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Hard X-ray Observations of Magnetic Cataclysmic Variables

Published online by Cambridge University Press:  12 April 2016

K. P. Singh ,
V. R. Rana ,
K. Mukerjee ,
P. Barrett  and
E. M. Schlegel
K. P. Singh
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai 400005, INDIA
V. R. Rana
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai 400005, INDIA
K. Mukerjee
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai 400005, INDIA
P. Barrett
Affiliation:
Space Telescope Science Institute, ESS/Science Software Group, Baltimore, M D 21218, U.S.A.
E. M. Schlegel
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, U.S.A.

Abstract

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Hard X-ray light curves and spectral parameters from our analysis of X-ray data of five AM Her type systems – V2301 Oph, V1432 Aql, EP Draconis, GG Leonis, & V834 Cen, and one intermediate polar – TV Col, observed using the Rossi X — ray Timing Explorer (RXTE) satellite are presented. A new improved ephemeris has been derived for V2301 Oph using the mid-eclipse timings. Average intensity variations, without any change of shape of the light curve or hardness ratio, are observed on timescales of a few days to a few months in V2301 Oph. V1432 Aql shows erratic variations on a timescale of a day, at least two sharp dips near orbital phases 0.35 and 0.5, and a total eclipse. Hard X-ray eclipses are also reported in EP Dra and GG Leo. V834 Cen shows intensity variations on yearly timescale and is found to be in a low state in 2002. In TV Col, a binary orbital modulation at 5.5h, in addition to the spin period of 1910s, is reported for the first time. Maximum spectral temperatures in Polars have been determined and used to estimate the masses of the white dwarfs.

Type
Part 3. A. Accretion Plasma diagnostics - Observations
Information
International Astronomical Union Colloquium , Volume 190: Magnetic Cataclysmic Variables , 2004 , pp. 135 - 141
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

Augusteijn, T., Heemskerk, M. H. M., Zwarthoed, G. A. A., & van Paradijs, J. 1994, A&AS, 107, 219 (A94)Google Scholar
Bailey, J., Axon, D. J., Hough, J. H., Watts, D. J., Giles, A. B., & Greenhill, J. G., 1983, MNRAS, 205, 1P (B83)Google Scholar
Barrett, P., O’Donoghue, D., & Warner, B. 1988, MNRAS, 233, 759 (BDW)Google Scholar
Barwig, H., Ritter, H., & Bärnbantner, O., 1994, A&A, 288, 204 (BRB)Google Scholar
Burwitz, V., Reinsch, K., Schwope, A. D. (+7 co-authors), 1998, A&A, 331, 262 (Bur98)Google Scholar
Cropper, M., 1990, Space Sci.Rev., 54, 195 (C90)CrossRefGoogle Scholar
Done, C., Osborne, J. P., & Beardmore, A. P., 1995, MNRAS, 276, 483.CrossRefGoogle Scholar
Geckeler, R. D. & Staubert, R., 1997, A&A, 325, 1070 (GS)Google Scholar
Hellier, C., 1993, MNRAS, 264, 132 (H93)CrossRefGoogle Scholar
Hessman, F. V., Beuermann, K., Burwitz, V., de Martino, D., & Thomas, H. C., 1997, A&A, 327, 245 (Hess97)Google Scholar
Jensen, K. A., Nousek, J. A., & Nugent, J. J., 1982, ApJ, 261, 625 (JNJ)Google Scholar
Mason, K. O., Middleditch, J., Cordova, F. A., Jensen, K. A., Reichert, G., Murdin, P. G., Clark, D., & Bowyer, S., 1983, ApJ, 264, 575 (M83)CrossRefGoogle Scholar
Norton, A. J., Beardmore, A. P. & Taylor, P., 1996, MNRAS, 280, 937 Google Scholar
Patterson, J., 1994, PASP, 107, 307 Google Scholar
Patterson, J., Skillman, D. R., Thorstensen, J. & Hellier, C., 1995, PASP, 107, 307 (P95)Google Scholar
Ramsay, G., 1997, MNRAS, 290, 99 CrossRefGoogle Scholar
Remillard, R. A., Stroozas, B. A., Tapia, S. & Silber, A., 1991, ApJ, 379, 715 (RSTS)CrossRefGoogle Scholar
Retter, A., Hellier, C., Augusteijn, T., Naylor, T., Bedding, T. R., Bembrick, C., McCormick, J., Velthuis, F., 2003, MNRAS, 340, 679 (R03)Google Scholar
Schlegel, E. M., 1999, AJ, 117, 2494 (S99)Google Scholar
Schmidt, G. D., & Stockman, H. S., 2001, ApJ, 548, 410 (SS)Google Scholar
Schwope, A. D., & Mengel, S., 1997, Astron. Nachr., 318, 25 (SM).CrossRefGoogle Scholar
Schwope, A. D., Thomas, H. C., Beuermann, K., & Reinsch, K., 1993, A&A, 267, 103 (S93)Google Scholar
Silber, A. D., Remillard, R. A., Horne, K. A. & Bradt, H. V. 1994, ApJ, 424, 955(SRHB)CrossRefGoogle Scholar
Steiman-Cameron, T. Y., & Imamura, J. N., 1999, ApJ, 515, 404 (SI)Google Scholar
Szkody, P., Armstrong, J., & Fried, R., 2000, PASP, 112, 228 (SzOO).Google Scholar
Watson, M. G., Rosen, S. R., O’Donoghue, D. (+6 co-authors), 1995, MNRAS, 273, 681. (W95)Google Scholar