellation Aries. The system is surrounded by a dusty ring, and probably orbited by a 0.48M☉ white dwarf on a wide (980 AU) orbit. An exceptionally large amount of warm, small, silicate dust particles around the solar-type star BD+20°307 (HIP 8920, SAO 75016) has been reported. The composition, quantity and temperature of the dust may be explained by recent, frequent or huge collisions between asteroids or other planetesimals whose orbits are being perturbed by a nearby planet. (en)
  • BD +20°307 — близкая двойная система в созвездии Овна на расстоянии около 300 световых лет от Солнца. Обе звезды похожи на Солнце, только немного более массивны. Они обращаются вокруг общего центра масс с периодом 3,42 дня. Если бы ось вращения была перпендикулярна взгляду наблюдателя, то с Земли она была видна как затменная переменная типа W UMa. Однако, никакой переменности у звезды не наблюдается, следовательно, можно предположить, что система видна с полюса. (ru)
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  • http://commons.wikimedia.org/wiki/Special:FilePath/Colliding_planets.jpg
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