Other
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.1002a&link_type=abstract
American Astronomical Society, 192nd AAS Meeting, #10.02; Bulletin of the American Astronomical Society, Vol. 30, p.827
Other
Scientific paper
The process of planet formation in our solar system had a time scale of order 10(7) to 10(8) years according to present models. During that epoch our system was a strong emitter of thermal IR radiation from the large surface area of dust reprocessing solar flux. This second-generation dust would have been produced by collisions and activity of planetesimals stirred into crossing orbits by the growing planets. beta Pictoris' and alpha Lyrae's dust disks are believed to be in evolutionary states corresponding to this period of ``heavy bombardment". We used photometry from ISO at 25 and 60 mu m to compare the circumstellar environments of A stars in two young groups, the Sco-Cen association with age ~ 10 Myr and IC 2602 with age ~ 30 Myr. The samples of stars in the clusters were chosen to resemble each other in luminosity and temperature, and the two clusters are approximately equally distant from earth. Both groups are old enough that remnant protostellar disks with first-generation grains have most likely disappeared. We detect optically thin far-IR emission well in excess of photospheric flux around stars in both clusters, with a significant decrease in the average 60 mu m flux density between ages of 10 and 30 Myr. These data support hypotheses that stars commonly have planetesimal-debris disks after their original protostellar gas+dust disks disperse, and that the density of second-generation dust declines with time as the parent planetesimals accrete into planets.
Angelova Anna M.
Backman Dana E.
Stauffer John R.
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