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Stellar magnetic field
Wikipedia
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Wikipedia
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A stellar magnetic field is a magnetic field generated by the motion of conductive plasma inside a star. This motion is created through convection, which is ...
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Stellar magnetism: empirical trends with age and rotation
Oxford Academic
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Oxford Academic
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由 AA Vidotto 著作2014被引用 424 次 — Magnetic fields play an important role in stellar evolution. For low-mass stars, the magnetic field is believed to regulate stellar rotation from the early ...
STELLAR MAGNETISM PB | Oxford University Press (China)
牛津大學出版社
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牛津大學出版社
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STELLAR MAGNETISM PB ; 作者／編者：, : MESTEL ; 出版日期, : 12-03-2004 ; ISBN, : 978019-852672-8 ; 系列, : ; 級別, : ...
Stellar Magnetism (International Series of Monographs on ...
Amazon.com
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Amazon.com
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This book by one of the leading figures in stellar magnetism provides an authoritative survey of this rapidly developing field. Based on a lifetime of research, ...
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Stellar Magnetism | Oxford Academic
Oxford Academic
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Oxford Academic
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由 L Mestel 著作2003被引用 525 次 — Abstract. Most stars appear to show some degree of magnetic activity. For example, the varying magnetic field of the Sun shows up in the familiar sun-spot.
Stellar magnetism.
Harvard University
https://ui.adsabs.harvard.edu › abs
Harvard University
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由 L Mestel 著作1999被引用 525 次 — The following topics were dealt with: theoretical basis, applications, magnetism and convection, magnetic fields in stellar interiors, stellar dynamos, ...
Stellar Magnetism (Chapter 15)
Cambridge University Press & Assessment
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Cambridge University Press & Assessment
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In this chapter we provide a brief introduction to stellar magnetism, focussed on our own star. We begin in §15.1 with the sun itself.
Stellar Magnetism
Inspire HEP
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Inspire HEP
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The role of magnetic fields in governing the angular momentum evolution of solar-type stars. #1. Jerome Bouvier. (Oct, 2008). Published in: EAS Publ.Ser.
Stellar Magnetic Field - an overview
ScienceDirect.com
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ScienceDirect.com
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The stellar magnetic field B☆ is defined as a fraction of the kinetic energy of the wind (Begelman and Li, 1992):(4)σ=B☆2R☆2M˙v∞vrotv∞2.