Spectroscopic Evidence for Mass Loss from CH Cygni

Details Spectroscopic Evidence for Mass Loss from CH Cygni Spectroscopic Evidence for Mass Loss from CH Cygni

Jan 1969

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1969ap%26ss...3..205f&link_type=abstract

Astrophysics and Space Science, Volume 3, Issue 1, pp.205-213

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

Some high-dispersion spectrograms of CH Cygni taken in epochs at which only the M6 spectrum is visible and after the explosions of June 1967 and July 1968 have been studied. The strong negative radial velocities of the Ca ii chromospheric absorptions and the turbulent motions broadening the emission, lines of Hi, He i, Fe ii, [Fe ii] prove that mass is lost from the star at a rate of the order of 10-8 solar masses per year. Arguments are given in favour of the hypothesis that CH Cygni is a close binary composed of an M giant and a blue unstable subdwarf.

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