Magnetic fields in AGB stars and (proto-) Planetary Nebulae

被引：0

作者：

Herpin, Fabrice ^{[1
,2
]}

Baudy, A. ^{[1
,2
]}

Josselin, E. ^{[3
]}

Thum, C. ^{[4
]}

Wiesemeyer, H. ^{[4
]}

机构：

[1] Univ Bordeaux, Lab Astrophys Bordeaux, F-33000 Bordeaux, France

[2] CNRS, INSU, UMR 5804, F-33271 Floirac, France

[3] Univ Montpellier 2, CNRS, ISTEEM, GRAAL, F-34095 Montpellier, France

[4] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France

来源：

COSMIC MAGNETIC FIELDS: FROM PLANETS, TO STARS AND GALAXIES | 2009年 / 259期

关键词：

Magnetic field; stars: evolution; radio lines: stars; ISM: molecules; SIO MASERS; OH MASER; POLARIZATION; PROTOPLANETARY; POLARIMETER; ENVELOPES; TELESCOPE; EMISSION; CN;

D O I：

10.1017/S1743921309030051

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

During its quick transition to the Planetary Nebula stage, the Asymptotic Giant Branch star will completely change its geometry. This AGB stellar evolution stage is characterized by a, high mass loss driven by the radiation pressure. Strong magnetic field amy rule the mass loss geometry and the global shaping of these objects. Following our previous work oil the polarization of the SiO maser emission in a representative sample of O-rich evolved stars, we present here a study towards C-rich objects and PPN/PN objects to obtain unbiased conclusions. Using Xpol at the IRAM-30 in telescope, we have conducted CN N=1-0 observations to investigate the Zeeman effect, in this molecule and draw conclusion on the evolution of the magnetic field and its influence during the transition of an AGB star to the PN stage. Following the analysis described by Crutcher et al. (1996) we derive an estimate of the magnetic field.

引用

页码：47 / +

页数：2

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