Results 11 to 20 of about 1,195,417 (237)
Heating mechanisms of the solar corona. [PDF]
Proc Jpn Acad Ser B Phys Biol Sci, 2017 The solar corona is a tenuous outer atmosphere of the Sun. Its million-degree temperature was discovered spectroscopically in the 1940s, but its origin has been debated since then without complete convergence. Currently there are two classes of models; the wave theory and the microflare/nanoflare theory.
Sakurai T.
europepmc +4 more sources
Astronomy & Astrophysics, 2023 Context. Vortex flows have been found in the photosphere, chromosphere, and low corona in observations and simulations. It has been suggested that vortices play an important role in channeling energy and plasma into the corona. However, the impact of vortex flows on the corona has not been studied directly in a realistic setup. Aims. We investigate the
C. Breu +3 more
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Current sheets in the solar corona : formation, fragmentation and heating [PDF]
, 2011 In this thesis we investigate current sheets in the solar corona. The well known 1D model for the tearing mode instability is presented, before progressing to 2D where we introduce a non-uniform resistivity.
Bowness, Ruth
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MHD turbulence and heating of the open field-line solar corona [PDF]
, 2003 This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations.
Dmitruk, Pablo +13 more
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Waves in the Solar Corona [PDF]
Symposium - International Astronomical Union, 2004 Waves at all scales, ranging in wavelength from the size of a loop (fraction of a solar radius) down to the gyroradii of coronal ions (about hundred meters), are believed to play a key role in the transport of mechanical energy from the chromosphere to the Sun's corona and wind, and through the dissipation of wave energy in the heating and sustaining ...
openaire +2 more sources
A new approach to the maser emission in the solar corona [PDF]
, 2015 Aims. The electron plasma frequency ωpe and electron gyrofrequency Ωe are two parameters that allow us to describe the properties of a plasma and to constrain the physical phenomena at play, for instance, whether a maser instability develops.
Regnier, Stephane, S. Régnier
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Topological structure of the magnetic solar corona [PDF]
, 2007 The solar corona is a highly complex and active plasma environment, containing many exotic phenomena such as solar flares, coronal mass ejections, prominences, coronal loops, and bright points.
Maclean, Rhona Claire
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Slow solar wind acceleration through the middle corona: Spacecraft radio studies
Frontiers in Astronomy and Space Sciences, 2022 The “Middle Corona”, defined by recent consensus as the region spanning 1.5–6 solar radii (R⊙, heliocentric), is an important zone through which several structural and dynamic changes occur in coronal streamer regions. Among these is a regime change from
David B. Wexler +3 more
doaj +1 more source