PPT-Classification of Stellar Spectra

Author : yoshiko-marsland | Published Date : 2017-04-20

Essentially all stars appear as point sources Only differences are brightness and spectra Many differences in spectra due to temperature Pseudo blackbody with chromosphere

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Classification of Stellar Spectra: Transcript

Essentially all stars appear as point sources Only differences are brightness and spectra Many differences in spectra due to temperature Pseudo blackbody with chromosphere outside photosphere. . atmospheres. a . very. . short. . introduction. Part I. Ewa Niemczura. Astronomical. . Institute. , . UWr. eniem@astro.uni.wroc.pl. Stellar. spectra. Stellar. spectra. One picture is worth 1000 words, but . . Gray and . Corbally. Chapter 8 . Karen Garcia. Georgia State University. Outline. Basic characteristics. Spectral . f. eatures. Mira variables. Carbon stars. H.-W. Rix IMPRS Galaxies Course March 11, 2011. Goal:. Determine . n. *. (M. *. ,. t. age. ,[Fe. /H],. R. ). . for a population of galaxies. How many stars of what mass and metallicity . formed when and where in galaxies?. Giuseppina. . Battaglia. Instituto. de . Astrofisica. de Canarias, Tenerife. Credit. : ESO/. H.H.Heyer. Credit. : ESO/L. . Calçada. Karachentsev. et al. 2014. Individual . Red . Giant Branch . stars. meeting #9. Spectroscopy. Spectral analysis provides:. . Redshift. /distance. Composition. Velocity/dynamics. Redshift. z=0 - Stars. Plate spectra. Modern stellar spectra: O star. He II. Modern stellar spectra: O/B. “Stars in transition”. Caroline Roberts. Polaris A and B, F-type stars; credit: NASA. Basic Information. 3% of solar neighborhood. Examples: Polaris, Dubhe, Canopus, Procyon. 6100-7400 K. 1.0-1.4 . Soroush Sotoudeh. . (University of Minnesota). Daniel . Weisz. , Andrew Dolphin, Evan Skillman. 06/29/2015 – . STScI. Workshop on IMF. Outline. Introduction. Observations and data. IMF analysis and results. 11/5/2014. T-Dwarfs. Artist's vision of a T-dwarf. M dwarf. L dwarf. T dwarf. Jupiter. ~1600 K. ~650 K. 160 K. ~2800 K. INTRODUCTION. T dwarfs. . are a class of low mass, low . temperature(600 –1300 . Stellar Evolution . Neda Hejazi. April, 2017. Proto-. PNe. and . PNe. . PPNe. :. Post AGB stars. . . ✪ . Intermediate-mass stars evolved from AGB. . ✪ . Ejecting shell of gas and dust. Transiting Exoplanets. Dainis Dravins. 1. , . Hans-Günter Ludwig. 2. ,. Erik Dahlén. 1. ,. Martin Gustavsson. 1. , . Hiva. Pazira. 1. . 1. . Lund Observatory, Sweden, . 2. . Landessternwarte. JEFFREY HALL. LOWELL OBSERVATORY, FLAGSTAFF, AZ. Project Timeline. 1988 1992 1996 2000 2004 2008 2012 . Construction/early observing. Rebuild 1. Broad survey. Solar analog survey. Rebuild 2. A/D boundary. Jeffrey . Linsky. JILA and APAS. Solar Focus Group. April 12, 2019. Why are the Lyman-α and EUV fluxes important?. Lyman-α is the brightest line in the solar UV spectrum.. Lyman-α is as bright as the entire UV spectra of M dwarf stars.. This is the first non-technical book on spectroscopy written specifically for practical amateur astronomers. It includes all the science necessary for a qualitative understanding of stellar spectra, but avoids a mathematical treatment which would alienate many of its intended readers. Any amateur astronomer who carries out observational spectroscopy and who wants a non-technical account of the physical processes which determine the intensity and profile morphology of lines in stellar spectra will find this is the only book written specially for them. It is an ideal companion to existing books on observational amateur astronomical spectroscopy. Russell A. Putnam. Rehse Group. Department of Physics, University of Windsor. Windsor, Ontario, Canada. Previous paper. 2012. LIBS ON Bacteria. DFA on 13 emission lines. New study. SAME DATA BUT WITH NEW TECHNIQUES AND NEW MODELS.

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