Astronomy and Astrophysics – Astronomy
Scientific paper
May 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245.1009h&link_type=abstract
Astrophysical Journal, Part 1, vol. 245, May 1, 1981, p. 1009-1017.
Astronomy and Astrophysics
Astronomy
39
Flare Stars, Radio Sources (Astronomy), Stellar Radiation, Stellar Spectrophotometry, Ultraviolet Astronomy, Variable Stars, X Ray Sources, Chromosphere, Electron Density (Concentration), Heao, Iue, Stellar Atmospheres, Stellar Coronas, Stellar Spectra
Scientific paper
Results of coordinated program of observations in the X-ray, UV, optical and radio regions of the dM5e flare star Proxima Centauri are presented. Simultaneous observations of the star were obtained on March 6 and March 7, 1979, by the Einstein Observatory IPC, the IUE SWP and LWR cameras at low dispersion, three ground-based optical telescopes in Australia and the Parkes 64-m radio telescope. A total of 10 radio bursts and six optical flares was detected during three nights of simultaneous radio and optical observations, which appear to be broadly correlated. A major X-ray flare event was detected with temperatures of 1.7 x 10 to the 7th and 1.2 x 10 to the 7th K during the rise and decay phases, respectively, respective X-ray fluxes of 3.0 x 10 to the -11th and 3.7 x 10 to the -11th ergs/sq cm per sec, and changes in spectral flux distribution. No radio, optical or UV flare emission corresponding to the X-ray flare was detected. The X-ray flare is interpreted in terms of an arch model with cooling predominantly by X-ray radiation, with an electron density of 1.0 x 10 to the 11th/cu cm during the decay phase and a total arch length comparable to the size of the star itself. The X-ray flare observed is thus more similar to a typical strong solar flare than heretofore seen on a flare star.
Candy M.
Haisch Bernard M.
Harwood D.
Linsky Jeffrey L.
Nikoloff Isobel
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