The Relationship between Ultraviolet Line Emission and Magnetic Field Strength in Magnetic Cataclysmic Variables

Details The Relationship between Ultraviolet Line Emission and Magnetic Field Strength in Magnetic Cataclysmic Variables The Relationship between Ultraviolet Line Emission and Magnetic Field Strength in Magnetic Cataclysmic Variables

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aj....117.1014h&link_type=abstract

The Astronomical Journal, Volume 117, Issue 2, pp. 1014-1022.

Astronomy and Astrophysics

Astronomy

4

Stars: Binaries: Close, Stars: Novae, Cataclysmic Variables, Stars: Individual: Alphanumeric: Re J0531-46, Stars: Individual: Alphanumeric: Re 1149+28, Stars: Individual: Alphanumeric: Re J1844-74, Stars: Individual: Constellation Name: Qs Telescopii, Stars: Individual: Constellation Name: Hu Aquarii, Stars: Individual: Constellation Name: Pq Geminorum, Stars: Individual: Constellation Name: Ef Eridani, Stars: Individual: Constellation Name: Bl Hydri, Stars: Individual: Constellation Name: Mr Serpentis, Sta

Scientific paper

We present the first UV spectral observations of six magnetic cataclysmic variables discovered by the ROSAT Wide Field Camera (WFC). Using the^ International Ultraviolet Explorer (IUE), 1200-3400 Å spectra were obtained of the AM Herculis stars RE 0531-46, RE 1149+28, RE 1844-74, QS Tel (RE 1938-46), and HU Aqr (RE 2107-05) and the DQ Herculis star PQ Gem (RE 0751+14). The high-state UV spectra are dominated by strong emission lines. Continuum flux distributions for these stars (from 100 to 5500 Å) reveal that over this entire range, none of the spectral energy distributions can be fitted by a single-valued blackbody. Our new UV observations and additional archival IUE spectra were used to discover a correlation between the strength of the high-state UV emission lines and the strength of the white dwarf magnetic field. Model spectral results are used to confirm the production of the UV emission lines by photoionization from X-ray and EUV photons.

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