Nova Cygni 1975 - Wind and variations

Details Nova Cygni 1975 - Wind and variations Nova Cygni 1975 - Wind and variations

Sep 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mnras.180..749f&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 180, Sept. 1977, p. 749-754. Research supported by the IBM Corp.

Astronomy and Astrophysics

Astronomy

15

Novae, Periodic Variations, Stellar Magnitude, Stellar Radiation, Stellar Winds, Astronomical Models, Binary Stars, Companion Stars, Electron Scattering, Magnetohydrodynamic Flow, Photosphere

Scientific paper

A simple model is proposed to explain the approximately 3-hr periodic variations seen in the radiation from Nova Cygni 1975. The underlying binary system creates a spiral density variation in the outflowing wind. Such a spiral may persist to large radii and is then observable where it intersects the scattersphere. Period changes in the observed magnitude variations can naturally occur, without any change in the underlying binary period.

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