High energy astronomy and

Gamma-ray bursts

Eli Waxman

Weizmann Institute, ISRAEL

Outline

• The origin of UHECRs (>1019eV): Unknown

• Part I: UHECR-GRBs

• Part II: The role of astronomy

What do we know about >1019eV CRs?

• J(>1011GeV)~1 / 100 km2 year 2 sr• Most likely X-Galactic (RL=/eB=40p,20kpc)• Composition? HiRes- p, Auger- becoming heavier? (Uncertain pp)• (An)isotropy: 2, consistent with LSS

• Production rate & spectrum:protons, 2(dQ/d) ~1043.7 erg/Mpc3 yr + GZK

• Acceleration (expanding flow): Confinement L>LB>1012 (2/) (/Z 1020eV)2 Lsun

Synch. losses > 102.5 (L52)1/10 (t/10ms)-1/5

!! No L>1012 Lsun at d<dGZK Transient Sources

[EW 95]

UHECR sources: Suspects• Constraints: - L>1012 (2/) Lsun

- 2(dQ/d) ~1043.7 erg/Mpc3 yr

- d(1020eV)<dGZK~100Mpc

!! No L>1012 Lsun at d<dGZK Transient Sources

• Gamma-ray Bursts (GRBs) L~ 1019LSun >1012 (2/) Lsun= 1017 (/ 102.5)2 Lsun

~ 102.5 (L52)1/10 (t/10ms)-1/5

2(dQ/d) ~ 1053erg*10-9.5/Mpc3 yr = 1043.5 erg/Mpc3 yr

Transient: T~10s << Tp~105 yr

• Active Galactic Nuclei (AGN, Steady): ~ 101 L>1014 LSun= few brightest

!! Non at d<dGZK Invoke:

* “Dark” (proton only) AGN * L~ 1014 LSun , t~1month flares

(from stellar disruptions)

[Blandford 76; Lovelace 76]

[EW 95, Vietri 95, Milgrom & Usov 95]

[EW 95]

[Boldt & Loewenstein 00]

[Farrar & Gruzinov 08]

UHECR per GRB

• Uncertainties: Absolute ECR calibration

ECR/EUHECR

z=0 high-L GRB rate

erg)0(Rate

yr1/Gpc

10105

erg)0(Rate

yr1/Gpc105

yr1/Gpc

yrerg/Mpc10

)0(Rate

)/(

353

352

3

37.432

,

zE

E

zE

E

E

E

z

ddQ

E

EE

GRBUHECR

CR

GRBUHECR

CR

UHECR

CR

GRB

UHECR

UHECR

CRGRBCR

[Guetta et al. 2010]

GRB int./ext. shock acceleration Confinement L>LB>1012 (2/) (/Z 1020eV)2 Lsun

• LB~L ??

• Internal shocks (~1): B~Bequip, LB~L

Does not necessarily require orders of magnitude amplification

GRB int./ext. shock acceleration• External (>>1): Bup~10-5 Bequip

?? LB<<L, No UHE acceleration??

• e- t(acceleration) < t(IC) X-ray AG B > 0.2 n0

5/8 mG >> 1G

100MeV B > 5 n05/8 mG

(0.1mG ) Upstream field generation, Possible UHE @

external Consistent with theoretical considerations

(Kumar & Barniol-Duran 09: No amplification? Parameter fit {B, e …} ignoring physics)

p

Shock frame

Downstream Upstream

[Li & EW 06]

[Li 10]

[Piran &Nakar 10]

[eg Keshet et al 09;Nishikawa et al. 09]

HE Astronomy• p + N + 0 2 ; + e+ + e + +

Identify UHECR sources Study BH accretion/acceleration physics

• E2dQ/dE=1044erg/Mpc3yr & p<1:

• If X-G p’s:

Identify primaries, determine f(z)

3

282

)1(,1)(for5,1

srscm

GeV10

zzf

d

dj

[EW & Bahcall 99; Bahcall & EW 01]

srscm

GeV10)eV10(

28192

d

dj[Berezinsky & Zatsepin 69]

HE experimentsOptical Cerenkov

- South Pole Amanda: 660 OM, 0.05

km3

IceCube: +660/yr OM (05/06…) 4800 OM=1 km3s - Mediterranean Antares: 10 lines (Nov 07), 750 OM 0.05 km3

Nestor: (?) 0.1 km3

km3Net: R&D 1 km3

•UHE: Radio Air shower Aura, Ariana (in Ice) Auger ()

ANITA (Balloon) EUSO (?) LOFAR

GRB ’s

• If: Baryonic jet

• Background free:

2GeV3.0// p

eV10,eV1010,MeV1 5.14165.2 p

yrkm/20

eV10,srscm

GeV102.0

2

5.142

82

J

WB

2.0pf

[EW & Bahcall 97, 99; Rachen & Meszaros 98; Guetta et al. 01; Murase & Nagataki 06]

;yrkm/TeV1005.0

104~ 22

3

EJ

oA

TeV1005.2

TeV1007.1

E

E

GRB & fp

• Prompt ~1MeV synch fp ~ (100MeV)~1

(100MeV)~1 ~300

Prompt GeV photons (100MeV)<<1, >>300, no ’s ??

Is (100MeV)<<1?• Challenge to prompt MeV sync production

• 95% of LGRB not detected by LAT For bright GRBs, non detection implies: F(>100MeV)/F(1MeV) < 0.1 (100MeV)>~1 ?

[Abdo et al. 09; Greiner et al. 09; Dermer 10]

MeV)ms10/()300/(

1,ms10

MeV100

)(/300

2

2/1

2/12/3.

6/1

52,52,

, t

L

tL

beb

synch

[Guetta et al. 10]

GRB ’s

• Caution in inferring min:

- No exponential cutoff at >1, rather f~1/ - GeV & MeV emission likely originate from

different radii (HE delay), (=1)~R

• Internal collisions at R0 “residual” coll. @ R>> R0

E(R)~1/Rq with q<2/3 f~1/q for >(=1,R= R0) May account for: prompt optical (avoid self-abs.) prompt GeV (avoid pair prod.)

GRB080916c HE delays ~300

[Li & EW 08]

[Li 10]

[Li 10]

The current limit

[Achterberg et al. 08 (The IceCube collaboration)]

TeV GRB ’s

• Collapsar jet penetration, failed SN jet : TeV ’s

[Meszaros & EW 01; Razzaque et al. 03, 04;Guetta & Granot 03; Dermer & Atoyan 03Ando & Beacom 05]

- physics & astro-physics

• decay e:: = 1:2:0 (Osc.) e:: = 1:1:1

appearance experiment

• GRBs: - timing (10s over Hubble distance) LI to 1:1016; WEP to 1:106

• EM energy loss of ’s (and ’s) e:: = 1:1:1 (E>E0) 1:2:2

GRBs: E0~1015eV

• Combining E<E0, E>E0 flavor measurements

may constrain CPV [Sin13 Cos]

[EW& Bahcall 97]

[Rachen & Meszaros 98; Kashti & EW 05]

[EW & Bahcall 97; Amelino-Camelia,et al.98; Coleman &.Glashow 99; Jacob & Piran 07]

[Blum, Nir & EW 05]

SummaryUHECRs • Origin- an outstanding puzzle• GRBs- only known sources satisfying all

constraints

astronomy• Detectors approach required ~1Gton scale

• Resolve UHECR puzzle: composition, sources• Resolve GRB physics open Q: Baryonic/Poynting

jet, , particle acceleration [test collapsar jets, X/FUV flares]

• Constrain physics, LI, WEP

Composition clues

HiRes 2005

Auger 2009Protons

Heavier at highest E?

Or: modified extrapolation? (s~300 TeV)

[E.g. Wibig 08,09; Ulrich et al. 09

Kusenko 10]

[EW 1995; Bahcall & EW 03]

[Katz & EW 09]

• protons, dQ/dE~(1+z)mE-

teff. : p + CMB N + Q=J/ teff.

• Consistent with protons, E2(dQ/dE) ~1043.7 erg/Mpc3 yr + GZK

Production rate & Spectrum

cteff [Mpc]GZK (CMB) suppression

log(E2dQ/dE) [erg/Mpc2 yr]

Back up slides

Anisotropy

• Anisotropy @ 98% CL; Consistent with LSS (Correlation with low-luminosity AGN? Trace LSS)

• Anisotropy/Compostion connection Acceleration of Z(>>1) to E Acceleration of p to E/Z Anisotropy of Z @ E Stronger anisotropy @ E/Z Anisotropy not observed @ E/Z Z~1 @ E~1019.7eV

Biased (source~gal for gal>gal )

[Kashti & Waxman 08]

[:Lemoine & EW 09]

AMANDA &IceCube

The Mediterranean effort

• ANTARES (NESTOR, NEMO) KM3NeT

Mark Westmoquette (University College London), Jay Gallagher (University of Wisconsin-Madison), Linda Smith (University College London), WIYN//NSF, NASA/ESA

Robert Gendler

M82 M81

A lower bound: Star bursts

• Star burst galaxies: - Star Formation Rate ~103Msun/yr >> 1 Msun/yr “normal”

(MW) - Density ~103/cc >> 1/cc “normal” - B ~1 mG >> 1G “normal”

• Most stars formed in (z>1.5) star bursts

• High density + B: CR e-’s lose all energy to synchrotron radiation CR p’s lose all energy to production

[Loeb & Waxman 06]

[Quataert et al. 06]

eepnpp ,

Synchrotron radio calibration

[Loeb & Waxman 06]

M82, NGC253: Hess, VERITAS 09

Fermi 09 dN/dE~1/Ep, p<~2.2

Starbursts

The 1020eV challenge

RB eBRBR

R

BR

ccV p c

v

c

v

v/

1~

1 2

cec

BRL p

222

v/2

1v

84

v

v

sun122

20,

2

46

2

20

2

L10

erg/s10eV10/v

p

p

cL

2R

tRF=R/c)

l =R/

2 2

[Waxman 95, 04, Norman et al. 95]

The GRB “GZK sphere”

• LSS filaments: D~1Mpc, fV~0.1, n~10-6cm-3, T~0.1keV

B=(B2/8nT~0.01 (B~0.01G), B~10kpc

• Prediction:

p

D

B

few~)eV103( 20GRBsN[Waxman 95; Miralda-Escude &

Waxman 96, Waxman 04]

BBVGRBs

GRB

BBVp

DelaySpread

BBVp

fDN

R

fDd

c

d

fDd

2220

3

2

2

2052

2/1

20

2/10

10~)eV10(

yrGpc/5.0~

eV10/

Mpc100/yr10~~~

eV10/

Mpc100/3.0

GRB Model Predictions

[Miralda-Escude & Waxman 96]

Indirect detection

3,000 km2

J(>1011GeV)~1 / 100 km2 year 2 sr

Ground array

Fluorescence detector

Auger:3000 km2