PPT-“X-ray Spectroscopy of the High-Mass X-ray Binary Pulsar

Centaurus X3 Over its Binary Orbit Sachindra Naik Biswajit Paul and Zulfikar Ali Introduction Interest Extended dips in the light curve CenX Eclipsing HMXRB pulsar Orbital period 21 days pulse period 48 s. Megan . DeCesar (UWM). In collaboration with Scott Ransom (NRAO), Paul Ray (NRL), Paul Demorest (NRAO), David Kaplan (UWM), and the . Fermi. LAT Collaboration. Discovery of a Highly Eccentric Binary Millisecond Pulsar. Jeremy Hare (GWU), Oleg . Kargaltsev. (GWU), . Martin . Durant (University of Toronto), George Pavlov (Penn State). The George Washington University. Introduction. B1259 is a binary star system in which a pulsar (neutron star) orbits a massive companion star. Each of these stars have their own energetic wind which is powered by the rotational energies of the stars. When these winds collide they interact and form an intra-binary shock. This shock gives rise to a spiral structure due to the . PULSAR PROPERTIES:. High Space Velocity . Rapid Spin Rate. Super Dense. Strong Gravitational Field. Strong Magnetic Field . Jocelyn Bell. “Little Green Men” Theory. Chandrasekhar Mass Limit. 1.4 solar masses =. is a supernova remnant which is a super dense, . rapidly spinning neutron star which emits . dipole electromagnetic . radiation and features a strong magnetic and gravitational . field and also high space velocity. . 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 . Ingrid Stairs. UBC Vancouver. CAWONAPS. TRIUMF. Dec. 9, . 2010. Pulsars are one manifestation of neutron stars:. spin periods ~. 1.4. ms to . 8.5 seconds,. magnetic fields ~10. 8. to ~5 x10. 13. G. . Introduction . to Spectroscopy. Spectroscopy involves an interaction between matter and light . (EMR). Light can be thought of as waves of energy or packets (particles) of energy called photons. Properties of light waves include wavelength and frequency. 衣川　智弥. 東. 大. 宇宙. 線研. 高エネルギー天体. グループ. 自己紹介. 出身地　山梨県. 京大　天体核研究室. ➝. 宇宙. 線. 研. ポスドク. 1. 年目. 研究テーマ　連星進化　初代星　重力波. Using . BH-NS Binary Systems. John . Simonetti. Physics Department, Virginia Tech. Physics, VT. Djordje. . Minic. Vipin. . Vijayan. ECE, VT. Umair. . Surani. Physics, . LIU. Mike . Kavic. …the Plan…. 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, . 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 . Piet Van Duppen. ISOLDE CERN, Switzerland. IKS-. K.U.Leuven. , Belgium. K.U. Leuven. University of Western Scotland, U.K. - . K.U.Leuven. , Belgium - SCK-CEN-Mol, Belgium - . U.Gent. , Belgium - . Commenius. 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...