Piero Galeotti Università di Torino and INFN GianVittorio Pallottino Università di Roma and INFN Guido Pizzella Università di Roma Tor Vergata INFN- Frascati.
MAGNETARS AS COOLING NEUTRON STARS WITH MAGNETARS AS COOLING NEUTRON STARS WITH INTERNAL HEATING INTERNAL HEATING A.D. Kaminker, D.G. Yakovlev, A.Y. Potekhin,
ICECUBE & Limits on neutrino emission from gamma-ray bursts IceCube collaboration Journal Club talk 4.15.2011 Alex Fry.
A two-zone model for the production of prompt neutrinos in gamma-ray bursts Matías M. Reynoso IFIMAR-CONICET, Mar del Plata, Argentina GRACO 2, Buenos.
Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%
Neutrinos from gamma-ray bursts, and tests of the cosmic ray paradigm GGI seminar Florence, Italy July 2, 2012 Walter Winter Universität Würzburg TexPoint.
Neutron Stars 3: Thermal evolution Andreas Reisenegger Depto. de Astronomía y Astrofísica Pontificia Universidad Católica de Chile.
X-Ray image of Crab Nebula Pulsar Credit: NASA/CXC/ASU/J. Hester et al.) Liliana Caballero With Pf. Horowitz Molecular Dynamics Simulations of Non-uniform.
This dish measured 20 millirad /hour when the counter was placed directly on it. The mantle measured 9 mr/hr. The No Salt has a lower level of radioactivity.
Neutron Stars 3: Thermal evolution Andreas Reisenegger ESO Visiting Scientist Associate Professor, Pontificia Universidad Católica de Chile.
Gravitational waves and neutrino emission from the merger of binary neutron stars Kenta Kiuchi Collaboration with Y. Sekiguchi, K. Kyutoku, M. Shibata.
COOLING OF NEUTRON STARS D.G. Yakovlev Ioffe Physical Technical Institute, St.-Petersburg, Russia Ladek Zdroj, February 2008, 1. Formulation of the Cooling.