X-ray spectrum of Capella and its relation to coronal structure and ultraviolet emission

Details X-ray spectrum of Capella and its relation to coronal structure and ultraviolet emission X-ray spectrum of Capella and its relation to coronal structure and ultraviolet emission

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..233m&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 1, 1982, p. 233-239. Research supported by the Koninklijke Nederlandse Akademie

Astronomy and Astrophysics

Astronomy

58

Binary Stars, Stellar Coronas, X Ray Astronomy, X Ray Spectra, Abundance, Coronal Loops, Heao 2, Ultraviolet Radiation

Scientific paper

The binary system Capella has been observed on 1979 March 15 and on 1980 March 15-17, with the objective grating spectrometer on board the Einstein Observatory. The spectrum measured with the 1000 1/mm grating covers the range 5-30 A with a resolution less than 1 A. The spectra show evidence for a bimodal temperature distribution of emission measure in an optically thin plasma with one component about 5,000,000 K and the other one about 10,000,000 K. Spectral features can be identified with line emissions from O VIII, Fe XVII, Fe XVIII, Fe XXIV, and Ne X ions. Good spectral fits have been obtained assuming standard cosmic abundances. The data are interpreted in terms of emission from hot static coronal loops rather similar to the magnetic arch structures found on the sun. It is shown that the conditions for such a model can exist on Capella. Typical values of loop base pressure and half-length are derived for both temperature components and discussed in relation to UV observations.

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