Results 221 to 230 of about 14,496 (257)

Solar Wind and Chromospheric Network

Solar Physics, 1997
A physical model of the transition region, including upflow of the plasma in magnetic field funnels that are open to the overlying corona, is presented. A numerical study of the effects of Alfven waves on the heating and acceleration of the nascent solar wind originating in the chromospheric network is carried out within the framework of a two-fluid ...
Marsch, E., Tu, C.
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Understanding the Solar Chromosphere

AIP Conference Proceedings, 2008
We discuss the latest high‐resolution ground and space‐based observations of the solar chromosphere and their relevance to problems of chromospheric modeling. In particular, we briefly review recent as well as previous attempts to understand the solar chromosphere as the atmospheric layer with an apparently increasing temperature.
P. Heinzel, Vasile Mioc, Cristiana Dumitrache, Nedelia A. Popescu   +3 more
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Solar chromosphere flare spectrograph

SPIE Proceedings, 2013
ABSTRACT This paper describes develop of a two channel echelle spectrograph, Solar Chromospheric Flare Spectreograph(SCFC), to observe the optical spectra at the locations of ares and explosive events on the Sun. The SCFS willrecord are spectra in two channels in the wavelength range of 350-890 nm, which has several chromosphericspectral lines.
Debi Prasad Choudhary, Vasyl Yurchyshyn, Sanjay Gosain   +2 more
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Solar Chromosphere

2019
This is an advance summary of a forthcoming article in the Oxford Research Encyclopedia of Physics. Please check back later for the full article. The solar chromosphere (color sphere) is a strongly structured and highly dynamic region (layer) of the Sun’s atmosphere, located above the bright, visible ...
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Solar and stellar chromospheric contrast

Solar Physics, 1994
We present an analysis of disk-integrated spectra of the Caii K line (3933.68 A). The selection of parameters in the line profile, and the correlations between them, follow the work of Smith (1960), but represent an innovative aspect in the fact that our data are spatially integrated.
Robert A. Donahue, Sergio R. Restaino, Stephen L. Keil   +2 more
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The dynamic solar chromosphere

AIP Conference Proceedings, 2007
With the new ground‐based and space instrumentation observing the solar atmosphere, it is clear nowadays that the quiet sun is of dynamical nature. The Swedish 1m telescope (SST) with its spatial resolution better than 0.2 arc sec. allows us to follow the dynamics of the fine structures observed in photospheric, as well in chromospheric lines.
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Solar and stellar chromospheres

2005
This review attempts to highlight two fundamental and complementary aspects of the chromospheric phenomenon; viz., global properties of stellar chromospheres and their variation among the stars, and the underlying fine structure that affects or determines these global properties.
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Chromospheric Evaporation in Solar Flares

EAS Publications Series, 2012
Chromospheric evaporation implies the mass flow from chromosphere to corona along the loop legs in the solar flares. From observations, radio emissions show the high-frequency cutoff and with a drift toward the low frequency, and the coronal lines display a strong blueshift on the Doppler diagram, and hard X-ray emissions tend to rise up the double ...
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Chromosphere, Corona, and Solar Wind

1989
In the preceding chapters we have learned about convection and rotation, the main causes of solar magnetism. And we have learned about this magnetism itself. We shall now recognize that the Sun¯s magnetic field is the main source of almost all structure and variability which we find in the outermost layers: the chromosphere, the corona, and the solar ...
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4.1.1.4 Solar photosphere and chromosphere

2009
Traditionally, the atmosphere of the Sun has been divided into four layers, starting with the photosphere at the bottom, followed by the chromosphere, the transition region, and the corona as the outermost region. The photosphere is a layer of only a few hundred kilometers thickness in which the temperature drops outwards from around 6000 K at the ...
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