frontiers in neutrino astrophysicsconferences.fnal.gov/win03/talks/john beacom.pdf · learned and...
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![Page 1: Frontiers in Neutrino Astrophysicsconferences.fnal.gov/win03/Talks/John Beacom.pdf · Learned and Mannheim, Ann.Rev.Nucl.Part.Sci 50, 679 (2000) John Beacom, Theoretical Astrophysics](https://reader035.vdocuments.us/reader035/viewer/2022081612/5f5e3b97e4478c69e00961bc/html5/thumbnails/1.jpg)
Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Astrophysics:Theoretical Status and Experimental Outlook
John BeacomTheoretical Astrophysics Group, Fermilab
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Introductory Remarks
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Past Frontiers• Bethe and Peierls, Nature (1934)“If [there are no new forces] ----one can conclude that there is no practicallypossible way of observing the neutrino.”
• 10 years agoSolar neutrino problemAtmospheric neutrino problemLarge neutrino massesNonzero magnetic moments, decay, etc.
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Lucky Neutrinos
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
State of the Field“There is nothing new to be discovered in physics now,All that remains is more and more precise measurement.”
-- Kelvin, c. 1900
•We now understand neutrinos(Yeah, right)
•We now understand cosmology(Yeah, right)
•We now understand high-energy astrophysics(Yeah, right)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Mixing
(graphic from Georg Raffelt)
e 1
2
3
jUµ
τ
ν ν ν = ν ν ν α
i13c s s e
s 2 c 2 1 2s 2 c 2 1 2
U
− δ −
−
atm 13solar45 , 35 , 10° ° °θ θ θ ≤
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino MassesNormal Hierarchy
Beacom and Bell, PRD 65, 113009 (2002)
1 1
2 22 1 solar
2 2 2atm3 1 solar
2atm32
2 solar
m m
m m m
m m m m
mm 10m m
=
= + δ
= + δ + δ
δ≤ ≤
δ
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Cosmological Parameterstotal
2matter
2baryon
2neutrino
1.02 0.02h 0.14 0.01h 0.022 0.001
h 0.010.71 0.04
etc.
0.70.23 eV
h
mΛ
ν
= ±
= ±
= ±
<
= ±
=
<
ΩΩΩ
Ω
Ω
(WMAP)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Number Densities
m nν ν νρ = ∑
N 4 (99%CL) BBNν <Abazajian, Astropart. 19, 303 (2003)
1.5 N 7.2 WMAPν≤ ≤ + +Crotty, Lesgourgues, and Pastor,PRD 67, 123005 (2003)
n nν νDolgov et al., NPB 632, 363 (2002);Wong, PRD 66, 025015 (2002);Abazajian, Beacom, and Bell,
PRD 66, 013008 (2002)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Dark Mattermatter CDMρ = ρ
baryons
neutrinos
+ ρ
+ ρ
m nν ν νρ =Future discovery range:
Abazajian & Dodelson,PRL 91, 041301 (2003)
Kaplinghat, Knox & Song,astro-ph/0303344
(graphic from Kev Abazajian) See Abazajian parallel talk
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Photon Windows
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Windows
Neutrino Facilities Assessment Committee, NAS (2002)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Astrophysical Neutrinos:Searching High
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
High Energy Messengers
Whipple
F. Krennrich et al., ApJ 575, L9 (2002)
Protons (diffuse) Photons (Markarian 421)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Beyond the Veil
Learned and Mannheim, Ann.Rev.Nucl.Part.Sci 50, 679 (2000)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Active Galaxies
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
UHE Neutrinos
e
initial fluxes are: : 1 : 2 : 0µ τν ν νϕ ϕ ϕ =
(graphic from Francis Halzen)
e
after oscillations: : 1 : 1 : 1µ τν ν νϕ ϕ ϕ =
Earth opacity effectsabove E ~ 100 TeV
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
ICECUBE
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Flavor Identification
10 PeV τν∼10 TeV µν∼e100 TeV ν∼
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
IceCube Sensitivity
AMANDA-B10
AMANDA-II
J. Ahrens et al. (IceCube), astro-ph/0305196
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino-Gamma Connection
J. Ahrens et al. (AMANDA-II), astro-ph/0309585
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutrino Decay
~ 5:1:1 ~ 0:1:1
30, , , ,4 2 4π π π
δ = π
Possible direct measurement of CP phase too!δ
Beacom, Bell, Hooper, Pakvasa, Weiler, PRL 90, 181301 (2003);Beacom, Bell, Hooper, Pakvasa, Weiler, hep-ph/0309267
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Nonstandard Flavor RatiosFlavor ratios can also deviate from 1:1:1 due to:•Tiny-δm2 mixing to steriles
Crocker, Melia, Volkas, ApJS 130, 339 (2000); 141, 147 (2002);Berezinsky, Narayan, Vissani, NPB 658, 254 (2003);Keranen, Maalampi, Myyrylainen, Riittinen, hep-ph/0307041;Beacom, Bell, Hooper, Learned, Pakvasa, Weiler, hep-ph/0307151
•CPT violationBarenboim, Quigg, PRD 67, 073024 (2003)
•For these and astrophysical reasons, it is veryimportant to test the flavor ratios directly!Barenboim, Quigg, PRD 67, 073024 (2003);Beacom, Bell, Hooper, Pakvasa, Weiler, hep-ph/0307025;Jones, Mocioiu, Reno, Sarcevic, hep-ph/0308042
See Bell parallel talk
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Astrophysical Neutrinos:Searching Very High
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
UHE Neutrino Prospects
Importanceof neutrinomixing
Spiering, J. Phys. G29, 843 (2003) See Besson parallel talk
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
GZK Neutrinos0
CR CMBp p n +
+ γ → ∆ → + π
→ + π
0
+ +µ
π → γγ
π → µ ν
Connected observables:
•Protons
•Photons
•Neutrinos
Cronin
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Protons, Photons, and Neutrinos
Semikoz, Sigl, hep-ph/0309328
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Existing Neutrino Limits
Semikoz, Sigl, hep-ph/0309328
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Future Neutrino Sensitivity
Semikoz, Sigl, hep-ph/0309328
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
ANITA
Funded 2003
Flies 2006
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Other Physics•Neutrino-nucleon cross section at high energies
Domokos, Kovesi-Domokos, Burgett, Wrinkle, JHEP 0107, 017 (2001);Tyler, Olinto, Sigl, PRD 63, 055001 (2001);Jain, Kar, McKay, Panda, Ralston, PRD 66, 065018 (2002);Anchordoqui, Feng, Goldberg, Shapere, PRD 66, 103002 (2002);Friess, Han, Hooper, PLB 547, 31 (2002)
•Z-bursts, supermassive dark matter, top-downGorbunov, Tinyakov, Troitsky, Astropart. Phys. 18, 463 (2003);Jones, Mocioiu, Reno, Sarcevic, hep-ph/0308042; Fodor, Katz, Ringwald, Tu, hep-ph/0309171
•New astrophysical sources
•New tests of neutrino properties
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Astrophysical Neutrinos:Searching Very Low
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Supernovae
SN Rates
SN Detection
Modeling (1d, 2d, 3d)
SN1999dk, z = 0.015
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Supernova Energetics
2 2NS NS 53 59
BcoreNS
GM GM3 3E 3 10 ergs 2 10 MeV5 R 5 R
∆ − × ×
2B
4B
K.E. of explosion 10 EE.M. radiation 10 E
−
−
∆
∆
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Supernova Neutrino Emission
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Supernova Neutrino Detection
IMB
KamIIe
4
3
SN1987A :
SN200?
20 p e n events
10 CC events10 NC events
? :
+ν →∼
∼
∼
Supernova physics (models, black holes, progenitors…)
Particle physics (neutrino properties, new particles, …)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Waiting Is Boring
“Everybody complains about the supernovarate, but nobody does anything about it.”
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Supernova Neutrino Background
Ando, Sato, and Totani, Astropart. Phys. 18, 307 (2003)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Relative Spectra
(M. Malek)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
SK Data Limit
•4.1 years of SK data
•Background limited
•Some improvement is possible
Malek et al. (SK), PRL 90, 061101 (2003)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
SNB Flux Limit•Predictions roughly agree on spectrum shape
•Main question is normalization of
Kaplinghat, Steigman, Walker, PRD 62, 043001 (2000)
Fukugita and Kawasaki, M
Malek et al. (SK), PRL 90, 0611
NRAS 3
01 (2
40, L7 (2003)
003)1.
2
2.2
0.4 0.
2/cm /s, E 19.3 Me
Ve
<
ν >ν
Ando, Sato, and Totani, Astropart. Phys. 18, 307 (2003)4
•Last two based on multiwavelength measurementsof the star formation rate as a function of redshift
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Inverse Beta Decay
e p e n+ν + → +
•Cross section is “large” and “spectral”2 42 20.095(E 1.3MeV) 10 cm
E E 1.3MeVe
−σ −ν−ν
Corrections in Vogel and Beacom, PRD 60, 053003 (1999)
•We must detect the neutron, but how?
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
A Proposed Solution
John Beacom and Mark Vagins, hep-ph/0309300
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Add Gadolinium to SK?
GadoliniumAntineutrinoDetectorZealouslyOutperformingOldKamiokande,Super!
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutron CaptureCapture on H: sigma = 0.3 barns
Egamma = 2.2 MeV
Capture on Gd: sigma = 49100 barnsEgamma = 8 MeV(Equivalent Ee ~ 5 MeV)
H H Gd GdHtotal Gd
1 1 1 n n= + = σ + σλ λ λ
At 0.2% GdCl3:Capture fraction = 90%
4cm, 20 sλ = τ = µ
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Cost of Gd
Based on 100 tons of GdCl3 in SK (0.2% by mass)
1984: $4,000/kg $400,000,000/SK
1993: $485/kg $48,500,000/SK
1999: $115/kg $11,500,000/SK
2002: $4/kg $400,000/SK
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Important GdCl3 Properties•Soluble in water (unlike mineral oil)
•Initial chemical and radiological purity excellent
•Initial water transparency tests excellent
•100 tons? No problem
•Gadolinium used in MRIcontrasting agents
•You could drink 12 liters ofGADZOOKS! water every day
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Gadolinium SupplementsTry “gadolinium health buy” in Google
1.25 ng/liter Gadolinium
“Supports healthy cellular functions”
“Not carcinogenic”
Note: sea water is 0.7 ng/liter Gadolinium
But it doesn’t come in raspberry flavor
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Neutron Backgrounds in SKDon’t want captures on Gdto dilute the solar signal Solar e e
~ 10/day
− −ν + → ν +
Backgrounds~ 100/day
How many neutrons are inSK anyway?
•Spallation ~ 105/daybut can be easily cut
•Reactor ~ 20/day (more likely a signal!)
•152Gd decay 1010 alpha/day, P(alpha,n) on 17O is 10-10
•U/Th contamination in GdCl3 must be controlled
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Correlated Backgrounds•Singles event rate above 5 MeV is ~ 1/ton/yearso accidental background rate is vanishing
•8He/9Li/11Li produced by spallation Beta decay followed by neutron emissionRare, controlled by timing and energy cuts
e
e
bound invisible free
Reactor p e n
Atmospheric p e n
Atmospheric p n invisible
+
+
+µ
ν + → +
ν + → +
ν + → µ + +
i
i
i
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Spectrum With GADZOOKS!
Beacom and Vagins, hep-ph/0309300
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Reactor Antineutrinos
KamLAND first data 0.16 kton yr
Just 3 days inSK GADZOOKS!
“High” energies only,less resolution
Eguchi et al. (KamLAND), PRL 90, 021802 (2003)
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Galactic Supernova Detectione
16
16e
16e
8000 p e n
700 O X (E 5 10 MeV)
300 e e (e is forward)100 O e X (buried)
O e X
−
+
+ν + → +
ν + → ν + γ + = −− − −ν + → ν +
ν + → +
ν + → +
∼
With GADZOOKS!, we can separate reactions
Real chance to see CC reactions on 16OHaxton, PRD 36, 2283 (1987)Oscillations can increase those yields by ~ 10
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Atm. Neutrinos and Proton Decay
16bound free
16bound free
p ( O) n Xn ( O) p X
+
−
ν + → + +
ν + → + +
•Atmospheric neutrino charged-current interactions
Flux ratio predictionsMatter effects in oscillationsCPT violation (Barenboim, Lykken, et al.) tests
•Nucleon decay15 15, p, n from O and N
following N Kγ γ γ
→ ν
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
Conclusions•GADZOOKS!Propose to add 0.2% GdCl3 to Super-Kamiokande
(Beacom and Vagins, paper in preparation)
•Potentially quick and inexpensive
•Detect the Supernova Neutrino Background (SNB)Astrophysical neutrinos from redshift z ~ 0.5Unique probe of the dark supernova rateMeasurement of supernova neutrino spectrumNew tests of neutrino properties
•New results on reactor, solar, atmospheric, andnucleon decay
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
ConclusionsNeutrinos are central to many important questions:
• Beyond the Standard ModelWhat chooses the neutrino masses and mixing angles?Are neutrinos Majorana or Dirac particles?Tests for exotic neutrino properties
• CosmologyCosmological parameter determinationDark matter propertiesDark energy? Lambda ~ (1 meV)4 ~ m4 ?
• High-energy astrophysicsConventional sources at highest energies, densities, and distancesUnconventional sources, e.g., dark matter decay or annihilationOrigins of the high-energy gamma and proton fluxes
And best of all…there’s data aplenty!
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
ConclusionsNot the beginning of the end in neutrino physics,but just the end of the beginning.
Neutrino astrophysics, lots of data just ahead,On three frontiers:1-10^4 TeV: AGN, GRB, etc in IceCube, others10^6 TeV: GZK, Z-burst, SDM, etc10^-6 TeV: supernova in GADZOOKS!
Neutrino telescopes approaching comparablesensitivity to photon observations.
Also key for testing dark matter models.
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Weak Interactions and Neutrinos Workshop, Lake Geneva, October 2003John Beacom, Theoretical Astrophysics Group, Fermilab
LutefiskCodfish soaked in lye (HNaO, see Material Safety Data Sheet)