scholarly journals EXTRASOLAR GIANT MAGNETOSPHERIC RESPONSE TO STEADY-STATE STELLAR WIND PRESSURE AT 10, 5, 1, AND 0.2 au

2016 ◽  
Vol 827 (1) ◽  
pp. 77 ◽  
Author(s):  
Matt A. Tilley ◽  
Erika M. Harnett ◽  
Robert M. Winglee
Keyword(s):  
Steady State ◽  
Stellar Wind ◽  
Wind Pressure

scholarly journals Magnetic Braking and the Oblique Rotator Model

1970 ◽  
Vol 4 ◽  
pp. 269-273
Author(s):  
L. Mestel ◽  
C. S. Selley
Keyword(s):  
Magnetic Field ◽  
Steady State ◽  
Stellar Wind ◽  
Rotation Axis ◽  
Dynamical Evolution ◽  
Magnetic Star ◽  
Rotator Model ◽  
Oblique Rotator ◽  
Magnetic Braking

This work investigates the dynamical evolution of a rotating magnetic star which drives a stellar wind. The basic magnetic field of the star is supposed symmetric about an axis, which is inclined at an angle X to the rotation axis k (Figure 1). We adopt the familiar equations of an inviscid perfectly conducting gas. In a steady state, the velocity as seen in a frame rotating with the star is taken as

scholarly journals Radiative steady-state colliding stellar wind models: are they correct?

1998 ◽  
Vol 298 (4) ◽  
pp. 1021-1029 ◽  
Author(s):  
A. V. Myasnikov ◽  
S. A. Zhekov ◽  
N. A. Belov
Keyword(s):  
Steady State ◽  
Stellar Wind

Quasi-Steady Marching-on in Time Approximation Technique of Numerical Simulation of Wind Pressures on Building

2011 ◽  
Vol 105-107 ◽  
pp. 576-582 ◽  
Author(s):  
Zhi Xiang Yu ◽  
Yan Jun Yan ◽  
Hao Wu
Keyword(s):  
Steady State ◽  
Research Result ◽  
Steady State Solution ◽  
Tolerance Test ◽  
Wind Pressure ◽  
Turbulence Theory ◽  
Approximation Technique ◽  
Time Step ◽  
Nonlinear Simulation ◽  
Steady State Method

Abstract. In order to improve the convergence of nonlinear simulation of wind pressure on buildings by turbulence theory pattern, QSMA technique is proposed based on full implicit marching-on in time method in CFX. During marching-on in time, the unit time step and non-convergence tolerance test are employed to approximate the steady state solution in this technique. Comparing with the traditional method, the proposed technique can reduce the restriction for time step and requirement for the target tolerance significantly. It is mathematically proved that the time discretization scheme is stable and the error transfer tends to zero with QSMA technique. Through numerical analysis for flow around Marakami 3D cubic, the research result indicates that solution accuracy and time consumption of QSMA are consistent with traditional steady state method, but the convergence is better.

Radiative steady-state colliding stellar wind models: are they correct?

1998 ◽  
Vol 298 (4) ◽  
pp. 1021-1029 ◽  
Author(s):  
A. V. Myasnikov ◽  
S. A. Zhekov ◽  
N. A. Belov
Keyword(s):  
Steady State ◽  
Stellar Wind

scholarly journals Modeling magnetized star-planet interactions: boundary conditions effects

2013 ◽  
Vol 8 (S300) ◽  
pp. 330-334 ◽  
Author(s):  
Antoine Strugarek ◽  
Allan Sacha Brun ◽  
Sean P. Matt ◽  
Victor Reville
Keyword(s):  
Steady State ◽  
Boundary Conditions ◽  
Numerical Simulations ◽  
Stellar Wind ◽  
Stellar Surface ◽  
Numerical Studies ◽  
Rotational Evolution ◽  
Further Development ◽  
Steady State Solutions

AbstractWe model the magnetized interaction between a star and a close-in planet (SPMIs), using global, magnetohydrodynamic numerical simulations. In this proceedings, we study the effects of the numerical boundary conditions at the stellar surface, where the stellar wind is driven, and in the planetary interior. We show that is it possible to design boundary conditions that are adequate to obtain physically realistic, steady-state solutions for cases with both magnetized and unmagnetized planets. This encourages further development of numerical studies, in order to better constrain and undersand SPMIs, as well as their effects on the star-planet rotational evolution.

scholarly journals The domain of radiatively driven mass loss in the H-R diagram

1979 ◽  
Vol 83 ◽  
pp. 235-240 ◽  
Author(s):  
David C. Abbott
Keyword(s):  
Steady State ◽  
Mass Loss ◽  
Radiation Pressure ◽  
Effective Temperature ◽  
Stellar Wind ◽  
Radiation Force ◽  
Theoretical Uncertainty ◽  
Line Radiation ◽  
Consistent Model ◽  
Self Consistent

Previous work by Castor, Abbott, and Klein (1975) presented a self-consistent model of a steady-state stellar wind. They also showed qualitatively that for O stars at least a static atmosphere could not exist. This paper extends that result by calculating in detail the minimum luminosity as a function of effective temperature required for the line radiation force to exceed gravity. Within the observational and theoretical uncertainty there is a one-to-one correspondence between a star's calculated ability to self-initiate a stellar wind by radiation pressure alone and the observed presence of outflowing material in the UV resonance lines.

scholarly journals Stellar influence on heavy ion escape from unmagnetized exoplanets

2019 ◽  
Vol 486 (1) ◽  
pp. 1283-1291 ◽  
Author(s):  
Hilary Egan ◽  
Riku Jarvinen ◽  
David Brain
Keyword(s):  
Solar System ◽  
Stellar Wind ◽  
Extreme Ultraviolet ◽  
Dynamic Pressure ◽  
Extreme Environments ◽  
Heavy Ion ◽  
Wind Pressure ◽  
Field Orientation ◽  
Plasma Environment ◽  
Ion Escape

Abstract Planetary habitability is in part determined by the atmospheric evolution of a planet; one key component of such evolution is escape of heavy ions to space. Ion-loss processes are sensitive to the plasma environment of the planet, dictated by the stellar wind and stellar radiation. These conditions are likely to vary from what we observe in our own Solar system when considering a planet in the habitable zone around an M-dwarf. Here, we use a hybrid global plasma model to perform a systematic study of the changing plasma environment and ion escape as a function of stellar input conditions, which are designed to mimic those of potentially habitable planets orbiting M-dwarfs. We begin with a nominal case of a solar wind experienced at Mars today, and incrementally modify the interplanetary magnetic field orientation and strength, dynamic pressure, and Extreme Ultraviolet input. We find that both ion-loss morphology and overall rates vary significantly, and in cases where the stellar wind pressure was increased, the ion loss began to be diffusion or production limited with roughly half of all produced ions being lost. This limit implies that extreme care must be taken when extrapolating loss processes observed in the Solar system to extreme environments.

scholarly journals Stellar Wind Equations in a New Steady State

1988 ◽  
Vol 108 ◽  
pp. 156-157
Author(s):  
Mariko Kato
Keyword(s):  
Steady State ◽  
Mass Flow ◽  
Mass Flux ◽  
Stellar Wind ◽  
Continuity Equation ◽  
Variable Mass ◽  
Surface Region ◽  
Deep Interior ◽  
Spherically Symmetry

AbstractA set of equations of stellar wind in a new steady state in spherically symmetry is presented. This equations are available also for the deep interior of stars, whereas the usual equations can be applied only to the surface region. The new equations have a variable mass flux which becomes zero at the inner boundary of the mass flow. The velocity also reduces zerj), whereas it diverges at r=0 in the usual continuity equation 4∏r2ρ v=constant. In the surface region, the present equations approach the usual equations.

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