Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1002.1864)
· References in the article
· Citations to the Article (21) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· Also-Read Articles (Reads History)
· Translate This Page
The standard model of star formation applied to massive stars: accretion discs and envelopes in molecular lines
Keto, Eric; Zhang, Qizhou
AA(Harvard-Smithsonian Center for Astrophysics, 160 Garden Street, Cambridge, MA 02420, USA), AB(Harvard-Smithsonian Center for Astrophysics, 160 Garden Street, Cambridge, MA 02420, USA)
Monthly Notices of the Royal Astronomical Society, Volume 406, Issue 1, pp. 102-111. (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
stars: individual: IRAS 20126+4104, stars: massive
Abstract Copyright:
(c) Journal compilation © 2010 RAS
Bibliographic Code:


We address the question of whether the formation of high-mass stars is similar to or differs from that of solar mass stars through new molecular line observations and modelling of the accretion flow around the massive protostar IRAS20126+4104. We combine new observations of NH3(1,1) and (2,2) made at the Very Large Array (VLA), new observations of CH3CN(13-12) made at the Submillimeter Array, previous VLA observations of NH3(3,3) and NH3(4,4) and previous Plateau de Bure observations of C34S(2-1), C34S(5-4) and CH3CN(12-11) to obtain a data set of molecular lines covering 15-419 K in excitation energy. We compare these observations against simulated molecular line spectra predicted from a model for high-mass star formation based on a scaled-up version of the standard disc-envelope paradigm developed for accretion flows around low-mass stars. We find that in accord with the standard paradigm, the observations require both a warm, dense, rapidly rotating disc and a cold, diffuse infalling envelope. This paper suggests that accretion processes around 10 Msolar stars are similar to those of solar mass stars.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints