Hostname: page-component-7479d7b7d-q6k6v Total loading time: 0 Render date: 2024-07-08T05:52:14.851Z Has data issue: false hasContentIssue false
  • English
  • Français

Coronal Activity on Rapidly-Rotating Solar-Like Stars: Chandra Observations of ER Vul

Published online by Cambridge University Press:  26 May 2016

Alexander Brown ,
Joanna M. Brown ,
Rachel A. Osten ,
Thomas R. Ayres  and
Edward Guinan
Alexander Brown
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389, USA
Joanna M. Brown
Affiliation:
Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
Rachel A. Osten
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389, USA National Radio Astronomy Observatory, Charlottesville, VA 22903-2475, USA
Thomas R. Ayres
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389, USA
Edward Guinan
Affiliation:
Department of Astronomy, Villanova University, Villanova, PA 19085, USA

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.

We investigate the coronal structure of rapidly-rotating, solar-like stars using Chandra HETGS spectra of the short-period binary ER Vul, and by comparison with X-ray observations of the Sun and other dwarf stars. ER Vul consists of two solar-like (G0 + G5) dwarfs with rotation rates ~ 40 times that of the Sun. This binary is not interacting and these stars are the fastest rotating G dwarfs suitable for high resolution X-ray spectroscopy. X-ray (1.8-40 Å) spectra were obtained on 2001 March 29-30 along with 10.5 hours of simultaneous VLA monitoring at 3.6 and 20 cm. These spectra show hot, multi-temperature coronal emission with emission lines ranging in temperature from O VII (2 MK) to Fe XXIV (30 MK). ER Vul showed only low-level variability during the X-ray observation. Unlike the behaviour of longer period active binaries, no large, long-duration flares were detected, consistent with previous X-ray observations of this binary. No evidence for eclipses is seen in either the X-ray or radio emission. The coronal emission measure distribution and elemental abundances were derived for ER Vul.

Type
Session 3 Rotation, Solar and Stellar Physics
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 334 - 335
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Brown, et al. 2002, in Stellar Coronae in the Chandra and XMM-Newton Era, (eds. Favata, F. & Drake, J.), ASP Conf. Ser. 277, p. 223 Google Scholar
Hill, G., et al. 1990, A&A 238, 145 Google Scholar
Osten, R.A. & Brown, A. 2000, ApJ 515, 746 Google Scholar