PPT-Probing the first stars with metal poor

stars T Sivarani Indian Institute of Astrophysics Bangalore Chemical abundances of metal poor stars Probing the first stars Stellar archeology Looking for the fossil records of early star formation and Galaxy evolution . cdcgovnchshealthdataforallageshtm RACE ETHNICITY Unreliable data Includes Hispanics brPage 3br brPage 4br EP A100F08029 1071242Open Hashing (Chaining)0123456789abdgcf Planet-Host Stars. 2013. 2. 22. . Wonseok. Kang . Kyung . Hee. University. Sang-. Gak. Lee. . Seoul National University. Why? : Abundances of Planet Host Stars. 2. Workshop on Stars, Planets, and Life 2013. Soprano I Hence  stars,  you  daz- zle but the sight,   you teach to Soprano II Hence  stars, \r \r \r Alto Hence  stars, hence   stars too  dim of light,  you  daz-  zle  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 . Way. Matthew Shetrone. University of Texas, McDonald Observatory. Giuseppina. . Battaglia. Instituto. de . Astrofisica. De Canarias. Jennifer . Johnson, . Joel . Zinn. Ohio State . University. Dennis . Elliptical Galaxies. Spiral Galaxies. Barred Spiral. Lenticular. Irregular (. L. arge . M. agellanic . C. loud). Dwarf Spheroidal Galaxy. Isochrone - 2.5x10. 8. yrs. Isochrone - 4x10. 9. yrs. IMF in the ρ Oph Association. Sahil. Singla. . (Carnegie Mellon University). Joint . Work (. Partly) With . ANUPAM GUPTA . and . VISWANATH NAGARAJAN. (2. nd. Feb, 2018). Combinatorial Optimization. Given a . Finite . Universe. SDSS. Timothy C. Beers. University of Notre Dame . First-generation objects of high mass presumably formed from . . metal-free gas. Lived short lives (. Myrs. not . Gyrs. ). Exploded. Distributed (pre or post explosion) their . Uri Zwick. Tel Aviv University. Started: . April . 2015. Last update: . January 12, 2017. Hashing with open addressing. “Uniform probing”. Insert key . in the first free position among.  . (Sometimes) assumed to be a . ν. -p process. How do we explain the abundances of “lighter heavy” nuclei . (38 . ≤ Z ≤ 40: . Sr. -Y-. Zr. )?. From . Jacobson, H. R., & . Frebel. , A. 2014, Journal of Physics G Nuclear Physics, 41, 044001. VEGA. . Recent. . results. and . ongoing. programs. CHARA 2017:. . Year 13 Science Review . –. Adaptive Optics and Open Access. The VEGA instrument. 4-beams visible combiner (3 in standard modes). Ultra Metal - Poor (UMP ; [Fe/H] - 4 . 0 ) stars hold the key to the nucleosynthesis processes associated with first - generation stars in the Universe . However, only about two dozen UMP stars have b : Parts I. Extremely. . metal-poor. (EMP) . stars as . probes of . earliest. . heavy. . elements. . nucleosynthesis. Abundance. . curve. in . solar. system & neutron capture . processes.