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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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观测天体数据

星座:鯨魚座
右阿森松:00h12m22.17s
赤纬:-08°42'35.2"
视星:8.895
距离:497.512 天文距离
右阿森松适当运动:46.9
赤纬适当运动:0.1
B-T magnitude:10.064
V-T magnitude:8.992

目录:
适当名称   (Edit)
HD 1989HD 805
TYCHO-2 2000TYC 5261-331-1
USNO-A2.0USNO-A2 0750-00047611
HIPHIP 993

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