Construction of a hadronic model for the production of neutrinos and the associated gamma-rays in galactic sources Prediction of neutrino signals in TeV-range (c.f. IceCube –south; Nemo -north) Analysis of correlated gamma-ray detection: luminosity and opacity
Prediction of neutrino signals in TeV-range
(c.f. IceCube –south; Nemo -north)
Analysis of correlated gamma-ray detection: luminosity and opacity
(c.f. MAGIC: Major Atm. Gamma Imaging Cerenkov E>30GeV –North
HESS: High Energy Stereoscopic System E>100GeV –South
GLAST satelite E>100MeV)
Primary: massive B star, generates a matter field around.
Secondary: compact object, a mass accretor, generates a jet (neutron star or BH, determined by Doppler shift of absortion lines of the primary –analysis of changes of radial velocity vs. orbital position).
Miniatures of quasars.
2004 September 24
2 and 2 mean energy E /4 each, for each mean energy E /2
E = E / 2
=2.2 (reproduces EGRET obs.); in lab/observer frame
namely Bjet>2.8 10^-6 G
Conservation of energy relates luminosities of neutrino & gamma
Average production kinematics in decay
In the reaction channel pp: D =1
V : interaction region between jet & wind
(e.g. Aharonian & Atoyan 1996):
Production of mu-neutrinos at the source
(c.f. upper limit of AMANDA II 2005)
flavoroscillations (e.g. SNO 2002, solar).
Relative neutrino production at source (pp):
Becomes 1 : 1 : 1 for astrophysical distances
such that (Athar et al. 2005)
50% reductionmu-nu flux
(Costantini & Vissani 2005)
(vide MAGIC 2005)
distance to the neutron star:
Threshold for pair creation:
Cross section of the reaction:
me, r0 electron mass and radius
nph1 (Be star), and nph2 (disk)
The black body bright function
= 22500 K, = 17500 K (Martí & Paredes 1995).
neutrino signal to noise relationship, and gamma
opacity: correlated ICECUBE and MAGIC briefly…