Chromospheric structure of cool carbon stars
A semiempirical chromospheric model is proposed for TX Psc which is a prototype for the N-type carbon stars. Observational data imply that the chromospheric temperature rise must begin at a low density, that the temperature gradient in the lower chromosphere must be steep, that partial redistributio...
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| Veröffentlicht in: | The Astrophysical journal 1989-10, Vol.345 (1), p.543-553 |
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| container_title | The Astrophysical journal |
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| creator | Luttermoser, Donald G. Johnson, Hollis R. Avrett, Eugene H. Loeser, Rudolf |
| description | A semiempirical chromospheric model is proposed for TX Psc which is a prototype for the N-type carbon stars. Observational data imply that the chromospheric temperature rise must begin at a low density, that the temperature gradient in the lower chromosphere must be steep, that partial redistribution must be employed in the Mg II calculation, and that the lower chromosphere is expanding away from the photosphere with a velocity of close to 50 km/s. The present model also shows that the microturbulent velocity is about 7 km/s at the temperature minimum region, dropping to 5 km/s in the chromosphere, and that the Lyman lines are optically thick in the chromosphere. |
| doi_str_mv | 10.1086/167929 |
| format | Article |
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Observational data imply that the chromospheric temperature rise must begin at a low density, that the temperature gradient in the lower chromosphere must be steep, that partial redistribution must be employed in the Mg II calculation, and that the lower chromosphere is expanding away from the photosphere with a velocity of close to 50 km/s. 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Observational data imply that the chromospheric temperature rise must begin at a low density, that the temperature gradient in the lower chromosphere must be steep, that partial redistribution must be employed in the Mg II calculation, and that the lower chromosphere is expanding away from the photosphere with a velocity of close to 50 km/s. The present model also shows that the microturbulent velocity is about 7 km/s at the temperature minimum region, dropping to 5 km/s in the chromosphere, and that the Lyman lines are optically thick in the chromosphere.</abstract><cop>Legacy CDMS</cop><pub>University of Chicago Press</pub><doi>10.1086/167929</doi><tpages>11</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 1989-10, Vol.345 (1), p.543-553 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_osti_scitechconnect_5021827 |
| source | NASA Technical Reports Server; Alma/SFX Local Collection |
| subjects | 640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources Astronomy Astrophysics ATMOSPHERES CARBON STARS CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS Earth, ocean, space EQUILIBRIUM Exact sciences and technology GIANT STARS LTE LYMAN LINES MAIN SEQUENCE STARS MATHEMATICAL MODELS Pre-main sequence objects, young stellar objects (yso's) and protostars (t tauri stars, orion population, herbig-haro objects, bok globules, bipolar outflows, cometary nebulae, etc.) RADIATION TRANSPORT RED GIANT STARS SPECTRA STAR MODELS STARS STELLAR ATMOSPHERES STELLAR CHROMOSPHERES STELLAR RADIATION |
| title | Chromospheric structure of cool carbon stars |
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