Neutrinos – Search, Detection and Applications| Neutrinos – Search, Detection and Applications |
In General > s.a. astrophysical and cosmological neutrinos;
gravitational-wave detection; types of neutrinos
[species, sterile neutrinos].
* Detection: 2010, Only two
astrophysical sources have actually been seen so far, the Sun and SN1987A.
* Motivation: Neutrinos are a 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 \(10^9\) eV from
γs producing \(e^+ e^-\) pairs off the cmb, and a similar one for
cosmic-ray \(p+\gamma\) into hadrons at about \(5\times10^{19}\) eV).
* Method: Telescopes based
on Cerenkov radiation from events in the 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, Super-Kamiokande;
NuBe (Neutrino Burster Experiment); IceCube; 2004, ANITA-lite prototype flight; 2016, SHiP,
an experiment at SPS to search for sterile neutrinos to be built by 2026.
@ Reviews: Grupen ap/96-conf;
Protheroe EPN-ap/99;
Bahcall & Davis PASP(00)ap/99 [history];
Halzen NPPS(04)ap;
news sr(06)nov [Antarctic];
Becker JPCS(08)-a0811;
Montaruli NPPS(09)-a0901;
Halzen a0911-conf;
Anchordoqui & Montaruli ARNPS(10)-a0912;
Gelmini et al SA(10)may [neutrino astronomy];
Kappes a1110-proc;
Karle NPPS(13)-a1210 [future experiments];
Kurahashi et IceCube a1402-proc.
@ Diffuse flux: Kowalski JCAP(05)ap;
Kravchenko et al PRD(06) [RICE];
Abbasi et IceCube PRD(11).
@ Experiments: Letessier-Selvon NPPS(03)ap/02 [Pierre Auger];
Spiering PS(05)ap-in [Amanda, Baikal, IceCube];
Chen et SNO NPPS(05);
Inoue et KamLAND NPPS(05);
Wischnewski et al IJMPA(05)ap-proc [Baikal];
Wischnewski a0710-conf,
a0710-conf [Baikal];
news pw(14)mar [future JUNO (Jiangmen Underground Neutrino Observatory) detector];
news pw(16)feb [future SHiP (Search for Hidden Particles) SPS experiment approved];
Aguilar-Arevalo et MiniBooNE PRL(18) [fixed-energy neutrino beam];
Fiorillo et al JCAP(21)-a2012 [IceCube constraints on equivalence principle violations];
news sn(21)may [first evidence for neutrino interactions at the LHC].
@ Ice detectors: Hulth et IceCube ap/06-conf [AMANDA to IceCube];
Barwick et al PRL(06) [flux results from ANITA-lite];
Barwick JPCS(07)ap/06 [ARIANNA].
@ Mediterranean underwater detectors:
Amore et al IJMPA(07) [NEMO project];
Cuoco et al JCAP(07)ap/06 [km3 detector];
Hernández-Rey JPCS(09)-a0904;
Margiotta et KM3NeT NIMA(14)-a1408 [KM3NeT, under construction].
@ Acoustic detection: Nahnhauer NIMA(11)-a1010-proc;
Vandenbroucke PhD(09)-a1201.
@ Other detectors / experiments:
news pt(17)aug [portable detectors];
> s.a. AMANDA; ANTARES;
IceCube; Super-Kamiokande.
Solar Neutrinos
> s.a. neutrino mixing; solar planets;
solar system [helioseismology]; types of
neutrinos [geoneutrinos].
* Problem: Only about 1/3
of the expected solar neutrinos are detected; It was solved by neutrino
oscillations, as confirmed in 2002.
* Experiments:
(1) R Davis et al since the 1960s monitor the amount of Ar in C\(_2\)Cl\(_4\);
Sensitive only to left-handed νes;
(2) Kamiokande II since 1987, higher threshold, neutrinos from the same reaction, can see
other flavors; (3) SAGE collaboration at Baksan, with Ga \(\mapsto\) 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 νes which interact
more with matter; Mostly νes are
produced, but their mass decreases traveling outwards, and, since the graphs of mass vs
density for the two νs cannot cross (second-order perturbation theory), most
of the neutrinos come out as νμs,
which are not seen by the ordinary experiments.
@ Status, reviews: Bahcall SA(69)may;
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-conf;
Parke PRL(95);
Dar & Shaviv PRP(99)ap/98;
Fiorentini & Ricci ap/98-proc;
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;
Peña-Garay & Serenelli a0811 [and solar composition problem];
Chavarria a1201-proc;
Antonelli et al AHEP-a1208;
Haxton et al ARAA(13)-a1208 [status and prospects];
Antonelli & Miramonti a1311-conf.
@ Oscillations: Mikheyev & Smirnov SJNP(85);
Bethe PRL(86);
Ahmed et SNO PRL(04)ne/02,
ne/03-proc [evidence].
@ Related topics: Bellini et al PRL(12)
+ news pw(12)feb
[neutrinos from solar proton-electron-proton fusion reactions].
Applications of Neutrinos
@ References:
Sugawara et al hp/03 [use to destroy nuclear weapons?];
Huber PLB(10),
news PhysOrg(12)mar [communication];
news wvtf(14)aug [monitoring nuclear reactors];
Luciano & Petruzziello a2007 [testing gravity].
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