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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 !
Francis Halzen, Hagar Landsman, Teresa Montaruli
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?
LBL, IceCube Meeting, Mar. 2005
Woods & Thompson, astro-ph/0406133
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 surfaceThe Magnetar Model and n emission
Rates strongly depend on beaming angle around polar axis
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 d21010
Detected radio afterglows imply relativistic outflows + huge luminosities with barion loading fireball
(Piran et al, astro-ph0502148, Ioka et al, astro-ph/0503279)
No spectral measurement of the 1st s available. X-ray detectors suffered saturation effects.
SGR 1900+14AMANDA B-10
Beppo-SAX: Spectrum for first 68s up to 700keV (1s resolution)
SGR 1806-20AMANDA-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 msGiant flare energy
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)
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
negative power law and vary it to account for the errorsSpectrum Extrapolation at TeV energies
Guidorzi private communication
At South Pole: d =-20˚ q = 70˚Muons from Gammas
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
For a source below horizon
But also horizontal muons
from neutrinos but 1/ 2.65
AMANDA can constrain it !