Ultrahigh Energy Cosmic Rays from Tidal Disruption Events: Origin, Survival, and Implications
|
|
- Berenice Johnston
- 6 years ago
- Views:
Transcription
1 arxiv: accepted by PRD Ultrahigh Energy Cosmic Rays from Tidal Disruption Events: Origin, Survival, and Implications Bing T. Zhang Peking University, Penn State University Collaborator: Kohta Murase, Foteini Oikonomou, Zhuo Li
2 1/14 Ultrahigh-Energy Cosmic Rays - Spectrum Cut-off Review of Particle Physics, Chin. Phys., 2016
3 Ultrahigh-Energy Cosmic Rays - Spectrum UHECRs: cosmic rays with energy larger than ev What is the composition? Cut-off Where are the sources? How can they be accelerated to ultrahigh energy? Review of Particle Physics, Chin. Phys., /14
4 2/14 What is the composition? A trend toward heavy nuclei Air Shower H He C N O Ne Mg Si Fe The Auger Collaboration, ICRC, 2017
5 Combined fit spectrum and composition data Spectrum The Auger Collaboration, 2017, JCAP Injection spectrum Composition data Source evolution Proton Helium m = 0 Nitrogen Iron 3/14
6 Combined fit spectrum and composition data Implications for the sources: heavy nuclei Intermediate mass, CNO, Ne, Mg, Si, Hard spectra Spectral index less than 2 Source evolution Prefer no evolution or negative evolution 3/14
7 Where are the sources? Gamma ray bursts Air Shower Heavy nuclei from the interior of progenitor stars Survival of nuclei : For GRBs, it is difficult in high-luminosity GRBs but easy in low-luminosity GRBs. Murase et al, 2006; Murase et al, 2008; Wang et al, 2007; Chakraborti et al, 2010; Liu et al, 2011; Horiuchi et al, 2012; Globus et al, 2014; Biehl et al, 2017 O Si Fe He P Data from Talys1.8 and Gent4 4/14
8 Where are the sources? Gamma ray bursts Air Shower Heavy nuclei from the interior of progenitor stars Survival of nuclei : For GRBs, it is difficult in high-luminosity GRBs but easy in low-luminosity GRBs. Murase et al, 2006; Murase et al, 2008; Wang et al, 2007; Chakraborti et al, 2010; Liu et al, 2011; Horiuchi et al, 2012; Globus et al, 2014; Biehl et al, 2017 Active galactic nuclei Heavy nuclei from the interstellar medium The fraction of heavy nuclei is too low Re-acceleration (galactic CRs) model Kimura, Murase, BTZ, /14
9 Heavy nuclei in Tidal disruption events Main-sequence stars Solar composition White dwarfs Composed of heavy nuclei He, C, O, Ne, Mg Helium White dwarfs Carbon-oxygen White dwarfs Oxygen-neon-magnesium White dwarfs 5/14
10 CR acceleration in jetted TDEs t dyn R/ c Forward shock t acc = E A ZeBc First order Fermi acceleration Reverse shock Internal shock Wind Constrain maximum energy t acc apple min(t dyn,t syn,t A ) Energy loss time scale Photodisintegration or photomeson 6/14
11 7/14 Internal shock model CRs can be accelerated to ultrahigh energy Difficult for UHECR nuclei to survive in luminous TDE jets such as Swift J A int UHECR nuclei mainly lose one nucleon in each interaction Inelasticity apple A ( ") E E = N N Interaction time scale A int / A ( ") Energy loss time scale A A / A ( ")apple A ( ")
12 Internal shock model CRs can be accelerated to ultrahigh energy Difficult for UHECR nuclei to survive in luminous TDE jets such as Swift J The survival is allowed for less powerful TDE jets A int A int A A 7/14
13 Forward shock model UHECR nuclei can survive at forward shock such as Swift J Si He O A int P Optical depth Fe f A A / dyn A P He O Si Fe Reverse shock: CRs can be accelerated to ultrahigh energy and survive Non relativistic wind: CRs cannot be accelerated to ultrahigh energy 8/14
14 9/14 Cosmic rays escaping from sources Acceleration spectral index s acc s esc Escape spectral index CRs can be confined and lose their energies during diffusive escape A harder spectrum s esc <s acc =2 Direct escape of CRs in internal shock Escape from a relativistic decelerating blast wave Two assumptions: The spectral index of escaped particles: s esc = s acc ( min (s acc 2) + E )/ max Baerwald, Bustamante and Winter, 2013 Katz, Meszaros and Waxman, 2010 The number of ejected CRs is similar to the number of particles at radius R "N esc (") "N(",R "max =") The minimum, maximum and total cosmic ray energies are power low functions of the radius E A,min ' 2 Am p c 2 / r min E A,max ' ZeBr / r max E CR / r E
15 UHECR nuclei injection spectrum UHECR nuclei follow a power-law distribution with an exponential cutoff Number fraction of different UHECR nuclei Maximum acceleration energy dn A 0 de 0 = f A 0N 0 E 0 ZE 0 sesc exp E 0 ZE 0 p,max E iso CR = CR E iso rad Normalization Depend on the total CR energy of TDEs CR 100 Spectral index Cosmic ray loading factor 10/14
16 11/14 Results of MS - SMBH tidal disruptions Solar composition ZE p,max = Z ev s esc =1 CR 100 Q CR, E 1 rad,53 Propagate with CRPropa 3-1D EBL: Gilmore 12 Proton dominated in nearly all the energy range
17 12/14 Results of CO WD - IMBH tidal disruptions X C =0.5,X O =0.5 ZE p,max = Z ev s esc =1 CR 100 Q CR, E 1 rad,53 Propagate with CRPropa 3-1D EBL: Gilmore 12 Poor fit to the UHECR spectrum
18 Results of ONeMg WD - IMBH tidal disruptions X O =0.12,X Ne =0.76,X Mg =0.12 ZE p,max = Z ev s esc =1 CR 1000 Q CR, E 1 rad,53 Propagate with CRPropa 3-1D EBL: Gilmore 12 Consistent with Auger data 13/14
19 Summary, conclusion and implications The production of UHECRs in TDEs accompanied by relativistic jets Internal shock Forward shock Reverse shock Non-relativistic wind Examine different composition models for TDEs MS-SMBH CO-IMBH ONeMg-IMBH WD-IMBH with ignition Secondary gamma rays and neutrinos signals are of interest to test the model Cosmogenic neutrinos flux High energy gamma rays The survival is allowed for less powerful TDEs Production and survival of UHECRs Production and survival of UHECRs CRs can only be accelerated to ~ PeV Proton dominate in nearly all the energy range Poor fit to the spectrum ~ 1/30 CO WDs The number density of ONeMg WDs is lower than CO WDs Difficult to reconcile Auger data E GeV cm 2 sr 1 s 1 Gamma rays can escape from sources Neutron pion decay, photodeexcitation, Bethe-Heitler process Simulation resolution 14/14
Tidal Disruption of Stars as a possible origin of ultra-high energy cosmic ray and neutrinos
Tidal Disruption of Stars as a possible origin of ultra-high energy cosmic ray and neutrinos Credit: CXC/M. Weiss Daniel Biehl DPG spring meeting March 22, 2018 [DB, D. Boncioli, C. Lunardini, W. Winter
More informationCosmic Ray Astronomy. Qingling Ni
Cosmic Ray Astronomy Qingling Ni What is Cosmic Ray? Mainly charged particles: protons (hydrogen nuclei)+helium nuclei+heavier nuclei What s the origin of them? What happened during their propagation?
More informationGamma-ray bursts as the sources of the ultra-high energy cosmic rays?
Gamma-ray bursts as the sources of the ultra-high energy cosmic rays? ACP seminar, IPMU Kashiwa, Japan Oct. 30, 2013 Walter Winter Universität Würzburg Contents Introduction Simulation of sources Multi-messenger
More informationarxiv: v1 [astro-ph.he] 14 Jul 2017
Cosmogenic gamma-rays and neutrinos constrain UHECR source models Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands E-mail: a.vanvliet@astro.ru.nl arxiv:1707.04511v1 [astro-ph.he]
More informationCosmic Rays in the Galaxy
1, Over View Cosmic Rays in the Galaxy Discovery : Legendary baloon flight of Victor Hess Observation of Cosmic Rays : Satellite, Balloon (Direct), Air shower (Indirect) Energy Spectrum of Cosmic Rays
More informationOn the GCR/EGCR transition and UHECR origin
UHECR 2014 13 15 October 2014 / Springdale (Utah; USA) On the GCR/EGCR transition and UHECR origin Etienne Parizot 1, Noémie Globus 2 & Denis Allard 1 1. APC Université Paris Diderot France 2. Tel Aviv
More informationUltrahigh Energy Cosmic Rays propagation II
Ultrahigh Energy Cosmic Rays propagation II The March 6th lecture discussed the energy loss processes of protons, nuclei and gamma rays in interactions with the microwave background. Today I will give
More informationHigh-Energy Neutrinos from Gamma-Ray Burst Fireballs
High-Energy Neutrinos from Gamma-Ray Burst Fireballs Irene Tamborra GRAPPA Center of Excellence, University of Amsterdam TAUP 2015 Turin, September 9, 2015 Outline IceCube detection of high-energy neutrinos
More informationPeV Neutrinos from Star-forming Regions. Hajime Takami KEK, JSPS Fellow
PeV Neutrinos from Star-forming Regions Hajime Takami KEK, JSPS Fellow Outline 0. Basic requirements for PeV neutrinos. Review on cosmogenic neutrinos for the PeV neutrinos. PeV neutrinos from Star-forming
More informationSecondary particles generated in propagation neutrinos gamma rays
th INT, Seattle, 20 Feb 2008 Ultra High Energy Extragalactic Cosmic Rays: Propagation Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Energy loss processes protons
More informationA few grams of matter in a bright world
A few grams of matter in a bright world Benjamin Rouillé d Orfeuil (LAL) Fellow Collaborators: D. Allard, C. Lachaud & E. Parizot (APC) A. V. Olinto (University of Chicago) February 12 th 2013 LAL All
More informationLow-Energy Cosmic Rays
Low-Energy Cosmic Rays Cosmic rays, broadly defined, are charged particles from outside the solar system. These can be electrons, protons, or ions; the latter two dominate the number observed. They are
More informationProbing the extragalactic cosmic rays origin with gamma-ray and neutrino backgrounds
Probing the extragalactic cosmic rays origin with gamma-ray and neutrino backgrounds Denis Allard laboratoire Astroparticule et Cosmologie (APC, CNRS/Paris 7) in collaboration with Noemie Globus, E. Parizot,
More informationUltra-high energy cosmic rays: gamma-ray bursts messengers?
Ultra-high energy cosmic rays: gamma-ray bursts messengers? School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel E-mail: noemie@wise.tau.ac.il Denis Allard Laboratoire Astroparticule
More informationUltra High Energy Cosmic Rays I
Ultra High Energy Cosmic Rays I John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020 ev. Problem: the microwave background radiation is discovered
More informationNeutrino Flavor Ratios Modified by Cosmic Ray Secondary- acceleration
Neutrino Flavor Ratios Modified by Cosmic Ray Secondary- acceleration ref.) NK & Ioka 2015, PRD accepted (arxiv:1504.03417) Norita Kawanaka (Univ. of Tokyo) Kunihito Ioka (KEK/Sokendai) TeV Particle Astrophysics
More informationMagnetic field and flavor effects on the neutrino fluxes from cosmic accelerators
Magnetic field and flavor effects on the neutrino fluxes from cosmic accelerators NUSKY 2011 June 20-24, 2011 ICTP Trieste, Italy Walter Winter Universität Würzburg Introduction Contents Simulation of
More informationAMS-02 Antiprotons Reloaded
AMS-02 Antiprotons Reloaded Rolf Kappl Bethe Center for Theoretical Physics & Physikalisches Institut der Universität Bonn based on RK, Annika Reinert, Martin Wolfgang Winkler JCAP 10 (2015) 034, arxiv:1506.04145
More informationQuestions 1pc = 3 ly = km
Cosmic Rays Historical hints Primary Cosmic Rays: - Cosmic Ray Energy Spectrum - Composition - Origin and Propagation - The knee region and the ankle Secondary CRs: -shower development - interactions Detection:
More informationPerspectives on Nuclear Astrophysics
Perspectives on Nuclear Astrophysics and the role of DUSEL Nuclear Astrophysics is a broad field that needs facilities from 1keV-100GeV A low energy accelerator DIANA a DUSEL is a unique instrument for
More informationOn (shock. shock) acceleration. Martin Lemoine. Institut d Astrophysique d. CNRS, Université Pierre & Marie Curie
On (shock ( shock) acceleration of ultrahigh energy cosmic rays Martin Lemoine Institut d Astrophysique d de Paris CNRS, Université Pierre & Marie Curie 1 Acceleration Hillas criterion log 10 (B/1 G) 15
More informationUltra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux
The 4th International Workshop on The Highest Energy Cosmic Rays and Their Sources INR, Moscow May 20-22, 2008 Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux Oleg Kalashev* (INR RAS)
More informationInvestigation on mass composition of UHE cosmic rays using CRPropa 2.0
Investigation on mass composition of UHE cosmic rays using CRPropa. G Rastegarzade B Parvizi,, Physics Department, Semnan University, Semnan, P.O. Box 596-599, Iran Email: G_ rastegar@alum.sharif.edu Abstract
More informationMULTIMESSENGER APPROACH:Using the Different Messengers
MULTIMESSENGER APPROACH:Using the Different Messengers PROTONS p NUCLEI (A,Z) NEUTRINOS νµ PHOTONS LECTURE PLAN: 1) COSMIC RAYS- proton interactions with photons, composition, nuclei interactions with
More informationarxiv:astro-ph/ v1 13 May 1999
Photomeson production in astrophysical sources arxiv:astro-ph/9905153v1 13 May 1999 1. Introduction A. Mücke 1, J.P. Rachen 2,3, R. Engel 4, R.J. Protheroe 1 and T. Stanev 4 (1) University of Adelaide
More informationarxiv: v1 [astro-ph.he] 6 Nov 2017
arxiv:1711.02091v1 [astro-ph.he] 6 Nov 2017 Neutrinos and Ultra-High-Energy Cosmic-Ray Nuclei from Blazars Xavier Rodrigues, Anatoli Fedynitch, Shan Gao, Denise Boncioli, and Walter Winter DESY, Platanenallee
More informationCosmogenic neutrinos II
Cosmogenic neutrinos II Dependence of fluxes on the cosmic ray injection spectra and the cosmological evolution of the cosmic ray sources Expectations from the cosmic ray spectrum measured by the Auger
More informationBlazars as the Astrophysical Counterparts of the IceCube Neutrinos
Blazars as the Astrophysical Counterparts of the IceCube Neutrinos Maria Petropoulou Department of Physics & Astronomy, Purdue University, West Lafayette, USA Einstein Fellows Symposium Harvard-Smithsonian
More informationNeutrino Flavor Ratios as a Probe of Cosmic Ray Accelerators( 予定 ) Norita Kawanaka (UTokyo) Kunihito Ioka (KEK, Sokendai)
Neutrino Flavor Ratios as a Probe of Cosmic Ray Accelerators( 予定 ) Norita Kawanaka (UTokyo) Kunihito Ioka (KEK, Sokendai) Introduction High Energy Neutrinos are produced in Cosmic Ray Accelerators (GRBs,
More informationAstronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused
More informationCharged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful
Charged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful Charged-particle astronomy coming of age How it is done The sources The signals What we have learned
More informationCitation PHYSICAL REVIEW LETTERS (2006), 97( RightCopyright 2006 American Physical So
Title High energy neutrino flashes from f flares in gamma-ray bursts Author(s) Murase, K; Nagataki, S Citation PHYSICAL REVIEW LETTERS (2006), 97( Issue Date 2006-08-04 URL http://hdl.handle.net/2433/50481
More informationIceCube neutrinos and the origin of cosmic-rays. E. Waxman Weizmann Institute of Science
IceCube neutrinos and the origin of cosmic-rays E. Waxman Weizmann Institute of Science E -2.7 E -3 log [dn/de] The origin of Cosmic Rays: Open Questions Detection: Space (direct) Ground (Air-showers indirect)
More informationCosmic Rays. Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon
Cosmic Rays Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon Nobel Prize in 1936 Origin of high energy cosmic rays is still not completely understood
More informationStellar Explosions (ch. 21)
Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least
More informationDetailed simulations of Fermi-LAT constraints on UHECR production scenarios
Detailed simulations of Fermi-LAT constraints on UHECR production scenarios Center for Cosmology and Particle Physics, Department of Physics, New York University, NY, NY 10003 USA E-mail: msm659@nyu.edu
More informationAMS-02 Antiprotons Reloaded
AMS-02 Antiprotons Reloaded Martin W. Winkler in collaboration with R. Kappl and A. Reinert based on JCAP 09/2014 and arxiv:1506.04145 TAUP 2015 Torino September 9 2015 Martin W. Winkler (Bonn University)
More informationEvolution of High Mass Stars
Luminosity (L sun ) Evolution of High Mass Stars High Mass Stars O & B Stars (M > 4 M sun ): Burn Hot Live Fast Die Young Main Sequence Phase: Burn H to He in core Build up a He core, like low-mass stars
More informationProduction of Beryllium and Boron by Spallation in Supernova Ejecta
Production of Beryllium and Boron by Spallation in Supernova Ejecta Deepa Majmudar 1, James H. Applegate 2 arxiv:astro-ph/9708010v1 1 Aug 1997 1:Dept. of Physics, Columbia University, 538 W. 120th Street,
More informationON GRB PHYSICS REVEALED BY FERMI/LAT
Proceedings of the 3rd Galileo Xu Guangqi Meeting International Journal of Modern Physics: Conference Series Vol. 23 (2013) 223 227 c World Scientific Publishing Company DOI: 10.1142/S2010194513011343
More informationarxiv: v1 [astro-ph.he] 27 Dec 2018
EPJ Web of Conferences will be set by the publisher DOI: will be set by the publisher c Owned by the authors, published by EDP Sciences, 018 arxiv:181.750v1 [astro-ph.he] 7 Dec 018 Ultra High Energy Cosmic
More informationSTATUS OF ULTRA HIGH ENERGY COSMIC RAYS
STATUS OF ULTRA HIGH ENERGY COSMIC RAYS Esteban Roulet (Bariloche) COSMO / CosPA 2010, Tokyo Power law flux stochastic (Fermi) acceleration in shocks cosmic ray flux Small fractional energy gain after
More informationHigh Energy Emission. Brenda Dingus, LANL HAWC
High Energy Emission from GRBs Brenda Dingus, LANL HAWC What are GRBs? Cosmological distance Typical observed z>1 Energy released is up to few times the rest mass of Sun (if isotropic) in a few seconds
More informationType II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with
Type II Supernovae Overwhelming observational evidence that Type II supernovae are associated with the endpoints of massive stars: Association with spiral arms in spiral galaxies Supernova in M75 Type
More informationImplications of recent cosmic ray results for ultrahigh energy neutrinos
Implications of recent cosmic ray results for ultrahigh energy neutrinos Subir Sarkar Neutrino 2008, Christchurch 31 May 2008 Cosmic rays have energies upto ~10 11 GeV and so must cosmic neutrinos knee
More informationHigh energy neutrino production in the core region of radio galaxies due to particle acceleration by magnetic reconnection
High energy neutrino production in the core region of radio galaxies due to particle acceleration by magnetic reconnection University of Sao Paulo) E-mail: bkhiali@usp Elisabete de Gouveia Dal Pino University
More informationSN1987A before(right) and during the explosion. Supernova Explosion. Qingling Ni
SN1987A before(right) and during the explosion Supernova Explosion Qingling Ni Overview Core-Collapse supernova (including Type II supernova) -Mechanism: collapse+rebound Type Ia supernova -Mechanism:
More informationExtensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware
Extensive Air Showers and Particle Physics Todor Stanev Bartol Research Institute Dept Physics and Astronomy University of Delaware Extensive air showers are the cascades that develop in the atmosphere
More informationNumerical simulations of radiation processes in AGN.
Numerical simulations of radiation rocesses in AGN. Effect of chemical comosition Xavier Rodrigues DESY, Zeuthen, Germany Astroteilchenschule, Bärnfels October 14, 2016 Introduction > Question: origin
More informationCosmic Ray Transport (in the Galaxy) Luke Drury. Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath
Cosmic Ray Transport (in the Galaxy) Luke Drury Dublin Institute for Advanced Studies Institiúid Ard-Léinn Bhaile Átha Cliath 1 A few disclaimers and preliminary remarks! Not my main field of research
More informationCosmic Accelerators. 2. Pulsars, Black Holes and Shock Waves. Roger Blandford KIPAC Stanford
Cosmic Accelerators 2. Pulsars, Black Holes and Shock Waves Roger Blandford KIPAC Stanford Particle Acceleration Unipolar Induction Stochastic Acceleration V ~ Ω Φ I ~ V / Z 0 Z 0 ~100Ω P ~ V I ~ V 2 /Z
More informationHigh energy events in IceCube: hints of decaying leptophilic Dark Matter?
High energy events in IceCube: hints of decaying leptophilic Dark Matter? 33rd IMPRS Workshop Max Planck Institute for Physics (Main Auditorium), Munich 26/10/2015 Messengers from space Messengers from
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More informationIntroductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
More informationEeV Neutrinos in UHECR Surface Detector Arrays:
EeV Neutrinos in UHECR Surface Detector Arrays: OBSERVATORY Challenges & Opportunities Karl-Heinz Kampert Bergische Universität Wuppertal High-Energy neutrino and cosmic ray astrophysics - The way forward
More informationLife of a High-Mass Stars
Life of a High-Mass Stars 1 Evolutionary Tracks Paths of high-mass stars on the HR Diagram are different from those of low-mass stars. Once these stars leave the main sequence, they quickly grow in size
More information1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker
46 1939 Baade&Zwicky 1949 Fermi 1977 (Krymski; Axford; Bell; Blandford & Ostriker From Aharonian et al. 2011 From Letessier-Sevon & Stanev 2011 Fermi 2-year sky map Outline 1. 2. 3. 4. knee ankle (b)
More informationScience case for recording protonoxygen collisions at the LHC
Science case for recording protonoxygen collisions at the LHC Hans Dembinski MPIK Heidelberg LHC WG Forward Physics and Diffraction 2018-03-20 KASCADE, IceCube, TUNKA Pierre Auger, Telescope Array data
More informationStrong collisionless shocks are important sources of TeV particles. Evidence for TeV ions is less direct but very strong.
Collisionless Shocks in 12 minutes or less Don Ellison, North Carolina State Univ. Andrei Bykov, Ioffe Institute, St. Petersburg Don Warren, RIKEN, Tokyo Strong collisionless shocks are important sources
More informationThe Secondary Universe
Secondary photons and neutrinos from distant blazars and the intergalactic magnetic fields UC Berkeley September 11, 2011 The talk will be based on A new interpretation of the gamma-ray observations of
More informationGRB : Modeling of Multiwavelength Data
GRB 090510: Modeling of Multiwavelength Data Soeb Razzaque NRC-NRL, Washington, DC Gamma Ray Bursts Workshop, Nov 8-12, GSFC Detection of GRB 090510 Fermi GBM and LAT observations Trigger on 2009 May 10
More informationarxiv: v1 [astro-ph.he] 4 Jan 2018
NEUTRINO ASTRONOMY 2017 arxiv:1801.01551v1 [astro-ph.he] 4 Jan 2018 T.K. Gaisser Department of Physics and Astronomy and Bartol Research Institute University of Delaware, Newark, DE 19716, USA This overview
More informationStrangelets from space. Jes Madsen University of Aarhus, Denmark
Strangelets from space Jes Madsen University of Aarhus, Denmark Strangelets from space What are strangelets? Why are they interesting as ultra-high energy cosmic rays? Could a significant cosmic strangelet
More informationAstroparticle Physics with IceCube
Astroparticle Physics with IceCube Nick van Eijndhoven nickve.nl@gmail.com http://w3.iihe.ac.be f or the IceCube collaboration Vrije Universiteit Brussel - IIHE(ULB-VUB) Pleinlaan 2, B-1050 Brussel, Belgium
More informationMattia Di Mauro. Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background. Trieste, May, 3, 2016
Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background Mattia Di Mauro On behalf of the Fermi- LAT Collaboration 1 Trieste, May, 3, 2016 THE ISOTROPIC GAMMA RAY BACKGROUND
More informationSupernova events and neutron stars
Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly
More informationUltra High Energy Cosmic Rays: Observations and Analysis
Ultra High Energy Cosmic Rays: Observations and Analysis NOT A NEW PROBLEM, STILL UNSOLVED John Linsley (PRL 10 (1963) 146) reports on the detection in Vulcano Ranch of an air shower of energy above 1020
More informationFrom the Knee to the toes: The challenge of cosmic-ray composition
New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg New Views of
More informationAbsorption and production of high energy particles in the infrared background
Roma I, 16 March 2007 Absorption and production of high energy particles in the infrared background Todor Stanev Bartol Research Institute University of Delaware Newark, DE19716 We discuss the role of
More informationAn Astrophysical Plasma Wakefield Accelerator. Alfven Wave Induced Plasma Wakefield Acceleration
An Astrophysical Plasma Wakefield Accelerator Alfven Wave Induced Plasma Wakefield Acceleration Laboratory Astrophysics at SLAC Study in a Laboratory setting: Fundamental physics Astrophysical Dynamics
More informationGalactic cosmic rays propagation
Galactic cosmic rays propagation Side view of the Galaxy The Solar system is 8.5 kpc away from the galactic center. One pc is 3.10 18 cm, so we are at a distance of 2.55 10 17 km and the light from it
More informationThe positron and antiproton fluxes in Cosmic Rays
The positron and antiproton fluxes in Cosmic Rays Paolo Lipari INFN Roma Sapienza Seminario Roma 28th february 2017 Preprint: astro-ph/1608.02018 Author: Paolo Lipari Interpretation of the cosmic ray positron
More informationNeutrinos from charm production: atmospheric and astrophysical applications
Neutrinos from charm production: atmospheric and astrophysical applications Mary Hall Reno Department of Physics and Astronomy University of Iowa Iowa City, Iowa, 52242, USA 1 Introduction High energy
More informationCosmic-ray energy spectrum around the knee
Cosmic-ray energy spectrum around the knee M. SHIBATA Department of Physics, Yokohama National University, Yokohama, 240-8501, Japan Interesting global and fine structures of cosmic-ray energy spectrum
More informationVery high energy photons and neutrinos: Implications for UHECR
EPJ Web of Conferences 53, 01012 (2013) DOI: 10.1051/epjconf/20135301012 C Owned by the authors, published by EDP Sciences, 2013 Very high energy photons and neutrinos: Implications for UHECR Thomas K.
More informationarxiv: v1 [astro-ph.he] 14 Nov 2011
Extragalactic propagation of ultrahigh energy cosmic-rays arxiv:1111.3290v1 [astro-ph.he] 14 Nov 2011 Denis Allard Laboratoire Astroparticule et Cosmologie (APC), Université Paris 7/CNRS, 10 rue A. Domon
More informationPoS(NOW2016)041. IceCube and High Energy Neutrinos. J. Kiryluk (for the IceCube Collaboration)
IceCube and High Energy Neutrinos Stony Brook University, Stony Brook, NY 11794-3800, USA E-mail: Joanna.Kiryluk@stonybrook.edu IceCube is a 1km 3 neutrino telescope that was designed to discover astrophysical
More informationCosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time.
Cosmic Rays 1. Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked' away in time, and this could never be prevented, no matter how good the
More informationarxiv: v2 [hep-ph] 23 Jun 2016
Energy and angular distributions of atmospheric muons at the Earth arxiv:1606.06907v [hep-ph] Jun 016 Prashant Shukla Nuclear Physics Division, Bhabha Atomic Research Centre, Mumbai 400085, India. Homi
More informationPossible high energy phenomena related to the stellar capture by the galactic supermassive black holes. K S Cheng University of Hong Kong China
Possible high energy phenomena related to the stellar capture by the galactic supermassive black holes K S Cheng University of Hong Kong China Outline Introduction Swift J1644+57 Positron Annihilation
More informationSupernova Remnants as Cosmic Ray Accelerants. By Jamie Overbeek Advised by Prof. J. Finley
Supernova Remnants as Cosmic Ray Accelerants By Jamie Overbeek Advised by Prof. J. Finley Cosmic Rays Discovered by Victor Hess in 1911 during a balloon flight through Austria He used an electroscope to
More informationPEV NEUTRINOS FROM THE PROPAGATION OF ULTRA-HIGH ENERGY COSMIC RAYS. Esteban Roulet CONICET, Bariloche, Argentina
PEV NEUTRINOS FROM THE PROPAGATION OF ULTRA-HIGH ENERGY COSMIC RAYS Esteban Roulet CONICET, Bariloche, Argentina THE ENERGETIC UNIVERSE multi-messenger astronomy γ ν p γ rays neutrinos Fermi Amanda UHE
More informationFermi: Highlights of GeV Gamma-ray Astronomy
Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy
More informationMulti-messenger light curves from gamma-ray bursts
Multi-messenger light curves from gamma-ray bursts 1409.2874, 1606.02325 Mauricio Bustamante Center for Cosmology and AstroParticle Physics (CCAPP) The Ohio State University 8th Huntsville Gamma-Ray Burst
More informationNeutrino sources. Atmospheric neutrinos Solar neutrinos Supernova neutrinos High energy neutrino sources Cosmic neutrino background
Neutrino sources Natural sources: Atmospheric neutrinos Solar neutrinos Supernova neutrinos High energy neutrino sources Cosmic neutrino background Artificial sources Accelerator neutrinos Reactor neutrinos
More informationStars with Mⵙ go through two Red Giant Stages
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Death of Stars Nuclear reactions in small stars How stars disperse carbon How low mass stars die The nature of white dwarfs
More informationParameters Sensitive to the Mass Composition of Cosmic Rays and Their Application at the Pierre Auger Observatory
WDS'12 Proceedings of Contributed Papers, Part III, 137 141, 2012. ISBN 978-80-7378-226-9 MATFYZPRESS Parameters Sensitive to the Mass Composition of Cosmic Rays and Their Application at the Pierre Auger
More informationPublications of Francesco Arneodo: journal articles
Publications of Francesco Arneodo: journal articles Figure 1: Citation report from ISI Web of Science (IF=31.0) [1] E. Aprile et al., First Axion Results from the XENON100 Experiment, arxiv.org (submitted
More informationParticle acceleration and generation of high-energy photons
Particle acceleration and generation of high-energy photons For acceleration, see Chapter 21 of Longair Ask class: suppose we observe a photon with an energy of 1 TeV. How could it have been produced?
More informationUltrahigh Energy cosmic rays II
Ultrahigh Energy cosmic rays II Today we will discuss the new data on UHECR presented during the last couple of years by the Auger observatory in Argentina. These data do not match previous analyses and
More informationCOSMIC RAYS DAY INTRODUCTION TO COSMIC RAYS WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII
COSMIC RAYS DAY WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII INTRODUCTION TO COSMIC RAYS MAJOR QUESTIONS: Are there forms of matter in the Universe that do not
More informationNeutrinos from GRBs, and the connection to gamma- and cosmic-rays
Neutrinos from GRBs, and the connection to gamma- and cosmic-rays Philipp Baerwald Institut für Theoretische Physik und Astrophysik Universität Würzburg in collaboration with Mauricio Bustamante, Svenja
More informationInterpretation of cosmic ray spectrum above the knee measured by the Tunka-133 experiment
Interpretation of cosmic ray spectrum above the knee measured by the Tunka-133 experiment L.G. Sveshnikova, L.A. Kuzmichev, E.E. Korosteleva, V.A. Prosin, V.S. Ptuskin et al Moscow State University Skobeltsyn
More informationThe FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley)
The FIR-Radio Correlation & Implications for GLAST Observations of Starburst Galaxies Eliot Quataert (UC Berkeley) w/ Todd Thompson & Eli Waxman Thompson, Quataert, & Waxman 2007, ApJ, 654, 219 Thompson,
More information> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!
> News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May
More informationCOSMIC RAYS AND AGN's
COSMIC RAYS AND AGN's RAZELE COSMICE ŞI NUCLEELE GALACTICE ACTIVE (don't worry, it is in Romanian) Sorin Roman sroman@mpifr-bonn.mpg.de We'll try to talk about: -History -Composition -CR Spectrum -Detection
More informationThe Physics of Ultrahigh Energy Cosmic Rays. Example Poster Presentation Physics 5110 Spring 2009 Reminder: Posters are due Wed April 29 in class.
The Physics of Ultrahigh Energy Cosmic Rays Example Poster Presentation Physics 5110 Spring 2009 Reminder: Posters are due Wed April 29 in class. 1 Introduction to Cosmic Rays References: http://www.phy.bris.ac.uk/groups/particle/pus/affo
More informationHigh Energy Particle Production by Space Plasmas
Plasmas in Astrophysics and in Laboratory, 20 21 June, 2011 High Energy Particle Production by Space Plasmas A.A.Petrukhin National Research Nuclear University MEPhI C o n t e n t s 1. Introduction 2.
More informationCh. 16 & 17: Stellar Evolution and Death
Ch. 16 & 17: Stellar Evolution and Death Stars have lives: born, evolve, die Mass determines stellar evolution: Really Low Mass (0.08 to 0.4 M sun ) Low Mass: (0.4 to 4 M sun ) Long lives High Mass (4
More informationImplication of AMS-02 positron fraction measurement. Qiang Yuan
Implication of AMS-02 positron fraction measurement Qiang Yuan (yuanq@ihep.ac.cn) Institute of High Energy Physics, Chinese Academy of Sciences Collaborated with Xiaojun Bi, Guo-Ming Chen, Yi-Qing Guo,
More information