The boundary line in the H-R diagram for stellar chromospheres and the theory of convection

Details The boundary line in the H-R diagram for stellar chromospheres and the theory of convection The boundary line in the H-R diagram for stellar chromospheres and the theory of convection

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..560b&link_type=abstract

Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 560-566.

Astronomy and Astrophysics

Astrophysics

50

Chromosphere, Convection, Emission Spectra, Hertzsprung-Russell Diagram, Stellar Magnitude, Stellar Spectra, Ultraviolet Spectra, A Stars, G Stars, Iue, Line Spectra, Stellar Luminosity, Stellar Rotation, Supergiant Stars

Scientific paper

Ultraviolet emission-line spectra of A, F, and early G stars have been observed with the International Ultraviolet Explorer. For supergiants, classical chromospheric and transition-layer emission is seen only on the red side of the Cepheid instability strip. For luminosity classes III-V, chromospheric emission can be detected for spectral types F2 and later. For none of the A stars was normal chromospheric emission detected, regardless of their rotational velocities or peculiarities (i.e., Am or Ap).

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