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The formation of Mg I 4571 Å in the solar atmosphere

✍ Scribed by Richard C. Altrock; C. J. Cannon

Publisher
Springer
Year
1973
Tongue
English
Weight
121 KB
Volume
30
Category
Article
ISSN
0038-0938

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The formation of Mgi4571 Å in the solar
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✍ Richard C. Altrock; C. J. Cannon 📂 Article 📅 1972 🏛 Springer 🌐 English ⚖ 426 KB

A one-dimensional analysis of the 4571 A, line of neutral magnesium is presented. The Harvard-Smithsonian Reference Atmosphere (HSRA) and the Bilderberg Continuum Atmosphere (BCA) are used to compute the emergent line profiles at various positions on the solar disc. The resultant profiles, when comp

The Formation of MgI 4571 Å in the solar
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✍ Richard C. Altrock; C. J. Cannon 📂 Article 📅 1975 🏛 Springer 🌐 English ⚖ 755 KB

The two-dimensional equation of transfer is solved for the case of locally-controlled source function (LTE) and radiationally-controlled ionization. Horizontal fluctuations in electron temperature and macroscopic velocity fields are superposed on the basic one-dimensional model (cf. Altrock and Cann

The formation of Mgi4571 Å in the solar
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✍ Richard C. Altrock; C. J. Cannon 📂 Article 📅 1973 🏛 Springer 🌐 English ⚖ 624 KB

An analysis of the 4571 A line of neutral magnesium is presented in which one-dimensional macroscopic velocity fields are included. It is shown that gradients over restricted heights in the vertical and horizontal components of the velocity field of order --0.005 s -1 and --0.004 s -1 (such that vel

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The possibility of surge formation as a result of plasma 'raking-up', the latter being associated with the growth of the local magnetic field in the solar atmosphere, is considered in this paper. The question is treated numerically in the MHD approximation for the case of the dipolar magnetic field.

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We report high resolution measurements of the center-to-limb variation of the MgI line at 4571.1 N. This forbidden line is of interest because it should be formed in LTE. Comparison of our measurements with the Harvard-Smithsonian Reference Atmosphere show that the line center radiation originates i

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A simple and reliable method has been established for the definition of the depth of formation of lines in a stellar atmosphere. It is based on the determination of the level of emission of the reemitted line radiation. The new definition, which is applied in this paper to the solar case, does not s