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Study of Solar spectrum



In this experiment you will study the solar spectrum taken from space and on Earth. You will identify some prominent spectral lines and determine their equivalent width. This will be used to estimate the column density of corresponding ions or atoms contributing to these lines. Finally these will be used to estimate the relative abundance of some elements in the solar atmosphere.

You will be provided with a data file, solar data, which contains solar spectral flux received in space in units of «math xmlns=¨http://www.w3.org/1998/Math/MathML¨»«mi mathvariant=¨bold-italic¨»W«/mi»«mi mathvariant=¨bold-italic¨»a«/mi»«mi mathvariant=¨bold-italic¨»t«/mi»«mi mathvariant=¨bold-italic¨»t«/mi»«mo»/«/mo»«mo»(«/mo»«msup»«mi mathvariant=¨bold-italic¨»m«/mi»«mn»2«/mn»«/msup»«mi mathvariant=¨bold-italic¨»n«/mi»«mi mathvariant=¨bold-italic¨»m«/mi»«mo»)«/mo»«/math». The flux is defined as the radiation energy received from sun per unit area per unit wavelength range. The wavelength is given in units of "nanometer". Also provided (below) are the high resolution graphs of CaII - H and K lines and Hydrogen Balmer line. Further you are also given a reference set of spectral lines, Reference Spectral Lines, and the relationship between the spectral line width and column density of atoms in stellar atmospheres.

Calcium II spectral lines :                             

Hydrogen Balmer lines :                               

General curve of growth for the sun :         


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