Disappearance of stellar debris disks around main-sequence stars after 400 million years

H. J. Habing, C. Dominik, M. Jourdain de Muizon (), M. F. Kessler, R. J. Laureijs, K. Leech, L. Metcalfe, A. Salama, R. Siebenmorgen and N. Trams
Additional contact information
H. J. Habing: Leiden Observatory, PO Box 9513
C. Dominik: Leiden Observatory, PO Box 9513
M. Jourdain de Muizon: DESPA, Observatoire de Paris
M. F. Kessler: Vilspa PO Box 50727
R. J. Laureijs: Vilspa PO Box 50727
K. Leech: Vilspa PO Box 50727
L. Metcalfe: Vilspa PO Box 50727
A. Salama: Vilspa PO Box 50727
R. Siebenmorgen: Vilspa PO Box 50727
N. Trams: Vilspa PO Box 50727

Nature, 1999, vol. 401, issue 6752, 456-458

Abstract: Abstract Almost 5 billion years ago, the Sun formed in a local contraction of a cloud of molecular gas. A rotating disk of gas and dust is believed to have fed material onto the proto-Sun for the first few million years of its life, and to have formed the planets, comets and other Solar System objects. Similar disks, but with less mass, have been observed around a few main-sequence stars such as Vega1. The dust particles orbiting stars like Vega will be removed on timescales of the order of 1 Myr (Vega is about 350 Myr old), and therefore must be resupplied1, at least for a time. But earlier surveys2,3 lacked the sensitivity to determine how many nearby stars have dust disks, and to investigate how long such disks survive. Here we report infrared observations indicating that most stars younger than 300 Myr have dust disks, while most older than 400 Myr do not: ninety per cent of the disks disappear when the star is between 300 and 400 Myr old. Several events that are related to the ‘clean up’ of debris in the early history of our Solar System have a similar timescale.

Date: 1999
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DOI: 10.1038/46749

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