PoS - Proceedings of Science

Supernovae: lights in the darkness

October 3-5, 2007
Maó (Menorca)
published October 31, 2008
Every year, at the end of the summer, the Section of Physics and Technique of the "Institut Menorquí d'Estudis" and the “Societat Catalana de Física" organize the "Trobades Científiques de la Mediterrània" with the support of several academic institutions. The 2007 edition has been devoted to stellar explosions, the true evolutionary engines of galaxies. Whenever a star explodes, it injects into the interstellar medium a kinetic energy of 1051 erg and between one and several solar masses of newly synthesized elements as a result of the thermonuclear reactions that have taken place within the stellar interior. Two mechanisms are able to provide these enormous amounts of energy: one of them thermonuclear and the other, gravitational. Thermonuclear supernovae are the result of the incineration of a carbon-oxygen white dwarf that is the compact star of a binary stellar system. If the two stars are sufficiently close to each other, the white dwarf accretes matter from its companion, approaches the mass of Chandrasekhar, and ends up exploding. The processes previous to the explosion, the explosion itself, as well as the exact nature of the double stellar system that explodes, are still a matter of discussion. This point is particularly important because these explosions, known as Type Ia Supernovae, are very homogenous and can be used to measure cosmological distances. The most spectacular result obtained, is the discovery of the accelerated expansion of the Universe, but it still feels uncomfortable that such a fundamental result is based on a "measuring system" whose origin and behaviour in time is unknown. At the end of their lives, massive stars generate an iron nucleus that gets unstable when approaching the Chandrasekhar mass. Its collapse gives rise to the formation of a neutron star or a black hole, and the external manifestation of the energy that is released, about a 1053 erg, consists of a Type II or Ib/c supernova, of a Gamma Ray Burst (GRB) or even of both things. From the beginning of the nineties, when CGRO discovered the cosmological character of these phenomena, the GRB have constituted one of the most exciting problems of modern Astrophysics. The stellar end products that leave supernovae, are as interesting as supernovae themselves. On one hand, as we previously said, they completely determine the chemical evolution of the Galaxy, which is fundamental for the formation of planets or, even, for the appearance of life. On the other hand, they leave collapsed objects such as neutron stars and black holes that give rise to a wide range of violent phenomena: x-rays eruptions, microquasars, acceleration of particles to high energies, etc. The goal of this workshop was to bring together scientists with a deep insight into these topics and advanced PhD students, with the purpose of discussing in depth the remaining problems. The organizers are specially grateful to DIUE-Generalitat de Catalunya, Ministerio de Educación y Ciencia, Balearic Island University, Barcelona University, Polythecnical University of Catalonia, Valencia University, CSIC and IFAE for their economical support.
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proceedings index
Joule heating governing the cooling of magnetized neutron stars
PoS(SUPERNOVA)001 pdf D. Aguilera and J.A. Pons
Ultrarelativistic outflows associated to progenitors of Gamma-Ray bursts
PoS(SUPERNOVA)002 pdf M.A. Aloy and P. Mimica
The role of Supernovae in Galaxy evolution
PoS(SUPERNOVA)003 pdf A. Artigas
STRESS a SN survey at ESO
PoS(SUPERNOVA)005 pdf M.T. Botticella
Small steps in thermonuclear supernova research
PoS(SUPERNOVA)006 pdf E. Bravo
Gravitational waves as tracers of nuclear equation of state.
PoS(SUPERNOVA)007 pdf R. Cabezon and D. Garcìa-Senz
Monte Carlo simulations of the Galactic binary population
PoS(SUPERNOVA)008 pdf J. Camacho, S. Torres and E. García-Berro
WD0433+270: an old Hyades stream member or an iron-core white dwarf?
PoS(SUPERNOVA)009 pdf S. Catalan
Precision of thermonuclear supernovae as distance indicators
PoS(SUPERNOVA)010 pdf I. Dominguéz, E. Bravo, L. Piersanti, O. Straniero, P. Höflich, J. Isern and A. Tornambé
PoS(SUPERNOVA)011 pdf N. Elias, J.E. Beckman, S. Benetti, E. Cappellaro and M. Turatto
Edge-lit double detonation in Subchandrasekhar-mass models for Type Ia supernovae
PoS(SUPERNOVA)012 pdf R. Forcada
Is there a chance for primordial SNeI1/2?
PoS(SUPERNOVA)013 pdf P. Gil-Pons
Accreting white dwarf
PoS(SUPERNOVA)014 pdf M. Hernanz and J. Jose
Gamma-ray Photons and Positrons from Type Ia Supernovae
PoS(SUPERNOVA)015 pdf A. Hirschmann
Evidence for short-lived SN Ia progenitors
PoS(SUPERNOVA)017 pdf R. Jimenez
Presupernova evolution of massive stars
PoS(SUPERNOVA)018 pdf M. Limongi
High resolution SPH simulations of merging white dwarfs binary systems
PoS(SUPERNOVA)019 pdf P. Loren
Pi of the Sky
PoS(SUPERNOVA)020 pdf K. Malek
An RMHD study of transition between prompt and afterglow GRB phases
PoS(SUPERNOVA)021 pdf P. Mimica, D. Giannios and M.A. Aloy
Very-High-Energy observations of X-ray binaries
PoS(SUPERNOVA)023 pdf M. Ribó
Thermonuclear Supernovae
PoS(SUPERNOVA)024 pdf F. Röpke
Gravitational wave astronomy: now and future
PoS(SUPERNOVA)025 pdf A. Sintes
Gravitational Radiation from Neutron Stars and Black Holes
PoS(SUPERNOVA)026 pdf C. Fernandez-Sopuerta
Galactic 26Al, 60Fe and 60Fe/26Al gamma-ray flux ratio from massive stars
PoS(SUPERNOVA)027 pdf attachments M. Suades
Cosmic-ray acceleration in supernova remnants
PoS(SUPERNOVA)028 pdf V. Tatischeff