dc.contributor.author |
Mallik, S. G. V |
|
dc.date.accessioned |
2008-09-24T14:46:23Z |
|
dc.date.available |
2008-09-24T14:46:23Z |
|
dc.date.issued |
1986-09 |
|
dc.identifier.citation |
Monthly Notices of Royal Astronomical Society, Vol. 222, No. 2, pp. 307 - 322 |
en |
dc.identifier.issn |
0035-8711 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/3883 |
|
dc.description.abstract |
The radiative transfer problem in non-LTE moving atmospheres has been explicitly solved for Hα line profiles. These computations have been done for a schematic model of the line-forming region over a wide range of optical depths and velocity gradients in order to cover the observed characteristics in 23 G and K supergiants. The best theoretical fits yield optical depths in the range 10 - 500 and velocity fields in the range 0.5 - 3 Doppler widths. The computed mass-flow rates lie in the range 10-5 - 10-7M_sun;yr-1; the higher the extent of the line-forming region, the lower the mass-loss rates. The effect of the extent on the Hα emission components has also been investigated in some detail. The temperature sensitivity of the mass-loss rates has been considered in an approximate manner. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Royal Astronomical Society |
en |
dc.relation.uri |
http://adsabs.harvard.edu/abs/1986MNRAS.222..307M |
en |
dc.subject |
Chromosphere |
en |
dc.subject |
G stars |
en |
dc.subject |
H alpha line |
en |
dc.subject |
K stars |
en |
dc.subject |
Late stars |
en |
dc.subject |
Radiative transfer |
en |
dc.subject |
Stellar mass ejection |
en |
dc.subject |
Supergiant stars |
en |
dc.subject |
Computational astrophysics |
en |
dc.subject |
Line shape |
en |
dc.subject |
Stellar models |
en |
dc.subject |
Temperature dependence |
en |
dc.subject |
Thermodynamic equilibrium |
en |
dc.title |
Expanding chromospheres of late G and K supergiants |
en |
dc.type |
Article |
en |