Add to ORKGA model of a radiatively driven, magnetohydrodynamic wind flow confined in theequatorial plane of the star is formulated and the basic eqations are preliminalily analyzed.It is shown that major singular points of the basic equations are slow magnetosonic, theAlfvenic and fast magnetosonic points. The two magnetosonic points are modified by theradiation terms. When the star does not rotate at a slower velocity than at its break-upvelocity, the slow magnetosonic point never exists outside the star
[[abstract]]We formulate the time-steady, axisymmetric problem of stellar magnetospheric inflow of g...
Axisymmetric stellar wind solutions are presented that were obtained by numerically solving the idea...
This is the final version of the article. Available from American Astronomical Society via the DOI i...
SEE ParentDocumentRecord|Ntt=19860015036 "NASA. Marshall Space Flight Center Research Reports: 1985 ...
Aims. We study the acceleration of the stellar winds of rapidly rotating low mass stars and the tran...
© 2012. The American Astronomical Society. This is the final published version of the work, which wa...
The hottest and most massive stars (spectral types O, B, Wolf-Rayet) have strong stellar winds that ...
A simplified model for the stationary, axisymmetric structure of magnetized winds with a polytropic ...
We present 2.5D stationary solar/stellar wind numerical simulation results obtained within the magne...
Final published version of article. Also available via the publisher website at: http://dx.doi.org/...
The article of record as published may be found at http://dx.doi.org/10.1086/163443A steady, axisymm...
The term “magnetosphere” originated historically from early spacecraft measurements of plasma trappe...
The topological analysis from Bjorkman (1995) for the standard model that describes the winds from h...
[[abstract]]We propose a generalized model for stellar spin-down, disk accretion, and truncation, an...
International audienceWe use two-dimensional axisymmetric magnetohydrodynamic simulations to compute...
[[abstract]]We formulate the time-steady, axisymmetric problem of stellar magnetospheric inflow of g...
Axisymmetric stellar wind solutions are presented that were obtained by numerically solving the idea...
This is the final version of the article. Available from American Astronomical Society via the DOI i...
SEE ParentDocumentRecord|Ntt=19860015036 "NASA. Marshall Space Flight Center Research Reports: 1985 ...
Aims. We study the acceleration of the stellar winds of rapidly rotating low mass stars and the tran...
© 2012. The American Astronomical Society. This is the final published version of the work, which wa...
The hottest and most massive stars (spectral types O, B, Wolf-Rayet) have strong stellar winds that ...
A simplified model for the stationary, axisymmetric structure of magnetized winds with a polytropic ...
We present 2.5D stationary solar/stellar wind numerical simulation results obtained within the magne...
Final published version of article. Also available via the publisher website at: http://dx.doi.org/...
The article of record as published may be found at http://dx.doi.org/10.1086/163443A steady, axisymm...
The term “magnetosphere” originated historically from early spacecraft measurements of plasma trappe...
The topological analysis from Bjorkman (1995) for the standard model that describes the winds from h...
[[abstract]]We propose a generalized model for stellar spin-down, disk accretion, and truncation, an...
International audienceWe use two-dimensional axisymmetric magnetohydrodynamic simulations to compute...
[[abstract]]We formulate the time-steady, axisymmetric problem of stellar magnetospheric inflow of g...
Axisymmetric stellar wind solutions are presented that were obtained by numerically solving the idea...
This is the final version of the article. Available from American Astronomical Society via the DOI i...