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Neutrinos and TeV photons from Soft Gamma Repeater giant flares. Francis Halzen, Hagar Landsman, Teresa Montaruli astro-ph/0503348. Neutrino telescopes can be used as TeV g detectors for short time scale events using m s from p photoproduction in g showers !

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neutrinos and tev photons from soft gamma repeater giant flares
Neutrinos and TeV photons from Soft Gamma Repeater giant flares

Francis Halzen, Hagar Landsman, Teresa Montaruli

astro-ph/0503348

Neutrino telescopes can be used as TeV g detectors for short time scale events using ms from p photoproduction in g showers !

Can AMANDA detect a signal from 27 Dec. giant flare from SGR 1806-20 (above horizon)? In what channels?

  • Review soft-g and X-ray observations on SGR giant flares
  • A toy model based on Beppo-SAX SGR 1900-14 spectrum
  • Muon and Neutrino signals
  • Backgrounds
  • Useful information for the blind data analysis

LBL, IceCube Meeting, Mar. 2005

what are sgr s
What are SGR’s?
  • X-ray stars emitting short (~100 ms) bursts in X/soft g-ray typically of energy 1041 D102 ergs
  • Steady X-ray emission with luminosities 1035-1036 D102 erg/s with OTTB+power law spectra E-(13)
  • From slow down rate of steady emission period (5-8 s) huge magnetic fields B ~1014-1015 G
  • Similar to 8 Anomalous X-ray Pulsars but typically these do not emit bursts (1 exception)
  • 5 galactic except for SGR 0526-66 in LMC

http://solomon.as.utexas.edu/magnetar.html

Woods & Thompson, astro-ph/0406133

the magnetar model and n emission

Steady X-ray emission powered by decay of n star magnetic field

Luminosities 1035-1036 D102 erg/s periodic (5-8 s)

Neutrinos: Zhang et al ApJ 595 (2003)

the potential drop through the magnetosphere of the rotating n star might accelerate

protons above photomeson threshold (depends on n star period and B and geometrical

factor)  interaction on thermal radiation from heated n star surface

The Magnetar Model and n emission

dN/dE E-2

Rates strongly depend on beaming angle around polar axis

why giant flares
Why giant flares?
  • Dec. 27, 2004 peak lasting 0.25 s followed by a 300 s long tail with 7.57 s
  • period and -140 s precursor (INTEGRAL, GCN2920) following previous series of bursts: Dec 21 and Oct 5. Still active.
  • 3 ‘giant’ flares: VERY HARD component dN/dE  E-1.5-1.7(Cheng et al., Nature 1996)

Rearrangements of magnetic field and formation and dissipation of strong localized currents. These may fracture the rigid crust that outbursts

Can be a process in which nucleons and nuclei are accelerated

Similar to small GRB’s:SGR giant flares are 106-7 less intense but d21010

Detected radio afterglows imply relativistic outflows + huge luminosities with barion loading fireball

(Piran et al, astro-ph0502148, Ioka et al, astro-ph/0503279)

giant flare energy

No spectral measurement of the 1st s available. X-ray detectors suffered saturation effects.

SGR 1900+14AMANDA B-10

Beppo-SAX: Spectrum for first 68s up to 700keV (1s resolution)

SGR 1806-20AMANDA-II (critical period)

 No spectrum available.

Similar flare. >2 orders of magnitude stronger

GEOTAIL (astro-ph/0502315) not saturated: measured fluence implies for d = 15 kpc a very efficient mechanism that releases ~1047 erg in 600 ms

Giant flare energy
the sgr 1900 14 aug 27 1998 giant outburst
The SGR 1900-14 Aug 27, 1998 giant outburst

A)0-67 sec 70-650 keV

OTTB+PL E-1 exp(-E/31.2 keV)+E-1.47

B) 68-195 sec 70-400 keV

OTTB E-1 exp(-E/34.2 keV) + E-4.5

C) 196-323 sec 70-400 keV

OTTB E-1 exp(-E/28.9 keV)

E-1.47

Beppo-Sax (Feroci et al, 1999)

Guidorzi et al, 2004: response function of GRBM was not well known at large off-axis angles

 70-600 keV only and 10% sys error

spectrum extrapolation at tev energies

New best fit accounts better for the <60 keV region but for HE we use

negative power law and vary it to account for the errors

Spectrum Extrapolation at TeV energies

OTTB+PL fits

Guidorzi private communication

muons from gammas

g spectra

At South Pole: d =-20˚  q = 70˚

Muons from Gammas
  • energy to produce m

of energy E

Competition of pion interaction and decay in the atmosphere

(Drees Halzen Hikasa, PRD39, 1989, Stanev Gaisser Halzen PRD32 1985):

Pion photoproduction cross

section in FLUKA

Em,th = 10 GeV

AMANDA-II horizontal averaged area = 30000 m2 and 0.3 s

muon signal

1 Hz in 82 deg2 and 0.3 s at 5 km depth

6

0.8

Muon signal

astro-ph/0110513

Gamma showers in MILAGRO

But this particular flare was at 68˚ and Milagro analyses are commonly performed up to 45˚

upward going muons and cascades in amanda
Upward-going muons and cascades in AMANDA

For a source below horizon

as SGR1900+14

But also horizontal muons

from neutrinos but 1/ 2.65

conclusions
Conclusions
  • We calculated possible muon and neutrino rates for Dec 27 giant flare as a function of spectrum.

AMANDA can constrain it !

  • Relevant time scale of the order of 0.1 s and spatial constraint allow a search using downgoing muons
  • We should use the neutrino cascade channel and look for neutrino induced muons
  • We will preferably use IceTray or SIEGLINDE
  • Start from raw data -> ROOT files