A two-component model for the corona of Lambda Andromedae

Details A two-component model for the corona of Lambda Andromedae A two-component model for the corona of Lambda Andromedae

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...169..178m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 169, no. 1-2, Nov. 1986, p. 178-184.

Astronomy and Astrophysics

Astrophysics

9

Andromeda Constellation, Binary Stars, Cool Stars, Plasma Radiation, X Ray Spectra, Late Stars, Stellar Coronas, Stellar Rotation

Scientific paper

The binary Lambda Andromedae (HD 222107) was studied with the low-energy (LE) and medium-energy (ME) X-ray detectors of Exosat on December 5, 1983 and on January 8, 1984, half a rotation period later. The ME data for the observations are compatible with emission from a plasma with a temperature of about 20 MK. If the strong variability in the hard X-ray flux is interpreted as due to rotational modulation the scale height of the hot plasma should be significantly smaller than the stellar radius. If the ME data are interpreted in terms of a model for quasi-static loops, the footpoints of these loops cover at most a few percent of the stellar surface, and the pressure of the hot plasma may exceed about 25 dyn/sq cm. The LE data require an additional, weaker contribution by a cooler component that does not vary significantly with time. A later observation of the object on August 6, 1984 shows no significant change in the two plasma components as inferred from the observations on January 8, 1984, when the same hemisphere of the primary star was observed.

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