A hybrid β Cephei-SPB star in a binary system:: γ Pegasi

被引：21

作者：

Chapellier, E ^{[1
]}

Le Contel, D ^{[1
]}

Le Contel, JM ^{[1
]}

Mathias, P ^{[1
]}

Valtier, JC ^{[1
]}

机构：

[1] Observ Cote Azur, Dept GEMINI, UMR 6203, F-06304 Nice 4, France

来源：

ASTRONOMY & ASTROPHYSICS | 2006年 / 448卷 / 02期

关键词：

stars : binaries : spectroscopic; stars : oscillations; stars : individual : beta Cephei; stars : variables : general;

D O I：

10.1051/0004-6361:20053815

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

High resolution and high signal to noise ratio spectroscopic observations of the classical beta Cephei star gamma Peg were obtained between 1991 and 2005. The analysis of these data combined with previously published results shows that. Peg is a spectroscopic binary with an orbital period of 370.5 d. We discovered three new frequencies in addition to the well-known 6.5897 d(-1) (0.15175 d) one. That at 6.01 d-1 is a typical beta Cephei frequency. The two others at 0.68 and 0.87 d(-1) are similar to the high degree g-mode frequencies found in SPB stars. Thus, gamma Peg is a hybrid beta Cephei-SPB star. Its position in the HR diagram is compatible with such a status. In addition, a small increase of the main period has been detected between the 1995 and 2005 observations.

引用

页码：697 / U107

页数：7

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