Magnetism in Cool Evolved Stars: the M giants EK Bootis and β Pegasi

被引：0

作者：

Georgiev, S. ^{[1
,2
,3
]}

Konstantinova-Antova, R. ^{[1
,2
]}

Lebre, A. ^{[3
]}

Auriere, M. ^{[4
]}

Charbonnel, C. ^{[4
,5
]}

Palacios, A. ^{[3
]}

Drake, N. ^{[6
,7
,8
]}

Bogdanovski, R. ^{[1
,2
]}

机构：

[1] Bulgarian Acad Sci, Inst Astron, Sofia 1784, Bulgaria

[2] Bulgarian Acad Sci, NAO, Sofia 1784, Bulgaria

[3] Univ Montpellier, LUPM, UMR 5299, CNRS, Pl Eugene Bataillon, F-34095 Montpellier, France

[4] Univ Toulouse, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France

[5] Univ Geneva, Dept Astron, Chemin Maillettes 51, CH-1290 Versoix, Switzerland

[6] St Petersburg State Univ, Lab Observat Astrophys, Univ Ski Pr 28, St Petersburg 198504, Russia

[7] MCTIC, Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil

[8] MCTIC, Lab Nacl Astrofis, Rua Estados Unidos 154, BR-37504364 Itajuba, Brazil

来源：

BULGARIAN ASTRONOMICAL JOURNAL | 2020年 / 33卷

基金：

俄罗斯基础研究基金会;

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a long-term spectropolarimetric study of the active M giants EK Bootis (M5III) and beta Pegasi (M2.5II-III). For each star, the variability of the disk-averaged longitudinal component of the magnetic field (B-l) is shown, along with the behavior of different spectral activity indicators. The possible nature of the secondary component of EK Boo is discussed. We compare the observed variations in the activity proxies of each of the two giants and discuss possible physical explanations for the structure of their respective magnetic fields. For both objects, observations in linear polarisation are also presented and briefly discussed.

引用

页码：87 / 98

页数：12

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