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].
@ 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 [rev];
Halzen ap/06-in
[rev]; Meszaros & Razzaque ap/06-in
[from GRBs]; Lipari ap/06-in;
Halzen & Hooper PRL(06) [flux bounds].
@ Constraints: Hansen et al PRD(02)ap/01 [nucleosynthesis
and cmb]; Mangano et al PLB(02)
[effective number]; Ichikawa a0706-in.
@ 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)
[
tau's];
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]; > s.a. contents
of
the
universe.
@ Cosmic background: Alpher et al PR(53);
Trotta & Melchiorri PRL(05)ap/04 [anisotropy];
Mangano ap/06-in
[non-thermal features]; Loeb & Waxman JCAP(06)
[from starburst galaxies]; Michney & Caldwell JCAP(07)
[anisotropy]; de Bernardis et al a0707 [and age of universe].
@ 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 GRB's]; Waxman ap/05-in
[high-E]; Vissani & Costantini ap/05-in
[supernovas]; Daigne et al PRD(05)
[first stars].
@ And neutrino properties: Serpico & Kachelrieß PRL(05)
[mixing angles]; > s.a. neutrinos [mass], spin-statistics.
Detection > s.a. 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 ap/99;
Bahcall & Davis PASP(00)ap/99 [history];
Halzen ap/04-in;
news sr(06)nov
[Antarctic].
@ Experiments: Letessier-Selvon ap/02-in
[Auger];
Spiering ap/05-in
[Amanda, Baikal, IceCube]; Chen et SNO NPPS(05);
Inoue et KamLAND NPPS(05);
Wischnewski ap/05-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 ap/06-in
[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].
@ AMANDA: Andres et al APP(00)ap/99;
Desiati ap/03-in;
Halzen ap/03-in;
Silvestri MPLA(07);
Ackermann et al a0711-ApJ.
@ ANTARES:
Montaruli
ap/02-in;
Katz EPJC(04)ap/03-in;
Korolkova et al ap/04-in;
Becherini ap/06-in;
Kouchner a0710-in.
@ IceCube: Kowalski JCAP(05)ap [diffuse
flux]; Karle ap/06-in;
Desiati ap/06-in;
Rott ap/06-in;
Waldenmaier a0802-in; > s.a. dark matter.
Solar Neutrinos > s.a. solar
system [helioseismology].
* Problem: Only about
1/3 of the expected solar 's
are detected; Solved by oscillations,
as confirmed in 2002.
* Experiments: (1) R
Davis et al since the 1960's monitor the amount of Ar in C2Cl4;
Sensitive only to left-handed e's;
(2) Kamiokande II
since 1987, higher threshold, 's
from 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, 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 ap/06-in.
@ Oscillations: Mikheyev & Smirnov SJNP(85);
Bethe PRL(86);
Ahmed et SNO PRL(04)ne/02,
ne/03-in
[evidence].
Main page – Abbreviations – Journals – Comments – Other
sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified
15 jun 2008