PPT-IGRINS for Stellar Abundances & Nucleosynthesis

Chris Sneden Natalie Gosnell Dan Jaffe Greg Mace Richard Seifert UT Austin Hwihyun Kim IGRINS team members KASI Melike Afşar Ege U Izmir Turkey Caty Pilachowski Indiana U. MESSENGER SAX & RHESSI. Brian Dennis. 31 October 2012. Mercury MESSENGER. Solar Assembly for X-rays (SAX). Si-PIN solid-state. 300 µm thick. 1 to 10 keV. ~300 . eV. resolution at 6 keV. 0.12 mm. 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. Michael Hayden (NMSU), Jo . Bovy. (IAS), Steve . Majewski. (. UVa. ), Jennifer Johnson (OSU), Gail . Zasowski. (JHU), Leo . Girardi. (. Padova. ), Carlos Allende-. Prieto. (IAC), Ana Garcia-Perez (. 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 . 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. 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: . 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. Transiting Exoplanets. Dainis Dravins. 1. , . Hans-Günter Ludwig. 2. ,. Erik Dahlén. 1. ,. Martin Gustavsson. 1. , . Hiva. Pazira. 1. . 1. . Lund Observatory, Sweden, . 2. . Landessternwarte. . SYFTET. Göteborgs universitet ska skapa en modern, lättanvänd och . effektiv webbmiljö med fokus på användarnas förväntningar.. 1. ETT UNIVERSITET – EN GEMENSAM WEBB. Innehåll som är intressant för de prioriterade målgrupperna samlas på ett ställe till exempel:. Donald D. Clayton\'s Principles of Stellar Evolution and Nucleosynthesis remains the standard work on the subject, a popular textbook for students in astronomy and astrophysics and a rich sourcebook for researchers. The basic principles of physics as they apply to the origin and evolution of stars and physical processes of the stellar interior are thoroughly and systematically set out. Clayton\'s new preface, which includes commentary and selected references to the recent literature, reviews the most important research carried out since the book\'s original publication in 1968. Boris Pritychenko. 1. 1 National Nuclear Data Center, Brookhaven National. Laboratory, Upton, NY 11973-5000, USA. Heavy Elements Production in a Neutron Star Merger. Can we apply nuclear data libraries to address current astrophysical observations such as a multi-messenger signal from the NGC 4993 galaxy? .