Common Solution Of Three Cosmic Puzzles ?*

Arnon Dar

TAUP, Torino, Italy 11/9/2015

In collaboration with Shlomo dado

* Origin of :

The high energy cosmic ray positrons (PAMELA, Fermi-LAT, AMS)

The high energy gamma ray background radiation (EGRET, Fermi-LAT)

The high energy astronomical neutrinos (IceCube)

0 0

π

π

π

p

p

p

γ γpp π X, π 2γ E <E > /( x >/2) ~ 10 E

pp π X, π E <E > / ( x >/4) ~ 20 E

pp π X, π E <E > / ( x >/4) ~ 20 E

e e

e e l

l l

l

e

e

Production of of High Energy Gamma Rays, Neutrinos and Positrons of Energy E<10 PeV, in Source, in the ISM and in the IGM, is mainly by Cosmic Rays of typical energy :

hadronic meson production is taken over by photo meson production only at very high energies

GZK (1966):Effective Threshold: 25 PeV 4 EeV 40 EeV

BKGp + γ πX BKG = DGL + FIR + CMB

Unique relations between the cosmic fluxes of +γ, ν, and e

GALPROP

+ + + + +

ISM

e μ

e+

e+ e+ j in

e+

pp μ X μ e ν ν <E(e )> E(μ )/3

d dE b(E)Φ J (E) b(E)=

dE dt

J (E) K (β ) σ (pp) c n

e+

2

p

-β

p

e+ e+e+

j

-2.7

in

j Φ (E) E

J (E) τ Φ where τ E/(dE/dt)= E/b(E)

(β -1)

Φ (E) 1.8 (E/GeV) [1/GeV cm sr s] for E<PeV (PDG 2014)

σ

0.058

e+ j

3

ISM

-3j

e+

(pp) 30 (E/GeV) mb; β 2.64 K (β ) 7×10

Local n =0.9 cm (Calberla and Dedes 2008)

1 / τ 1 / τ 1 / τ

escrad

Positron Production In The Local ISMBy High Energy Primary Cosmic Ray Nucleons

Model: Steady State Leaky Box Model + Fynman Scaling

AMS02 proton spectrum break

2 1/3214

dif

2 2

erad 3

T

2

DGL FIR CBR

1 -116

R R Et = 7.5×10 s

2D 4 kpc GeV

In the Thomson regime:

3(m c ) U E= 10

4σ cUE eV/cm GeV

U=U +U +U +B /8π

τ s

Kolmogorov (1941), … CR Be10 / Be9 ratio … ,… Lipari(2014):

Porter, Moskalenko and Strong 2006

AMS02Agiular et al. 2014

LOCAL ISM

transition to KN

2.84 2.70

p 20E ) E E( e

IceCube Astronomical Neutrino Background

Puzzle 2

AstronomicalNeutrinos BKG

Atmosphericneutrinos ?

0

γ γ

γ

β -1j±

ν ν

ν ππ2

Φ (E)=(K /K ) Φ (E)

K /K ( ( K decay +...m / m )

which cannot be tested directly :

The EGB observed with Fermi-LAT (at E< 820 GeV ) is attenuated by

The IceCube observed at E>50 TeV

But, obtained from the observed EGB and GBR at E~100 GeV can be extrapolated to E>20 TeV using at source

νΦ (E)

Hadronic production by cosmic ray nucleons yields:

γΦ (E)

νΦ (E)

+

BKG

-γ + γ e + e

ν pΦ (E) Φ (20 <1+z> E)

The Extragalactic Gamma Ray Background (EGB)

Fermi-LAT (Ackermann et al. 2015)

2

γE

+

EBL

-γ + γ e +e

0.30 0.02E

0.61 0.03E

The Extragalactic Neutrino Background (ENB)

γ

-7 E/366 GeVEGB E/GeV

2.306.4×10Φ ( )

--( ( ) e fu

Ackermann et al. 2015: Absorbed EGB:

Estimated Unabsorbed EGB

-7

γ

1 2 1 1

EGB EGB-2.30

0.64 Φ ( ) Φ ( ) 4.1×10 E/GeV

GeV

per ν flavor and E< 20 TeV:

( ) fu

where fu= s sr is the flux unitcm

For a universal CR flux, max SFR/AGN around 1+z=2.5 ==> knee around 20 TeV,

2 -8 2EGB

-0.61E Φ ( ) 0.80×10 E/100 TeV GeV( ) fu

ν pΦ (E) Φ (20 <1+z> E)

per ν flavor and E> 20 TeV:

2 8 2

EG

2 8 2

MW

0.61 .05

0.61 .05

E Φ (0.80 .13) 10 (E/100 TeV) GeV fu

E Φ (1.03 .15) 10 (E/100 TeV) GeV fu

Expected NBR from the measured GBR with Fermi-LAT compared to the NBR measured with IceCube (2014)

28 0.611.83 10 (E/100 TeV) GeV fu

NBR=MW+EG

2 2

MW MWγE Φ From E Φ

at 100 GeV (Fermi-LAT)

or 1 TeV (H.E.S.S).

The predicted sky distribution of the neutrino background radiation is the sky distribution of the HE unabsorbed gamma background radiation, i.e., roughly that of the GBR at 100 GeV

0 10

0.76%4

o ob

E>GeV

90

The observed fluxes, spectra, and sky distributions of the high energy diffuse backgrounds of astronomical

satisfy simple relations, which are expected from their common production in high energy hadronic collisions of cosmic rays in their Galactic and extragalactic sources. Their observed spectra indicate: The observed near Earth are produced in the local ISM.The high energy are produced inside/near source

Conclusions

γ's and ν's

+e 's

γ's and ν's, and the CR e ' observed near Earth,s