Hostname: page-component-cd9895bd7-q99xh Total loading time: 0 Render date: 2024-12-26T04:31:52.707Z Has data issue: false hasContentIssue false
  • English
  • Français

The X-ray and EUV Turnoff of GQ Mus and V1974 Cyg

Published online by Cambridge University Press:  12 April 2016

S. Starrfield ,
J. Krautter ,
S. N. Shore ,
I. Idan ,
G. Shaviv  and
G. Sonneborn
S. Starrfield
Affiliation:
Dept. of Physics & Astronomy, Arizona State University, Tempe, AZ 85287, USA
J. Krautter
Affiliation:
Landessternwarte, Königstuhl, D69117, Heidelberg, Germany
S. N. Shore
Affiliation:
Dept. of Physics and Astronomy, Indiana University at South Bend, 1700 Mishawaka Ave, South Bend, IN 46634, USA
I. Idan
Affiliation:
Dept. of Physics, The Technion, 32000 Haifa, Israel
G. Shaviv
Affiliation:
Dept. of Physics, The Technion, 32000 Haifa, Israel
G. Sonneborn
Affiliation:
Lab. for Astr. and Solar Phys., Code 681, NASA Goddard Space Flight Center, Greenbelt, MD 20771, 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.

Both GQ Mus and V1974 Cyg were observed to turnoff in X-rays by ROSAT. The turnoff of V1974 Cyg was also observed with EUVE. GQ Mus was observed near the beginning of its outburst with EXOSAT and then 7 years later by ROSAT in the all-sky survey. Later ROSAT PSPC observations showed that its X-ray intensity was slowly declining with time and it was not detected in the last pointing that occurred in August 1993. We observed GQ Mus with IUE over the entire active phase of its outburst and found a change in the slope of the UV continuum around the time that the X-rays turned off. V1974 Cyg was observed by ROSAT throughout its entire active phase in X-rays which lasted about 18 months. V1974 Cyg was detected in the EUVE all-sky survey, but not in pointed observations that occurred in August 1993 (and June and November 1994). We use the measured times of the active phases to determine important properties of these two novae. For example, for V1974 Cyg we predict that more than 10−5M⊙ of helium rich material was left on the white dwarf when it returned to quiescence. For GQ Mus, ~ 10−4M⊙ was left on the white dwarf. These results imply that a significant amount of the helium seen in nova ejecta was produced in outbursts prior to the one that was just observed. They also imply that the mechanism which mixes core material into the ejecta must be efficient.

Type
VIII. Novae, X-ray Binaries
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 419 - 424
Copyright
Copyright © Kluwer 1996

References

Andreä, J., Drechsel, H., & Starrfield, S. 1994, A&A, 291, 869 Google Scholar
Austin, S.J., Wagner, R.M., Starrfield, S., Shore, S.N., Sonneborn, G., & Bertram, R. 1995, ApJ, in preparationGoogle Scholar
Crenshaw, D.M., Norman, D.J., & Bruegman, O.W. 1990, PASP, 102, 463 CrossRefGoogle Scholar
Hamuy, M., Phillips, M., & Williams, R.E. 1994, IAUC #5953Google Scholar
Hassell, B.J.M. et al., 1990, in Physics of Classical Nova, ed. Cassatella, A. & Viotti, R., Berlin: Springer-Verlag, NY, 202 Google Scholar
Iben, I. Jr. 1982, ApJ, 259, 244 Google Scholar
Idan, I., Starrfield, S., Shore, S., Krautter, J., Sonneborn, G., & Shaviv, G. 1995, Apj, in preparationGoogle Scholar
Krautter, J., et al., 1984, A&A, 137, 307 Google Scholar
Krautter, J., Ögelman, H., Starrfield, S., Wichmann, R. & Pfefferman, R., 1995, ApJ, in pressGoogle Scholar
Krautter, J. & Williams, R.E. 1989, ApJ, 341, 968 CrossRefGoogle Scholar
MacDonald, J., Fujmoto, M.Y., & Truran, J.W. 1985, ApJ, 294, 263 Google Scholar
Ögelman, H., Krautter, J., & Beuermann, K. 1987, A&A, 177, 110 Google Scholar
Ögelman, H., Orio, M., Krautter, J., & Starrfield, S. 1993, Nature, 361, 331 CrossRefGoogle Scholar
Paczynski, B. 1971, Acta Astron., 21, 271 Google Scholar
Péquignot, D., Petitjean, P., Boisson, C., & Krautter, J. 1993, A&A, 271, 219 Google Scholar
Prialnik, D. & Kovetz, A. 1984, ApJ, 281, 367 Google Scholar
Savage, B., & Mathis, J. 1979, ARAA, 17, 73 Google Scholar
Shanley, L., Ögelman, H., Gallagher, J.S., Orio, M., & Krautter, J. 1994, ApJL, 438, L95 Google Scholar
Shore, S.N., Sonneborn, G., Starrfield, S., Gonzelez-Riestra, R., & Ake, T.B. 1993, AJ, 106, 2408 Google Scholar
Shore, S.N., Sonneborn, G., Starrfield, S., Gonzelez-Riestra, R., & Polidan, R.S. 1994, ApJ, 421, 344 CrossRefGoogle Scholar
Starrfield, S. 1989, in Classical Novae, ed. Bode, M. and Evans, A.N., Wiley Press, New York, 39 Google Scholar
Starrfield, S. 1992, in Variability in Stars and Galaxies: Reviews in Modern Astronomy, 5, ed. Klare, G., Heidelberg: Springer-Verlag, 73 Google Scholar
Starrfield, S., Sparks, W.M., & Truran, J.W. 1974, ApJS, 28, 247 Google Scholar
Starrfield, S., Truran, J.W., Sparks, W.M., & Kutter, G.S. 1972, ApJ, 176, 169 Google Scholar
Starrfield, S., Truran, J., Sparks, W.M., & Krautter, J. 1991, in Extreme Ultraviolet Astronomy, ed. Malina, R., & Bowyer, S., 168 Google Scholar
Stringfellow, G., & Bowyer, C.S. 1995, in Proceedings EUVE IAU Colloquium, ed. Bowyer, S., Berkeley, CA, these proceedingsGoogle Scholar
Truran, J.W. 1982, in Essays in Nuclear Physics, ed. Barnes, C.A., Clayton, D.D., and Schramm, D.N., Cambridge, University Press, 467 Google Scholar