Results 171 to 180 of about 1,455,996 (195)

Observation of super-Alfvénic slippage of reconnecting magnetic field lines on the Sun. [PDF]

Nat Astron
Lörinčík J, Dudík J, Sainz Dalda A, Aulanier G, Polito V, De Pontieu B.   +5 more
europepmc   +1 more source

Mancha3D Code: Multipurpose Advanced Nonideal MHD Code for High-Resolution Simulations in Astrophysics. [PDF]

Sol Phys
Modestov M, Khomenko E, Vitas N, de Vicente A, Navarro A, González-Morales PA, Collados M, Felipe T, Martínez-Gómez D, Hunana P, Luna M, Koll Pistarini M, Popescu Braileanu B, Perdomo García A, Liakh V, Santamaria I, Gomez Miguez MM.   +16 more
europepmc   +1 more source

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Heating of the solar chromosphere and corona

Astrophysics and Space Science, 1976
The generalized inhomogeneous wave equation that governs magnetoacoustic, vortical and thermal motions in compressible fluids and that thus is applicable to the problem of the heating of the solar chromosphere and corona is obtained. The effects of kinematic and bulk viscosity, heat conduction, Joule dissipation and magnetic diffusivity are included ...
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Wave heating of the solar chromosphere

Journal of Astrophysics and Astronomy, 2008
The nonmagnetic interior of supergranulation cells has been thought since the 1940s to be heated by the dissipation of acoustic waves. But all attempts to measure the acoustic flux have failed to show sufficient energy for chromospheric heating. Recent space observations with TRACE, for example, have found 10% or less of the necessary flux.
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Heating of the Solar Chromosphere by MHD-Waves

1991
We calculate a semi-theoretical model of the lower part of the chromosphere with the aid of the Vernazza et al. (1981) emission coefficients. The equality of the radiative emission coefficient and the absorption coefficient of weak MHD shock waves is assumed.
R. Erdélyi, M. Marik
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Vertical and horizontal heating in solar chromosphere

Chinese Astronomy and Astrophysics, 1985
Abstract Anisotropy of the stress tensor of turbulent waves is used in this paper to explain the effects of Alfven waves in a magnetic tube. Under the conditions of a force-free field with negligible thermal conduction and convection, the equations governing the behaviour of a one-dimensional steady flow are derived.
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An analysis of heat transfer in the solar photosphere and chromosphere

Geomagnetism and Aeronomy, 2017
The prevailing heat transfer processes—convection in the photosphere and wave propagation in the chromosphere—are principally different. Despite this fact, there is a direct link between these processes: it is precisely convective photospheric flows that excite intense Alfven waves in the chromosphere.
I. A. Molotkov, S. A. Vakulenko
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High-frequency acoustic waves are not sufficient to heat the solar chromosphere

Nature, 2005
One of the main unanswered questions in solar physics is why the Sun's outer atmosphere is hotter than its surface. Theory predicts abundant production of high-frequency (10-50 mHz) acoustic waves in subsurface layers of the Sun, and such waves are believed by many to constitute the dominant heating mechanism of the chromosphere (the lower part of the ...
Astrid, Fossum, Mats, Carlsson
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Theories of Heating of Solar and Stellar Chromospheres

1981
In the outer atmosphere of stars a rise of the kinetic temperature to values above Teff is possible only if a large and persistent amount of mechanical heating is present. Constraints derived from empirical chromosphere models allow selection of important heating mechanisms from among a great number of possible processes.
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Radiation loss and mechanical heating in the solar chromosphere

Solar Physics, 1974
The raditation loss of the solar chromosphere is evaluated on the basis of the Harvard Smithsonian Reference Atmosphere. The total radiative flux is found to be between 2.5 and 3.3 E6 erg cm−2 s−1. A discussion of possible heating mechanisms shows that the short period acoustic wave theory is the only one able to balance the chromospheric radiation ...
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