BD+20°307

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 0.48 white dwarf on a wide (980 AU) orbit.

The dust that orbits around several hundred main-sequence stars is cold and comes from a Kuiper-belt analogous region. In the Solar System the ongoing collisions between asteroids generate a tenuous cloud of dust known as the zodiacal light. When the Solar System was young such collisions were more common and the rate of dust production was probably many times higher. Zodiacal dust around stars much younger than the Sun has been rarely found. Only a few main-sequence stars have revealed warm (>120 K) zodiacal dust.

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.

Spectroscopic binary Both stars of the close binary are considered to be solar-type stars that are slightly more massive than the Sun. The two stars differ in effective temperature by only ~250 K and have a mass ratio of 0.91. The two orbit a common center of mass every 3.42 days. Within the spectra of the two stars the Li lines show different equivalent widths. The Li 6707 Å line though weak is detected only from the primary star, suggesting that it is older than 1 Gyr. If so, the large amount of zodiacal dust around the binary must be from a very large and recent collision of planetesimals.

Dust cloud The dust cloud orbiting BD+20°307 has about 1 million times more dust than is orbiting the Sun. Furthermore, the dust is made up of extremely tiny particles, and its temperature is over 100 K, which is unusually high. It is hypothesized that, within the past few hundred thousand years and perhaps much more recently, these particles were formed by a collision between two bodies similar to Earth. "It's as if Earth and Venus collided," said Prof. Benjamin Zuckerman, UCLA professor of physics and astronomy. "Astronomers have never seen anything like this before. Apparently, major catastrophic collisions can take place in a fully mature planetary system." This hypothesis explains why the bulk of this dust has not spiraled into BD+20°307, or been pushed out by stellar winds yet. The National Science Foundation (NSF), NASA, Tennessee State University (TSU) and the State of Tennessee funded the work by Zuckerman and his collaborators.

Sun-like stars with hot dust As of 2006 there were seven Sun-like stars that have hot dust system at semi-major axis < 10 AU. These are

+ Sun-like Stars with hot dust disksStarStellar classificationDistance from Earth (ly)ConstellationDust (or debris) temperature (K)SystemDust (or debris) location (AU)Cool dust > 10 AUStellar age (Myr) Eta Corvi F2V 59 Corvus > 80 Unary < 3.5 yes 1,500 HD 113766 F3V 424 Centaurus ~440 Binary 1.8 yes ~10–16 BD+20°307 G0V ~300 Aries > 100 Binary 1 no > 1,000 Pi1 Ursae Majoris G1.5Vb 46.5 Ursa Major unknown Unary 0.23 yes 400 HD 12039 G3-5V 138 Cetus 110 close stellar companion 4–6 no 7.5–8 HD 69830 K0V 40.6 Puppis unknown 3 Neptune planets < 1 AU 1 no 2,000–5,000 HD 98800B K5Ve ~150 Crater unknown Binary 2.2 AU inner disk ~5.9 outer disk no 10

BD+20°307

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