PPT-I ntermediate-mass evolved star winds: an observer’s pers

Jacco van Loon Keele University Kalirai et al 2008 Kalirai et al 2009 Kalirai et al 2008 Javadi et al 2011 from Marigo et al 2008 A GB RSG Super AGB Sloan et al 2009. the Supernova Engine. Bounce Masses. Mass at Explosion. Fallback . Neutron Star Masses. Observations of neutron star binaries provide a growing list of neutron star mass estimates.. Current observations predict a range of NS masses from 1.0 to >2 solar masses.. Lecture 11: Extra-Solar Planets. Outline. Finding Extra-Solar Planets. The Two-Body Model. A Celestial Cubic. Example-51-Pegasi. 2. Finding Extra-Solar Planets. Recent discoveries of planets orbiting stars rely on a type of problem known as an . Cole Miller. University of Maryland. 1. Collaborators: . Romain. . Artigue. , Didier . Barret. ,. Sudip. Bhattacharyya, . Stratos. . Boutloukos. , . Novarah. . Kazmi. , Fred Lamb, . Ka. Ho Lo. Outline. Stars born with more than 8 — 10 M.  . cannot . lose enough mass to become white dwarfs. . These stars die by supernova explosions.. Ignition of “metals”. The core of an old high-mass star gets little . A little bit on its . metallicity. (. Z. ). Sometimes influenced by nearby stars. Low mass stars (. M < . 8. M. Sun. ) live a long life and die slowly. High mass stars (. M. > 8. M. Sun. ) live fast and die violently. progenitors a simple mass relationship?. John . Bray. PhD candidate. Supervisor Dr. J.J Eldridge. Crab nebula : . Image Credit : . NASA, ESA, J. Hester, A. Loll (ASU). Outline. The evidence for `kicks’. Steven R. . Cranmer. Harvard-Smithsonian Center for . Astrophysics. . with A. van . Ballegooijen. , S. Saar, A. Dupree, N. . Brickhouse. , et al.. Stellar winds across the H-R Diagram. Massive stars: radiation-driven winds. Wind entirely perpendicular to beam. Wind entirely along-beam. Analytic Evaluation. If the horizontal wind components . u. and . v. are known, and vertical velocity is negligible, then the radial velocity . represents the . apparent locations . of some of the constellations that are visible to an observer at approximately 40° N latitude at 9 . p.m. in . April. The point directly above the observer is labeled . are . relatively widely . separated. , . their . evolution proceeds much as it . would . have if they were not . companions.... If they are . closer. , it is possible for . material . to transfer from one star to another, . Chap 17-18: Stellar Evolution – the Life and Death of a Star… Here’s the story we’ll tell… Lowest mass stars and their evolution Low mass star evolution High mass star evolution Stellar death, and stellar corpses of Type II. b. supernova progenitors. Midwest Workshop on . SUPernovae. and . TRansients. Niharika Sravan. FEB 26, 2019. Stripped Envelope (SE) . Sn. e. H. He. Core. SUPERNOVA. H. He. Core. SUPERNOVA. 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...