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Coronal activity in F-, G-, and K-type stars. II - Coronal structure and rotation
Einstein Observatory soft X-ray spectra for a sample of 34 late-typestars are analyzed in order to determine coronal temperatures andemission features per unit area at the stellar surface. No obviousrelation between coronal temperature and (B-V) color index could befound. Coronal temperature is dependent on stellar luminosity class. Thedata are discussed in terms of a model for static magnetic loops, andindications are found for a variety of coronae in which the sizes of thedominating loops range from more compact than loops in solar-activeregions to loops that are comparable to the pressure scale height (oreven greater). Despite observed structural differences, a single, strictrelation holds between X-ray surface flux density and the Ca II H + Kexcess flux density of these stars. Coronal activity and structure arenoted to be related to the stellar rotation rate.
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Balina |
| Sað Açýklýk: | 01h52m38.36s |
| Yükselim: | +02°29'53.8" |
| Görünürdeki Parlaklýk: | 7.529 |
| Uzaklýk: | 202.429 parsek |
| özdevim Sað Açýklýk: | 67.6 |
| özdevim Yükselim: | -16 |
| B-T magnitude: | 8.744 |
| V-T magnitude: | 7.63 |
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