Supernovae in stellar clusters as CR pevatrons. Collaborators: D.C.Ellison, P.E.Gladilin, S.M. Osipov
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1 Supernovae in stellar clusters as CR pevatrons Collaborators: D.C.Ellison, P.E.Gladilin, S.M. Osipov
2 Gamma Ray Spectral Energy Distribu6on: Starburst galaxies Ackermann + 12 A&ARv v.22, p.54, 2014 S.Ohm, CRePhy, v.17, p. 585, 2016
3 Gamma Ray Spectral Energy Distribu6on: Starburst galaxies Ackermann + 12 A&ARv v.22, p.54, 2014 S.Ohm, CRePhy, v.17, p. 585, 2016
4 Madau & Dickinson, ARAA 2014 SFR from FUV+IR
5 Core-collapse - SN rate Madau & Dickinson, ARAA 2014
6 M82 Starbursts (T.Thompson 2007) IRAS M51 NOAO NGC 253 Arp 220
7 Nearest Merger The Antennae WFPC2, with CO overlay (Whitmore et al. 1999; Wilson et al. 2000) VLA 5 GHz image (Neff & Ulvestad 2000) 5 mjy 30,000 O7-equivalent stars
8 Magnetic Fields in starbursts from radio observations If a fraction ~1% of ergs per SN goes to CR electrons, and they cool rapidly, the observed trend is reproduced. Thompson et al. (2006)
9 What are the HECR sources in starforming / starburst regions?
10 SNR in Molecular Clouds M.Ackermann 2013 Pion-Decay Signatures see: Tavani , Uchiyama+ 2010, Giuliani+ 2011, Ackermann+ 2013, Cardillo+ 2014
11 Observed gamma- ray spectra of SNRs S. Funk 2015 What are the sources of PeV regime CRs?
12 PeV CRs are likely accelerated in the Galaxy
13 How to get PeV energy CRs? Rare SNe with a special CSM type IIn? Rare magnetar-driven SNe? SNR- Stellar/Custer Wind collision?
14 From a general constraint on the CR accelera6on rate the luminosity of NR MHD flow should exceed: L tot > Z 2 β 1 sh Θ2 E 18 erg s 1 for a SN in SSC (age 400 yrs) L kin erg s 1 cf F.Aharonian, M.Lemoine, E.Waxman
15 PeV proton accelera6on in young SNe
16 CR proton acceleration by radio SNe and trans-relativistic SNRs V. Tatischeff:Radioemissionandnonlineardiffusive shock acceleration in SN 1993J [p/(m p c)] 4 f(p) [(m p c) 3 /n u ] a) b) c) p η inj = 10-4 p η inj = p η inj = 10-5 e η inj = 10-5 e η inj = e η inj = Kinetic energy (ev) Kinetic energy (ev) Kinetic energy (ev) V.Tatischeff 2009 S.Chakraborti, A.Ray, A.Soderberg, A.Loeb, P.Chandra 2011
17 CR proton acceleration by SNe type IIn with dense pre- SN wind CR proton acceleration in trans-relativistic SNe Ibc SNe Ibc occur mostly in gasrich star-forming spirals CR proton acceleration by Type IIn SNe V. Zirakashvili & V. Ptuskin 2015 CR proton acceleration by trans-relativistic SNe β/γ ~ 1 Ellison, Warren, AB ApJ v.776, 46, 2013
18 PeV proton accelera6on by SNe in young compact stellar clusters & starbursts
19 SNR - cluster wind accelerator MNRAS V. 429, 2755, 2013
20 Stellar wind shock ( thin shell approximation) Wilkin 1996 Colliding shock flow geometry used
21 SNR-stellar wind accelerator Non-linear kinetic model Transport equation for CR distribution function MNRAS V. 429, 2755, 2013
22 SNR-stellar wind accelerator cf Malkov 97; Amato & Blasi 05; Caprioli + 11 MNRAS V. 429, 2755, 2013
23 SNR-stellar wind accelerator MNRAS V. 429, 2755, 2013
24 SNR-stellar wind accelerator AB+ MNRAS V. 429, 2755, 2013
25 Par6cle accelera6on between approaching shocks is the most efficient version of Fermi I accelera6on
26 Par6cle accelera6on in colliding shocks is the most plausible scenario for SNe in young compact stellar clusters & starbursts
27 Acceleration time in the test particle approximation for Bohm diffusion τ a cr g(p) u s u w. Acceleration time is about 500 yrs for PeV τ a E PeV (η b n) 0.5 u 2 s3 u 1 w3 (s) Magnetic field amplification by CR current driven instabilities: Bell s and LW ApJ v.789, 137, 2014
28 MAGNETAR-POWERED SUPERNOVAE IN TWO DIMENSIONS. SUPERLUMINOUS SUPERNOVAE Chen, Woosley & Sukhbold 2016
29 SNe in COMPACT CLUSTER of YOUNG MASSIVE STARS
30 A Galactic Super Star Cluster Distance: 5kpc Mass: 10 5 M sun Core radius: 0.6 pc Extent: ~6 pc across 2MASS Atlas Image from M.Muno Core density:~10 6 pc -3 Age: 4 +/- 1 Myr Supernova rate: 1 every 10,000 years
31 Chandra Observations WR/O star binaries, plus unresolved pre- MS stars Two exposures: 2005 May, 18 ks 2005 June, 38 ks M.Muno This is a pulsar - magnetar!
32 Westerlund 1 Muno+ 05 Clark+ 05
33 H.E.S.S. image of Westerlund I MNRAS V. 453, p. 113, 2015
34 Gamma Rays and Neutrinos gamma- rays and high- energy neutrinos : gamma rays we also get γ s from electrons (NB, inverse Compton)
35 Gamma-rays from a Pevatron AARv v.22, p.54, 2014 MNRAS V. 453, p. 113, 2015
36 Gamma-rays from a Pevatron MNRAS V. 453, p. 113, 2015
37 Neutrinos from a Pevatron MNRAS V. 453, p. 113, 2015
38 Secondary pairs synchrotron X-ray counterpart to the Pevatron A cloud nearby: SRG perspective? Fermi SRG? MNRAS V. 453, p. 113, 2015
39 All Sky Map IceCube 4 years
40 IceCube events in the vicinity of Wd I MNRAS V. 453, p. 113, 2015 A.B
41 H.E.S.S. J power-law photon index of 2.3 ± 0.2stat ± 0.3sys Lvhe ~ ^(34)[D/8.7 kpc]^2 erg/s Extended very high-energy gamma-ray source towards the luminous blue variable candidate LBV , massive stellar cluster Cl* , and magnetar SGR of estimated age about 650 years. H.E.S.S. collaboration arxiv
42 Yeung FGL J1809
43 H.E.S.S. J
44 another component rel. shock? H.E.S.S. J model
45 Poten6al IceCube events from galac6c IceCube events in the vicinity of Wd I SNe in young star clusters A.B Wd I = ; b = (black filled circle) SGR MNRAS V. 453, p. SGR , 2015 l= ; b= (black open circle) l20
46 Thanks for your attention! ac765 Acknowledge support from RSF grant
47 U(x),P cr (x),p w (x),p g (x), E (x) u(x) 10 3 P g (x) P cr (x) 10P w (x) E(x) x/x 0
48 Monte Carlo modeling of DSA Magne6c Field Amplifica6on
49 ρ Conserva6on laws in MC modeling ( xux ) ( ) = ρ0u0 - mass ( xu ) 2 ( x) P( x) P( x) P( x) ρ =Φ ρ 3 ( xu ) ( x) 2 ( ) = ( ) g th Fth x u x γ γ g th cr w P0 ( ) ( ) ( ) Energy flux background plasma + F x + F x + F x + Q =Φ th cr w esc E0 P ( x) 1 - momentum - energy Energy flux and turbulent pressure 3 W x k Fw ( x, k) = u( x) W( x, k) Pw ( x, k ) = 2 2 Magne6c Fluctua6on Spectral Evolu6on (, ) Π ( xk, ) ( ) (, ) F x k P x k w x ( xkw, ) ( x, k) L( xk, ) w + = u x + Γ x x (, ) ( ) df cr dx ( x) ( ) dfw x dpw x = u( x) + Γ( xkw, ) ( xkd, ) k L dx dx ( k) cr ( ) v ( x) = u x + scat dp dx Energy flux components ( x) th ( ) ( ) ( ) df x dp x dx th = u x + ( k ) dx L ( x) dpcr vscat ( x) = Γ( x, k ) W ( x, k) dk dx
50 Bulk velocity and magne6c field profiles r g 0 = mcu p eb км n0 = 0.3 см ; u0 = 5000 ; B0 = 3 мкгс с AB +., ApJ, 789:137, 2014.
51 Magne6c turbulence spectra ApJ, 789:137, км n0 = 0.3 см ; u0 = 5000 ; B0 = 3 мкгс с
52 , ApJ, 789:137, Fluctuabng magnebc field and magnebc pressure scalings Beff n u θ, B eff,2 3 u0 n0 θ : 1.5
53 CR spectra scalings Maximal momentum of accelerated CRs p n u L δ max 0 0 FEB δ : 0.25 ApJ, 789:137, 2014.
54 Sca_ering center velocity vs Alfven speed 3 км n0 = 0.3 см ; u0 = 5000 ; B0 = 3 мкгс с ApJ, 789:137, 2014.
55 IceCube neutrinos galac6c la6tude profile > 100 TeV Evidence for the Galactic contribution to the IceCube astrophysical neutrino flux Neronov & Semikoz Astroparticle Physics, Volume 75, p , 2016
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