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Magnetic higher-mass stars in the early stages of their evolution

Published online by Cambridge University Press:  07 August 2014

Jason H. Grunhut  and
E. Alecian
Jason H. Grunhut
Affiliation:
ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany email: jgrunhut@eso.org
E. Alecian
Affiliation:
UJF-Grenoble 1 CNRS-INSU, IPAG, UMR 5274, Grenoble, F-38041, France email: evelyne.alecian@obs.ujf-grenoble.fr
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Abstract

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Over the past decade, significant investigations have been made through the use of high-resolution spectropolarimetry to probe the surface magnetic field characteristics of young higher-mass (M ≳ 1.5 M⊙) stars from pre-main sequence to zero-age main sequence evolutionary phases. The results of these observational campaigns suggest that these young higher-mass stars host similar magnetic properties to their main sequence descendants - strong, stable, globally-ordered fields that are detected in approximately 10 percent of all stars. This strongly contrasts with lower-mass stars, where it is generally accepted that a solar-like dynamo is in operation that generates more complex, globally-weak fields that are ubiquitous. The consensus is magnetic fields in higher-mass stars are fossil remnants of a magnetic field present in the molecular cloud, or generated very early during stellar formation. This review discusses the spectropolarimetric observations of higher-mass stars and how these observations have guided our current understanding of the magnetic characteristics of young higher-mass stars.

Keywords

stars: magnetic fieldsstars: ealry-typestars: pre–main-sequencestars: statisticstechniques: polarimetric

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