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Underground megatons detectors :<strong>Solar</strong> <strong>Solar</strong> v<br />
Flares and Andromeda SN prompt v -GW GW discover<br />
Flares<br />
D.Fargion-Rome<br />
D.Fargion Rome University1, INFN, Italy<br />
�� A first , few MeVs <strong>Solar</strong> Neutrino Astronomy was opened by Davis, SK, Gallex, Gallex,<br />
SNO last four decades. decades<br />
�� Supernova neutrino 1987A Astronomy was oneshoot event two decades ago.<br />
�� UHE GeVs- GeVs TeVs (Muon) Neutrino Astronomy are masked by abundant<br />
atmospheric neutrino noise.. noise..Maybe<br />
Maybe soon ICECUBE may rise clustering. clustering<br />
�� UHE Cosmogenic Tau Neutrino in EeV energy , via Tau Airshowers in AUGER<br />
is within horizons a few years from now. now<br />
�� Supernovae Relic background via Gadolinium at edge. edge<br />
�� <strong>Solar</strong> tens MeVs Neutrino Flare is low energy garanteed , but not too rare, new<br />
solar Astronomy testing in principle all Neutrino Flavours Astronomy, Astronomy,<br />
at SK or<br />
UNO detection mass thresholds : for energetic events muons and taus might be<br />
born too. too.<br />
SN neutronization neutrinos versus GW<br />
detecting neutrino mass splitting<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 1
No one but 6 Neutrinos<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 2
The lepton thresholds<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 3
Neutrino events by SN 1987A in<br />
LMC in KII<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 4
(1987)<br />
Supernova Neutrinos<br />
Expected for<br />
Super-KAMIOKANDE at 10kpc,<br />
(ν-oscillation effects not included)<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 5
Additional Anti-Matter Anti Matter signals from <strong>Solar</strong> Flare: Flare:<br />
(as ( as<br />
OSSE Neutrons June 1991) an earlier and rarest<br />
Anti-Neutron<br />
Anti Neutron (above above threshold 6.5 GeV) GeV)<br />
signal in<br />
GLAST followed by more abundant Neutrons and<br />
latest protons<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 6
From half century ago..1956<br />
Neutron <strong>Solar</strong> Flare (J.Simpson J.Simpson)<br />
:In one hour tenfold CR neutrons�� neutrons almost half a day CR�� CR 3-4 4 neutrino<br />
atmospheric expected<br />
expected �� 3-4 4 from <strong>Solar</strong> Flare?<br />
Flare<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 7
Detecting <strong>Solar</strong> Neutrino Flare and Flavors<br />
by D.Fargion :<br />
JHEP 0406 (2004) 045<br />
see also D.F. Phys.Scripta<br />
Phys.Scripta T127 (2006) 22-24 22 24<br />
D.Fargion, D.Fargion,<br />
P.Di Giacomo,astro<br />
Giacomo, astro-ph ph 0812.4592, Nucl. PhysB <strong>2009</strong><br />
D.Fargion,F.Moscato<br />
" Muon and Tau Neutrinos Spectra from <strong>Solar</strong><br />
Flares",<br />
Chin. J.<br />
Astron. Astrophys.Vol 3.Suppl.75-86. 2003.<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 8
Flare-Supernova<br />
Flare Supernova 1987A<br />
energy Fluence Ratio<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 9
Neutrino event expected in SK from SN 1987A versus<br />
SOLAR FLARE = 242 : 30 = 8<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 10
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 11
<strong>Solar</strong> Flares are energetic, energetic<br />
prompt and not too rare<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 12
Why so much interest for the 20°<br />
January <strong>Solar</strong> Flare for Neutrinos?<br />
Neutrinos<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 13
GAMMA Spectra on 20 Jen. Jen.<br />
2005<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 14
The neutral-pion<br />
neutral pion signature: signature:<br />
a clear trace of a<br />
LOWER BOUND of charged pions<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 15
Super Kamiokande Bounds<br />
ν e<br />
ν μ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 16<br />
ν μ<br />
ν τ
SK<br />
ν e<br />
ν μ<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 17
MEGATON<br />
ν e<br />
ν μ<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 18
Correct cross section<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 19
MEGATON<br />
ν e<br />
ν μ<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 20
ν e<br />
5 MEGATON<br />
TITAND<br />
ν μ<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 21
10<br />
Megaton:ICECUBE<br />
ν e<br />
ν μ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 22<br />
ν
GIGATON<br />
ν e<br />
�� ICECUBE<br />
ν μ<br />
ICE-CUBE km 3<br />
P<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 23
Best signals: signals:<br />
by Anti Neutrino e before mixing<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 24
SK Anti ν e after in SK<br />
ν e<br />
ν μ<br />
ν τ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 25
The SK Detector<br />
41.4m 41.4m<br />
40m<br />
50000 tons ultra-pure water<br />
22500 tons fiducial volume<br />
1 km overburden = 2700 m.w.e.<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 26
12 MeV<br />
solar ν<br />
The low energy<br />
ν-e<br />
elastic<br />
scattering<br />
Still points back<br />
To the Sun<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 27
492 MeV<br />
atmospheric<br />
electron ν<br />
Note diffuse<br />
edge of ring<br />
from electron<br />
produced by<br />
ν e-nucleon<br />
interaction<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 28
603 MeV<br />
atmospheric<br />
muon ν<br />
Note sharp<br />
edge of ring<br />
from muon<br />
produced by<br />
ν μ-nucleon<br />
interaction<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 29
Tau signal<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 30
Highest energetic solar particles<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 31
Flavor Neutrino Mixing by neutrino<br />
mass splitting :<br />
The rare Tau Appearence<br />
because of large Oscillation Lenghts<br />
versus Earth Diameter<br />
The allowable neutrino tau appearence from the Sun<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 32
A first SK Tau ν candidate event (~3 GeV)<br />
2250<br />
2000<br />
1750<br />
1500<br />
1250<br />
1000<br />
750<br />
500<br />
250<br />
0<br />
(Still Fully Contained)<br />
800 1000 1200 1400 1600 1800<br />
1<br />
0.8<br />
0.6<br />
0.4<br />
0.2<br />
0<br />
800 1000 1200 1400 1600 1800<br />
0 2 4 6 8 10 12 14 16 18 20<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 33<br />
140<br />
120<br />
100<br />
80<br />
60<br />
40<br />
20<br />
0<br />
0. 0.5 1. 1.5 2.<br />
0. 0.5 1. 1.5 2.
# of events<br />
140<br />
120<br />
100<br />
80<br />
60<br />
40<br />
20<br />
0<br />
Super-Kamiokande Preliminary<br />
1289.4 days<br />
The pion-signature<br />
pion signature<br />
0 50 100 150 200 250 300<br />
MeV/c<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 34<br />
2<br />
Invariant Mass
Probability Meaning<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 35
Why <strong>Solar</strong> Neutrino Flare have not<br />
been yet observed? observed?<br />
Maybe because<br />
of low density acceleration target<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 36
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 37
Conclusions:<br />
Conclusions<br />
1) Nearly equal electron-muon<br />
electron muon neutrino Flux Flare<br />
2) A first ANTI-Neutrino<br />
ANTI Neutrino signal in electron-positron<br />
electron positron tracks<br />
3) A Hard electron neutrino spectra than SN ones<br />
4) A first Muon appearence in harder spectra above 400 MeV<br />
5) A rarest Tau appearence in harder spectra, spectra,<br />
4 GeV, GeV,<br />
6) Few events in future HK might occur in Oct –Nov Nov 2003<br />
A probable transient event on 20 January 2005<br />
7) A <strong>Solar</strong> Neutrino and Anti Neutrino Flare Astronomy<br />
must be born almost garanteed in larger Gd-UNO Gd UNO (440 kton)<br />
and-or and or HSK and Deep TITAND.<br />
8) More <strong>Solar</strong> Flare than SN at the edge.<br />
9) The rare Andromeda SN neutronization neutrino delay<br />
versus GW may test neutrino mass splitting.<br />
splitting<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 38
Thank You for the attention<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 39
Forbush after all…<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 40
Present -Future Future Neutrino Detectors versus FLARE<br />
HK and UNO<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 41
Anti mu after<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 42
<strong>Solar</strong> Standard Model: a noisy<br />
neutrino electron sky<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 43
E dN�dE�Log 10�cm 2 s sr� �1 �<br />
10<br />
5<br />
0<br />
�5<br />
�10<br />
�15<br />
�20<br />
Radio<br />
CMB<br />
Cosmological MasslessΝ<br />
IR<br />
Optical<br />
UV<br />
X<br />
Cosmic SuperNovaΝ<br />
AtmosphericΝΜ<br />
Γ<br />
Flux Number<br />
WB limit<br />
�5 0 5 10 15 20<br />
E�Log 10 eV�<br />
ΝΤ<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 44<br />
C.R.<br />
AGNΝ<br />
Hires2<br />
AGASA<br />
Hires1
Neutron and Gamma…and<br />
Neutrinos?<br />
Neutrinos<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 45
Earliest Estimate 2003-2006 2003 2006-versus versus 2008<br />
gauged by gamma bound 2005<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 46
Neutrino muon before mixing<br />
Fargion D.-<strong>TAUP</strong> D. <strong>TAUP</strong>-01 01-07 07-<strong>2009</strong> <strong>2009</strong>-Rome Rome 47
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