Activity modulation of Capella as observed in He I 10830 A

Details Activity modulation of Capella as observed in He I 10830 A Activity modulation of Capella as observed in He I 10830 A

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..205s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 205-210.

Astronomy and Astrophysics

Astrophysics

15

Binary Stars, Helium Ions, Infrared Spectra, Stellar Activity, F Stars, G Stars, Late Stars, Stellar Atmospheres

Scientific paper

High dispersion CCD spectra in the region of the chromospheric infrared line He I 10830 A of the binary system of Capella have been analyzed over several orbital periods. It is concluded that the He I line is formed in the G-type primary component of the system, which is generally considered to be the less active component. These observations suggest that a relatively small hot region exists in the atmosphere of the G-type component, whose position relative to the orbit does not vary. The most probable explanation of this is that the axial rotation of the primary component is synchronous with the orbital motion, in contrast to that of the more rapidly rotating secondary component. This interpretation is consistent with the values of v sin i and the observed angular diameters of the two components, and gives 104 days for the rotational period of the primary. This implies also that the nature and the efficiency of the synchronization mechanism differs between the primary and the secondary. For example, the components may differ from each other with respect to the depth of the convective envelope.

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