Ultraviolet observations of cool stars. IV - Intensities of Lyman-alpha and MG II in epsilon Pegasi and epsilon Eridani, and line width-luminosity correlations

Details Ultraviolet observations of cool stars. IV - Intensities of Lyman-alpha and MG II in epsilon Pegasi and epsilon Eridani, and line width-luminosity correlations Ultraviolet observations of cool stars. IV - Intensities of Lyman-alpha and MG II in epsilon Pegasi and epsilon Eridani, and line width-luminosity correlations

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202..733m&link_type=abstract

Astrophysical Journal, vol. 202, Dec. 15, 1975, pt. 1, p. 733-740. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

50

Cool Stars, Emission Spectra, K Stars, Late Stars, Line Spectra, Stellar Evolution, Ultraviolet Spectra, Atmospheric Radiation, Calcium, Chromosphere, Giant Stars, Lyman Spectra, Radiant Flux Density, Spectral Line Width, Stellar Luminosity, Stellar Spectra

Scientific paper

A spectrometer on the Copernicus satellite has been used to confirm the existence of a line width-luminosity relation for the Ly-alpha and Mg II 2800-A chromospheric emission lines in K-type stars by observation of a K2 dwarf (epsilon Eri) and a K2 supergiant (epsilon Peg). Combined with previously reported observations of lines in three K giants (alpha Boo, alpha Tau, and beta Gem), the data are consistent with an identical dependence of line width on absolute visual magnitude for the Ca II K, Ly-alpha, and Mg II 2795-A lines. Surface fluxes of Ly-alpha, Mg II 2800-A, and O V 1218-A (upper limit) for epsilon Eri, and of Mg II 2800-A for epsilon Peg are also compared with values reported previously for the three giant stars.

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