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What can X-rays tell us about accretion, mass loss and magnetic fields in young stars?

Published online by Cambridge University Press:  01 May 2007

Thierry Montmerle
Thierry Montmerle*
Affiliation:
Laboratoire d'Astrophysique de Grenoble, BP 53X, 38400 St Martin d'Hères, France email: montmerle@obs.ujf-grenoble.fr
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Abstract

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Until recently, X-rays from low-mass young stars (105–106 yr) were thought to be a universal proxy for magnetic activity, enhanced by 3-4 orders of magnitude with respect to the Sun, but otherwise similar in nature to all low-mass, late-type convective stars (including the Sun itself). However, there is now evidence that other X-ray emission mechanisms are at work in young stars. The most frequently invoked mechanism is accretion shocks along magnetic field lines (“magnetic accretion”). In the case of the more massive A- and B-type stars, and their progenitors the Herbig AeBe stars, other, possibly more exotic mechanisms can operate: star-disk magnetic reconnection, magnetically channeled shocked winds, etc. In any case, magnetic fields, both on small scale (surface activity) and on large scale (dipolar magnetospheres), play a distinctive role in the emission of X-rays by young stars, probably throughout the IMF.

Keywords

accretion disksline: identificationplasmasstars: activitystars: coronaestars: early-typestars: magnetic fieldsstars: pre–main-sequencestars: windsoutflowsX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 23 - 30
Copyright
Copyright © International Astronomical Union 2007

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