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Journal ArticleDOI

The Angular Momentum of the Solar Wind

Edmund J. Weber, +1 more
- 01 Apr 1967 - 
- Vol. 148, pp 217-227
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TLDR
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 effects

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Journal ArticleDOI

Efficiency of Magnetized Thin Accretion Disks in the Kerr Metric

Charles F. Gammie, +1 more
- 01 Sep 1999 - 
TL;DR: In this paper, the authors estimate the torque on a magnetized disk using a steady magnetohydrodynamic inflow model originally developed by Takahashi et al. They find that the efficiency can depart significantly from the classical thin disk value.
Journal ArticleDOI

MAGNETO-THERMAL DISK WINDS from PROTOPLANETARY DISKS

Xue-Ning Bai, +3 more
- 17 Feb 2016 - 
Journal ArticleDOI

Kinetic models of the solar and polar winds.

Joseph Lemaire, +1 more
- 01 May 1973 - 
TL;DR: In this paper, the application of the kinetic theory to the collisionless regions of the polar and solar winds is discussed, and a brief historical review is given to illustrate the evolution of the theoretical models proposed to explain the main phenomenon and observations.
Journal ArticleDOI

Large-scale structure of the interplanetary medium. I - High coronal source longitude of the quiet-time solar wind

J.T. Nolte, +1 more
- 01 Nov 1973 - 
TL;DR: In this article, an extension of the quasi-radial hypervelocity (QRH) approximation yields a proper estimate of the high coronal source location at the ( elease zone'' where the solar wind makes its transition to radial interplanetary flow.
Journal ArticleDOI

Evidence of Possible Spin-Orbit Misalignment Along the Line of Sight in Transiting Exoplanet Systems

Kevin C. Schlaufman
- 14 Jun 2010 - 
TL;DR: In this paper, the Rossiter-McLaughlin (RM) effect is used to measure the angle between the orbit of a transiting exoplanet and the spin of its host star projected in the plane of sky.