ASYMMETRIES IN THE ATMOSPHERE OF MIRA

被引：53

作者：

KAROVSKA, M ^{[1
]}

NISENSON, P ^{[1
]}

PAPALIOLIOS, C ^{[1
]}

BOYLE, RP ^{[1
]}

机构：

[1] VATICAN OBSERV,VATICAN CITY 00120,VATICAN

来源：

ASTROPHYSICAL JOURNAL | 1991年 / 374卷 / 02期

关键词：

INTERFEROMETRY; STARS; INDIVIDUAL; (OMICRON-CETI);

D O I：

10.1086/186069

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A two-dimensional high angular resolution study of o Ceti (Mira), carried out at four epochs from 1983 November to 1988 November using speckle interferometry techniques, detected asymmetries in the extended atmosphere of this pulsating star. The reconstructed speckle images show that the strength and the shape of this asymmetry changes as a function of wavelength and time. We determined the position angles of the major axes of the asymmetries at different epochs and measured accurately the axes as a function of wavelength. The origin of the observed asymmetries has not yet been identified. Plausible causes include instabilities in the pulsating atmosphere, nonspherical pulsation, or the interaction with the nearby companion.

引用

页码：L51 / L54

页数：4

共 22 条

[1]

BAIZE P, 1989, ASTRON ASTROPHYS SUP, V77, P497

[2] DISTRIBUTION OF DUST ABOUT OMICRON CETI AND ALPHA ORIONIS BASED ON 11 MICRON SPATIAL INTERFEROMETRY [J].

BESTER, M ;

DANCHI, WC ;

DEGIACOMI, CG ;

TOWNES, CH ;

GEBALLE, TR .

ASTROPHYSICAL JOURNAL, 1991, 367 (01) :L27-L31

[3]

BONNEAU D, 1982, ASTRON ASTROPHYS, V106, P235

[4]

BOWEN GH, 1988, APJ, V329, P241

[5]

BOYLE RP, 1986, ASTRON ASTROPHYS, V164, P310

[6]

BOYLE RP, 1991, COMMUNICATION

[7]

CELIS L, 1981, ASTRON ASTROPHYS, V99, P58

[8]

COYNE GV, 1988, POLARIZED RAD CIRCUM, P511

[9]

JOY AH, 1926, APJ, V63, P333

[10]

KAROUSKA M, 1990, BAAS, V21, P1117

← 1 2 3 →