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Magnetic star-planet interaction in the young exoplanet system DS Tucanae Ab
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Solar Wind and Chromospheric Network
Solar Physics, 1997A 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, 2008We 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 +3 more
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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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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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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, 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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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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