PPT-Classification of Stellar Spectra

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. multitemperature. approach. . B. Sylwester, J. Sylwester, A. Kępa. . Space . Research. Centre, PAS, Wrocław, Poland. K.J.H. Phillips. Natural . History. . Museum. , London, UK. . V.D. . Kuznetsov. Mark Morris. UCLA. ABSTRACT -- The . well-defined, massive disk of young stars orbiting within 0.5 pc of the Galactic black hole (GBH) is strongly tilted with respect to the Galactic plane. In the context of in situ formation mechanisms, this orientation is inherited from that of the gas disk that formed these stars on the order of 6 million years ago. The tilt can be understood by positing that clouds fall toward the GBH on near-zero angular momentum orbits and form dispersion rings as they self-intersect after . . 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. 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. 1. /28. Important for transits (see next slides).. . Transit depth = [ . R. planet. (. λ. ,t. ) / . R. star. (. λ,t. ) ]. 2. Not so important for eclipses because the eclipse is a simple difference, and the stellar variability typically is slower than the eclipse: . Extending this to Hydrogen. Results from solving the . Shrodinger. equation for the hydrogen atom. Z is the atomic number. m. e. is the mass of an electron. e is the charge of an electron or proton. Sergey L. Sheetlin. ,. Yuri A. Mirokhin, Dmitrii V. Tchekhovskoi, Xiaoyu Yang, Stephen E. Stein. NIST Mass Spectrometry Data Center, Biomolecular Measurement Division,. National Institute of Standards and Technology. Key variable is . mass. of star. directly measured only for binary stars, but it determines position on main sequence. Cluster ages. Main-sequence luminosity increases . much. faster than mass. therefore massive stars use up their fuel much faster. 5. H. 5. ). Ketan Sharma*, Terry A. Miller*, John F. Stanton. #. & David J. Nesbitt. ^. * The Ohio State University, Columbus, OH. #. University of Florida, Gainesville, FL. ^. JILA CU-NIST, Boulder, CO. 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 . 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.. Sergey L. Sheetlin. ,. Yuri A. Mirokhin, Dmitrii V. Tchekhovskoi, Xiaoyu Yang, Stephen E. Stein. NIST Mass Spectrometry Data Center, Biomolecular Measurement Division,. National Institute of Standards and Technology.