Stellar chromospheric temperatures

Details Stellar chromospheric temperatures Stellar chromospheric temperatures

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..91..157g&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 91, no. 1, March 1983, p. 157-165.

Astronomy and Astrophysics

Astrophysics

3

Abundance, Chromosphere, H Lines, Stellar Spectrophotometry, Stellar Temperature, Atmospheric Ionization, Electron Energy, Emission Spectra, Hydrogen, Line Spectra, Lyman Alpha Radiation, Magnesium, Spectral Energy Distribution

Scientific paper

The emission doublet 2800 Mg II of stellar chromospheric origin is always stronger than the emission in the Lα line of hydrogen. At the same time, the ratio of their fluxes, Q = F(Mg II)/F(Lα), varies over a wide range - from 2 up to 20 in stars of one and the same type. Assuming that both emission structures, 2800 Mg II and Lα, are excited in one and the same region of the chromosphere, an attempt is made to represent the ratio Q as a function of one physical parameter only - chromospheric electron temperature. Such an approach explains easily the observed behaviour of the ratio Q in different stars.

Affiliated with

Also associated with

No associations

Rating

Stellar chromospheric temperatures does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Stellar chromospheric temperatures, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stellar chromospheric temperatures will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1465775