Ultra High Energy Cosmic Rays. UHECRs from Mildly Relativistic Supernovae

Size: px
Start display at page:

Download "Ultra High Energy Cosmic Rays. UHECRs from Mildly Relativistic Supernovae"

Transcription

1 Ultra High Energy Cosmic Rays from Mildly Relativistic Supernovae Tata Institute of Fundamental Research Mumbai, India March 13, 2012

2 Outline UHECRS Chakraborti, Ray, Soderberg, Loeb, Chandra 2011 Nature Communications 2, UHECRS

3 Ultra High Energy Cosmic Rays One Problem Many Solutions Yet another solution Pack a LOT of energy Cant be caught by satellites Detected by air-showers

4 Who ordered that? UHECRS One Problem Many Solutions Yet another solution Interact with Lorentz boosted CMB photons Must come from within the GZK horizon Must have right combination of B-R Must have right rates and energetics Where are the sources?

5 Possible sources UHECRS One Problem Many Solutions Yet another solution Galactic (but with very high galactic magnetic field) Cosmological (but with Lorentz Violation during propagation) Active Galactic Nuclei (AGNs) Gamma Ray Bursts (GRBs) Hypernovae...

6 Why another solution? One Problem Many Solutions Yet another solution None of the existing astronomical sources are satisfactory Must investigate all potential sources before modifying physics New sources in hand

7 Mildly Relativistic Supernovae The prototype SN 2009bb Host Galaxy Map Our Scheme Figure: Comparison of SN 2009bb blastwave velocity and energy with those of type Ibc SNe and nearby GRBs. (Soderberg et al. Nature 2010)

8 SN 2009bb UHECRS The prototype SN 2009bb Host Galaxy Map Our Scheme Found in radio follow up of > 100 type Ibc SNe Bright radio emission seen by VLA and GMRT Requires engine driven relativistic ejecta

9 Giant Metrewave Radio Telescope The prototype SN 2009bb Host Galaxy Map Our Scheme

10 GMRT map of host galaxy The prototype SN 2009bb Host Galaxy Map Our Scheme NGC3278 on AUGUST 2009 STOKES I at MHZ DECLINATION (J2000) RIGHT ASCENSION (J2000) Grey scale flux range= MilliJY/BEAM Cont peak flux = E-02 JY/BEAM Levs = 2.500E-04 * (1, 2, 4, 8, 16, 32) Figure: 617 MHz map of the host galaxy from the GMRT, showing the location of the supernova

11 UHECRS The prototype SN 2009bb Host Galaxy Map Our Scheme Mildly Relativistic Supernovae

12 B-R Combination UHECRS Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field From Waxman

13 B-R Combination UHECRS Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field

14 How to figure out B-R? Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field Use Rybicki and Lightman

15 How to figure out B-R? Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field Chevalier s Prescription for SSA «1/19 «9/19 «18/19 R α 1/19 f Fop D ν 1 cm, 0.5 mjy Mpc 5 GHz (1) «4/19 «2/19 «4/19 B 1.1α 4/19 f Fop D ν 0.5 mjy Mpc 5 GHz G. (2)

16 SN 2009bb: Spectrum UHECRS Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field Figure: Radio spectrum (F ν ) of SN 2009bb, obtained from coordinated observations using the VLA and GMRT. The spectrum at high frequencies is given by optically thin synchrotron, while it is suppressed at low frequencies by SSA. (Soderberg et al. Nature 2010)

17 SN 2009bb: B-R Evolution Maximum energy SSA Estimates SSA Spectrum Size-Magnetic Field Figure: Hillas Diagram: SN 2009bb may accelerate Fe to 166 EeV

18 Rate UHECRS Energy Budget SN 2009bb: Energetics Γ inj = (0.7 20) erg Mpc 3 yr 1 At the rate of SN 2009bb like objects, each of them has to put in around E SN = (0.3 9) ergs Much more than the E eq ergs required to naively explain the radio emission in SN 2009bb Re-examine energy budget

19 SN 2009bb: Energy Budget Energy Budget SN 2009bb: Energetics Collisional slowdown dγ γ 2 1 = dm M (3) de = c 2 (γ 1)dm (4) and ρ r 2 (5) Z m(r γ2 2) = (γ 1 1) 1/2 (γ 1 + 1) 1/2 m(r 1) + M 0 γ 1 (γ 1) 3/2 (γ + 1) 3/2 dγ (6)

20 Energy Budget SN 2009bb: Energetics Radius Evolution in Observer s Time: R(t) SN 2009bb M 0 =10-1 M sol M 0 =10-2 M sol M 0 = M sol R lat (cm) T obs (days) Figure: R lat (t obs ) evolution in the observer s frame, determined from SSA

21 Blastwave Energetics UHECRS Energy Budget SN 2009bb: Energetics Mass-Energy estimates M M (7) E Baryons ergs (8) Coupled with (uncertain) rates for these objects, gives the correct energy for the energy injection rate required in UHECRs.

22 Are there enough of them? Magnetic deflections Rate of X-Ray transients Rate of Radio transients Hosted by gas rich spirals (remember HIPASS correlation?) 21 cm fluxes of NGC3278 indicates M of HI. SNe Ibc occur at a rate of Gpc 3 yr 1 SN 2009bb like events 0.7% Mpc 3 yr 1 XRF like Mpc 3 yr 1 > 60 arrival directions need to be explained How do we spot these objects?

23 Are there enough of them? Magnetic deflections Rate of X-Ray transients Rate of Radio transients 4 objects within 200 Mpc per year Cosmic rays of different energies have different travel delays due to deflections by magnetic fields τ delay 10 5 yrs May receive particles from any of possible sources at any time.

24 X-Ray transients UHECRS Magnetic deflections Rate of X-Ray transients Rate of Radio transients Assuming that, the accelerated electrons have the same initial power-law index for their energy spectrum as the protons, and that they lose all their energy radiatively (Waxman & Loeb 2009). Rate of X-Ray transients ṅ t ɛ Γ inj «10 44 erg Mpc 3 yr 1 νl ν erg s 1 «1 Mpc 3 SN 2009bb had an X-ray luminosity of L X = 4.4 ± erg s 1. This luminosity and the rate of the relativistic SNe, together can account for the UHECR flux, if they remain active accelerators for t of order 1 year. (9)

25 Radio transients UHECRS Magnetic deflections Rate of X-Ray transients Rate of Radio transients Assuming that the electrons and magnetic fields together have a fraction ɛ of the energy of the relativistic protons (which is assumed to be divided equally into 10 logarithmic bins, assuming p 2 for the protons), we compute the minimum required rate of such transients with peak radio luminosity L op, which remain mildly relativistic at least until the SSA peak frequency drops to ν, as Rate of X-Ray transients ṅ Γ inj ` ɛ 23/19 L op erg Mpc 3 yr ergs/sec/hz ` ν Mpc 3 yr 1 (10) 0.5 GHz 2 η 11 (1+η 17 ) Radio analogue of Waxman & Loeb s equation for X-Ray transients.

26 Another 09bb-like SN Thanks Questions SN 2012ap: A new broad-lined Sn Ib/c

27 SN 2012ap: Relativistic Ejecta Another 09bb-like SN Thanks Questions

28 Thanks UHECRS Another 09bb-like SN Thanks Questions My collaborators Alak, Alicia, Avi and Poonam VLA (run by NRAO) and GMRT (run by TIFR) for observations All of you for coming to the talk

29 Questions? UHECRS Another 09bb-like SN Thanks Questions If you have a question later, me at sayan@tifr.res.in

arxiv:astro-ph/ v1 18 Nov 2003

arxiv:astro-ph/ v1 18 Nov 2003 Low frequency radio and X-ray properties of core-collapse supernovae arxiv:astro-ph/0311419 v1 18 Nov 2003 A. Ray 1, P. Chandra 1,2, F. Sutaria 3, and S. Bhatnagar 4,5 1 Tata Institute of Fundamental Research,

More information

arxiv: v2 [astro-ph.he] 3 Jan 2011

arxiv: v2 [astro-ph.he] 3 Jan 2011 DRAFT October 1, 018 Preprint typeset using L A TEX style emulateapj v. 5/5/10 BARYON LOADED RELATIVISTIC BLASTWAVES IN SUPERNOVAE Sayan Chakraborti 1 & Alak Ray 1 Department of Astronomy and Astrophysics,

More information

Multi-Messenger Astonomy with Cen A?

Multi-Messenger Astonomy with Cen A? Multi-Messenger Astonomy with Cen A? Michael Kachelrieß NTNU, Trondheim [] Outline of the talk 1 Introduction 2 Dawn of charged particle astronomy? Expectations vs. Auger data Effects of cluster fields

More information

Ultra High Energy Cosmic Rays I

Ultra 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 information

Mass Composition Study at the Pierre Auger Observatory

Mass Composition Study at the Pierre Auger Observatory OBSERVATORY Mass Composition Study at the Pierre Auger Observatory Laura Collica for the Auger Milano Group 4.04.2013, Astrosiesta INAF Milano 1 Outline The physics: The UHECR spectrum Extensive Air Showers

More information

Cosmic Ray Astronomy. Qingling Ni

Cosmic 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 information

Ultrahigh Energy Cosmic Rays propagation II

Ultrahigh 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 information

On (shock. shock) acceleration. Martin Lemoine. Institut d Astrophysique d. CNRS, Université Pierre & Marie Curie

On (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 information

An AstroParticle perspective for SKA and CTA

An AstroParticle perspective for SKA and CTA NRF/NWO Meeting Oct. 18 th, 2012 An AstroParticle perspective for SKA and CTA Sergio Colafrancesco Wits University - DST/NRF SKA Research Chair Email: Sergio.Colafrancesco@wits.ac.za CAP Center for Astroparticle

More information

The 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) 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

The Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar

The Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar The Mystery of Fast Radio Bursts and its possible resolution Outline Pawan Kumar FRBs: summary of relevant observations Radiation mechanism and polarization FRB cosmology Wenbin Lu Niels Bohr Institute,

More information

Ultra-High Energy Cosmic Rays and the GeV-TeV Diffuse Gamma-Ray Flux

Ultra-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 information

Dr. John Kelley Radboud Universiteit, Nijmegen

Dr. John Kelley Radboud Universiteit, Nijmegen arly impressive. An ultrahighoton triggers a cascade of particles mulation of the Auger array. The Many Mysteries of Cosmic Rays Dr. John Kelley Radboud Universiteit, Nijmegen Questions What are cosmic

More information

Secondary particles generated in propagation neutrinos gamma rays

Secondary 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 information

A few grams of matter in a bright world

A 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 information

Radiative Processes in Astrophysics

Radiative Processes in Astrophysics Radiative Processes in Astrophysics 11. Synchrotron Radiation & Compton Scattering Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Synchrotron Self-Absorption synchrotron emission is accompanied

More information

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons

More information

GW from GRBs Gravitational Radiation from Gamma-Ray Bursts

GW from GRBs Gravitational Radiation from Gamma-Ray Bursts GW from GRBs Gravitational Radiation from Gamma-Ray Bursts Tsvi Piran Racah Inst. of Jerusalem, Israel Dafne Guetta,, Ehud Nakar, Reem Sari Once or twice a day we see a burst of low energy gamma-rays from

More information

Shear acceleration in large scale AGN jets and possible application in explaining X-ray emissions

Shear acceleration in large scale AGN jets and possible application in explaining X-ray emissions Shear acceleration in large scale AGN jets and possible application in explaining X-ray emissions Ruo-Yu Liu (MPIK) Collaborators: Frank Rieger, Felix Aharonian, Nayantara Gupta 13.09.2016, IAP, Paris

More information

Ultra- high energy cosmic rays

Ultra- high energy cosmic rays Ultra- high energy cosmic rays Tiina Suomijärvi Institut de Physique Nucléaire Université Paris Sud, Orsay, IN2P3/CNRS, France Atélier CTA, IAP, Paris, 30-31 June 2014 Outline Pierre Auger Observatory:

More information

MULTIMESSENGER APPROACH:Using the Different Messengers

MULTIMESSENGER 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 information

Radio emission from galaxies in the Bootes Voids

Radio emission from galaxies in the Bootes Voids Radio emission from galaxies in the Bootes Voids Mousumi Das, Indian Institute of Astrophysics, Bangalore Large Scale Structure and galaxy flows, Quy Nhon, July 3-9, 2016 Collaborators K.S. Dwarkanath

More information

High Energy Astrophysics

High Energy Astrophysics High Energy Astrophysics Introduction Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk January 2012 Today s introduction - The sky at different

More information

Overview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data

Overview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data Overview: UHECR spectrum and composition Arrival directions and magnetic field Method for search for UHE nuclei sources Application to the Auger data Acceleration of UHECR A.G.N. GRB Radio Galaxy Lobe

More information

Particle Acceleration in the Universe

Particle Acceleration in the Universe Particle Acceleration in the Universe Hiroyasu Tajima Stanford Linear Accelerator Center Kavli Institute for Particle Astrophysics and Cosmology on behalf of SLAC GLAST team June 7, 2006 SLAC DOE HEP Program

More information

Exploring the Ends of the Rainbow: Cosmic Rays in Star-Forming Galaxies

Exploring the Ends of the Rainbow: Cosmic Rays in Star-Forming Galaxies Exploring the Ends of the Rainbow: Cosmic Rays in Star-Forming Galaxies Brian Lacki With Todd Thompson, Eliot Quataert, Eli Waxman, Abraham Loeb 21 September 2010 The Cosmic SED Nonthermal Thermal Nonthermal

More information

An Auger Observatory View of Centaurus A

An Auger Observatory View of Centaurus A An Auger Observatory View of Centaurus A Roger Clay, University of Adelaide based on work particularly done with: Bruce Dawson, Adelaide Jose Bellido, Adelaide Ben Whelan, Adelaide and the Auger Collaboration

More information

UHECRs sources and the Auger data

UHECRs sources and the Auger data UHECRs sources and the Auger data M. Kachelrieß Institutt for fysikk, NTNU Trondheim, Norway I review the evidence for a correlation of the arrival directions of UHECRs observed by the Pierre Auger Observatory

More information

Low-Energy Cosmic Rays

Low-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 information

RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY

RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY RECENT RESULTS FROM THE PIERRE AUGER OBSERVATORY (Neutrino 2008, Christchurch, NZ) Esteban Roulet (Bariloche) the Auger Collaboration: 17 countries, ~100 Institutions, ~400 scientists Argentina, Australia,

More information

GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!

GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts! Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short

More information

Fermi: Highlights of GeV Gamma-ray Astronomy

Fermi: 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 information

Radio followup of ransient sources: Feasibility and practicality

Radio followup of ransient sources: Feasibility and practicality Radio followup of ransient sources: Feasibility and practicality C. H. Ishwara Chandra National Centre for Radio Astrophysics Tata Institute of Fundamental Research Pune University Campus, Pune - India

More information

Detecting High Energy Cosmic Rays with LOFAR

Detecting High Energy Cosmic Rays with LOFAR Detecting High Energy Cosmic Rays with LOFAR Andreas Horneffer for the LOFAR-CR Team LOFAR CR-KSP: Main Motivation Exploring the sub-second transient radio sky: Extensive Air showers as guaranteed signal

More information

Supernova Remnants and Cosmic. Rays

Supernova 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 information

Simultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections

Simultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections Simultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections Ashley Lianne King, University of Michigan Advisor: Jon M. Miller Collaborators: John Raymond, Michael Rupen, Kayhan Gültekin,

More information

COSMIC RAYS AND AGN's

COSMIC 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 information

The AUGER Experiment. D. Martello Department of Physics University of Salento & INFN Lecce. D. Martello Dep. of Physics Univ. of Salento & INFN LECCE

The AUGER Experiment. D. Martello Department of Physics University of Salento & INFN Lecce. D. Martello Dep. of Physics Univ. of Salento & INFN LECCE The AUGER Experiment D. Martello Department of Physics University of Salento & INFN Lecce The Pierre Auger Collaboration Argentina Australia Bolivia Brazil Croatia Czech Rep. France Germany Italy Mexico

More information

Cosmogenic neutrinos II

Cosmogenic 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 information

Gamma-ray Astrophysics

Gamma-ray Astrophysics Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background

More information

The Supernova/Gamma-Ray Burst Connection. Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen

The Supernova/Gamma-Ray Burst Connection. Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen The Supernova/Gamma-Ray Burst Connection Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Galama et al. 1998; Fynbo et al. 2000 SN 1998bw/GRB 980425 Galama et al. 1998 Collapsar

More information

Ultra-High Energy Cosmic Rays and Astrophysics. Hang Bae Kim Hanyang University Hangdang Workshop,

Ultra-High Energy Cosmic Rays and Astrophysics. Hang Bae Kim Hanyang University Hangdang Workshop, Ultra-High Energy Cosmic Rays and Astrophysics Hang Bae Kim Hanyang University Hangdang Workshop, 2012. 08. 22 Ultra High Energy Cosmic Rays Ultra High Energy Cosmic Ray (UHECR)» E 3 E & 10 18 ev Energy

More information

High energy neutrino signals from NS-NS mergers

High energy neutrino signals from NS-NS mergers High energy neutrino signals from NS-NS mergers He Gao 高鹤 University of Nevada Las Vegas Collaborators: Bing Zhang, Xue-Feng Wu & Zi-Gao Dai 2013-05-08 Multi-Messenger Workshop @ KIAA EM signals for a

More information

Cosmological Fast Radio Bursts from Binary White Dwarf Mergers

Cosmological Fast Radio Bursts from Binary White Dwarf Mergers Cosmological Fast Radio Bursts from Binary White Dwarf Mergers Kunihito Ioka (KEK) Kashiyama, KI & Mészáros 13 ~10 yr ago GRB Cosmology Massive star origin High redshift GRBs Like QSO Like SN Star formation

More information

News from the Niels Bohr International Academy

News from the Niels Bohr International Academy News from the Niels Bohr International Academy What is a gamma-ray burst? The development of our understanding of the phenomenon illustrated by important events (including very recent results on gravitational

More information

Radio emission in clusters of galaxies. An observational perspective

Radio emission in clusters of galaxies. An observational perspective Radio emission in clusters of galaxies An observational perspective Tiziana Venturi INAF, IRA, Bologna IV ESTRELA Workshop, Bologna, 19 January 2009 Overview - What are galaxy clusters - Radio emission

More information

Diffusive Particle Acceleration (DSA) in Relativistic Shocks

Diffusive Particle Acceleration (DSA) in Relativistic Shocks Diffusive Particle Acceleration (DSA) in Relativistic Shocks Don Ellison & Don Warren (NCSU), Andrei Bykov (Ioffe Institute) 1) Monte Carlo simulation of Diffusive Shock Acceleration (DSA) in collisionless

More information

CIRCUMSTELLAR EMISSION FROM TYPE Ib AND Ic SUPERNOVAE

CIRCUMSTELLAR EMISSION FROM TYPE Ib AND Ic SUPERNOVAE The Astrophysical Journal, 6:381Y391, 2006 November 1 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. A CIRCUMSTELLAR EMISSION FROM TYPE Ib AND Ic SUPERNOVAE Roger A.

More information

The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005

The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005 The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005 OUTLINE Introduction Messengers,, energy scales, & questions. Detecting Very High Energy

More information

High 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 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 information

Supernovae with SKA. Massimo Della Valle Capodimonte Observatory-INAF Naples

Supernovae with SKA. Massimo Della Valle Capodimonte Observatory-INAF Naples Supernovae with SKA Massimo Della Valle Capodimonte Observatory-INAF Naples Summary Supernova Taxonomy Radio-SN Observations (SKA will do it better) The impact of SKA on SN studies (CC-SNe; SNe-Ia; GRB-SNe,

More information

VHE emission from radio galaxies

VHE emission from radio galaxies VHE emission from radio galaxies Martin Hardcastle The future of gamma-ray astronomy and the CTA Leicester, October 2010 Outline Recap: radio galaxy physics Inverse-Compton emission Locations of high-energy

More information

Lecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble

More information

PoS(IX EVN Symposium)066

PoS(IX EVN Symposium)066 Constraint on the early expansion of XRF 080109, related to supernova SN 28D JIVE, Dwingeloo, The Netherlands MTA Research Group for Physical Geodesy and Geodynamics, Penc, Hungary E-mail: zparagi@jive.nl

More information

Galaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes

Galaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories

More information

Study of the arrival directions of ultra-high-energy cosmic rays detected by the Pierre Auger Observatory

Study of the arrival directions of ultra-high-energy cosmic rays detected by the Pierre Auger Observatory Study of the arrival directions of ultra-high-energy cosmic rays detected by the Pierre Auger Observatory Piera L. Ghia*, for the Pierre Auger Collaboration * IFSI/INAF Torino, Italy, & IPN/CNRS Orsay,

More information

A zoo of transient sources. (c)2017 van Putten 1

A zoo of transient sources. (c)2017 van Putten 1 A zoo of transient sources (c)2017 van Putten 1 First transient @ first light UDFj-39546284, z~10.3 Bouwens, R.J., et al., Nature, 469, 504 Cuchiara, A. et al., 2011, ApJ, 736, 7 z=9.4: GRB 090429B, z~9.4

More information

Occurrence of Radio Halos in galaxy clusters Insight from a mass-selected sample Virginia Cuciti

Occurrence of Radio Halos in galaxy clusters Insight from a mass-selected sample Virginia Cuciti Occurrence of Radio Halos in galaxy clusters Insight from a mass-selected sample Virginia Cuciti In collaboration with: Gianfranco Brunetti, Rossella Cassano, Daniele Dallacasa Coma WSRT radio contours

More information

This presentation was created based on the slides by Vitor de Souza from his talk at the 4th

This presentation was created based on the slides by Vitor de Souza  from his talk at the 4th This presentation was created based on the slides by Vitor de Souza http://cosmicraysschool.ufabc.edu.br/pres/vitor.odp from his talk at the 4th School on Cosmic Rays and Astrophysics UFABC - Santo André

More information

Active Galactic Nuclei OIII

Active Galactic Nuclei OIII Active Galactic Nuclei In 1908, Edward Fath (1880-1959) observed NGC 1068 with his spectroscope, which displayed odd (and very strong) emission lines. In 1926 Hubble recorded emission lines of this and

More information

Recent Results of the Observatory Pierre Auger. João R. T. de Mello Neto Instituto de Física Universidade Federal do Rio de Janeiro

Recent Results of the Observatory Pierre Auger. João R. T. de Mello Neto Instituto de Física Universidade Federal do Rio de Janeiro Recent Results of the Observatory Pierre Auger João R. T. de Mello Neto Instituto de Física Universidade Federal do Rio de Janeiro S. Tomé e Príncipe, September 2009 Outline Cosmic ray detection and the

More information

Possible sources of very energetic neutrinos. Active Galactic Nuclei

Possible sources of very energetic neutrinos. Active Galactic Nuclei Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical

More information

Chapter 17. Active Galaxies and Supermassive Black Holes

Chapter 17. Active Galaxies and Supermassive Black Holes Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study

More information

Mikhail V. Medvedev (KU)

Mikhail V. Medvedev (KU) Students (at KU): Sarah Reynolds, Sriharsha Pothapragada Mikhail V. Medvedev (KU) Collaborators: Anatoly Spitkovsky (Princeton) Luis Silva and the Plasma Simulation Group (Portugal) Ken-Ichi Nishikawa

More information

Physics of Short Gamma-Ray Bursts Explored by CTA and DECIGO/B-DECIGO

Physics of Short Gamma-Ray Bursts Explored by CTA and DECIGO/B-DECIGO Physics of Short Gamma-Ray Bursts Explored by CTA and DECIGO/B-DECIGO Hiroyasu Tajima Institute for Space Earth Environmental Research Nagoya University 17th DECIGO Workshop Nov 1, 18 Nagoya University

More information

Higher Statistics UHECR observatories: a new era for a challenging astronomy

Higher Statistics UHECR observatories: a new era for a challenging astronomy CRIS 2010 100 years of Cosmic Ray Physics: from Pioneering Experiments to Physics in Space 1 Higher Statistics UHECR observatories: a new era for a challenging astronomy Etienne Parizot APC University

More information

Active Galactic Nuclei

Active Galactic Nuclei Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright

More information

Gamma-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? 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 information

Multi-wavelength Astronomy

Multi-wavelength Astronomy astronomy Multi-wavelength Astronomy Content What do we measure Multi-wavelength approach Data Data Mining Virtual Observatory Hands on session Larmor's formula Maxwell's equations imply that all classical

More information

A few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda

A few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda A few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda Radio/X constraints on CSM around SNe Ia Useful limit for SN 2011fe: Mdot/v w < ~10-8 M yr -1 /100km s -1 Radio Chomiuk+

More information

Probing radio emission in Seyfert Galaxies on parsecand kiloparsec-scales

Probing radio emission in Seyfert Galaxies on parsecand kiloparsec-scales The Metrewavelength Sky ASI Conference Series, 2014, Vol. 13, pp 111 115 Edited by J. N. Chengalur & Y. Gupta Probing radio emission in Seyfert Galaxies on parsecand kiloparsec-scales P. Kharb 1, V. Singh

More information

Quasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs

Quasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Goals: Quasars and AGN What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Discovery of Quasars Radio Observations of the Sky Reber (an amateur

More information

Cosmic Rays in Galaxy Clusters: Simulations and Perspectives

Cosmic Rays in Galaxy Clusters: Simulations and Perspectives Cosmic Rays in Galaxy Clusters: Simulations and Perspectives 1 in collaboration with Volker Springel 2, Torsten Enßlin 2 1 Canadian Institute for Theoretical Astrophysics, Canada 2 Max-Planck Institute

More information

Cosmic Rays, Photons and Neutrinos

Cosmic Rays, Photons and Neutrinos Cosmic Rays, Photons and Neutrinos Michael Kachelrieß NTNU, Trondheim [] Introduction Outline Plan of the lectures: Cosmic rays Galactic cosmic rays Basic observations Acceleration Supernova remnants Problems

More information

UHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory

UHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory UHE Cosmic Rays and Neutrinos with the Pierre Auger Observatory Gonzalo Parente Bermúdez Universidade de Santiago de Compostela & IGFAE for the Pierre Auger Collaboration Particle Physics and Cosmology

More information

High Energy Emission. Brenda Dingus, LANL HAWC

High 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 information

Extensive 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 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 information

The AGN / host galaxy connection in nearby galaxies.

The AGN / host galaxy connection in nearby galaxies. The AGN / host galaxy connection in nearby galaxies. A new view of the origin of the radio-quiet / radio-loud dichotomy? Alessandro Capetti & Barbara Balmaverde (Observatory of Torino Italy) The radio-quiet

More information

The Superbubble Power Problem: Overview and Recent Developments. S. Oey

The Superbubble Power Problem: Overview and Recent Developments. S. Oey The Superbubble Power Problem: Overview and Recent Developments S. Oey It has been known for decades that superbubbles generated by massive star winds and supernovae are smaller than expected based on

More information

Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP

Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP Cherenkov Telescope Array A SENSITIVE PROBE OF EXTREME UNIVERSE ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP 2015 1 The CTA Observatory SST ( 4m) LST ( 23m) MST ( 12m) South North

More information

Cosmic Explosions. Greg Taylor (UNM ) Astro 421

Cosmic Explosions. Greg Taylor (UNM ) Astro 421 Cosmic Explosions Greg Taylor (UNM ) Astro 421 1 Cassiopeia A: Supernova Remnant E total ~ 10 46 J 2 An early gamma ray-burst Vela satellite 3 A Gamma Ray Burst Sampler 4 Burst Alert 5 The BeppoSAX Satellite

More information

Ultra High Energy Cosmic Rays: Observations and Analysis

Ultra 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 information

A New View of the High-Energy γ-ray Sky with the Fermi Telescope

A New View of the High-Energy γ-ray Sky with the Fermi Telescope A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11

More information

STATUS OF ULTRA HIGH ENERGY COSMIC RAYS

STATUS 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 information

Radio Afterglows. What Good are They? Dale A. Frail. National Radio Astronomy Observatory. Gamma Ray Bursts: The Brightest Explosions in the Universe

Radio Afterglows. What Good are They? Dale A. Frail. National Radio Astronomy Observatory. Gamma Ray Bursts: The Brightest Explosions in the Universe Radio Afterglows What Good are They? Dale A. Frail National Radio Astronomy Observatory Gamma Ray Bursts: The Brightest Explosions in the Universe The 2 nd Harvard-Smithsonian Conference on Theoretical

More information

Absorption and production of high energy particles in the infrared background

Absorption 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 information

AGN in hierarchical galaxy formation models

AGN in hierarchical galaxy formation models AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction

More information

Electromagnetic counterparts to binary neutron star mergers. Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP)

Electromagnetic counterparts to binary neutron star mergers. Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP) Electromagnetic counterparts to binary neutron star mergers Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP) Summary Electromagnetic counterparts to gravitational waves

More information

Detectors for 20 kev 10 MeV

Detectors for 20 kev 10 MeV Gamma-Ray Bursts Detectors for 20 kev to 10 MeV Discovery The early years BATSE Fast versus slow bursts Uniformity and log N log S relation BeppoSAX and discovery of afterglows Redshift measurements Connection

More information

Topic 7. Relevance to the course

Topic 7. Relevance to the course Topic 7 Cosmic Rays Relevance to the course Need to go back to the elemental abundance curve Isotopes of certain low A elements such as Li, Be and B have larger abundances on Earth than you would expect

More information

Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002

Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays

More information

Radio infrared correlation for galaxies: from today's instruments to SKA

Radio infrared correlation for galaxies: from today's instruments to SKA Radio infrared correlation for galaxies: from today's instruments to SKA Agata P piak 1 T.T. Takeuchi 2, A. Pollo 1,3, A. Solarz 2, and AKARI team 1 Astronomical Observatory of the Jagiellonian University,

More information

Cosmic Rays, GammaRays and the Universal. Background Radiation

Cosmic Rays, GammaRays and the Universal. Background Radiation Cosmic Rays, GammaRays and the Universal Background Radiation Malcolm Longair Cavendish Laboratory, Cambridge Celebrating Occhialini I met Occhialini only a few times, in connection with ESA projects and

More information

Neutrinos, nonzero rest mass particles, and production of high energy photons Particle interactions

Neutrinos, nonzero rest mass particles, and production of high energy photons Particle interactions Neutrinos, nonzero rest mass particles, and production of high energy photons Particle interactions Previously we considered interactions from the standpoint of photons: a photon travels along, what happens

More information

Particle acceleration at relativistic shock waves and gamma-ray bursts

Particle acceleration at relativistic shock waves and gamma-ray bursts Particle acceleration at relativistic shock waves and gamma-ray bursts Martin Lemoine Institut d Astrophysique de Paris CNRS, Université Pierre & Marie Curie Outline: 1. Particle acceleration and relativistic

More information

Charged-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 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 information

Synchrotron Radiation: II. Spectrum

Synchrotron Radiation: II. Spectrum Synchrotron Radiation: II. Spectrum Massimo Ricotti ricotti@astro.umd.edu University of Maryland Synchrotron Radiation: II. Spectrum p.1/18 ds=v dt_em dt=ds cos(theta)/c=v/c cos(theta)dt_em Synchrotron

More information

Can blazar flares be triggered by the VHE gamma-rays from the surrounding of a supermassive black hole?

Can blazar flares be triggered by the VHE gamma-rays from the surrounding of a supermassive black hole? Can blazar flares be triggered by the VHE gamma-rays from the surrounding of a supermassive black hole? Department of Astrophysics, University of Lodz, Lodz, Poland E-mail: p.banasinski@uni.lodz.pl Wlodek

More information

White Paper on Ultra-High Energy Cosmic Rays

White Paper on Ultra-High Energy Cosmic Rays White Paper on Ultra-High Energy Cosmic Rays Corresponding author: A. V. Olinto 1, (olinto@kicp.uchicago.edu) Co-Authors: J. H. Adams 2, C. D. Dermer 3, J.F. Krizmanic 4, J.W. Mitchell 4, P. Sommers 5,

More information

Particle acceleration in the universe

Particle acceleration in the universe Particle acceleration in the universe Some issues and challenges Etienne Parizot (APC Université Paris Diderot - France) Astrophysics 2 Everything we know about the universe comes from the observation

More information