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HST Eclipse Studies of Magnetic CVs: Resolving the UV Hot Spot and Accretion Stream

Published online by Cambridge University Press:  12 April 2016

H.S. Stockman
H.S. Stockman*
Affiliation:
Space Telescope Science Institute1, 3700 San Martin Drive, Baltimore, MD 21218

Abstract

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Time-resolved photometry and spectroscopy of cataclysmic variables (CV) are powerful tools for clarifying the physical size, placement, and conditions of emission regions in these compact systems. We present HST time resolved UV spectroscopic data for one self-eclipsing mCV system, ST LMi, and two secondary eclipsing systems, DP Leo and UZ For. These observations clearly show the relative contributions of three emission components: the white dwarf, a hotter region surrounding the accretion shock, and the photoionized accretion stream. UZ For was observed in an unusually active state by both HST and EUVE. These data provide strong evidence that the accretion stream is “clumpy”, with overdensities 100–1000 times the average density. Using photoionization codes such as XSTAR and CLOUDY, we find that steady, supersonic, and homogenous flow in the UZ For accretion stream is unstable to compression heating. As a consequence, we propose a two-phase model for the stream and obtain density enhancements comparable to those deduced from the strengths of the UV emission lines and EUVE absorption features. Similar behavior may be expected from active, asynchronous magnetic CVs with coupling radii greater than several white dwarf radii.

Type
Part 9. Accretion Curtains and Funnels
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 396 - 402
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Bailey, J. & Cropper, 1991, MNRAS, 253, 27 CrossRefGoogle Scholar
Beuermann, K. 1988, in “Polarized Radiation of Circumstellar Origin”, ed. Coyne, C.V. et al. (Vatican City State: Vatican Observatory) 125.Google Scholar
Beuermann, K., Fischer, A., Rousseau, T. & Woelk, U., 1996, this workshop.Google Scholar
Cropper, M. & Horne, K. 1994, MNRAS, 267, 481 CrossRefGoogle Scholar
Dulk, G.A., & Marsh, K.A. 1982, ApJ, 259, 350 CrossRefGoogle Scholar
Frank, J., King, A.R., & Lasota, J.-P. 1988, A&A, 193, 113 Google Scholar
Kuijpers, J. & Pringle, J.E., 1982, A&A, 114, L4 Google Scholar
Lamb, D.Q. & Masters, A.R. 1978, ApJ, 234, 117 CrossRefGoogle Scholar
Paerels, F., Hur, M.Y., Mauche, C.W., & Heise, J. 1996, ApJ, 464, 884 CrossRefGoogle Scholar
Ramsay, G., Mason, K.O., Cropper, M., Watson, M.G. & Clayton, K.L. 1994, MNRAS, 270, 692 CrossRefGoogle Scholar
Robinson, C.R. & Cordova, F.A., 1994, ApJ, 437, 436 CrossRefGoogle Scholar
Stockman, H.S., Schmidt, G.D., Angel, J.R.P., Liebert, J., Tapia, S., & Beaver, E.A. 1977, ApJ, 217, 815 CrossRefGoogle Scholar
Stockman, H.S., Schmidt, G.D., Liebert, J., & Holberg, J.B. 1994, ApJ, 430, 323 CrossRefGoogle Scholar
Stockman, H. 1995 the Cape Workshop on Magnetic Cataclysmic Variables, ASP Conf. Series, eds. Buckley, D.A.H. & Warner, B., 85, 153 Google Scholar
Stockman, H.S., & Schmidt, G.D. 1996, ApJ, 468, 883 CrossRefGoogle Scholar
Woelk, U. & Beuermann, K. 1993, A&A, 280, 169 Google Scholar