The coronal line spectrum of AS 295

Details The coronal line spectrum of AS 295 The coronal line spectrum of AS 295

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202l..41h&link_type=abstract

Astrophysical Journal, vol. 202, Nov. 15, 1975, pt. 2, p. L41-L45. NSF-supported research.

Astronomy and Astrophysics

Astrophysics

14

Coronas, Giant Stars, Line Spectra, Stellar Luminosity, Stellar Spectra, Emission Spectra, H Alpha Line, Helium, Hydrogen, K Stars, Light Curve, Luminous Intensity, Novae, Oxygen, Radial Velocity

Scientific paper

AS 295 was discovered originally as a twelfth magnitude star having H-alpha in emission. It has now been found that the twelfth magnitude star at that position is a normal K giant and that the emission spectrum actually originates in a much fainter star 3 sec distant (here called AS 295 B), which in addition to bright lines of H, He I, He II, and O I shows a number of the stronger coronal lines. The two stars have quite different radial velocities and are probably only aligned. Upon examination of the Maria Mitchell and Harvard plate collections, AS 295 B was found to have undergone a hitherto undetected nova-like outburst in 1965. However, the persistence of its coronal spectrum 10 years later is unprecedented among the novae that have shown coronal lines, although it may be related to the fact that AS 295 B is the slowest nova of the group.

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