Magnetic coronae of active main-sequence stars

Moira Jardine, Jean-Francois Donati

Research output: Chapter in Book/Report/Conference proceedingConference contribution

1 Citation (Scopus)

Abstract

The coronal structure of main sequence stars continues to puzzle us. While the solar corona is relatively well understood, it has become clear that even stars of the same mass as the Sun can display very non-solar coronal behaviour, particularly if they are rapid rotators or in a binary system. At masses greater than and also less than that of the Sun, the non-solar internal structure appears to affect both the geometry and dynamics of the stellar corona and the nature of the X-ray and radio emission. In this talk I will describe some recent advances in our understanding of the structure of the coronae of some of the most active (and interesting) main sequence stars.

Original languageEnglish
Title of host publicationCOSMIC MAGNETIC FIELDS: FROM PLANETS, TO STARS AND GALAXIES
EditorsKG Strassmeier, AG Kosovichev, JE Beckman
Place of PublicationCAMBRIDGE
PublisherCambridge University Press
Pages357-362
Number of pages6
ISBN (Print)978-0-521-88990-2
DOIs
Publication statusPublished - 2009
Event259th Symposium of the International-Astronomical-Union - Puerto Santiago
Duration: 3 Nov 20087 Nov 2008

Conference

Conference259th Symposium of the International-Astronomical-Union
CityPuerto Santiago
Period3/11/087/11/08

Fingerprint

Dive into the research topics of 'Magnetic coronae of active main-sequence stars'. Together they form a unique fingerprint.

Cite this