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HD 805


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Magnetic structure in cool stars. XV - The evolution of rotation rates and chromospheric activity of giants
For cool giants and subgiants the observed dependence of rotationalvelocity and Ca II H and K line-core emission on color B-V isinterpreted in terms of changes in the moment of inertia by stellarevolution. Modeling of the rotational velocity during the evolution ofcool giants with masses between 2.0 and 3.0 solar masses, by taking intoaccount the change in the moment of inertia and assuming rigid-bodyrotation and conservation of angular momentum, describes the observeddecrease of v sin i with B-V. The computed evolution of the rotationalvelocity, together with the empirical relation between the Ca IIline-core emission and the rotation rate, explain the observed drop inthe Ca II line-core emission for giants at B-V = about 0.95. Forsubgiants with masses of about 1.5 solar mass, the change in the momentof inertia by itself cannot explain the observed v sin i distribution:there are indications of loss of angular momentum, presumably bymagnetic braking.

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Observation and Astrometry data

Constellation:Baleine
Right ascension:00h12m22.17s
Declination:-08°42'35.2"
Apparent magnitude:8.895
Distance:497.512 parsecs
Proper motion RA:46.9
Proper motion Dec:0.1
B-T magnitude:10.064
V-T magnitude:8.992

Catalogs and designations:
Proper Names   (Edit)
HD 1989HD 805
TYCHO-2 2000TYC 5261-331-1
USNO-A2.0USNO-A2 0750-00047611
HIPHIP 993

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