The low level of debris disk activity at the time of the Late Heavy Bombardment: a Spitzer study of Praesepe

Details The low level of debris disk activity at the time of the Late Heavy Bombardment: a Spitzer study of Praesepe The low level of debris disk activity at the time of the Late Heavy Bombardment: a Spitzer study of Praesepe

2009-03-24

arxiv.org/abs/0903.4193v1

Astrophys.J.697:1578-1596,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

22 pages, 14 figures, 9 tables, emulateapj format; Accepted for publication in The Astrophysical Journal

Scientific paper

10.1088/0004-637X/697/2/1578

We present 24 micron photometry of the intermediate-age open cluster Praesepe. We assemble a catalog of 193 probable cluster members that are detected in optical databases, the Two Micron All Sky Survey (2MASS), and at 24 micron, within an area of ~ 2.47 square degrees. Mid-IR excesses indicating debris disks are found for one early-type and for three solar-type stars. Corrections for sampling statistics yield a 24 micron excess fraction (debris disk fraction) of 6.5 +- 4.1% for luminous and 1.9 +- 1.2% for solar-type stars. The incidence of excesses is in agreement with the decay trend of debris disks as a function of age observed for other cluster and field stars. The values also agree with those for older stars, indicating that debris generation in the zones that emit at 24 micron falls to the older 1-10 Gyr field star sample value by roughly 750 Myr. We discuss our results in the context of previous observations of excess fractions for early- and solar-type stars. We show that solar-type stars lose their debris disk 24 micron excesses on a shorter timescale than early-type stars. Simplistic Monte Carlo models suggest that, during the first Gyr of their evolution, up to 15-30% of solar-type stars might undergo an orbital realignment of giant planets such as the one thought to have led to the Late Heavy Bombardment, if the length of the bombardment episode is similar to the one thought to have happened in our Solar System. In the Appendix, we determine the cluster's parameters via boostrap Monte Carlo isochrone fitting, yielding an age of 757 Myr (+- 36 Myr at 1 sigma confidence) and a distance of 179 pc (+- 2 pc at 1 sigma confidence), not allowing for systematic errors.

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