HEATING OF THE MAGNETIZED SOLAR CHROMOSPHERE BY PARTIAL IONIZATION EFFECTS
نویسندگان
چکیده
منابع مشابه
The role of partial ionization effects in the chromosphere.
The energy for the coronal heating must be provided from the convection zone. However, the amount and the method by which this energy is transferred into the corona depend on the properties of the lower atmosphere and the corona itself. We review: (i) how the energy could be built in the lower solar atmosphere, (ii) how this energy is transferred through the solar atmosphere, and (iii) how the ...
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The Sun’s corona is millions of degrees hotter than its 5,000 K photosphere. This heating enigma is typically addressed by invoking the deposition at coronal heights of non-thermal energy generated by the interplay between convection and magnetic field near the photosphere. However, it remains unclear how and where coronal heating occurs and how the corona is filled with hot plasma. We show tha...
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A two dimensional, steady state, resistive magnetohydrodynamic (MHD) model with flow is used to support the proposition that a major source of heating for the solar middle chromosphere is resistive dissipation of large scale electric currents driven by a convection electric field. The currents are large scale in that their scale heights range from hundreds of kilometers in the network to thousa...
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Spectral diagnostic features formed in the solar chromosphere are few and difficult to interpret — they are neither formed in the optically thin regime nor in local thermodynamic equilibrium (LTE). To probe the state of the chromosphere, both from observations and theory, it is therefore necessary with modeling. I discuss both traditional semi-empirical modeling, numerical experiments illustrat...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2012
ISSN: 0004-637X,1538-4357
DOI: 10.1088/0004-637x/747/2/87