Inner Rim of A Molecular Disk Resolved in Infrared CO Lines

Details Inner Rim of A Molecular Disk Resolved in Infrared CO Lines Inner Rim of A Molecular Disk Resolved in Infrared CO Lines

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..381g&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Optics

Infrared, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Binary And Multiple Stars

Scientific paper

The disk around HD 141569 A is in transition from protoplanetary to debris disk with dust opacity at the inner most region being optically thin. Infrared spectroscopy of CO v = 2-1 with the adaptive optics system uncovered that the line emission is spatially extended up to 50 AU with a central clearing opened at r = 11 AU. The position velocity map is consistent with Keplerian rotation down to its inner truncation. The size of the inner cavity is apparently larger than the dust sublimation radius, or possible magnetospherical truncation. The inner cavity is about half of the nominal gravitational radius of the star (rg = 18 AU), which is more consistent with the latest photoevaporation model that takes into account the FUV irradiation and the gas pressure gradient. The photoevaporation must be the most natural explanation of the cavity formation in the case of HD 141569 A. In contrast to CO v = 2-1, the hydrogen recombination lines are broad (+/-300 km s-1 in FWZI) with clear double peaks implying that ionized gas is in a close orbit to the central star (r = 0.01 to 0.1 AU) inside the inner cavity of the molecular disk.

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