Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5096
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dc.contributor.authorSurendiranath, R-
dc.date.accessioned2010-04-09T14:25:59Z-
dc.date.available2010-04-09T14:25:59Z-
dc.date.issued1988-
dc.identifier.citationVelusamy, T and Venugopal, V. R eds., Image processing in astronomy: Proceedings of the workshop in imaging processing in astronomy held in Ooty 23 - 27 March 1987, pp. 87 - 89en
dc.identifier.urihttp://hdl.handle.net/2248/5096-
dc.descriptionOpen Accessen
dc.description.abstractMany of the stellar and nebular spectroscopic problems need the inputs of the line flux (or equivalent width if the line is in absorption) and the wavelength of the line peak. These input parameters are then used in the analysis for obtaining physical parameters like electron temperature, electron density, abundances of the elements, radial velocities etc.en
dc.language.isoenen
dc.publisherTata Institute of Fundamental Researchen
dc.rights© Tata Institute of Fundamental Researchen
dc.subjectMarquardt Algorithmen
dc.subjectStellaren
dc.subjectNebular Spectroscopicen
dc.subjectLine Fluxen
dc.subjectElectron Temperatureen
dc.subjectElectron Densityen
dc.subjectRadial Velocitiesen
dc.titleProfile fitting by marquardt algorithmen
dc.typeArticleen
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