Computer Science
Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8205g&link_type=abstract
HST Proposal ID #8205
Computer Science
Hst Proposal Id #8205 Young Stars And Circumstellar Material
Scientific paper
Models for the formation of the Solar System predict that an intermediate stage in planet formation was the assembly of material in the disk into planetesimals, and that this should be a common step in the evolution of planetary systems. Planetesimals are difficult to detect directly except by activity in renewing the small grain population in mature {e.g. t>100 Myr} planetary disks, or by the presence of cometary activity. Cometary activity can provide a marker for the presence of planetesimals in younger systems where much of the dust is a remnant of the original protoplanetary disk. The presence of such cometary activity has been inferred from redshifted absorption features in the optical & UV spectra of Beta Pic and a large number of younger, intermediate-mass pre- Main Sequence stars. However, if the interpretation of these features as the aggregate comae of swarms of star-grazing bodies is correct, similar activity must be present and remotely detectable in the disk s of young, solar analogs. We propose using HST STIS to obtain the first UV spectroscopic observations of infall activity in the disks of young, Solar- type stars, supplemented by a comparison intermediate- mass star. The data will be used to determine whether infall activity around young Suns evolves on the same time scale as for disks around more massive and luminous stars.
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