Astrophysical sources sources of of high high- - Astrophysical - PowerPoint PPT Presentation

Astrophysical sources sources of of high high- - Astrophysical energy neutrinos neutrinos energy Karl Mannheim Karl Mannheim Institut für Theoretische Physik und Astrophysik Institut für Theoretische Physik und Astrophysik Universität Würzburg, Germany Universität Würzburg, Germany Neutrino 2004, Paris 14- -19 19 June June, 2004 , 2004 Neutrino 2004, Paris 14

� � � � � � � � ✁ � � ✁ Neutrino Astrophysics Astrophysics Neutrino Top questions questions in in astrophysics astrophysics in in the the Top pre- -cosmology cosmology era era: : pre • How • How do do stars stars work work? ? Thermonuclear reaction Thermonuclear reaction rates rates disagree disagree with with neutrino neutrino deficit deficit 6 K 0.3 10 6 Central temperature Central temperature of 15.7+ of 15.7+- -0.3 10 K confirmed confirmed by by helioseismology helioseismology Davis ν e ν µ to ν ν Neutrino deficit deficit due due to oscillations seen seen by by SNO SNO Neutrino µ oscillations e • How • How do do stars stars evolve evolve? ? Core collapse collapse produced produced neutrino neutrino bursts bursts Core Koshiba Confirmed by by observation observation of of SN1987A SN1987A Confirmed 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 2 K. Mannheim 2

� ✂ ✁ � ✁ � � � � ✂ ✂ ✂ ✂ ✂ ✂ ✂ Top questions questions in in cosmology cosmology era era Top • • How do How do first first stars stars form ( form (PopIII PopIII)? )? Collapse of massive of massive metal metal- -poor poor stars stars involves involves accretion accretion disk disk/ /jet jet phase phase Collapse • • GRBs with with nonthermal nonthermal neutrino neutrino production production (Schneider et al. 2002) (Schneider et al. 2002) GRBs • Enhanced • Enhanced neutrino neutrino flux flux due due to to progenitor progenitor shell shell ( (Razzaque Razzaque et al. 2004) et al. 2004) • • What is is dark dark matter? matter? What Massive weakly weakly interacting interacting relics relics top- -down down production production of of neutrinos neutrinos Massive top • Cosmogenic • Cosmogenic SUSY (Els SUSY (Elsä ässer & Mannheim 2004) sser & Mannheim 2004) • Supermassive • Supermassive dark dark matter ( matter (Crotty Crotty 2002) 2002) • • What is is dark dark energy energy? ? What Coupling with with scalar scalar field field Coupling as ∆ ∆ m • Energy • Energy scale scale of of dark dark energy energy same same as m ν ν ( (Paes Paes et al. 2004) et al. 2004) • Modified • Modified neutrino neutrino mixing mixing over over Gpc Gpc baselines baselines (Barenboim & (Barenboim & Quigg Quigg 2003) 2003) • • Where do do cosmic cosmic rays rays come come from from? ? Where • Pulsar • Pulsar wind wind nebulae nebulae ( (Nagataki Nagataki 2004) 2004) • AGN • AGN jets jets disk disk photon photon target target ( (Atoyan Atoyan & & Dermer Dermer 2004) 2004) synchrotron photon photon target target (Mücke et al. 2002) (Mücke et al. 2002) synchrotron • GRB • GRB jets jets Neutrinos from from internal internal and and external external shock shock waves waves ( (Dermer Dermer 2000) 2000) Neutrinos Neutrinos from from dirty dirty fireballs fireballs ( (Dermer Dermer 2000) 2000) Neutrinos 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 3 K. Mannheim 3

21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 4 K. Mannheim 4

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Infering neutrino neutrino fluxes fluxes Infering U n k n o w n m a g n e t ic f ie ld e . m . c a s c a d in g is o t r o p y 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 6 K. Mannheim 6

✖ ✒ ☛ ✡ ✏ ✠ ✖ ☞ ✂ ✌ ✄ ✏ ✌ ✒ ✟ ✍ ✂ ☞ ✍ ✝ ✗ ✗ ✗ ✙ ✗ ✗ ✘ ✖ ✎ ✕ ✔ ✓ ✖ ✒ ✑ ✏ ✞ � ☎ ✂ ✄ � ☎ ✄ ✄ ✍ ✎ ☎ ☎ ✍ ✂ ☞ ✎ ✁ � ✂ ✒ ✌ ✏ ✏ � ✑ ☎ ✆ ✌ ✁ Cosmic ray ray escape escape in in magnetically magnetically confined confined Cosmic sources by by „ „neutron neutron bomb“ bomb“ sources − Φ E 4 s E = E ~ γγ p 3 Φ 2 π p = Φ 1 → ∆ p γ p e ν Φ 1 = π n Φ 1 µ ν Φ 1 = pp → ... e ν ν Φ 1 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 7 K. Mannheim 7

� � � � � � � � � � � � � � Galactic sources sources Galactic • Chemical • Chemical composition composition, , absence absence of of intergalactic intergalactic IC, and diffuse IC, and diffuse Galactic gamma gamma ray ray emission emission supports supports Galactic Galactic origin origin of of CRs CRs Galactic up to knee knee up to • Candidates • Candidates Sun Sun OB associations OB associations with with stellar stellar winds winds ISM ISM GC GC SNR SNR Microquasars Microquasars PWN PWN 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 8 K. Mannheim 8

▼ ✮ ✸ ✷ ✵✶ ✴ ✳ ✲ ✱ ✰ ✯ ✭ ✺ ✬ ✫ ✫ ✫ ✪ ✩ ✧ ✦ ✍ ✹ ✻ ✤ ❉ ❑▲ ❏ ■ ❍ ● ❇ ❊ ❋ ❊ ❈ ✼ ❇ ❆ ❅ ❄ ❄ ❃❄ ✽ ✺ ✿ ✽✾ ✥ ★ ✘ ✟ ✎ ✍ ✌ ☞ ☛ ✡ ✠ ✞ ✒ ✝ ✆ ✁ ☎ ✄ ✂ ✁ � ✠ ✠ ☛ ✟ ✏ ✜ ✛ ✟ ✚ ✙ ✠ ✢ ✘ ✗ ✖ ✕ ✔ ✏ ✓ ✏ ❀❂❁ @ ∆ ∆θ ∆ ∆ θ < θ θ @ @ @ 1 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 9 K. Mannheim 9 ☞✣✏ ✠✑✏

✪ ✕ ✄ ✒ ✂ ✓ ✑ ✘ ✗ ✚ ✑ ✓✛ ☞ ✒ ✍ ✒ ✑ ☞ ✏✂ ✘ ✙ ✝ ✕ ✓ ✏ ✍ ☎ ☞ ✖ ✄ ✍ ✒ ✑ ✔ ✕ ✏ ✍ ✒ ✝ ✂ ★ ✂ ✖ ✏ ✒ ✑ ✢ ✣✤ ✦ ✩ ✒ ✌ ✘ ✒ ✏ ✤ ✕ ✞ ✂ ✖ ✓ ✚ ✂ ✝ ✝ ✑ ✢ ✜ ✠ ✒ ✎ ✒ ✝ ✒ ✒ ✗ ✎✂ ✄ ✞ ✄ ✒ ✑ ✂ ✏ ✂ ✍ ✂ ✌ ☞ ☛ ✏ ✡ ✠ � ✂ ✟ ✞ ✝ ✄ ✂ ✁ � ✓ ✄ ✝ ✓✘ ✟ ✌ ✂ ✁ ✝ ✕ ✔ ✖ ✁ ✑ ✒ ✟ ✂ ✏✗ ✍ ✂ ✂ ✓ ✔ ✄ ✕ ✔ ✖ ✁ ✂ TeV- -detection detection of of Cas Cas A A with with HEGRA IACT HEGRA IACT array array TeV ✄✆☎ ✥✧✦ 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 10 K. Mannheim 10

� � � � Extragalactic sources sources Extragalactic • GZK • GZK cutoff cutoff • Hillas Plot • Hillas Plot 18 eV • Isotropy • at > 10 18 Isotropy at > 10 eV • Light • Light chemical chemical composition composition (?) (?) • Gamma • Gamma- -ray ray sources sources AGN jets jets AGN GRBs GRBs • Bolometric • Bolometric gamma gamma ray ray limit limit due to to cascading cascading due 21.06.04 21.06.04 K. Mannheim - - Neutrino 2004, Paris 14 Neutrino 2004, Paris 14- -18 June, 2004 18 June, 2004 11 K. Mannheim 11

✪ ✂ ✏ ✝ ✘ ✂ ✒ ✍ ☞ ✑ ✘ ✗ ✂ ✏ ✝ ✍ ✓ ☛ ✗ ✕ ✂ ✂ ✗ ✓ ✕ ✝ ✁ ✁ ✓ ✝ ✍ ✟ ✝ ✑ ✂ ✒ ✄ ☞ ✂ ✍ ✒ ✏ ✖ ✑ ☞ ✝ ✑ ✗ ✒ ✄ ✦ ✩ ✒ ✎ ✏✂ ✂ ✝ ✝ ✒ ✦ � ✙ ✆ ✝ ✣✤ ✤ ✤ ✕ ✟ ✄ ✍ ✒ ✑ ✟ ✓ ✄ ✒ ✑ ✕ ✒ ✓ ✝ ✕ ✓ ✏ ✕ ✏ ✝ ✁ ✂ ✔ ✏ ✂ ✂ ✓ ☛ ✘ ✒ ✎ ✏ ✕ ✓ ✗ ☛ ✕ ✂ ✄ ✖ ✏ ✕ ✏ ✝ � ✖ ✕ ✒ ✚ ✒ ✕ ✍ ✗ ✂ ✌ ✟ ✒ ✏ ✕ ✝ ✁ ✂ ✂ ✒ ✄ ☞ ✂ ✍ ✗ ✂ ✓ ✏ ✍ ✕ ✍ ✝ ✑ ✜ ✎ ✕ ✝ ✍ ✑ ✂ ✛ ☞ ✏ ✑ ✂ ✍ ✍ ✝ ✑ ✓ 12 12 s ) t e j GN -18 June, 2004 18 June, 2004 ✄ ☎✄ A ( 5 2 -1 Neutrino 2004, Paris 14- - Neutrino 2004, Paris 14 Γ = K. Mannheim - K. Mannheim 21.06.04 21.06.04