Dust evolution and gas dissipation in the protoplanetary disks

Details Dust evolution and gas dissipation in the protoplanetary disks Dust evolution and gas dissipation in the protoplanetary disks

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004asthe..97..216h&link_type=abstract

The Astronomical Herald (ISSN 0374-2466), Vol. 97, No. 4, p. 216 - 221 (2004)

Astronomy and Astrophysics

Astronomy

Protoplanetary Disks

Scientific paper

Recent progress of mid-infrared observations is revealing evolution of dust and gas in the protoplanetary disks in detail. In particular, detection of crystalline silicate dust in the protoplanetary disks is important not only as the origin of crystalline silicate dust in comets and meteorites, but also as a new probe to understand the planet formation process taking place in the protoplanetary disks. Furthermore, studies of gas in the protoplanetary disks are proceeding using pure rotational H2 emission lines in the mid-infrared. Here we introduce current observational studies of dust and gas in the protoplanetary disks using COMICS/Subaru.

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