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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Lecture 3: Supernova NeutrinosLecture 3: Supernova NeutrinosJohnJohn BeacomBeacom, The Ohio State University, The Ohio State University
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Elevator PitchElevator PitchWe need complementary searches for new physics
Type II SN: iron white dwarf in core of star;neutrinos reveal (gravitational) explosion energy;hot + dense --> nu + nubar
Type Ia SN: carbon-oxygen white dwarf in binary;gammas reveal (thermonuclear) explosion energy;56Ni --> 56Co --> 56Fe with gammas
“nearby” supernovae are rare
diffuse neutrino background: not seen, is SNII (!?)
diffuse gamma background: is seen, not SNIa (?!)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Main Sequence
t ~ 10-100 Myr
Core-Collapse, Neutrino Emission
Massive Stars (> 8 Solar Mass)
Optical SNII (+Fe)
Black Hole
t ~ sec
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Intermediate Mass Stars (3-8 Solar Mass)
Main Sequence, Binary
t ~ Gyr
Accreting White Dwarf
t ~ Gyr
SNIa (+Fe)
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Two Types of SupernovaeTwo Types of Supernovae
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Core Collapse SupernovaeCore Collapse Supernovae
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
SupernovaeSupernovae
SN1999dk, z = 0.015Modeling (1d, 2d, 3d)
Mezzacappa et al, PRL 86, 1935 (2001)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
SupernovaSupernova EnergeticsEnergetics
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Supernova Neutrino EmissionSupernova Neutrino Emission
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Galactic SupernovaeGalactic Supernovae
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Supernova Neutrino DetectionSupernova Neutrino Detection
Supernova physics (models, black holes, progenitors…)
Particle physics (neutrino properties, new particles, …)
IMB
KamII
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Super-KamiokandeSuper-Kamiokandee- , e+ , �convert to Cerenkov light
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Detection YieldsDetection YieldsAssume a Galactic supernova at 10 kpc
Yields in 22.5 kton Super-Kamiokande:
~ 1 kton detectors: SNO, KamLAND, MiniBooNE~ 1 Gton (but very noisy) detector: IceCube
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Waiting Is BoringWaiting Is Boring
“Everybody complains about the supernovarate, but nobody does anything about it.”
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Nearby SupernovaeNearby Supernovae
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Nearby Star Formation RateNearby Star Formation Rate
Ando, Beacom, and Yüksel, astro-ph/0503321
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Supernova DiscoveriesSupernova Discoveries
(Hasan Yüksel)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
NearbyNearby SupernovaeSupernovae
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
More Than a SnowballMore Than a Snowball’’s Chances Chance
Ando, Beacom, and Yüksel, astro-ph/0503321
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Nearby SupernovaNearby Supernova DetectionDetection
Ando, Beacom, and Yüksel, astro-ph/0503321
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
DSNB, Take 1: First Good LimitDSNB, Take 1: First Good Limit
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Supernova Neutrino BackgroundSupernova Neutrino Background
Ando, Sato, and Totani, Astropart. Phys. 18, 307 (2003)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Relative SpectraRelative Spectra
(M. Malek)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
SK Data LimitSK Data Limit
Malek et al. (SK), PRL 90, 061101 (2003)
•4.1 years of SK data
•Background limited
•Some improvementis possible
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
DSNB Flux LimitDSNB Flux Limit•Predictions roughly agree on spectrum shape
•Main question is normalization of
1.0 Strigari, Kaplinghat, Steigman, Walker, JCAP 0403, 007 (2004)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
SK +SK + Gadolinium: DSNB DetectionGadolinium: DSNB Detection
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Inverse Beta DecayInverse Beta Decay
•Cross section is “large” and “spectral”
Corrections in Vogel and Beacom, PRD 60, 053003 (1999)
•We must detect the neutron, but how?
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Add Gadolinium to SK?Add Gadolinium to SK?
GadoliniumAntineutrinoDetectorZealouslyOutperformingOldKamiokande,Super!
Beacom and Vagins, PRL (2004)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Neutron CaptureNeutron Capture
Capture on H: sigma = 0.3 barnsEgamma = 2.2 MeV
Capture on Gd: sigma = 49100 barnsEgamma = 8 MeV(Equivalent Ee ~ 5 MeV)
At 0.2% GdCl3:
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Cost ofCost of GdGd
1984: $4,000/kg $400,000,000/SK
1993: $485/kg $48,500,000/SK
1999: $115/kg $11,500,000/SK
2002: $3/kg $300,000/SK
Based on 100 tons of GdCl3 in SK (0.2% by mass)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Important GdClImportant GdCl33 PropertiesProperties•Soluble in water (unlike mineral oil)
•Initial chemical and radiological purity excellent
•Initial water transparency tests excellent
•100 tons? No problem
•Used in MRI contrasting agents
You could drink 12 liters ofGADZOOKS! water every day
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Gadolinium SupplementsGadolinium Supplements
Try “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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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Spectrum With GADZOOKS!Spectrum With GADZOOKS!
Beacom and Vagins, PRL (2004) [hep-ph/0309300]
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Neutron Backgrounds in SKNeutron Backgrounds in SKDon’t want captures on Gdto dilute the solar signal
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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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Correlated BackgroundsCorrelated Backgrounds•Singles event rate above 5 MeV is ~ 1/ton/yearso accidental background rate is vanishing
•8He/9Li/11Li produced by spallationBeta decay followed by neutron emissionRare, controlled by timing and energy cuts
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Galactic Supernova DetectionGalactic Supernova Detection
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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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
IsIs There an Easier Route?There an Easier Route?
Photo thanks to Alex Kusenko
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
DSNB, Take 2: AstrophysicsDSNB, Take 2: Astrophysics
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Star Formation Rate Constraints (?)Star Formation Rate Constraints (?)
Fukugita and Kawasaki, MNRAS 340, L7 (2003)
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
New Constraint on SFRNew Constraint on SFR
Strigari, Beacom, Walker, Zhang, astro-ph/0502150
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Corresponding SupernovaCorresponding Supernova RatesRates
Strigari, Beacom, Walker, Zhang, astro-ph/0502150
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Supernova Gamma-ray BackgroundSupernova Gamma-ray Background
Strigari, Beacom, Walker, Zhang, astro-ph/0502150
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
ConclusionsConclusions
Understanding supernovae is essential for:
particle physics: SNII energy loss channelsneutrino properties
nuclear physics: production of the elementsneutron star equation of state
astrophysics: cycle of stellar birth, life, deathconstraints on new sources
cosmology: supernova distance indicatorsdark matter decay, annihilation
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ICTP Summer School on Particle Physics, Trieste, Italy, June 2005John Beacom, The Ohio State University
Further ReadingFurther Reading
• Georg Raffelt’s online talks:http://wwwth.mppmu.mpg.de/members/raffelt/
• “Identifying the Neutrino Mass Spectrum from the NeutrinoBurst from a Supernova,” Dighe & Smirnov, PRD 62, 033007 (2000)
• “Neutrinos as Astrophysical Probes,” Cavanna, Costantini,Palamara, Vissani, astro-ph/0311256
• Mark Vagins’ talk at Neutrino 2004 (video)http://neutrino2004.in2p3.fr/
• “APS Neutrino Study: Report of the Neutrino Astrophysics andCosmology Working Group,'’ Barwick et al., astro-ph/0412544