scholarly journals The Effects of Alfven Waves and Radiation Pressure in Dusty Winds of Late‐Type Stars. II. Dust‐Cyclotron Damping

2006 ◽  
Vol 639 (1) ◽  
pp. 416-422 ◽  
Author(s):  
A. A. Vidotto ◽  
V. Jatenco‐Pereira
Keyword(s):  
Radiation Pressure ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Late Type

scholarly journals The Effects of Alfven Waves and Radiation Pressure in Dust Winds of Late‐Type Stars

2002 ◽  
Vol 576 (2) ◽  
pp. 976-981 ◽  
Author(s):  
D. Falceta‐Goncalves ◽  
V. Jatenco‐Pereira
Keyword(s):  
Radiation Pressure ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Late Type

Winds from Luminous Late‐Type Stars. I. The Effects of Nonlinear Alfven Waves

2000 ◽  
Vol 528 (2) ◽  
pp. 965-971 ◽  
Author(s):  
V. S. Airapetian ◽  
L. Ofman ◽  
R. D. Robinson ◽  
K. Carpenter ◽  
J. Davila
Keyword(s):  
Alfven Waves ◽  
Alfvén Waves ◽  
Late Type

Mass loss from Wolf-Rayet stars due to radiation pressure and Alfven waves

1993 ◽  
Vol 410 ◽  
pp. 732 ◽  
Author(s):  
L. C. Dos Santos ◽  
V. Jatenco-Pereira ◽  
R. Opher
Keyword(s):  
Mass Loss ◽  
Radiation Pressure ◽  
Alfven Waves ◽  
Alfvén Waves

scholarly journals Winds in late-type stars: Mechanisms of mass outflow

1981 ◽  
Vol 59 ◽  
pp. 187-212
Author(s):  
Jeffrey L. Linsky
Keyword(s):  
Shock Waves ◽  
Mass Loss ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Pressure Gradients ◽  
Late Type ◽  
Periodic Shock ◽  
Thermally Driven ◽  
Mass Outflow ◽  
Field Lines

AbstractFour basic mechanisms have been proposed to explain the acceleration of winds in late-type stars –– thermal pressure gradients, radiation pressure on circumstellar dust grains, momentum addition by Alfvén waves, and momentum addition by periodic shock waves. In this review I describe recent work in applying these mechanisms to stars, and consider whether these mechanisms can work even in principle and whether they are consistent with recent ultraviolet and X-ray data from the IUE and Einstein spacecraft. Thermally-driven winds are likely important for late-type dwarfs, where the mass loss rates are small, and perhaps also in G giants and supergiants, but they cannot operate alone in the K and M giants and supergiants. Radiatively-driven winds are probably unimportant for all cool stars, even the M supergiants with dusty circumstellar envelopes. In principle, Alfvén waves can accelerate winds to high speeds provided the field lines are initially open or forced open by some mechanism, but detailed calculations are needed. Magnetic reconnection is an interesting suggestion for an acceleration mechanism when the field lines are initially closed. For the Mras and semiregular variable supergiants, periodic shock waves provide a simple way of producing rapid mass loss. Thus we are making some progress in understanding mass loss mechanisms for the cool half of the H-R diagram.

scholarly journals Alfvén waves and radiation pressure in the winds of Wolf-Rayet stars

1995 ◽  
Vol 163 ◽  
pp. 166-167
Author(s):  
L. C. Dos Santos ◽  
V. Jatenco-Pereira ◽  
R. Opher
Keyword(s):  
Energy Flux ◽  
Radiation Pressure ◽  
Alfven Waves ◽  
Alfvén Waves

We recently showed that Alfvén waves acting jointly with radiation pressure in Wolf-Rayet winds can possibly solve the momentum problem (dos Santos, Jatenco-Pereira and Opher 1993a, 1993b). In these analyses, however, constant radiation luminosity as a function of the distance to the star was assumed. We impose here conservation of the energy flux and examine the effect on the radiation luminosity.

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