PPT-Stellar

Masses Binary Stars The HR Diagram Again A Diagram for People Q What is happening here A People grow They are born small and then grow in height and mass as they age with a fair bit of individual scatter. - 201 3 Welcome to Stellar Partner Program Our partner prog ram, aims at building a select group of Partners to work together as a team, to reach the next level of success in the field of data recov . 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 . LLC. April 2013. Indian Coastal . Barge Proposal. Disclaimer. While this presentation has been prepared in good . faith . Stellar Ocean Transport, . LLC (“SOT”) does . not take responsibility for any third party representation or warranty, explicitly or implied, as to the truth, accuracy or completeness of the information in this presentation or any other information relating to it whether written, oral or in a visual or an electronic form. The presentation may include references to and summaries of valuations and reports prepared by third parties that have not been independently verified by or on behalf of . Patricia . Sánchez-Blázquez. (UAM). Jairo. Mendez-Abreu (IAC). Sebastian F Sánchez (UNAM). Isabel Perez (UGR). Fabian Rosales-Ortega (UAM). And . the CALIFA collaboration. Resolved stellar . population. Transits and Starspots. Jeremy Tregloan-Reed. Ph.D. Research Student. jtr@astro.keele.ac.uk. Supervisor:. John Southworth. High Precision Photometry. Orbital Based . Photometry. Ground Based Defocused Photometry. . Greg . Feiden. & Brian . Chaboyer (Dartmouth). Three color EUV image of the Sun. White lines show a model of the Sun’s magnetic field . (. Schrijver. & Title 2011). Measurements of average magnetic fields in M dwarfs. Jupiters. Fred Adams, Univ. Michigan. Extreme Solar Systems II. Jackson, Wyoming, September 2011. Hot . Jupiters. can Evaporate. HD209458b (Vidal-. Madjar. et al. 2003, 2004; Desert et al. 2008; Sing et al. 2008; . 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?. Metallicity. Relation at High . Redshifts. Stellar-mass . Metallicity. Relation at . ｚ～. １．. 4. Kouji. OHTA. 　（. Kyoto University. ）. K. Yabe. , F. . Iwamuro. , S. Yuma, M. Akiyama, N. Tamura, FMOS team et al.. versus convective . blueshifts. , and wavelength variations across stellar disks. Dainis Dravins. – Lund . Observatory. , Sweden. www.astro.lu.se. /~. dainis. KVA. IAU Comm.30, IAU XXVIII GA Beijing, August 2012. 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. 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: . Dainis . Dravins. – Lund . Observatory. , Sweden. www.astro.lu.se. /~. dainis. KVA. Towards the science case for E-ELT . HIRES. , Cambridge UK, September 2012. STELLAR SURFACES. … where starlight and stellar spectra originate. 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.