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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)
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Astronomy Keywords:
stars: individual: IRAS 20126+4104, stars: massive
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(c) Journal compilation © 2010 RAS
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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.
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