Investigating the missing link between disks around Pre Main Sequence and Main Sequence stars

Details Investigating the missing link between disks around Pre Main Sequence and Main Sequence stars Investigating the missing link between disks around Pre Main Sequence and Main Sequence stars

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7857l&link_type=abstract

HST Proposal ID #7857

Computer Science

Hst Proposal Id #7857 Hot Stars High-Mass Stars

Scientific paper

Various observations and models of the circumstellar {CS} disk around the Main Sequence {MS} IR excess star beta Pictors tend to show that the optically thin dust disk is the result of destruction processes among planetesimals. Such large bodies are also needed to explain the infall of ionized gaz toward the star. Dust disks around young Pre-Main Sequence {PMS} stars have also been evidenced. Theory predicts that these gas-rich disks are blown away before the star reaches the MS. In order to be consistent with the observation of disks around a large number of MS stars and with planetary formation theory, planetesimals should be already efficiently formed before the disk is dissipated. The evolved PMS stars give the missing link between young protoplaneta ry systems and evolved ones. One should expect those stars to be surrounded by a large population of planetesimals, able to substain an optically thin dust disk, such as the beta Pictoris one. To directly investigate the evolution of such CS environments, from PMS to MS stages, we propose to use the unique capabilities of HST- NICMOS in its coronographic mode to look for faint, optically thin disks around a few carefully selected PMS stars close to the MS. This will enable to test the nature and history o f this CS dust, in comparison to younger or older disks proto- types.

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