Spectral behavior of AM Her and QQ Vul in high and intermediate states in the UV

Details Spectral behavior of AM Her and QQ Vul in high and intermediate states in the UV Spectral behavior of AM Her and QQ Vul in high and intermediate states in the UV

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ap%26ss.330..337s&link_type=abstract

Astrophysics and Space Science, Volume 330, Issue 2, pp.337-345

Astronomy and Astrophysics

Astrophysics

1

Accretion—Binaries: Close—Stars: Individual: Am Her—Qq Vul: Ultraviolet—Stars: Magnetic Fields—White Dwarfs

Scientific paper

We present low resolution UV spectra of two polar systems, AM Her and QQ Vul from the observations taken by the IUE (International Ultraviolet Explorer) of the period between 1978-1996 and 1983-1996 for both systems respectively, to accomplish a large scale study of what happens to the ultraviolet flux of C IV 1550 Å spectral line during different orbital phases. Two spectra for both systems showing the variations in line fluxes and line widths at different orbital phases in high and intermediate states are presented. We concentrated on calculating the line fluxes and line widths of C IV 1550 Å emission line originating in the accretion stream. Our results show that there is spectral variability for the aformentioned physical parameters at different times, similar to that known for the light curve (Heise and Verbunt, Astron. Astrophys. 189:112, 1988; Gansicke et al., Astron. Astrophys. 303:127, 1995; Kafka and Honeycutt, Astron. J. 125:2188K, 2003). We attribute it to the variations of both density and temperature as a result of changing the mass transfer rate (Hutchings et al., Astron. J. 123:2841H, 2002; King and Lasota, Astron. Astrophys. 140L:16K, 1984) which is responsible for this spectral variability. Also we found that the line fluxes of AM Her are greater than the line fluxes of QQ Vul, while the line widths of both systems are approximately the same.

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