SiO MASERS IN ASYMMETRIC MIRAS. II. R CANCRI

被引：6

作者：

Cotton, W. D. ^{[1
]}

Ragland, S. ^{[2
]}

Pluzhnik, E. A. ^{[3
]}

Danchi, W. C. ^{[4
]}

Traub, W. A. ^{[5
]}

Willson, L. A. ^{[6
]}

Lacasse, M. G. ^{[7
]}

机构：

[1] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[2] WM Keck Observ, Kamuela, HI 96743 USA

[3] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[5] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[6] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA

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

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2009年 / 185卷 / 02期

关键词：

radio lines: stars; stars: AGB and post-AGB; stars: atmospheres; VARIABLE TX CAM; LATE-TYPE STARS; EVOLVED STARS; MASS-LOSS; EMISSION; AGB; INTERFEROMETER; TELESCOPE;

D O I：

10.1088/0067-0049/185/2/574

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This is the second paper in a series of multi-epoch observations of the SiO masers at 7 mm wavelength in several asymptotic giant branch stars from a sample of Mira variable stars showing evidence of asymmetric structure in the infrared. These stars have been observed interferometrically in the infrared by the Infrared Optical Telescope Array and with Very Long Baseline Array measurements of the SiO masers. In this paper, we present the observations of R Cancri (R Cnc). The systemic velocity of R Cnc is estimated to be 15.8 +/- 0.2 km s(-1). A comparison is made with the model calculations of Gray et al. which predict some but not all observed features.

引用

页码：574 / 585

页数：12

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