Vulcano Workshop 2012
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Europe/Rome
Vulcano Island, Sicily
Vulcano Island, Sicily
Support
Participants
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08:50
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09:00
Welcome address
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09:00
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Opening Remarks
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Highlights from the Opera Experiment 25mThe Opera Experiment (Oscillation Project with Emulsion tRacking Apparatus) is a long baseline neutrino experiment in the CERN Neutrino to Gran Sasso (CNGS) beamline. The muon neutrino beam produced at CERN is directed to the LNGS (Laboratori Nazionali del Gran Sasso) and after a flight of 730km detected in the Opera detector, situated underground in Hall C of the laboratory. The goal of the Opera experiment is to detect the muon to tau neutrino oscillation in appearance mode, i.e. by detecting tau decays. The technique used for this is the so-called emulsion cloud chamber (ECC) together with an electronic detector. This talk will give an update on the neutrino oscillation studies, the statistics of the year 2008/09 with an outlook on the results for 2010 and on possible new tau candidates. Finally the issues on the neutrino speed measurement will be presented and discussed.Speaker: Dr Thomas Strauss (LHEP Universitaet Bern)
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coffee break 30m
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Study of the time dependence of radioactivity 20mIn the last years many papers have been published on the time dependence of the decay constant. In particular, its annual modulation with amplitude of about 0.1% has been claimed, with the maximum in February and the minimum in August. In the talk we will give the results of a dedicated experiment performed underground in Gran Sasso with a 137Cs source and a germanium detector. The experiment is sensitive to an effect smaller than 0.01% on the time dependence of the 137Cs decay constant.Speaker: Dr Carlo Broggini (PD)
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interval 4h 15m
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Cosmology
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interval 2h 30m
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Astrophysics of High Energy Cosmic Sources
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Cataclysmic Variables: Their Impact on Astroparticle Physics 25mWe review the processes and conditions that lead to the production of non-thermal radiation in cataclysmic variables (CVs). We focus on the cases when such emission was really observed in various spectral bands, from gamma rays including TeV emission to radio. Detection of this radiation suggests the presence of highly energetic particles in these CV systems. Synchrotron and cyclotron emissions also suggest the presence of strong magnetic fields in CV. The propeller effect in the case of the rapidly rotating magnetized white dwarf (WD) or a shock in the case of a strongly magnetized WD can lead to the strong acceleration of the particles; even Cherenkov radiation is possible in the extreme cases. In some CVs, e.g. during some dwarf nova outbursts, the magnetic field generated in the accretion disk leads to the synchrotron jets. Even gamma-ray production via $\pi^{\rm o}$ decay was observed in the ejecta of an explosion of a symbiotic classical nova (CN). Nuclear reactions during thermonuclear runaway in the outer layer of the WD undergoing CN explosion lead to the production of radioactive isotopes; they are the sources of gamma-ray emission.Speaker: Dr Vojtech Simon (Astronomical Institute AS CR)
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interval 3h 55m
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Galactic and Extragalactic SNRs as Sites of Particle Acceleration 25mSupernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into acceleration of particles to high energies. I will review the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implication on the Galactic cosmic ray distribution will be discussed.Speaker: Dr Manami Sasaki (Institute for Astronomy and Astrophysics Tuebingen)
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RX J0852.0-4622 - the nearest historical supernova remnant 20mThe supernova remnant RX J0852.0-4622, also called by its nickname Vela Jr., was discovered in X-rays by ROSAT. Gamma-rays from the radioactive decay have been reported as well. The combination of the X-ray and gamma-ray measurements allows a fairly precise determination of distance (200 pc) and age (680 yrs). However, later on, the gamma-ray measurements were heavily disputed, so that doubts arise about the distance and age values. Meanwhile, the expansion rate of the SNR has been measured, which, in angular terms, is the fastest of all known SNRs, but less than expexted, so that the age could be 1000 yrs - 3000 yrs and the distance 1 kpc. Even then, RX J0852.0-4622 would be the nearest historical SNR known. But I will show that a hydrodynamical evolution slightly more complex than the straight application of the Sedov relations predict, could bring age and distance back to the originally reported values.Speaker: Dr Bernd Aschenbach (PRV)
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The impact of SUZAKU measurements on Astroparticle Physics 25mResults from Suzaku observations of clusters of galaxies are reviewed, particularly from the point of view of gas heating and constraint on non-thermal emission from merging clusters.Speaker: Dr Naomi Ota (Nara Women's University)
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interval 2h 15m
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Astrophysics of High Energy Cosmic Sources
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official photo and coffee break 35m
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Astrophysics of High Energy Cosmic Sources
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Black Hole Spin in AGN and its Implications for Galaxy Evolution 25mThe angular momentum of a supermassive black hole (SMBH) is a vitally important quantity in astrophysics. Measuring the spins of SMBHs in active galactic nuclei (AGN) can inform us about the relative role of gas accretion vs. mergers in recent epochs of the life of the host galaxy and its AGN. Black hole spin is also thought to play a pivotal role in triggering relativistic jets, enabling the SMBH to influence its surroundings out to scales much larger than its gravity allows. Advances in theoretical modeling as well as observational sensitivity in the Chandra/XMM-Newton/Suzaku era are finally producing robust constraints on the spins of a handful of SMBHs, but this science is still very much in its infancy. I will discuss our current knowledge of the distribution of SMBH spins in the local universe. I will also address prospects for improving the accuracy, precision and quantity of these spin constraints in the next decade and beyond with instruments such as NuSTAR, Astro-H and ATHENA.Speaker: Dr Laura Brenneman (Harvard-Smithsonian Center for Astrophysics)
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coffee break 30m
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Jet Sources and Gamma-Ray Bursts
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Gamma-Ray Bursts in the Fermi era 25mThe Fermi observatory carries two complementary instruments for the observation of the gamma-ray sky, which allow for joint analyses of Gamma-Ray Bursts (GRB) over seven decades of energy. The Gamma-Ray Burst Monitor (GBM) covers the entire unocculted sky and is designed for gamma-ray transients' detection, monitoring and spectroscopy between 8 keV and 40 MeV. The Large Area Telescope (LAT) is a pair-conversion detector of high-energy gamma rays of energies ranging from 20 MeV to more than 300 GeV. Since July 2008, the GBM detected over 800 GRB, of which 36 had a significant emission in LAT data. I will present GRB observations provided by Fermi and discuss how these fit in with both current and future space- and ground-based multi-messenger experiments: catalogs and population studies, some spectral and temporal characteristics including additional spectral components, searches for spectral cutoffs at high energies, delays between low- and high-energy gamma-ray emissions, long-lived emissions at GeV energies. Theoretical implications of these observations will be discussed: emission mechanisms, limits on the jet's bulk Lorentz factor from opacity constraints, limits on Lorentz invariance violation models.Speaker: Dr Veronique Pelassa (University of Alabama in Huntsville)
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interval 3h 50m
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The Challenge of Cosmic Ray Production
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Precise cosmic rays measurements with PAMELA 25mThe PAMELA experiment was launched on board of the Resurs-DK1 satellite on 15th of June 2006. The apparatus was designed to conduct precision studies of the charged cosmic radiation over a wide energy range, from tens of MeV up to several hundred GeV, with unprecedented statistics. In five years of continuous data taking in space, PAMELA accurately measured the energy spectra of cosmic ray antiprotons and positrons, as well as protons, electrons and light nuclei, sometimes providing data in unexplored energetic regions. These important results have shed new light in several astrophysical fields like: indirect search for Dark Matter, search for cosmological antimatter (anti-Helium), and the validation of acceleration, transport and secondary production models of cosmic rays in the Galaxy. Some of the most important items of the Solar and Magnetospheric physics were also investigated. Here we present the most recent results obtained by the PAMELA experiment.Speaker: Dr Alessandro Bruno (INFN sezione di Bari, Bari, Italy)
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UHECR event map and multiplets made by Lightest and Heaviest radioactive nuclei 20mThe puzzle of UHECR origination is related to their composition, spectra and maps. The main signal that srvived in last AUGER data is a clustering along Cen A. Very recent multiplet ar 20 EeV do cluster also along Cen A. These events fit a UHECR Lignt nuclei for extragalactic sources. Most of remanents UHECR may be heavy nuclei radioactive originated mostly by nearby SN-GRB whose traces are found in correlated gamma TeV-MeV-UHECR maps. We show that recent ARGO-ICECUBE data do hint for Vela, Magellanic stream and even Crab connection with UHECR. Tau Netrino at PeVs energy may shine similar anisotropies in the sky.Speaker: Dr Daniele Fargion (ROMA1)
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The Challenge of Cosmic Ray Production
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Iron Peak in CRs 20mRecent measurements of the cosmic ray (CR) energy spectrum in the PeV region and above have confirmed the remarkable sharpness of the knee and revealed another structure at about 70 PeV which we call 'an Iron Peak'. The position and the shape of this structure lead us to associate its likely origin with the same single source responsible for the formation of the knee. We have analysed the shape of the CR energy spectrum from the single source and concluded that their mass composition may be rather similar to the composition of sources for the bulk of CR in the TeV-PeV region. Since it is generally accepted that these CR originate mainly in supernova explosions, the similarity of the mass composition gives an additional argument in favour of our single source being a supernova remnant. Although we cannot exclude that yet another nearby recent source, viz. a pulsar may contribute, it is argued that at the knee at $\sim$3-4 PeV less than about 10\% of the CR intensity is due to just a few sources rather than a single source.Speaker: Prof. Anatoly Erlykin (P.N.Lebedev Physical Institute)
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Gravitational Waves
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coffee break 30m
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Neutrino Astronomy
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Analysis of the past MACRO data to compare multiple muon times. 20mThe arrival times of muons in a bundle produced by one cosmic ray interaction in the atmosphere should return a value compatible with the time resolution, while if neutrinos have larger velocity than muons some of the muons may arrive slightly earlier in a bundle of particles than others. There are strong theoretical arguments against this possibility, however this measurement could verify the OPERA hints on the possibility that neutrinos have a velocity larger than the speed of light.Speaker: Dr Francesco Ronga (LNF)
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interval 4h
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The GERDA esperiment: status and future plans 20mThe GERDA esperiment: status and future plansSpeaker: Paolo Zavarise
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Direction for Next Generation Experiments
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coffee break 30m
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