Emission feature lambda 3,470 of VV Puppis may be a cyclotron line

Details Emission feature lambda 3,470 of VV Puppis may be a cyclotron line Emission feature lambda 3,470 of VV Puppis may be a cyclotron line

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980natur.283..176m&link_type=abstract

Nature, vol. 283, Jan. 10, 1980, p. 176, 177.

Physics

4

Binary Stars, Cyclotron Frequency, Stellar Spectra, Dwarf Stars, Emission Spectra, H Lines, Line Spectra, Stellar Luminosity

Scientific paper

It is found that the observed emission feature at a wavelength of 3470 A may be a cyclotron line arising due to the accretion at a rate of 3 x 10 to the 11th g/s in the heated region with S = 5 x 10 to the 15th sq cm, d = 10 cm, n = 10 to the 14th per cu cm, and Te = 1,000,000 K above the surface of the degenerated dwarf with B = 3.1 x 10 to the 8th G. Several implications follow from this conclusion: Some of the energy emitted in the cyclotron line should be absorbed by the surface of the degenerated dwarf giving rise to a hot spot. The increase of the accretion rate leads to increasing temperature and concentration in the heated region. Variation of the cyclotron line with the orbital period 100 min may be expected. Finally, it may be possible to observe the cyclotron line in AM Her and AN Ursae Majoris spectra when they have low luminosity.

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