Modelling stellar coronal magnetic fields

Moira Jardine, Jean-Francois Donati, Doris Arzoumanian, Aline de Vidotto

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


Our understanding of the structure and dynamics of stellar coronae has changed dramatically with the availability of surface maps of both star spots and also magnetic field vectors. Magnetic field extrapolations from these surface maps reveal surprising coronal structures for stars whose masses and hence internal structures and dynamo modes may be very different from that of the Sun. Crucial factors are the fraction of open magnetic flux (which determines the spin-down rate for the star as it ages) and the location and plasma density of closed-field regions, which determine the X-ray and radio emission properties. There has been recent progress in modelling stellar coronae, in particular the relative contributions of the field detected in the bright surface regions and the field that may be hidden in the dark star spots. For the Sun, the relationship between the field in the spots and the large scale field is well studied over the solar cycle. It appears, however, that other stars can show a. very different relationship.

Original languageEnglish
Title of host publicationPHYSICS OF SUN AND STAR SPOTS
EditorsDP Choudhary, KG Strassmeier
Place of PublicationCAMBRIDGE
PublisherCambridge University Press
Number of pages7
ISBN (Print)978-0-521-76062-1
Publication statusPublished - 2011
Event273th Symposium of the International-Astronomical-Union - Ventura
Duration: 22 Aug 201026 Aug 2010


Conference273th Symposium of the International-Astronomical-Union


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