Results 1 to 10 of about 1,105,860 (262)
Alfvén wave dissipation in the solar chromosphere [PDF]
Nature Physics, 2018 Magneto-hydrodynamic (MHD) Alfv n waves have been a focus of laboratory plasma physics and astrophysics for over half a century. Their unique nature makes them ideal energy transporters, and while the solar atmosphere provides preferential conditions for their existence, direct detection has proved difficult as a result of their evolving and dynamic ...
Samuel D. T. Grant +9 more
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The role and contribution of magnetic fields, characterized via their magnetic flux, to the statistical structuring of the solar atmosphere [PDF]
Scientific Reports, 2022 The anomalous heating of the solar upper atmosphere is one of the eight key problems in modern astronomy. Moreover, the stratification of the solar atmosphere is an outstanding key-problem in solar physics.
K. J. Li, J. C. Xu, W. Feng
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FARLEY-BUNEMAN INSTABILITY IN THE SOLAR CHROMOSPHERE [PDF]
The Astrophysical Journal, 2009 The Farley-Buneman instability is studied in the partially ionized plasma of the solar chromosphere taking into account the finite magnetization of the ions and Coulomb collisions. We obtain the threshold value for the relative velocity between ions and electrons necessary for the instability to develop.
Gogoberidze, Grigol +3 more
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How Are the Abnormally Hot Chromosphere and Corona Heated by the Solar Magnetic Fields? [PDF]
The Astrophysical JournalThe corona is a structure possessed by stars, including the Sun. The abnormal heating of the solar corona and chromosphere is one of the greatest mysteries in modern astronomy.
K. J. Li +5 more
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The Astrophysical JournalThis paper offers a fresh perspective on solar chromosphere heating and plasma outflows, focusing on the contribution of waves generated by solar granulation.
M. Kumar +5 more
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Ionisation in the Solar Chromosphere [PDF]
Nature, 1920 IT is well known that the spectrum of the upper layers of the solar chromosphere is chiefly composed of those lines which are relatively more strengthened in the spark than in the arc, and which Sir Norman Lockyer originally styled enhanced lines. The best-known examples are the calcium H and K and the strontium pair (4216, 4077).
M. Saha
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RADIATING CURRENT SHEETS IN THE SOLAR CHROMOSPHERE [PDF]
The Astrophysical Journal, 2012 An MHD model of a Hydrogen plasma with flow, an energy equation, NLTE ionization and radiative cooling, and an Ohm's law with anisotropic electrical conduction and thermoelectric effects is used to self-consistently generate atmospheric layers over a $50$ km height range.
Goodman, Michael L., Judge, Philip G.
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Resonance Lines in the Solar Chromosphere [PDF]
Symposium - International Astronomical Union, 1970 Stigmatic balloon spectra of the Sun in the vicinity of 2800 Å were obtained on September 22, 1968 and April 30, 1969. We compare the observed profiles of the H and K lines of ionized magnesium with the computed profiles of Athay and Skumanich and of Dumont. The discrepancy between observed and computed profiles of the Mgii lines is considerable. It is
P. Lemaire
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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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On the Nature of the Solar Chromosphere [PDF]
, 2006 Proceedings 23th NSO Workshop, ASP Conference Series, 354, 282, in ...
Robert J. Rutten
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