Journal ArticleDOI
The Angular Momentum of the Solar Wind
Edmund J. Weber,Leverett Davis +1 more
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Steady state model of solar wind flow in equatorial plane solved for radial and azimuthal motions, taking into account pressure gradient, magnetic field and gravitational effects as discussed by the authors.Abstract:
Steady state model of solar wind flow in equatorial plane solved for radial and azimuthal motions, taking into account pressure gradient, magnetic field and gravitational effectsread more
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Journal ArticleDOI
Simulations of Dynamo Action in Fully Convective Stars
TL;DR: In this paper, the authors present three-dimensional nonlinear magnetohydrodynamic simulations of the interiors of fully convective M dwarfs using the Anelastic Spherical Harmonic code, with the spherical computational domain extending from 0.08 to 0.96 times the overall stellar radius.
Journal ArticleDOI
Magnetar spin-down, hyperenergetic supernovae, and gamma-ray bursts
TL;DR: In this article, the authors estimate spin-down timescales for magnetized, rotating proto-neutron stars and construct steady state models of neutrino-magnetocentrifugally driven winds, showing that if magnetars are born rapidly rotating, with initial spin periods (P) of ~1 ms, then of order 1051-1052 ergs of rotational energy can be extracted in ~10 s.
Book ChapterDOI
Large-scale structure of the interplanetary medium
TL;DR: In this paper, it was shown that the solar corona is highly structured and changes its shape enormously during the solar activity cycle, and it was no great surprise when both spatial structure and temporal variability were found to be reproduced in the corona's offspring.
Journal ArticleDOI
Atmospheric Escape from Hot Jupiters
TL;DR: In this paper, the authors show that mass loss takes the form of a hydrodynamic ("Parker") wind, emitted from the planet's dayside during lulls in the stellar wind.
Journal ArticleDOI
The polar heliospheric magnetic field
J. R. Jokipii,József Kóta +1 more
TL;DR: In this article, it is suggested that the polar heliospheric magnetic field at large heliocentric distances may deviate considerably from the generally accepted Archimedean spiral, and that the large-scale field near the poles may be dominated by randomly oriented transverse magnetic fields with magnitude much larger than the average spiral.