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X-ray Emission from Young Stars in Suburban Orion

Published online by Cambridge University Press:  26 May 2016

K. Briggs ,
M. Güdel ,
M. Audard ,
K. Smith ,
R. Mewe  and
T. den Boggende
K. Briggs
Affiliation:
Paul Scherrer Institut, Villigen PSI, CH 5232, Switzerland
M. Güdel
Affiliation:
Paul Scherrer Institut, Villigen PSI, CH 5232, Switzerland
M. Audard
Affiliation:
Columbia Astrophysics Laboratory, New York, NY 10027, USA
K. Smith
Affiliation:
Max-Planck-Institut für Radioastronomie, D-53121, Bonn, Germany
R. Mewe
Affiliation:
SRON, 3584 CA, Utrecht, The Netherlands
T. den Boggende
Affiliation:
SRON, 3584 CA, Utrecht, The Netherlands

Abstract

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X-ray emission from > 100 pre-main sequence (PMS) stars in the Orion star-forming complex is studied in a 20-ks observation by XMM-Newton. No relation between the ratio of X-ray and bolometric luminosities, LX/Lbol, and rotation period or Rossby number is exhibited, though the action of a solar-like dynamo is not excluded because all stars would appear to be in the “saturated regime” of such a dynamo. Low-mass stars showing a strong U — V excess have lower median X-ray luminosity, suggesting that accretion suppresses magnetic activity.

Type
Part 5: Stellar Magnetic Activity and Evolution
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 228 - 232
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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