Results 101 to 110 of about 881 (218)
Chromospheric Evaporation in Solar Flares
, 2012 Chromospheric evaporation suggests the mass upflows from chromosphere to corona after the electron heating at the chromosphere during the solar flares. It takes place at the rising phase, and has a typical timescale about 100 s and a typical speed about ...
Z. Ning, Zongjun Ning
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Heating of Solar and Stellar Chromospheres and Coronae by MHD Waves [PDF]
Highlights of Astronomy, 1992 Ground-based and satellite observations have shown that all late-type dwarfs possess hot outer envelopes, and that the chromospheric and coronal emissions observed from these envelopes vary significantly for a given, fixed spectral type. In addition, there is growing evidence for nonhomogeneous and locally strong magnetic fields in the atmospheres of ...
openaire +1 more source
The Astrophysical JournalAccurately assessing the balance between acoustic wave energy fluxes and radiative losses is critical for understanding how the solar chromosphere is thermally regulated.
J. M. da Silva Santos +5 more
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Solar flux emergence : a three-dimensional numerical study
, 2008 Flux is continually emerging on the Sun, making its way from the solar interior up into the atmosphere. Emergence occurs on small-scales in the quiet Sun where magnetic fragments emerge, interact and cancel and on large-scales in active regions where ...
Murray, Michelle J.
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The FIP and Inverse FIP Effects in Solar and Stellar Coronae
Living Reviews in Solar Physics, 2015 We review our state of knowledge of coronal element abundance anomalies in the Sun and stars. We concentrate on the first ionization potential (FIP) effect observed in the solar corona and slow-speed wind, and in the coronae of solar-like dwarf stars ...
J. Martin Laming
doaj +1 more source
Numerical studies of solar chromospheric jets
, 2016 The solar chromospheric jet is one of the most characteristic structures near the solar surface. The quantitative understanding of chromospheric jets is of substantial importance for not only the partially ionized phenomena in the chromosphere but also ...
Iijima, Haruhisa
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Topological structure of the magnetic solar corona
, 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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, 1997 A model of the solar corona and wind is developed which includes for the first time the heating and acceleration effects of high-frequency Alfven waves in the frequency range between 1 Hz and 1 kHz.
Marsch, E., Tu, CY, Marsch, E, Tu, C.
core +1 more source
Kelvin-Helmholtz instability in solar chromospheric jets: theory and observation [PDF]
, 2016 Using data obtained by the high-resolution CRisp Imaging SpectroPolarimeter instrument on the Swedish 1 m Solar Telescope, we investigate the dynamics and stability of quiet-Sun chromospheric jets observed at the disk center.
Kuridze, D. +7 more
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Energy Transport and Heating by Nonthermal Electrons in a Turbulent Solar Flare Environment
The Astrophysical JournalThe impulsive phase of a solar flare is known to generate strong turbulence and to transfer magnetic energy into accelerated electrons. Recognizing the importance of angular diffusion on the dynamics of the accelerated electrons, we extend previous ...
A. Gordon Emslie, Eduard P. Kontar
doaj +1 more source