Hostname: page-component-6bf8c574d5-956mj Total loading time: 0 Render date: 2025-02-20T14:54:36.643Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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 

References

Bouvier, J. 1990, AJ, 99, 946.CrossRefGoogle Scholar
Carpenter, J. M., Hillenbrand, L. A., & Skrutskie, M. F. 2001, AJ, 121, 3160.CrossRefGoogle Scholar
Cutri, R. M. et al. 2003, VizieR Online Data Catalog, 2246.Google Scholar
Damiani, F. & Micela, G. 1995, ApJ, 446, 341.CrossRefGoogle Scholar
Feigelson, E. D., Casanova, S., Montmerle, T., & Guibert, J. 1993, ApJ, 416, 623.CrossRefGoogle Scholar
Feigelson, E. D., Gaffney, J. A., Garmire, G., Hillenbrand, L. A., & Townsley, L. 2003, ApJ, 584, 911.CrossRefGoogle Scholar
Flaccomio, E., Damiani, F., Micela, G., Sciortino, S., Harnden, F. R., Murray, S. S., & Wolk, S. J. 2003, ApJ, 582, 398.CrossRefGoogle Scholar
Flaccomio, E., Micela, G., & Sciortino, S. 2003, A&A, 397, 611.Google Scholar
Gagné, M., Caillault, J., & Stauffer, J. R. 1995, ApJ, 445, 280.CrossRefGoogle Scholar
Getman, K. V., Feigelson, E. D., Townsley, L., Bally, J., Lada, C. J., & Reipurth, B. 2002, ApJ, 575, 354.CrossRefGoogle Scholar
Grosso, N., Montmerle, T., Bontemps, S., André, P., & Feigelson, E. D. 2000, A&A, 359, 113.Google Scholar
Kim, Y. & Demarque, P. 1996, ApJ, 457, 340.CrossRefGoogle Scholar
Lawson, W. A., Feigelson, E. D., & Huenemoerder, D. P. 1996, MNRAS, 280, 1071.Google Scholar
Neuhäuser, R., Sterzik, M. F., Schmitt, J. H. M. M., Wichmann, R., & Krautter, J. 1995, A&A, 297, 391.Google Scholar
Pizzolato, N., Maggio, A., Micela, G., Sciortino, S., & Ventura, P. 2003, A&A, 397, 147.Google Scholar
Preibisch, T. & Zinnecker, H. 2002, AJ, 123, 1613.CrossRefGoogle Scholar
Randich, S. 2000, in ASP Conf. Ser. Vol. 198: Stellar Clusters and Associations: Convection, Rotation, and Dynamos, ed. Pallavicini, R., Micela, G., & Sciortino, S. (San Francisco: ASP), 401.Google Scholar
Rebull, L. M. 2001, AJ, 121, 1676.CrossRefGoogle Scholar
Rebull, L. M., Hillenbrand, L. A., Strom, S. E., Duncan, D. K., Patten, B. M., Pavlovsky, C. M., Makidon, R., & Adams, M. T. 2000, AJ, 119, 3026.CrossRefGoogle Scholar
Stassun, K. G., Mathieu, R. D., Mazeh, T., & Vrba, F. J. 1999, AJ, 117, 2941.CrossRefGoogle Scholar
Stelzer, B. & Neuhäuser, R. 2001, A&A, 377, 538.Google Scholar
Wichmann, R. et al. 2000, A&A, 359, 181.Google Scholar