Astrophysical
and Cosmological Neutrinos| Astrophysical
and Cosmological Neutrinos |
In General > s.a. astrophysics;
dark energy; dark
matter; equivalence
principle; modified
lorentz symmetry; quantum-gravity phenomenology.
* Abundance: Can be determined indirectly from cmb anisotropy; Contributes
to the dark matter.
* Sources: 2004, Only
two individual ones known so far, the Sun and SN1987A, none above 108 eV.
@ General references: Kim & Pevsner 93; Sarkar NPPS(98)hp/97;
Roulet ap/00-ln;
Bahcall IJMPA(01)hp/00;
Dolgov PRP(02)hp;
Beacom a0706-in
[rev]; Lipari et al PRD(07)
[flavor composition and energy spectrum]; Fargion et al a0708 [role
of tau neutrino]; Halzen & Klein PT(08)may
[rev]; Haxton a0808 [introductory];
Lipari PRD(08) [and proton astronomy].
@ High-energy:
Vietri PRL(98)
[from GRBs]; Stasto IJMPA(04)ap/03;
Weiler IJMPA(03)ap-in;
Halzen ap/05-ln;
Mocioiu IJMPA(05),
Quigg ap/06-in
[rev]; Halzen ap/06-in
[rev]; Meszaros & Razzaque ap/06-in
[from GRBs]; Lipari NIM-ap/06-in;
Halzen & Hooper PRL(06)
[flux bounds]; Chiarusi & Spurio a0906 [rev];
Scholten et al a0910/PRL [E > 1022 eV].
@ Constraints on number of species: Hansen et al PRD(02)ap/01 [nucleosynthesis
and cmb]; Mangano et al PLB(02)
[effective number]; Ichikawa a0706-in;
Ichikawa et al PRD(08)
[from cmb].
@ And cmb: López et al PRL(99)
+ pn(99)apr;
Bhattacharyya et al PLB(03),
Hannestad
JCAP(03)ap,
ap/03-in
[WMAP and 2dF].
@ Large-scale structure: Hu et al PRL(98);
Gawiser ap/00-in;
Novosyadlyj et al ap/00-in;
Elgarøy et al PRL(02)
[2dF galaxy survey].
@ Cosmological: López et al PRL(99)
[Nnu/Ngamma];
Fodor et al JCAP(03)
[bounds on flux]; Crocker et al
PRD(04)hp/03 [interferometry
from curved spacetime]; Altaie CQG(03)gq/02 [back-reaction
on static universe]; Gorham et al PRL(04)
[UHE,
flux limits]; Athar & Kim PLB(04)
[
taus];
Pisanti & Serpico ap/05-in
[rev]; Seckel & Stanev PRL(05)
[and uhecr sources]; Hannestad PPNP(06)ap/05-in
[rev]; Pfenniger & Muccione A&A(06)ap [entanglement
and pressure]; Krauss ap/06-in
[rev]; Cirelli & Strumia JCAP(06)ap [and
other light particles]; Quigg a0802-in;
Pritchard & Pierpaoli a0805 [constraints
from 21-cm observations]; Dodelson & Vesterinen a0907 [last-scattering
surfaces]; > s.a. contents
of
the
universe.
@ Cosmic background: Alpher et al PR(53);
Mangano ap/06-in
[non-thermal features]; Loeb & Waxman JCAP(06)
[from starburst galaxies]; de Bernardis et al JCAP(08)-a0707 [and
age of universe]; Ringwald a0901-in
[detection prospects]; Hannestad et al a0910 [anisotropy].
@ Cosmic background, anisotropy: Trotta & Melchiorri PRL(05)ap/04;
Michney & Caldwell JCAP(07);
> s.a. Copernican
Principle.
@ Geoneutrinos:
Araki et KamLAND Nat(05)jul
+ pw(05)jul; Fiorentini
et al PRP(07)
[and Earth's interior].
@ Other sources: Razzaque et al PRD(03)
[stellar collapse and GRBs]; Waxman ap/05-in
[high-E]; Vissani & Costantini ap/05-in
[supernovas]; Daigne et al PRD(05)
[first stars]; Caballero et al a0910/PRD [bh-ns mergers].
@ And neutrino properties: Serpico & Kachelrieß PRL(05)
[mixing angles]; > s.a. neutrinos [mass], spin-statistics.
Detection > s.a. detection
of gravitational waves; solar
planets.
* Motivation: Unique
source of information on deep processes inside stars and galaxies; Neutrinos
are not affected by processes that stop other particles, and in their spectrum
there
are no "walls" (like the electromagnetic ones at about 109 eV
from 
's
producing e+e– pairs
off the cmb, and a similar one for cosmic ray p + into
hadrons at about 5
× 1019 eV).
* Method: Telescopes
based on Cerenkov radiation from events in detector mass; Need huge detectors
(low event rates), located deep below the surface (large backgrounds);
Use
mines, ocean water, antarctic ice; The challenge is to lower the detection
threshold below 1019 eV.
* Experiments: 1999,
AMANDA (Antarctic Muon and Neutrino Detector Array), NESTOR, Baikal, ANTARES
(Astronomy with a Neutrino Telescope and Abyss
environmental
RESearch), Superkamiokande; NuBe (Neutrino Burster Experiment); IceCube; 2004,
ANITA-lite prototype flight.
@ Reviews: Grupen ap/96-in;
Protheroe EPN-ap/99;
Bahcall & Davis PASP(00)ap/99 [history];
Halzen ap/04-in;
news sr(06)nov
[Antarctic]; Becker a0811-in;
Montaruli a0901-in;
Halzen a0911-in.
@ Experiments: Letessier-Selvon NPPS-ap/02
[Auger];
Spiering PS-ap/05-in
[Amanda, Baikal, IceCube]; Chen et SNO NPPS(05);
Inoue et KamLAND NPPS(05);
Wischnewski IJMPA(05)ap-in
[Baikal]; Hulth et IceCube ap/06-in
[AMANDA to IceCube]; Kravchenko et al PRD(06)
[RICE,
diffuse flux]; Barwick et al PRL(06)
[flux results from ANITA-lite]; Barwick JPCS(07)ap/06
[ARIANNA]; Cuoco et al JCAP(07)ap/06 [km3 detector
in the Mediterranean]; Amore et al IJMPA(07)
[NEMO project]; Wischnewski a0710-in, a0710-in
[Baikal]; Hernández-Rey JPCS(09)-a0904 [in
the Mediterranean]; > s.a. experimental projects.
Solar Neutrinos > s.a. solar
system [helioseismology].
* Problem: Only about
1/3 of the expected solar neutrinos
are detected; Solved by oscillations,
as confirmed in 2002.
* Experiments: (1) R
Davis et al since the 1960s monitor the amount of Ar in C2Cl4;
Sensitive only to left-handed e's;
(2) Kamiokande II
since 1987, higher threshold, neutrinos
from the same reaction, can see other flavors;
(3) SAGE collaboration at Baksan, with Ga 
Ge; (4) Gallex collaboration at
Gran Sasso, start end of 1990; (5) Sudbury, ON.
* Oscillations: The effective m depends
on matter density, and in the Sun's core the masses are much higher than usual,
especially for e's
which interact more with matter; Mostly e's
are produced, but their mass decreases traveling outwards, and, since the graphs
of mass
vs density
for the two 's cannot
cross (second-order perturbation theory), most of the neutrinos come out as mu's,
which are not seen by the ordinary experiments.
@ Status, reviews: Pinch 86 [constructivist history]; Wolfenstein &
Beier PT(89)jul;
Schwarzschild PT(90)oct;
Sciama Nat(90)dec, PRL(90);
Bahcall SA(90)may, in(98)ap/97-ln, he/00;
Parke PRL(95);
Dar & Shaviv PRP(99)ap/98;
Fiorentini & Ricci
ap/98-in;
Pennicott pw(01)jul
[solution]; Miramonti & Reseghetti RNC(02);
Smy MPLA(02);
Bahcall IJMPA(02);
McDonald et al SA(03)apr [solution]; Bahcall & Pinsonneault
PRL(04)ap;
Bahcall phy/04-in,
in(05)phy/04 [I],
et al JHEP(04)hp;
Nakahata & Super-K NPPS(05);
Turck-Chièze NPPS(05);
Waxman Sci(07)ap/06;
Pena-Garay & Serenelli a0811 [and
solar composition problem].
@ Oscillations: Mikheyev & Smirnov SJNP(85);
Bethe PRL(86);
Ahmed et SNO PRL(04)ne/02,
ne/03-in
[evidence].
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nov 2009