Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic On-line Article (HTML)
· Table of Contents
· References in the Article
· Citations to the Article (1) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Links between Photospheric Activity and Formation of Circumstellar Structures of Be Stars
Authors:
Rivinius, T.
Publication:
Active OB-Stars: Laboratories for Stellare and Circumstellar Physics, ASP Conference Series, Vol. 361, Proceedings of the conference held 29 August - 2 September, 2005 at Hokkai-Gakuen University, Sapporo, Japan. Edited by S. Stefl, S. P. Owocki, and A. T. Okazaki. San Francisco: Astronomical Society of the Pacific, 2007., p.219
Publication Date:
03/2007
Origin:
ASP
Bibliographic Code:
2007ASPC..361..219R

Abstract

The circumstellar environment of Be stars is filled and shaped by the stars themselves through some still to be identified ejection process(es). Nevertheless the recent years have seen significant progress toward constraining these processes. In particular, it was shown that the two main candidates considered in the past decades, magnetic fields and nonradial pulsation, fall short of the goal aimed at, if considered as being the only contributor to this task. Only for a few stars a direct link between the photospheric activity and the ejected matter could be made. This includes the timing of the ejection of matter through pulsational beating, the observations of strongly blue-shifted short-lived absorption features, and transient V/R-variations. These variations possibly indicate orbiting inhomogeneities just after their ejection from the central star. However, multi periodic beating can be thoroughly excluded for some of the best investigated Be stars, and the direct observational evidence for magnetic ejections is sparser still. Single-mode pulsations alone are unable to transfer matter from a ``canonical model Be star'', i.e. an early type B star rotating at about 80 % of its critical rate; there is a substantial lack of energy and angular momentum. A traditional approach to solve this problem consists of adding new qualities such as binarity to the standard model, but such attempts have not led to overwhelming success. It seems much more promising to abolish the traditional quantitative barrier of 80 \ critical rotation, especially since recent calculations show this to be a viable - if not even necessary - option.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints