Description
poster session + beer/refreshment
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Dr Thierry Foglizzo (CEA-Saclay, France)10/08/2011, 17:30Massive stars end their life with the gravitational collapse of their core and the formation of a neutron star. Their explosion as a supernova depends on the revival of a spherical accretion shock, located in the inner 200km and stalled during a few hundred milliseconds. Numerical simulations suggest that an asymmetric explosion is induced by a hydrodynamical instability named SASI....Go to contribution page
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Mr itay Rabinak (Weizmann institute of science)10/08/2011, 17:35We derive a simple approximate model describing the early, up to a few days, UV/optical supernova emission, which is produced by the expansion of the outer hundredth solar mass of the shock-heated envelope, following the shock breakout and preceding the optical emission driven by radioactive decay. Our model includes an approximate description of the time dependence of the opacity...Go to contribution page
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Dr Rhaana Starling (University of Leicester)10/08/2011, 17:40A growing number of long Gamma-Ray Bursts are indisputably associated with core-collapse supernovae, discovered through optical spectroscopy and/or photometry of the GRB afterglow. Three such bursts show evidence of a thermal component in the early X-ray afterglow emission, claimed by some to be a signature of supernova shock breakout. This component could equally be attributed to central...Go to contribution page
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Mr Ondrej Pejcha (Department of Astronomy, Ohio State University)10/08/2011, 17:45The mechanism of core-collapse supernovae is unknown. Despite considerable effort, most simulations of supernovae are not successful, and it has proven difficult to revive the stalled accretion shock, particularly for more massive stellar progenitors. Although it is known that the stalled accretion shock turns into explosion when the neutrino luminosity from the collapsed core exceeds a...Go to contribution page
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Patrick Slane (Harvard-Smithsonian Center for Astrophysics)10/08/2011, 17:50As a pulsar wind nebula evolves inside its host supernova remnant, its gamma-ray emission becomes increasingly brighter due to the buildup of energetic particles injected by its pulsar. When the SNR reverse shock collides with the PWN, the resulting increase in the magnetic field results in rapid synchrotron losses, modifying the particle spectrum of the nebula. Gamma-ray observations of...Go to contribution page
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Dr Dovi Poznanski (UC Berkeley & LBL)10/08/2011, 17:55Dust extinction is generally the least tractable systematic uncertainty in astronomy, and particularly in supernova science. Often in the past, studies have used the equivalent width of Na I D absorption measured from low-resolution spectra as proxies for extinction, based on tentative correlations that were drawn from limited data sets. We have recently shown, based on 443...Go to contribution page
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Dr George Sonneborn (NASA Goddard Space Flight Center)10/08/2011, 18:00The nature and quantity of dust produced in supernovae (SNe) is still poorly understood. Recent IR observations of freshly-formed dust in supernova remnants (SNRs) have yielded significantly lower dust masses than predicted by theoretical models and observations high-redshift galaxies. The Crab Nebula's pulsar wind is thought to be sweeping up freshly-formed SN dust along with the SN...Go to contribution page
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Dr Ross Church (Lund University)10/08/2011, 18:05The presence of a binary companion can have a significant effect on a supernova explosion. Mass transfer affects the evolution of the stars; a massive star may transfer so much mass that it fails to explode as a supernova, whilst conversely an accreting lower-mass star may gain enough material to cause it to explode. Massive stellar cores in close binaries can be spun up by...Go to contribution page
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Ms Io Kleiser (University of California at Berkeley)10/08/2011, 18:10The vast majority of Type II supernovae (SNe) are produced by red supergiants (RSGs), but SN 1987A revealed that blue supergiants (BSGs) can produce members of this class as well, albeit with some peculiar properties. This best studied event revolutionized our understanding of SNe, and linking it to the bulk of Type II events is essential. We present here optical photometry and...Go to contribution page
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Mr Takashi Moriya (IPMU, University of Tokyo)10/08/2011, 18:15We investigate the effect of non-steady dense mass loss on the shock breakout in dense wind. We found that the effect of the dense wind from non-steady mass loss can account for two types of interaction-powered luminous supernovae: 06gy-like LSNe which show the narrow emission lines from wind and 08es-like LSNe which do not show them.Go to contribution page
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Dr Salvatore Orlando (INAF - Osservatorio Astronomico di Palermo)10/08/2011, 18:20During the evolution of SNRs, Rayleigh-Taylor (RT) instability develop at the contact discontinuity between the ejecta and the shocked interstellar medium (ISM). The nonlinear instability evolves, giving rise to a turbulent structure with preferentially radial components, the so-called RT fingers. Current multi-dimensional models of SNRs describe the development of these structures....Go to contribution page
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Francesco Taddia (Stockholm University, department of Astronomy)10/08/2011, 18:25Supernova 1987A revealed that a blue supergiant (BSG) can end its life as a core-collapse supernova (SN). Such objects show peculiar properties distinguishing them from ordinary Type IIP SNe, whose progenitors are believed to be red supergiants. A similarity among 1987A-like events include a long rise to maximum and peak luminosities which are fainter than Type IIP SNe and mainly powered...Go to contribution page
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Dr Omer Bromberg (Racah Institute of Physics, The hebrew University, Jerusalem, Israel)10/08/2011, 18:30According the Collapsar model long GRBs (LGRBs) arise during the collapse of a massive star and involve the emergence of a relativistic jet through the envelope of the exploding star. This model naturally explains the links between LGRBs and SNe, such as the the association of half a dozen LGRBs with broad-line Ic SNe. However, a closer look at this association reveals that four out of...Go to contribution page
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Dr Patrick BLOTTIAU (CEA, DAM, DIF, Arpajon, France and Laboratoire Univers et Thรฉories, Observatoire de Paris, Meudon, France)10/08/2011, 18:35A complete description of the core-collapse supernova mechanism requires an appropriate treatment of both the hydrodynamics and the microphysics. Indeed, despite the crucial role played by hydrodynamics (e.g. hydrodynamical instabilities, rotation, convection or General Relativistic effects), to produce type II supernovae explosions, the influence of nuclear physics inputs on the outcome...Go to contribution page
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Dr Tabetha Hole (East Tennessee State U.)10/08/2011, 18:40Constraining the structure and asymmetries within supernova (SN) ejecta is of great importance to understanding the explosion mechanism and for constructing better models of SN feedback mechanisms. SN forbidden line profiles at later times, when the ejecta is optically thin in the continuum, provide a potential diagnostic of densities and the distribution of individual ionic species...Go to contribution page
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Dr Bernhard Mueller (MPA Garching)10/08/2011, 18:45The collapse of an iron core to a neutron star and the subsequent supernova explosion are among the greatest challenges in computational astrophysics due to the complex interplay of multi-dimensional hydrodynamics, neutrino transport, and strong-field gravity. Due to the compactness of the newly-born proto-neutron star and the occurrence of high velocities (up to ~0.3c), general...Go to contribution page
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Dr Rino Bandiera (INAF - Osservatorio Astrofisico di Arcetri)10/08/2011, 18:55Bamba et al. (2010) used deep X-ray observations, with Chandra and Suzaku, to estimate the sizes of faint and old Pulsar Wind Nebulae (PWNe). They found a steady increase in size with the nebular age, up to ages of about 10^5 yr. Their conclusion was that these PWNe keep expanding up to large ages, in apparent contradiction with the idea that a reverse shock from the associated...Go to contribution page
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Dr Yudai Suwa (Kyoto University)10/08/2011, 19:00Core-collapse supernovae are violent explosion of massive stars at their end of life. The standard model of the supernova explosion is so-called ``delayed explosion scenario'', in which the neutrino heating plays an important role. In order to investigate whether this model works properly, we must solve raditation hydodynamic equations incorporating the neutrino radiative transfer with...Go to contribution page
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Dr Leloudas Giorgos (Dark cosmology Centre)10/08/2011, 19:05Stripped-envelope core-collapse SNe are supposed to result from the explosions of stars that have lost their outer hydrogen layers but the exact nature of their progenitor and (possible) companion stars remains unknown. By comparing their locations to those of WR stars we show that they are indeed compatible. Furthermore, SN Ib locations are more closely related to those of WN stars,...Go to contribution page
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Dr Tea Temim (NASA Goddard Space Flight Center / ORAU)10/08/2011, 19:10We present deep Chandra observations and Spitzer Space Telescope infrared (IR) spectroscopy of the shell in the composite supernova remnant (SNR) Kes 75. The remnant is composed of a central pulsar wind nebula (PWN) and a bright partial shell in the South that is visible at radio, IR, and X-ray wavelengths. The X-ray emission from the shell is dominated by a two-component thermal model...Go to contribution page
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Dr Gaston Folatelli (IPMU, University of Tokyo)10/08/2011, 19:15We present a detailed study of the Type Ib/c SN 2010as based on optical and near-infrared imaging and spectroscopy, plus radio observations. The data span from about two weeks before to about 150 days after maximum light. SN colors and spectra indicate this object suffered considerable reddening by dust. Intermediate resolution X-Shooter spectra cover the time of maximum light and show...Go to contribution page
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Dr Shin-ichiro Fujimoto (Kumamoto National College of Technology)10/08/2011, 19:20We examine explosive nucleosynthesis during neutrino-driven, aspherical supernova (SN) explosion aided by standing accretion shock instability, based on two-dimensional hydrodynamic simulations of the explosion of 15-40$M_\odot$ stars with zero metallicity. The magnitude and asymmetry of the explosion energy are estimated with the simulations, for a given set of neutrino luminosities...Go to contribution page
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Dr Jennifer Hoffman (University of Denver)10/08/2011, 19:25Supernovae of all types are known to be polarized, and many display complex line polarization effects that evolve over time as the supernova evolves. Such behavior reveals details of the clumpy nature of the ejecta, as well as illuminating the characteristics of the circumstellar material lost by the star in its pre-supernova evolution. With the aid of diagnostic tools developed through...Go to contribution page
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Dr Melina Bersten (IPMU)10/08/2011, 19:30We present a model for the Type Ib SN 2008D, associated with the X-ray Flash 080109, which assumes a double-peaked 56Ni distribution. This assumption is fundamental to explain the plateau observed in the light curve a few days after the explosion. The presence of this high-velocity radioactive material may be caused by the formation of jets during the explosion. We briefly discuss the...Go to contribution page
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Ms Eveline Helder (Pennsylvania State University)10/08/2011, 19:35The evidence for supernova remnants as the main sources for Galactic cosmic rays has accumulated over the past decades. However, the physics of the acceleration mechanism is still unclear. In particular, there is a lack of empirical data to test current shock acceleration models. RCW 86 is an excellent source to test these models, as the shock velocities of the remnant vary by an order...Go to contribution page
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Mr Jason Dittmann (Harvard University)10/08/2011, 19:40We present time series radio data of the type Ic supernova SN 2004C taken with the VLA from January 2004 through April 2009 at 4.9 GHz, 8.5 GHz, 15 GHz, and 22 GHz. We also present 3 epochs of Chandra data taken 110, 170, and 1150 days after the initial explosion. We model our radio data for each epoch with a synchrotron self absorbed spectrum, and apply the dynamical model of...Go to contribution page
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Ms Sarah Wellons (Harvard University)10/08/2011, 19:45We present extensive radio observations of the nearby Type Ibc supernovae (SNe Ibc) 2004cc, 2004dk, and 2004gq spanning $\Delta t\approx 8-1800$ days after explosion. Using a dynamical model developed for synchrotron emission from a slightly decelerated blastwave, we estimate the velocity and energy of the fastest ejecta and the density profile of the circumstellar medium. The...Go to contribution page
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Ms Kate Alexander (Harvard-Smithsonian Center for Astrophysics)10/08/2011, 19:50We present radio observations of the type Ic supernova 1994I, reanalyzed as part of a search for radio transients in M51 conducted using archival data from the Very Large Array. The data includes a detailed 4.9 GHz light curve of SN 1994I and three spectra of this object from epochs on April 10, May 4, and August 8, 1994, each spanning frequencies of 1.5-22.5 GHz. We find that the...Go to contribution page