DETECTION OF VIBRATIONALLY EXCITED CO IN IRC+10216

被引：12

作者：

Patel, Nimesh A. ^{[1
]}

Young, Ken H. ^{[1
]}

Bruenken, Sandra ^{[1
,2
]}

Menten, Karl M. ^{[3
]}

Thaddeus, Patrick ^{[1
]}

Wilson, Robert W. ^{[1
]}

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] Ecole Polytech Fed Lausanne, LCPM, SB ISIC, CH-1015 Lausanne, Switzerland

[3] Max Planck Inst Radio Astron, D-53121 Bonn, Germany

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2009年 / 691卷 / 01期

关键词：

circumstellar matter; radio lines: stars; stars: individual (IRC+10216); stars: late-type; submillimeter; LATE-TYPE STARS; MASER EMISSION; SIO MASERS; IRC &10216; EXCITATION; ENVELOPE; GHZ; C4H;

D O I：

10.1088/0004-637X/691/1/L55

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the Submillimeter Array we have detected the J = 3-2 and 2-1 rotational transitions from within the first vibrationally excited state of CO toward the extreme carbon star IRC+10216 (CW Leo). The emission remains spatially unresolved with an angular resolution of similar to 2 '' and, given that the lines originate from energy levels that are similar to 3100 K above the ground state, almost certainly originates from a much smaller (similar to 10(14) cm) sized region close to the stellar photosphere. Thermal excitation of the lines requires a gas density of similar to 10(9) cm(-3), about an order of magnitude higher than the expected gas density based on previous infrared observations and models of the inner dust shell of IRC+10216.

引用

页码：L55 / L58

页数：4

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