PPT-Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebul

SP Reynolds et al Martin Tseng Chao Hsiung 20131218 Which contents I will cover Shell Supernova Remnants Obliquity Dependence and Summary Magnetic Fields in PulsarWind Nebulae. In addition magnetic fields create a force only on moving charges The direction the magnetic field produced by a moving charge is perpendicular to the direction of motion The direction of the force due to a magnetic field is perpendicular to the dir 8.5 – Applications of Electric and Magnetic Fields. Agenda. Quiz. Lesson on Section on 8.5. Lots of Video’s. Story Time. Cyclotron Particle Accelerator. http://. www.youtube.com/watch?v=cNnNM2ZqIsc. Dayal Wickramasinghe and Lilia . Ferrario. Australian National University. Canberra. . . The chemically peculiar . Ap. , Bp stars ( ~ 1.8 -5 . M. sun. ) are magnetic, and . have ordered large. scale fields, . Poynting. dominated outflows. Yuri . Lyubarsky. Ben-Gurion . University . Ubiquity . of relativistic . outflows in astrophysics. Crab nebula in X-rays. M 87. GRB lightcurves. R. elativistic outflows are associated with: . Supernova Remants and Pulsar Wind Nebulae in the Chandra Era. 1. Modeling the Dynamical and Radiative Evolution of a Pulsar Wind Nebula inside a Supernova Remnant. Joseph Gelfand (NYU / NSF). Patrick Slane (CfA), Weiqun Zhang (NYU). Xia Fang. Problems. Thanks for your time. Andrii Neronov. University of Geneva. Durrer. & AN, . A&ARev. , 21, 62 (2013) . Overview . Magnetic fields in astronomy and cosmology. Characterization. of cosmological magnetic fields. Generation. 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 . 2013/12/18. Speaker . : Yu-. Hsun. Cheng. Professor: Yosuke Mizuno. Introduction. Supernova remnants(SNR):. . This is . the structure resulting from the explosion of a star in a supernova. . It is formed by that the interactive between interstellar and . 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. . N. eutron . Stars Foreseen. . Supernova . End Products?. When a . supernova. goes off, we can speculate that:. The star might blow itself to smithereens, . scattering all its material into space and leaving . Systems. Frank Barnes.  . Department of Electrical, Computer, and Energy Engineering, University of Colorado, Boulder, Colorado. Acknowledgement. Ben Greenebaum. . Lucas Portelli . Carlos Martino . Open: Venus – solar wind. Closed: Venus – Venus. Draped: solar wind – solar wind. Magnetic fields guide ion and electron motions. The connectivity (topology) of these field lines helps us to understand how the upper atmosphere interacts with the solar wind..