Physics Journal

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Analysis of Radiation from Photosphere of the Sun

Pages: 127-139 Views: 1063 Downloads: 739

[01]
D. P. Nandedkar, Department of Electrical Engineering, Indian Institute of Technology, Bombay, Powai, Mumbai, India.

In the present paper an analysis of the continuous radiation from photosphere of the Sun at equilibrium temperature of it is carried out. The radiation is assumed due to quantum jumps of the electron, in a high density ionized semi-gaseous type material of the photosphere of the Sun, from its amplitude states considering types of damped frequency oscillations and eigen frequency damped oscillations analogous to that exit in a low density plasma with electron-molecule collisions (Nandedkar 2016) [8]. Damped and eigen frequency damped oscillations of the electron result due to density fluctuations of the charge-carriers with opposite signs in the body of the photosphere due to nuclear processes going deep in the core of the Sun. The density fluctuations alternatively builds up and withdraws a d.c. electric field in the body of the photosphere. The necessary damping for the type of damped oscillations mentioned, is provided by electron-ion collision type interaction at equilibrium temperature of the photosphere. The minimum value of the amplitude the electron takes which can be quantized in the field of the neighbouring ion and in the absence of the d.c. electric field when eigen-frequency damped oscillations result, govern the minimum value of the wavelength of radiation from the continuous spectrum of the photosphere. In general the wavelength is shown to be a function of the average density of the charge-carriers. Thus lower limit of the electron density corresponding to an intermediate value of the chromosphere, brings an upper limit for the radiation-wavelength of the radiation spectrum of the photosphere. The continuous radiation from photosphere of the Sun corresponds to electron density N_{e} variations in the range 4.7774(2) x 10^{29} m^{-3} ≥N_{e} ≥ 1 x 10^{16} m^{-3} which corresponds to wavelength λ of radiation in the range 0.2476(8) x 10^{-6} m ≤λ≤ 8.984(9) x 10^{-3} m. However recently the solar spectrum is photographed up to a wavelength of about 0.2099 x 〖10〗^(-6) m which can be explained due to a mixture of a doubly charged ion and a singly charged ion in right proportion with one of electrons in each cases be considered, then the average distance of the electron from the ion can tend to lower down the minimum value of radiation wavelength.

Solar-Spectrum, Photosphere, Ultra-Violet, Cut-Off, Plasma-Model, Quantum-Jumps

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