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Transience of Hot Dust around Sun‐like Stars

2007; IOP Publishing; Volume: 658; Issue: 1 Linguagem: Inglês

10.1086/510999

1538-4357

M. C. Wyatt, Rowan J. Smith, J. S. Greaves, Charles Beichman, G. Bryden, C. M. Lisse,

Astrophysics and Star Formation Studies

In this paper a simple model for the steady state evolution of debris disks due to collisions is developed and confronted with the properties of the emerging population of seven Sun-like stars that have hot dust at 10 AU (η Corvi and HD 72905); one has three Neptune mass planets at <1 AU (HD 69830); all exhibit strong mid-IR silicate features. We consider the most likely origin for this transient dust to be a dynamical instability that scattered planetesimals inward from a more distant planetesimal belt in an event akin to the late heavy bombardment in our own system, the dust being released from such planetesimals in collisions and sublimation.