CS LINE PROFILES IN HOT CORES

被引：5

作者：

Bayet, E. ^{[1
]}

Yates, J. ^{[1
]}

Viti, S. ^{[1
]}

机构：

[1] UCL, Dept Phys & Astron, London WC1E 6BT, England

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 728卷 / 02期

关键词：

astrochemistry; ISM: molecules; line: profiles; methods: numerical; stars: formation; submillimeter: general; RADIATIVE-TRANSFER PROBLEMS; GHZ SPECTRAL SURVEY; MASS STAR-FORMATION; ORION-KL; MOLECULAR CORES; CLOUD CORES; MODELS; EMISSION; DENSITY; REGIONS;

D O I：

10.1088/0004-637X/728/2/114

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a theoretical study of CS line profiles in archetypal hot cores. We provide estimates of line fluxes from the CS(1-0) to the CS(15-14) transitions and present the temporal variation of these fluxes. We find that (1) the CS(1-0) transition is a better tracer of the Envelope of the hot core whereas the higher-J CS lines trace the ultracompact core (UCC); (2) the peak temperature of the CS transitions is a good indicator of the temperature inside the hot core; (3) in the Envelope, the older the hot core the stronger the self-absorption of CS; (4) the fractional abundance of CS is highest in the innermost parts of the UCC, confirming the CS molecule as one of the best tracers of very dense gas.

引用

页数：10

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