Studying the massive accretion disk candidate in IRAS18089-1732

Details Studying the massive accretion disk candidate in IRAS18089-1732 Studying the massive accretion disk candidate in IRAS18089-1732

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007atnf.prop..873b&link_type=abstract

ATNF proposal C1687, Semester: April, 2007

Physics

Stellar, Atca

Scientific paper

The understanding of accretion processes and specifically of massive accretion disks is considered the holy grail in high-mass star formation. We propose to study the recently identified massive accretion disk candidate IRAS18089-1732 at high angular resolution (<0.7'') in the highly excited NH3(4,4) and (5,5) lines. These lines trace only the densest and warmest regions and are hence well suited to isolate the accretion disk from its envelope. The proposed observation will reveal the kinematic structure of the inner rotating entity and likely allow us to differentiate whether the expected disk is in Keplerian rotation, like their low-mass counterparts, or not. Furthermore, the chosen line pair is a very good tool to investigate the temperature structure of the dense inner core. Combining the temperature information with the kinematic structure and the density profile determined from previous submm continuum observations, we will derive a detailed physical model of this young massive star-forming region.

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