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

SLIDE 1

Astrophysical Astrophysical sources sources of

• f high

high-

• energy

energy neutrinos neutrinos

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 Neutrino 2004, Paris 14-

• 19

19 June June, 2004 , 2004

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 2 2

Neutrino Neutrino Astrophysics Astrophysics

Top Top questions questions in in astrophysics astrophysics in in the the pre pre-

• cosmology

cosmology era era: :

• How

How do do stars stars work work? ?

• Thermonuclear

Thermonuclear reaction reaction rates rates disagree disagree with with neutrino neutrino deficit deficit

• Central

Central temperature temperature of 15.7+

• f 15.7+-
• 0.3 10

0.3 106

6 K

K confirmed confirmed by by helioseismology helioseismology

• Neutrino

Neutrino deficit deficit due due to to ν νe

e

✁ ✁

ν νµ

µ oscillations

• scillations seen

seen by by SNO SNO

• How

How do do stars stars evolve evolve? ?

• Core

Core collapse collapse produced produced neutrino neutrino bursts bursts

• Confirmed

Confirmed by by observation

• bservation of
• f SN1987A

SN1987A

Davis Koshiba

SLIDE 3

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• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 3 3

Top Top questions questions in in cosmology cosmology era era

• How

How do do first first stars stars form ( form (PopIII PopIII)? )?

• Collapse

Collapse of massive

• f massive metal

metal-

• poor

poor stars stars involves involves accretion accretion disk disk/ /jet jet phase phase

• GRBs

GRBs with with nonthermal nonthermal neutrino neutrino production production (Schneider et al. 2002) (Schneider et al. 2002)

• Enhanced

Enhanced neutrino neutrino flux flux due due to to progenitor progenitor shell shell ( (Razzaque Razzaque et al. 2004) et al. 2004)

• What

What is is dark dark matter? matter?

• Massive

Massive weakly weakly interacting interacting relics relics

✁ ✁

top top-

• down

down production production of

• f neutrinos

neutrinos

• Cosmogenic

Cosmogenic SUSY (Els SUSY (Elsä ässer & Mannheim 2004) sser & Mannheim 2004)

• Supermassive

Supermassive dark dark matter ( matter (Crotty Crotty 2002) 2002)

• What

What is is dark dark energy energy? ?

• Coupling

Coupling with with scalar scalar field field

• Energy

Energy scale scale of

• f dark

dark energy energy same same as as ∆ ∆m mν

ν (

(Paes Paes et al. 2004) et al. 2004)

• Modified

Modified neutrino neutrino mixing mixing over

• ver Gpc

Gpc baselines baselines (Barenboim & (Barenboim & Quigg Quigg 2003) 2003)

• Where

Where do do cosmic cosmic rays rays come come from from? ?

• 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 synchrotron photon photon target target (Mücke et al. 2002) (Mücke et al. 2002)

• GRB

GRB jets jets

✂ ✂

Neutrinos 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)

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• Neutrino 2004, Paris 14

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• 18 June, 2004

18 June, 2004 4 4

SLIDE 5

• ✁

✂ ✂ ✄ ☎ ✆ ✝ ✂✞ ✄✟ ✠ ✡ ☎ ✆ ☛ ☞ ✌ ✍ ✌✎ ✏ ✡ ☎ ✆ ☎ ✑ ☎ ✒ ✍ ☞ ✌✎ ✏

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• K. Mannheim -
• Neutrino 2004, Paris 14

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• 18 June, 2004

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Infering Infering neutrino neutrino fluxes fluxes

U n k n

• w

n m a g n e t ic f ie ld e . m . c a s c a d in g is

• t

r

• p

y

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• Neutrino 2004, Paris 14

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• 18 June, 2004

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✄

• ✁

✂ ✄ ☎ ✄ ✎ ☎ ☎ ✍ ☞ ✂ ✎ ✌ ✆ ✑ ☎ ✁

• ✏

✏ ✌ ✒ ✂

• ✍

☎ ✝ ✞ ✂ ✍ ✟ ✒ ✌ ✏ ✄ ✂ ✒ ☞

• ✠

✏

γγ

✡

ν ν

☛

e

☞ ✌

ν µ

✍ ✎

∆ → γ p

p

✏

π n

✑

π

✒

e p ν

✓ ✔ ✕

E E 3 4 = 1 2 = Φ Φ

✖ ✗ ✘

1 1 = Φ Φ

✖ ✖ ✗ ✗

1 1 = Φ Φ

✙ ✗ ✗ ✖

... → pp

s

~

−

Φ E

p

Cosmic Cosmic ray ray escape escape in in magnetically magnetically confined confined sources sources by by „ „neutron neutron bomb“ bomb“

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• 18 June, 2004

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Galactic Galactic sources sources

• Chemical

Chemical composition composition, , absence absence of

• f intergalactic

intergalactic IC, and diffuse IC, and diffuse Galactic Galactic gamma gamma ray ray emission emission supports supports Galactic Galactic origin

• rigin of
• f CRs

CRs up to up to knee knee

• Candidates

Candidates

• Sun

Sun

• OB

OB associations associations with with stellar stellar winds winds

• ISM

ISM

• GC

GC

• SNR

SNR

• Microquasars

Microquasars

• PWN

PWN

SLIDE 9

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• Neutrino 2004, Paris 14

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• 18 June, 2004

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• ✁

✂ ✄ ☎ ✁ ✆ ✝ ✞ ✟ ✠ ✠ ✡ ☛ ☞ ✌ ✍ ✎ ✠ ✠✑✏ ✒ ☛ ✓ ✏ ✔ ✕ ✖ ✗ ✘ ✏ ✟ ✠ ✙ ✚ ✟ ✛ ✜ ✏ ✢ ✘ ☞✣✏ ✤ ✥ ✍ ✦ ✧ ★ ✩ ✪ ✫ ✫ ✫ ✬ ✭ ✮ ✯ ✰ ✱ ✲ ✳ ✴ ✵✶ ✷ ✸ ✹ ✺ ✻ ✼ ✽✾ ✿ ✺ ✽ ❀❂❁ ❃❄ ❄ ❄ ❅ ❆ ❇ ❈ ❉ ❊ ❋ ❊ ❇

• ❍

■ ❏ ❑▲

@ @ @ @ ∆ ∆ ∆ ∆θ θ θ θ< 1

▼

SLIDE 10

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 10 10

TeV TeV-

• detection

detection of

• f Cas

Cas A A with with HEGRA IACT HEGRA IACT array array

• ✁

✂ ✄ ✄✆☎ ✝ ✞ ✟ ✂

• ✠

✡ ☛ ✄ ☞ ✌ ✂ ✍ ✎✂ ✏ ✂ ✑ ✒ ✄ ✄ ✞ ✓ ✏ ✝ ✁ ✂ ✄ ✓ ✔ ✍ ✕ ✖ ✂ ✔ ✁ ✂ ✏✗ ✓✘ ✟ ✒ ✑ ✂ ✖ ✔ ✕ ✝ ✁ ✂ ✌ ✟ ✂ ✗ ✝ ✒ ✝ ✕ ✓ ✏ ✍ ☎ ✙ ☞ ✄ ✍ ✒ ✑ ✔ ✕ ✏ ✖ ✏✂ ✚ ☞ ✄ ✒ ✂ ✓ ✑ ✘ ✕ ✗ ✑ ✓✛ ☞ ✒ ✍ ✒ ✑ ✍ ✘ ✒ ✞ ✖ ✓ ✚ ✂ ✝ ✝ ✂ ✑ ✜ ✠ ✒ ✎ ✒ ✝ ✒ ✢ ✕ ✣✤ ✤ ✥✧✦ ★ ✂ ✖ ✏ ✒ ✑ ✂ ✢ ✦ ✩ ✒ ✌ ✘ ✒ ✏ ✪

SLIDE 11

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

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• 18 June, 2004

18 June, 2004 11 11

Extragalactic Extragalactic sources sources

• GZK

GZK cutoff cutoff

• Hillas Plot

Hillas Plot

• Isotropy

Isotropy at > 10 at > 1018

18 eV

eV

• Light

Light chemical chemical composition composition (?) (?)

• Gamma

Gamma-

• ray

ray sources sources

• AGN

AGN jets jets

• GRBs

GRBs

• Bolometric

Bolometric gamma gamma ray ray limit limit due due to to cascading cascading

SLIDE 12

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 12 12

Γ= 2 -1 5 ( A GN j e t s )

• ✖

✕ ✒ ✚ ✒ ✝ ✕ ✗ ✂ ✌ ✟ ✒ ✏ ✍ ✕ ✓ ✏ ✓ ☛ ✘ ✒ ✎ ✏ ✂ ✝ ✕ ✗ ☛ ✕ ✂ ✄ ✖ ✕ ✏ ✁ ✂ ✝ ✍ ✑ ✂ ✛ ☞ ✕ ✑ ✂ ✍ ✍ ✝ ✑ ✓ ✏ ✎ ✂ ✑ ✂ ✒ ✄ ☞ ✂ ✍ ✜ ✗ ✓ ✏ ✍ ✕ ✍ ✝ ✂ ✏ ✝ ✔ ✕ ✝ ✁ ✁ ✓ ✝ ✍ ✟ ✓ ✝ ✂ ✒ ✄ ☞ ✂ ✍ ✒ ✏ ✖ ✑ ✂ ✗ ✂ ✏ ✝ ✘ ✂ ✒ ✍ ☞ ✑ ✂ ✘ ✂ ✏ ✝ ✍ ✓ ☛ ✗ ✕ ✑ ✗ ☞ ✄ ✒ ✑ ✟ ✓ ✄ ✒ ✑ ✕ ✍ ✒ ✝ ✕ ✓ ✏ ✕ ✏ ✝ ✁ ✂ ✓ ✟ ✝ ✕ ✗ ✒ ✄ ✦ ✩ ✒ ✎ ✏✂ ✑ ✂ ✝ ✒ ✄☎✄ ✦

• ✙✆

✝ ✣✤ ✤ ✤ ✪

SLIDE 13

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 13 13

AGN AGN jets jets: : cosmic cosmic accelerators accelerators of

• f

UHE UHE cosmic cosmic rays rays? ?

• ✁

✂ ✄ ☎ ✆ ✝ ✂ ✄

• ✁

✂ ✄ ☎ ✆ ✝ ✂ ✄ ✆✞ ✟ ✆✞ ✄ ✂ ✆✞ ✟ ✆✞ ✄ ✂ ✟ ✠ ✂ ✆ ✝ ✁ ✡ ☛ ✟ ✠ ✂ ✆ ✝ ✁ ✡ ☛ ✡ ✠ ✝ ☞ ✡ ✠ ✝ ☞ ☛ ✡ ✌ ✝ ☎ ☛ ✡ ✌ ✝ ☎ ✍ ✍ ✎ ✂ ✏ ✎ ✂ ✏ ☎ ✑ ☎ ✑ ✞ ✒ ✁ ✂ ✂ ☛ ✂ ✑ ✝ ✞ ✒ ✁ ✂ ✂ ☛ ✂ ✑ ✝ ✓ ☎ ✝ ✔ ✓ ☎ ✝ ✔ ✄ ✂ ✝ ✂ ✆ ✝ ☎ ☞ ✑ ✟ ✄ ✂ ✝ ✂ ✆ ✝ ☎ ☞ ✑ ✟ ✕ ✕ ✟ ✂ ✂ ✟ ✂ ✂ ✄ ☎ ✟ ✆ ✡ ✟ ✟ ☎ ☞ ✑ ✄ ☎ ✟ ✆ ✡ ✟ ✟ ☎ ☞ ✑ ☎ ✑ ✖ ✞ ✑ ✑ ✔ ✂ ☎ ☛✘✗ ✙✚ ✚ ✛ ✗ ☎ ✑ ✖ ✞ ✑ ✑ ✔ ✂ ☎ ☛✘✗ ✙✚ ✚ ✛ ✗ ✜ ✢ ✣ ✜ ✢ ✣ ✤ ✥ ✦ ✧✩★ ✪✫ ✬ ✭ ✤ ✥ ✦ ✧✩★ ✪✫ ✬ ✭

SLIDE 14

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• Neutrino 2004, Paris 14

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• 18 June, 2004

18 June, 2004 14 14

G a mm a

• r

a y b a c k g r

• u

n d e n e r g y f lu x Φ(γ) ~ 10

• ✪

G e V / ( c m

✥

s s t )

SLIDE 15

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• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 15 15

SLIDE 16

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 16 16

• ✁

✂ ✄ ☎ ✆ ✝✞ ✟ ✂ ✠ ✝✁ ✄ ✡ ☛☞ ✌ ✍ ✎ ✏ ✍ ✑ ✎ ✝✁ ✏ ✒ ✁ ✄ ✒ ✓ ✔ ✕ ✖ ✗ ✘ ✙ ✚ ✛ ✕ ✜ ✙ ✔ ✖ ✢ ✣ ✤ ✥✦ ✧ ★ ✙ ✔ ✥ ✩ ✔ ✖ ✩ ✪ ✫ ✬ ✭ ✫ ✮ ✯✰ ✫ ✮ ✮ ✱ ✲ ✳ ✭ ✴✵ ✵✶

SLIDE 17

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• K. Mannheim
• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 17 17

SLIDE 18

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• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 18 18

Experimental Experimental upper upper limits limits

SLIDE 19

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• K. Mannheim
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• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 19 19

Structure Structure in in spectrum spectrum of

• f extragalactic

extragalactic gamma gamma ray ray background background due due to 500 to 500 GeV GeV neutralinos neutralinos ? ?

(Elsässer&Mannheim2004, PRL (Elsässer&Mannheim2004, PRL submitted submitted) )

SLIDE 20

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• K. Mannheim -
• Neutrino 2004, Paris 14

Neutrino 2004, Paris 14-

• 18 June, 2004

18 June, 2004 20 20

Cosmogenic Cosmogenic high high-

• energy

energy neutrino neutrino background background

(Elsässer & Mannheim 2004, (Elsässer & Mannheim 2004, Aph Aph, in press) , in press)

SLIDE 21

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• 18 June, 2004

18 June, 2004 21 21

Summary Summary

I. I. Guaranteed Guaranteed sources sources ( (Galactic Galactic disk disk, Sun, GZK) , Sun, GZK) II. II. Likely Likely steady steady sources sources at 100 at 100 TeV TeV ( (Knee Knee-

• CR

CR sources sources, AGN) , AGN) Φ Φν

ν ~ [10

~ [10-

• 9

9-

• 10

10-

• 10

10]

] GeV GeV/(cm2 s) /(cm2 s) III. III. Omnidirectional Omnidirectional intensity intensity from 100 from 100 TeV TeV to GZK to GZK energies energies I Iν

ν ~ [5 10

~ [5 10-

• 8

8 -

• 5 10

5 10-

• 7

7]

] GeV GeV/(cm2 s sr) /(cm2 s sr) ( (due due to to sources sources of

• f extragalactic

extragalactic cosmic cosmic rays rays and and γ γ-

• ray

ray background background) ) IV. IV. GRB GRB contribution contribution to I to Iν

ν small

small ( (unless unless splendid splendid TeV TeV emitters emitters), ), nevertheless nevertheless likely likely neutrino neutrino sources sources V. V. Neutralino Neutralino-

• induced

induced cosmogenic cosmogenic tau tau-

• neutrino

neutrino flux flux at ~50 at ~50-

• 100

100 GeV GeV