Magnetism in the AM Herculis variable CW 1103+254

Details Magnetism in the AM Herculis variable CW 1103+254 Magnetism in the AM Herculis variable CW 1103+254

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271..735s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 15, 1983, p. 735-743.

Astronomy and Astrophysics

Astrophysics

72

Binary Stars, Dwarf Novae, Magnetic Stars, Variable Stars, Balmer Series, Emission Spectra, Stellar Mass, Stellar Spectrophotometry, White Dwarf Stars, Zeeman Effect

Scientific paper

Time-resolved spectropolarimetry and spectrophotometry of the recently discovered magnetic binary CW 1103+254 show Zeeman-split Balmer polarization and absorption features corresponding to a mean photospheric field on the white dwarf primary having a strength of (19 + or - 2) x 10 to the 6th gauss. The simple polarimetric and photometric behavior of this system gives very well determined values for the orbital inclination (69 deg) and latitude of the accreting magnetic pole (-56 deg). From this point of view, the polar field strength is estimated to be (30 + or - 5) x 10 to the 6th gauss. With the system geometry derived here, the extreme emission-line variations reported by Stockman et al. (1983) can be successfully modeled by accretion in a hollow cone where the velocities of infall and orbital motion dominate the observed kinematics. Mass transfer is seen to take place in a hollow funnel that is only loosely contained by the magnetic field near the secondary but proceeds in an increasingly collimated flow as the supersonic gas approaches the approximately 0.6 solar mass primary. It is considered very likely that line emission occurs throughout the system but reaches a maximum in output approximately midway between the two stars. The evidence indicates that the infalling material must follow a slightly spiral path, as the low-mass companion apparently lags the magnetic pole in its orbit.

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