Alpha2 Canum Venaticorum Star
Wiley Book of Astronomy:
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Alpha2 Canum Venaticorum star
Alpha2 Canum Venaticorum star (α2 CVn star)
A type of rotating variable, also known as a spectrum variable, that consists of a main-sequence star of spectral type B8p to A7p with a strong magnetic field. α2 CVn stars have spectra with abnormally strong lines of silicon, strontium, chromium, and rare earths, the intensities of which vary with rotation. They also show magnetic field and brightness changes with periods of 0.5 to 160 days and visual amplitudes of 0.01 to 0.1 magnitude. It is thought the powerful magnetic field of an α2 CVn star gives rise to different compositions and brightness at different parts of the stellar surface, in the same way that the Sun's (much weaker) field produces sunspots. The prototype is the companion of Cor Caroli.
A type of rotating variable, also known as a spectrum variable, that consists of a main-sequence star of spectral type B8p to A7p with a strong magnetic field. α2 CVn stars have spectra with abnormally strong lines of silicon, strontium, chromium, and rare earths, the intensities of which vary with rotation. They also show magnetic field and brightness changes with periods of 0.5 to 160 days and visual amplitudes of 0.01 to 0.1 magnitude. It is thought the powerful magnetic field of an α2 CVn star gives rise to different compositions and brightness at different parts of the stellar surface, in the same way that the Sun's (much weaker) field produces sunspots. The prototype is the companion of Cor Caroli.
Oxford Dictionary of Astronomy:
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Alpha2 Canum Venaticorum Star
A type of main-sequence, extrinsic variable star; abbr. ACV. Stellar rotation produces brightness variations of 0.01–0.1 mag., accompanied by changes in the strengths of the spectral lines and the magnetic fields. The rotational periods range from 0.5 days to more than 160 days. The spectra (B8p–A7p) exhibit abnormally strong lines of silicon, strontium, chromium, and rare-earth elements. Stars in the ACVO subtype undergo non-radial pulsation (periods 0.004–0.01 days), with small (0.01-mag.) variations superimposed on the fluctuations caused by the rotation.
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