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High-E phenomena from GRBs
EM and non-EM observatories
Ralph A.M.J. Wijers Astronomical Institute `Anton Pannekoek'

Zeldovich 90, Moscow, 19 Decemb er 2004 ­ p. 1/16


Introduction
Basic properties of GRBs High-E neutrinos and cosmic rays from afterglow Engine and lower-E neutrinos Extreme radio supernovae

Zeldovich 90, Moscow, 19 Decemb er 2004 ­ p. 2/16


GRB Basics
z 1, d 1028 cm E 1052 erg Photon compactness:
LT m p c3 R

10

12

`Neutrino compactness': > 1

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GRB Basics

Zeldovich 90, Moscow, 19 Decemb er 2004 ­ p. 3/16


GRB Basics
Baryon-dominated collisionless relativistic shock Synchrotron radiation, perhaps also IC

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GRB Jets

1997: high redshift = E 1054 erg?

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GRB Jets



Energy in jets, jet 10 Reduces E from 1053.5 to 1051.5 erg.

Zeldovich 90, Moscow, 19 Decemb er 2004 ­ p. 4/16


Basic Collapsar Notions
-15.5

GRB 030329/SN 2003dh
April April April April April May 3.10 8.13 10.04 17.01 22.00 1.02

-16.0 log f (erg s-1 cm-2е-1)

-16.5

-17.0

-17.5

SN 1998bw after 33 d 4000 6000 8000 10000 Observed Wavelength (е)

1998/2003: Supernovae of type Ic

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Basic Collapsar Notions
20.0

V (mag)



Huge expansion speed, non-relativistic explosion is few times 1052 erg Large amounts of 3 material inferred from radio Total energy in excess of 1053 erg (!?) = different engine than SN?

20.5 21.0 21.5 22.0 50 vexp (103 km s-1) 40 30 20 10 0 0 SN 2003dh SN 1998bw

5

10 15 20 25 Time since GRB (days)

30

Zeldovich 90, Moscow, 19 Decemb er 2004 ­ p. 5/16


Basic Collapsar Notions

Is jet EM- or -driven? How to get > 100?

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There Are Baryons!

But: this is far from source. Initial or swept-up?

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Consequences of Baryonic Jets
Reverse shock = ejecta are baryonic = Cosmic-ray and (photo-pion) neutrino production

AGN could have EM jets. Also, a luminous AGN gives 1054 erg/yr, a GRB 1053 erg/(10 sec), so: GRBs are best-bet high-E sources

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The importance of early alerts

60 m

40 km

14.5 m 2.4 km

500 m

µ µ

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The importance of early alerts
Large gain by all-data-to-shore PLUS fast alerts
10

1
-1

10

10

-2

10

-3

10

-4

10

-5

10

2

10

3

10

4

10

5

10

6

10

7

(Bouwhuis 2003, 2005)

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Initial fireball neutrinos?
T = 30E
1/4 52

R

-3/4 -1/4 6.5 g

MeV ( : g = 1; e± : g = 43/8)

E 3T 60 MeV Detectable with IceCube up to z 0.1! And drives SN!

(Koers & Wijers 2005)

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Initial fireball neutrinos?
Fireball evolution with neutrinos

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Tale of two neutrinos
High-energy (E > 100 GeV): For KM3Net (best at lowest E ) and IceCube Beamed Detect 10 neutrinos per year per 100 GRBs, or 100 neutrinos per GRB 030329 Low-energy (E 100 MeV) For IceCube only Not or little beamed Detect a few neutrinos per year per GRB 030329, many per GRB 980425, PLUS the 99 others!!

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Radio: numbers and energy
GRB 030329 seen at 800 MHz WSRT, 1.5yr later

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A Radio Surprise!?
Early shock could give coherent (proton-synchrotron) emission High flux (>10 Jy at 30 MHz) Lasts <100 s, could preceed gamma rays, so all-sky monitor needed Dispersion measures cosmic density Escape from source?

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Swift
Last Friday, GRB 041217 became the first burst localized by Swift! (12' error, afterglow found by Gorosabel)

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Conclusions
GRBs are beamed/collimated, but very diverse GRBs offer complementary opportunities to study jet acceleration and baryon loading Nothing like high-energy neutrinos to probe their inner workings, provided we keep all-sky monitors in orbit To count them all: LOFAR 200 MHz all-sky monitoring!

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Distant Galaxies

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Distant Galaxies

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Origin Short GRB: Mergers?



Still speculation Swift launched 19 November 2004 LIGO/LISA connection

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