Phase-Dependent Observations of Intermediate Polars and The Broad Emission and Absorption Line Region in NGC 3516

Details Phase-Dependent Observations of Intermediate Polars and The Broad Emission and Absorption Line Region in NGC 3516 Phase-Dependent Observations of Intermediate Polars and The Broad Emission and Absorption Line Region in NGC 3516

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995stsc.rept.....k&link_type=abstract

Technical Report, Space Telescope Science Inst. Baltimore, MD United States

Physics

Dwarf Stars, Electromagnetic Spectra, White Dwarf Stars, Cataclysmic Variables, Magnetic Fields, X Rays, Pulse Amplitude, Main Sequence Stars, Magnetic Poles

Scientific paper

The Intermediate Polars (IP's) constitute a class of Cataclysmic Variables (CV's), which are binary star systems in which mass is transferred from a late-type main-sequence star to a white dwarf via Roche lobe overflow. In the IP's, the inner accretion disk is evidently disrupted by the magnetic field of the white dwarf. High-temperature shocks at the white dwarf's magnetic poles (where accretion occurs) produce X-rays, which are reprocessed into photons over a broad energy band across the electromagnetic spectrum. Because the white dwarf typically spins rapidly (rotation periods a few 10s to a few 100s of seconds), the signals due to both the X-rays and reprocessed photons are pulsed. The shape of the spectrum of pulse amplitude as a function of wavelength yields information about both the temperature and size of the pulse-emitting region. It has been noted by several investigators that the optical pulsation amplitudes rise steeply toward short wavelengths. It is therefore a fair surmise that pulsation amplitudes peak in the ultraviolet. The scientific goal of this project was to observe a representative sample of IP's, using IUE, in search of the expected strong UV pulsations, and hence to further our understanding of pulse-producing mechanisms.

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