PPT-Nucleosynthesis in decompressed Neutron stars crust matter

Sarmistha Banik Collaborators Smruti Smita Lenka amp B Hareesh Gautham BITSPILANI Hyderabad Advances in Astroparticle Physics and Cosmology AAPCOS 2015 SINP Kolkata . Varun Bhalerao. California Institute of Technology. Collaborators: F. Harrison, S. . Kulkarni. , Marten van . Kerkwijk. , and others. Weighing in on Neutron Stars. Varun Bhalerao. Why?. How?. What?. Classes of objects. (Saga Univ.). Dark matter . capture in . c. ompact stars. -stellar constraints on dark matter-. Oct. 20, 2014 . ＠. QCS2014, . KIAA, . Beijin. . Dark matter . capture . . in . Stars: . Insights . into their Formation. , Evolution & . Structure from their. Masses and Radii. Feryal Ozel. University of Arizona. In collaboration with T. . Guver. , M. . Baubock. , L. . Camarota. . Ana Becerril-Reyes, Sanjib S. Gupta and Hendrik Schatz. . Comparison between the two compilations of electron capture rates:. We start by comparing the EC rates at the lowest values of temperature and density (T9=0.01 and Log. Nathalie . Degenaar. . University of Michigan. X-ray observations. Interior properties. Thermal evolution. Quiescence. No/little accretion. Neutron star visible. Accretion outburst. Rapid accretion. By. . Kraml E.. 09.01.2017. A Neutron-Star. (not . actually. ). The Sun. Source: NASA. A Neutron-Star. Comparison. Diameter:. Mass. :. Density. :. Diameter:. Mass. :. Density. :. 1.4 x 10^6 km. 2 x 10^30 kg. ＠. Baryons2013, Glasgow . Motoi Tachibana (Saga Univ.). Dark matter . capture . in . n. eutron . stars . with exotic . phases. A modern physics perspective. . “. UROBOROS” = unity of matters & universe. 20.11. 1. Neutron stars. T. he . remains of cores of some massive stars that have become supernovae. .. Cores are . a degenerate gas of mostly neutrons.. So much compression at each stage of core contraction that final radius is . Prof Wladimir . Lyra. Live Oak, 1119-G. Office Hours: Mon 4pm-5pm. Class hours: Mon/Wed 5pm-6:15pm. Evolution of high mass stars. The evolution we covered in last class is for low mass stars (. M < 4 M. Nuclear. Structure and . Reactions. : Building . Together. for the Future. 9 October 2017 GANIL. Present. . c. ollaborators. . along. . this. . research. line:. ENSAR2. , . JRA . TheoS. . (. Theoretical. and . astrophysical . observations. David E. . Á. lvarez. . C. .. Sept 2013. S. . Kubis. , D. . Blaschke. and T. . Klaehn. The Modern Physics of Compact Stars and Relativistic Gravity. Outline. Introduction to neutron stars. Rudy . Wijnands. Anton . Pannekoek. Institute for Astronomy. University of Amsterdam. 15 December 2015. Texas Symposium 2015, Geneva. X-. ray. . luminosity. Quiescence. Outburst. Low-mass X-ray binary transients. Big Bang . Nucleosynthesis. takes place when the universe is a few minutes old. makes . 2. H, . 3. He, . 4. He and . 7. Li. Fusion in stars. in stars like the Sun, makes . 4. He and C, N, O . in massive stars, makes elements up to iron-56. Frederick Seward. ABSTRACT. Neutron stars are predicted to be stable over the mass range ≈ 0.1 to ≈ 3M. ⊙. . At 1.4 M. ⊙. , 98% of the mass is in a core with . supernuclear. density and 1-2 % forms a thin crust and atmosphere . As mass decreases, the fraction of mass in the crust increases until at .