temperature distribution in the solar chromosphere
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temperature distribution in the solar chromosphere

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Published by National Aeronautics and Space Administration; for sale by the Clearinghouse for Federal Scientific and Technical Information, Springfield, Va. in [Washington] .
Written in English



  • Sun


  • Solar chromosphere.,
  • Sun -- Temperature.

Book details:

Edition Notes

Bibliography: p. 106-114.

Statementby Stuart D. Jordan.
SeriesNASA technical report,, NASA TR R-291, NASA technical report ;, R-291.
LC ClassificationsTL521 A3312 no. 291, QB528 A3312 no. 291
The Physical Object
Paginationiii, 125 p.
Number of Pages125
ID Numbers
Open LibraryOL5738307M
LC Control Number70604630

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  Influence of temperature distribution in the chromosphere on the spectrum of the S-component of solar radio emission. M. N. Fasakhova & O. I. Yudin Radiophysics and Quantum Electronics vol pages – ()Cite this articleAuthor: M. N. Fasakhova, O. I. Yudin.   The described investigation is concerned with the solution of the non-LTE optically thick transfer equations for hydrogen, carbon, and other constituents to determine semiempirical models for six components of the quiet solar chromosphere. For a given temperature-height distribution, the solution is obtained of the equations of statistical equilibrium, radiative transfer for lines and continua Cited by:   Influence of Temperature Distribution in the Chromosphere on the Spectrum of the S-Component of Solar Radio EmissionAuthor: M. N. Fasakhova, O. I. Yudin. The chromosphere is a pink-glowing region of gas at a temperature of 10, Kelvin. Its light is mainly the red H 2 emission line. The chromosphere can be seen by the naked eye during a total solar eclipse. When the Moon covers the rest of the solar disk, this thin .

MRinTMR;er25, Magnetic reconnection in strongly magnetized regions of the low solar chromosphere LeiNi 1;2,3 1, 4andJunLin 1Yunnan Observatories, Chinese Academy of Sciences, P. O. Box , Kunming, Yunnan. Although fire is one of the warmest parts of our daily life, the chromosphere's temperature ranges between 6, degrees Fahrenheit. At this temperature, molecules absorb so . At first, the temperature decreases with height - from roughly 6,° C (11,° F) at the photosphere to about 4,° C (7,° F) a couple hundred kilometers higher up. Strangely, temperatures begin to climb in the upper reaches of the chromosphere, reaching a few tens of thousands of degrees. Spicules occur at the edges of the chromosphere’s magnetic network, which traces areas of enhanced field strength. Temperatures in the chromosphere range from about 4, to , Kelvins (K), increasing with altitude; the mean temperature is about 6, K. Solar prominences are primarily chromospheric phenomena.

Abstract. We calculate a semi-theoretical model of the lower part of the chromosphere with the aid of the Vernazza et al. () emission coefficients. The equality of the radiative emission coefficient and the absorption coefficient of weak MHD shock waves is assumed.   The increase in temperature does not stop with the chromosphere. Above it is a region in the solar atmosphere where the temperature changes f K (typical of the chromosphere) to nearly a million degrees. The hottest part of the solar atmosphere, which has a temperature of a million degrees or more, is called the corona.   Solar System Temperatures Average Temperature on Each Planet Planetary surface temperatures tend to get colder the farther a planet is from the Sun. Venus is the exception, as its proximity to the Sun and dense atmosphere make it our solar system's hottest planet. The widespread tendency in solar physics to divide the solar atmosphere into separate layers and to distinguish phenomena of solar activity from phenomena of the quiet Sun emphasizes the wide ranging diversity of physical conditions and events occurring in the solar atmosphere. This diversity.