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Published by: \apj Published on: 09/2016
YEAR: 2016   DOI: 10.3847/0004-637X/828/2/66
Knowledge of the electron density distribution in the solar corona put constraints on the magnetic field configurations for coronal modeling and on initial conditions for solar wind modeling. We work with polarized SOHO/LASCO-C2 images from the last two recent minima of solar activity (1996-1997 and 2008-2010), devoid of coronal mass ejections. The goals are to derive the 4D electron density distributions in the corona by applying a newly developed time-dependent tomographic reconstruction method and to compare the result ...
Published by: The Astrophysical Journal Published on: 11/2015
YEAR: 2015   DOI: 10.1088/0004-637X/814/1/68
The tenuous supersonic solar wind that streams from the top of the corona passes through a natural boundary\textemdashthe Alfv\ en surface\textemdashthat marks the causal disconnection of individual packets of plasma and magnetic flux from the Sun itself. The Alfv\ en surface is the locus where the radial motion of the accelerating solar wind passes the radial Alfv\ en speed, and therefore any displacement of material cannot carry information back down into the corona. It is thus the natural outer boundary of the solar co ...
Published by: The Astrophysical Journal Published on: 06/2014
YEAR: 2014   DOI: 10.1088/0004-637X/787/2/124