Mhd waves in stellar winds and accretion disks
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| Formato: | Artículo científico |
| Lenguaje: | en |
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Universidad Nacional Autónoma de México
2000
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| _version_ | 1876451662268203008 |
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| author | M. J. Vasconcelos |
| author_facet | M. J. Vasconcelos |
| contents | Mhd waves in stellar winds and accretion disks M. J. Vasconcelos V. Jatenco Pereira R. Opher Física, Astronomía y Matemáticas MHD TYPE STARS: PRE STARS: LATE STARS: EARLY Alfven waves have been used to explain the heating of stellar coronae andthe production of stellar winds in many regions of the Hertzsprung-Russell (HR)diagram. The waves were used as a major acceleration mechanism in the wind ofprotostars, late-type stars, early-type stars and in the solar wind. They are also veryimportant in the creation of inhomogeneities in the wind of early-types stars viathermal instability. On the other hand, Alfvenic heating generated by nonlinear andturbulent damping can be an important source of energy for ionizing protostellardisks, enabling angular momentum transport to occur through the Balbus-Hawleyinstability (BHI). We analysed the role of the damping of Alfven waves in the innerand intermediate regions of protostellar disks (0:1 < R(AU) < 1:4). We show thatwhen viscous dissipation is insucient to ensure the necessary degree of ionizationfor BHI to occur, the damping of Alfven waves can be an alternative source ofenergy for ionization. 2000 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57100918 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Vol.9 |
| format | Artículo científico |
| id | redalyc_57100918 |
| institution | Redalyc |
| language | en |
| publishDate | 2000 |
| publisher | Universidad Nacional Autónoma de México |
| spellingShingle | Mhd waves in stellar winds and accretion disks M. J. Vasconcelos Física, Astronomía y Matemáticas MHD TYPE STARS: PRE STARS: LATE STARS: EARLY Mhd waves in stellar winds and accretion disks M. J. Vasconcelos V. Jatenco Pereira R. Opher Física, Astronomía y Matemáticas MHD TYPE STARS: PRE STARS: LATE STARS: EARLY Alfven waves have been used to explain the heating of stellar coronae andthe production of stellar winds in many regions of the Hertzsprung-Russell (HR)diagram. The waves were used as a major acceleration mechanism in the wind ofprotostars, late-type stars, early-type stars and in the solar wind. They are also veryimportant in the creation of inhomogeneities in the wind of early-types stars viathermal instability. On the other hand, Alfvenic heating generated by nonlinear andturbulent damping can be an important source of energy for ionizing protostellardisks, enabling angular momentum transport to occur through the Balbus-Hawleyinstability (BHI). We analysed the role of the damping of Alfven waves in the innerand intermediate regions of protostellar disks (0:1 < R(AU) < 1:4). We show thatwhen viscous dissipation is insucient to ensure the necessary degree of ionizationfor BHI to occur, the damping of Alfven waves can be an alternative source ofenergy for ionization. 2000 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57100918 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Vol.9 |
| title | Mhd waves in stellar winds and accretion disks |
| topic | Física, Astronomía y Matemáticas MHD TYPE STARS: PRE STARS: LATE STARS: EARLY |
| url | https://www.redalyc.org/articulo.oa?id=57100918 |