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 . Like ordinary classical matter it is made up of many inter acting particles In classical matter however it is poss ible to think of each particle as an individual entity whereas in quantum matter Heisenbergs uncertainty principle prevents us from te Secs. 37.1-37.3. Reminders. Lab . D1-LFA: . Light from Atoms . due Friday @ 4 (this will be the last lab for the semester). In-class Quiz #6 Thursday, November 20???. Keep, reschedule, or delete . will address chapter 37 only. (Saga Univ.). Dark matter . capture in . c. ompact stars. -stellar constraints on dark matter-. Oct. 20, 2014 . ＠. QCS2014, . KIAA, . Beijin. . Dark matter . capture . . in . Nathalie . Degenaar. . University of Michigan. X-ray observations. Interior properties. Thermal evolution. Neutron stars . in transient X-ray binaries. Quiescence. :. No/little accretion. Faint X-ray emission. Phil Rosenfield, . Fridolin. Weber, Horst . Lenske. Outline. Neutron stars: a short synopsis. The structure of neutron stars. Modeling neutron stars. The equation of state. . Rotating or non-rotating. Nathalie . Degenaar. . University of Michigan. X-ray observations. Interior properties. Thermal evolution. Quiescence. No/little accretion. Neutron star visible. Accretion outburst. Rapid accretion. Theory & Observations. Hovik Grigorian. Yerevan State University. Summer School Dubna – 2012. Compact stars Physics. • physics of compact stars,. • astrophysics of compact stars,. • . ＠. 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. The Night Sky. The Milky Way. Stars (individual, binary, variable). Clusters (globular and open). Nebulae (reflection, emission, dark, planetary). SNRs, Neutron Stars, & Black Holes. Galaxies. The 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 . . constraints. : AGB . stars. and . grains. S.Palmerini. AGB . stars. , . s-process. and . presolar. . grains. :. the story so far. Molecular Cloud. Meteorite. Presolar. grains. Despite their low masses LMS are so numerous to contribute for 75% to the total mass return from stars to the ISM (. 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 . 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...