Radiation pressure-driven shocks in winds from hot stars

1985 ◽  
Vol 298 ◽  
pp. 660 ◽  
Author(s):  
J. H. Krolik ◽  
J. C. Raymond
Keyword(s):  
Radiation Pressure ◽  
Hot Stars ◽  
Pressure Driven

scholarly journals Radiation-pressure-driven dust waves inside bursting interstellar bubbles

2014 ◽  
Vol 566 ◽  
pp. A75 ◽  
Author(s):  
B. B. Ochsendorf ◽  
S. Verdolini ◽  
N. L. J. Cox ◽  
O. Berné ◽  
L. Kaper ◽  
...  
Keyword(s):  
Radiation Pressure ◽  
Pressure Driven

scholarly journals A Hot Corona Model for O-Stars and WR Stars

1982 ◽  
Vol 99 ◽  
pp. 209-213
Author(s):  
W. Robbrecht ◽  
C. de Loore ◽  
G. Olson
Keyword(s):  
Radiation Pressure ◽  
Slow Component ◽  
Energy Sources ◽  
X Rays ◽  
Stored Energy ◽  
Atmospheric Models ◽  
Hot Stars ◽  
Two Component ◽  
Hot Corona ◽  
Radiation Cooling

Atmospheric models are presented for the outer layers of hot stars, O, of and Wolf-Rayet stars. The model is a two component hybrid model, consisting of a rapidly expanding component and a slower component. for the rapidly expanding component the energy sources are radiation pressure, a deposit of internally generated and stored energy, and radiation cooling. In this way a coronal layer with temperatures of the order of 4–7 million K is generated, with an extent of 1 to 2 stellar radii. The mass loss rates range between 10−6 and 10−4 Mo yr−1. The stellar wind velocity at infinity is of the order of 4000 km s−1. It is assumed that this rapid component interacts with the slow component, and gives rise to shocks. The corona as well as the shocks generated by the interaction of the two components can explain the observed X-rays.

scholarly journals Atmospheric parameters and accelerations in the outer parts of luminous hot stars

1989 ◽  
Vol 113 ◽  
pp. 287-288
Author(s):  
Hans Nieuwenhuijzen ◽  
Cornells de Jager
Keyword(s):  
Radiation Pressure ◽  
Dynamic Pressure ◽  
Great Part ◽  
Hydrostatic Equilibrium ◽  
Stellar Winds ◽  
Gravitational Acceleration ◽  
Atmospheric Parameters ◽  
Hot Stars ◽  
Plane Parallel ◽  
Turbulent Pressure

In the atmospheres of the most extreme luminous stars, close to the Humphreys-Davidson limit, the inward gravitational acceleration is for a great part compensated by outward accelerations due to radiation pressure, turbulent pressure and dynamic pressure of the stellar winds. As a result the effective acceleration is very small, resulting in blown-up atmospheres that can no longer be considered plane-parallel or in hydrostatic equilibrium.

scholarly journals A Novel Jet Model: Magnetically Collimated, Radiation-Pressure Driven Jet

2010 ◽  
Vol 62 (5) ◽  
pp. L43-L47 ◽  
Author(s):  
Shun Takeuchi ◽  
Ken Ohsuga ◽  
Shin Mineshige
Keyword(s):  
Radiation Pressure ◽  
Pressure Driven

scholarly journals Radiation Pressure-Driven Plasma Surface Dynamics in Ultra-Intense Laser Pulse Interactions with Ultra-Thin Foils

2018 ◽  
Vol 8 (3) ◽  
pp. 336 ◽  
Author(s):  
Bruno Gonzalez-Izquierdo ◽  
Remi Capdessus ◽  
Martin King ◽  
Ross Gray ◽  
Robbie Wilson ◽  
...  
Keyword(s):  
Laser Pulse ◽  
Radiation Pressure ◽  
Intense Laser ◽  
Surface Dynamics ◽  
Intense Laser Pulse ◽  
Plasma Surface ◽  
Thin Foils ◽  
Pressure Driven
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