Results 101 to 110 of about 3,957 (226)

Hydrogen Atmospheres in the Absence of Thermodynamic Equilibrium. IV. The Solar Chromosphere

, 1948
A discussion of the observational data shows that in the range 0<z<2.5 x 108 cm. the electron concentration in the lower chromosphere may be expressed as Ne=5x 1011 exp(-6 x 10-9z) per cc., where z cm. is the height measured from a level 500 km.
RG Giovanelli
core   +1 more source

Farley-buneman instability in the solar chromosphere

, 2009
The Farley-Buneman instability ( FBI) is studied in the partially ionized plasma of the solar chromosphere taking into account the finite magnetization of the ions and Coulomb collisions.
Gogoberidze, Grigol, Poedts, Stefaan, Goossens, Marcel, Voitenko, Y.   +3 more
core   +1 more source

Dynamics of the solar chromosphere

, 2001
We analyze oscillations in the solar atmosphere using image sequences from the Transition Region and Coronal Explorer (TRACE) in three ultraviolet passbands which sample the upper solar photosphere and low chromosphere.
T. D. Tarbell, R. J. Rutten, J. M. Krijger, B. W. Lites, R. A. Shine, Th. Straus   +5 more
core   +1 more source

Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results [PDF]

, 2015
The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves propagating through the chromosphere can supply significant
Jess, D.B., Jess, D. B.; id_orcid, I. Giagkiozis, S. D. T. Grant, G. Verth, Verth, G., D. B. Jess, Morton, R.J., Grant, S. D. T., Fedun, V., Giagkiozis, Ioannis, Morton, Richard, R. J. Morton, Morton, R. J., Jess, David, Giagkiozis, I., Verth, Gary, V. Fedun, Grant, S.D.T., Fedun, Viktor, Grant, Samuel   +20 more
core   +1 more source

A single frequency approach to nonequilibrium modeling of the chromosphere

Astronomy & Astrophysics
Context. The solar chromosphere is a region where radiation plays a critical role in energy transfer and interacts strongly with the plasma. In this layer, strong spectral lines, such as the Lyman lines, contribute significantly to radiative energy ...
Ruan W., Przybylski D., Cameron R., Solanki S. K.   +3 more
doaj   +1 more source

Effect of Magnetic Diffusion in the Chromosphere on the Solar Wind

The Astrophysical Journal
We investigate nonideal magnetohydrodynamical (MHD) effects in the chromosphere on the solar wind by performing MHD simulations for Alfvén-wave-driven winds, explicitly including ohmic and ambipolar diffusion.
Masato Matsuoka, Takeru K. Suzuki, Takato Tokuno, Kensuke Kakiuchi   +3 more
doaj   +1 more source

Structure and dynamics of the internetwork solar chromosphere: Results of a small-scale dynamo simulation

Context. The heating and structure of the solar chromosphere depends on the underlying magnetic field, among other parameters. The lowest magnetic flux of the solar atmosphere is found in the quiet Sun internetwork and is thought to be provided by the ...
S. K. Solanki, J. Leenaarts, D. Przybylski, R. Cameron, M. Rempel, S. Danilovic   +5 more
core   +1 more source

Magnetic flux emergence into the solar photosphere and chromosphere

, 2009
Aims. We model the emergence of magnetized plasma across granular convection cells and the low atmosphere, including layers up to the mid-chromosphere. Methods.
A. Tortosa-Andreu, F. Moreno-Insertis
core   +1 more source

Numerical Experiment on the Influence of Granulation-induced Waves on Solar Chromosphere Heating and Plasma Outflows in a Magnetic Arcade

The Astrophysical Journal
This paper offers a fresh perspective on solar chromosphere heating and plasma outflows, focusing on the contribution of waves generated by solar granulation.
M. Kumar, K. Murawski, B. Kuźma, E. K. J. Kilpua, S. Poedts, R. Erdélyi   +5 more
doaj   +1 more source

The differential rotation of the chromosphere and the quiet chromosphere in the falling and rising period of a solar cycle

The full-disk chromosphere was routinely monitored in the He I 10830\AA\, line at the National Solar Observatory/Kitt Peak from 2004 Nov. to 2013 March, and thereby, synoptic maps of He I line intensity from Carrington rotations 2032 to 2135 were ...
Xu, JC, Li, KJ
core