PPT-Review: Evolution of High-Mass Stars

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 highmass star gets little . Stellar Evolution. “We . are stardust. Billion year old carbon. We are . golden”. Woodstock by Joni Mitchell. Units of Chapter 12. Leaving the Main Sequence. Evolution of a Sun-like Star. The Death of a Low-Mass Star. Go to the Physics and Astronomy Department website.. www.pa.uky.edu. Click on “. Online Course Evaluation. ” link. Link is open now. Do it soon.. The nearest stars to the Sun.. Barnard’s Star. Pre-Main Sequence. Triples. Erez Michaely. Advisor : Prof. Hagai Perets . Israel Institute of Technology, Haifa. Observations : Binaries. Introduction. Close Low Mass binaries are likely to be a part of a triple system . Evolved Stars. Lee Anne Willson. Iowa State University. April 30, 2014. STScI. 1 AU is in the habitable zone for our Sun, now.. The planetary temperature scales as. . T. planet. /T. Earth. 回転単独星モデルと連星モデル. 梅田　秀之. （東京大学　天文学専攻）. Introduction. (L-)GRB progenitor – . associated with . Hypernovae. . . Massive Stars. Central engine (popular models):. Evolution off the Main Sequence. Main Sequence Lifetimes. Most massive (O and B stars): millions of years. Stars like the Sun (G stars): billions of years. Low mass stars (K and M stars): a trillion years! . Bruce Cockburn Got it Wrong. Lyrics:. . When the sun goes nova. And the world turns over. I don't want to be alone. So honey come on home. If you're in the valley. When the dam breaks, . palley. You is going to feel alone. 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 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. A talk for Hans . Zinnecker. (sort of).. Alison Sills, McMaster University. Collision Models . Sills (1997-2009), . Glebbeek. (2008-2010). head-on (S97, G08) and off-axis collisions (S01). With rotation (S05). PowerPoint Created by: Alexander J. Hawkins. Information documented from . DK Smithsonian UNIVERSE Definitive Visual Guide. Stellar Life. As human beings go through cyclic lives, maturing from birth to maturity to old age, stars also follow a series of stages from their creation until death. Stars follow varying sequences of change depending greatly on their solar mass, or their gravitational weight . 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...