The outer atmosphere of Procyon (Alpha CMi F5IV-V) - Evidence of supergranulation or active regions

Details The outer atmosphere of Procyon (Alpha CMi F5IV-V) - Evidence of supergranulation or active regions The outer atmosphere of Procyon (Alpha CMi F5IV-V) - Evidence of supergranulation or active regions

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.218..465j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 218, Feb. 1, 1986, p. 465-476.

Astronomy and Astrophysics

Astronomy

17

A Stars, Late Stars, Stellar Atmospheres, Stellar Spectrophotometry, Stellar Structure, X Ray Spectra, Dwarf Stars, Exosat Satellite, Heao 2, Radiant Flux Density, Scaling Laws, Spaceborne Astronomy, Stellar Models

Scientific paper

Observations made with the Einstein X-ray observatory and Exosat have shown Procyon (Alpha CMi) to have a measurable X-ray flux. The flux observed is similar to the upper limits previously reported. The interpretation of the X-ray data in the context of models made previously by Brown and Jordan (1981) based on spectra obtained with the IUE satellite. The X-ray data lead to a higher electron pressure than does the UV spectrum. These results support the conclusion by Brown and Jordan that the UV data cannot be reconciled with a hot corona in a spherically symmetric uniform model. Two types of models are explored; one in which the X-ray emission originates from an isothermal corona but the UV emission is restricted to limited regions of the disk, analogous to solar supergranulation structure; the other in which hot loop structures are embedded in a cool (T(e) of about 300,000 K) corona. Monitoring of Procyon to search for variability is urgently required to distinguish between these models. Some comparisons with the predictions of scaling laws are made. This hot isothermal coronal model agrees quite well with the predictions of Hearn's (1977) minimum flux model.

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