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The top documents tagged [roche lobe overflow]
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roche lobe overflow
Scuola Nazionale di Dottorato Cagliari, May 25 2007 Proprietà Osservative delle Binarie X Contenenti Stelle di Neutroni Tiziana Di Salvo Dipartimento di.
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Multiwavelength observations of_na_st1_(wr122)_equatorial_mass_loss_and_x_rays_from_an_interacting_wolf_rayet_binary
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Accretion in Binaries Two paths for accretion –Roche-lobe overflow –Wind-fed accretion Classes of X-ray binaries –Low-mass (BH and NS) –High-mass (BH and.
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Binary Star Evolution Half of all stars are in binary systems - stellar evolution in binaries is important Roche Lobe: 3-D boundary where the gravity of.
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INPE Advanced Course on Compact Objects Course IV: Accretion Processes in Neutron Stars & Black Holes Ron Remillard Kavli Center for Astrophysics and Space.
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Hydrogen burning under extreme conditions Scenarios: Hot bottom burning in massive AGB stars (> 4 solar masses) (T 9 ~ 0.08) Nova explosions on accreting.
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X-ray binaries. Rocket experiments. Sco X-1 Giacconi, Gursky, Hendel 1962.
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Neutron Star Physics a kind of introduction Ulrich R.M.E. Geppert November 4th 2011U.R.M.E., Univ. of Zielona Gora1.
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He star evolutionary channel to intermediate-mass binary pulsars with a short-orbital-period Chen Wen-Cong School of Physics, Peking University Department.
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Makishima-Nakazawa lab seminar Oct.3, 2013 An Introduction to Low- Mass X-ray Binaries Dipping LMXBs -- Suzaku observation of XB 1916-053 Zhongli Zhang.
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Asteroseismology of evolved stars: from hot B subdwarfs to white dwarfs
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ULXs @ non-X-ray wavelengths Manfred Pakull 0bservatoire Astronomique de Strasbourg coll: Roberto Soria, Christian Motch, Fabien Grisé ULX and Middle Weight.
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