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Solar chromosphere flare spectrograph
SPIE Proceedings, 2013ABSTRACT 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 +2 more
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Solar and stellar chromospheric contrast
Solar Physics, 1994We 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 +2 more
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The dynamic solar chromosphere
AIP Conference Proceedings, 2007With 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
2005This 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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The Brightness Temperature of the Quiet Solar Chromosphere at 2.6 mm
, 2016The absolute brightness temperature of the Sun at millimeter wavelengths is an important diagnostic of the solar chromosphere. Because the Sun is so bright, measurement of this property usually involves the operation of telescopes under extreme ...
K. Iwai +6 more
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Chromospheric Evaporation in Solar Flares
EAS Publications Series, 2012Chromospheric 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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Structure of the Solar Chromosphere
Nature, 1964THE suggestion of Biermann1 and Schwarzschild2, that the radially increasing temperature of the solar atmosphere is to be ascribed to propagation of non-thermal energy, such as acoustic waves, is now generally accepted. The effect of magnetic field, and the possibility that the energy-carrying waves are of a magnetohydrodynamic character rather than ...
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Chromosphere, Corona, and Solar Wind
1989In 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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Structure of the solar chromosphere. III. Models of the EUV brightness components of the quiet sun
, 1981J. Vernazza, E. Avrett, R. Loeser
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4.1.1.4 Solar photosphere and chromosphere
2009Traditionally, 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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