Neutrino Astronomy - California Institute of Technologygolwala/ph135c...Advantages of Neutrino...
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Transcript of Neutrino Astronomy - California Institute of Technologygolwala/ph135c...Advantages of Neutrino...
![Page 1: Neutrino Astronomy - California Institute of Technologygolwala/ph135c...Advantages of Neutrino Astronomy Can see through nearly anything Wide viewing angle Disadvantages of Neutrino](https://reader033.fdocuments.us/reader033/viewer/2022051508/5aab476a7f8b9a8f498bb3c7/html5/thumbnails/1.jpg)
Neutrino Astronomy
Ph 135Scott Wilbur
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Why do Astronomywith Neutrinos?
Stars, active galactic nuclei, etc. are opaque tophotons
High energy photons are absorbed by the CMBbeyond ~100 Mpc
1020 eV protons, which should be created withneutrinos, have been seen
Can be used to observe possible dark matterreactions
In short: we can probe new phenomena andlook farther back
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Why do Astronomywith Neutrinos?
Three main areas of research: Astronomy
More information about high-energy protons and γ rays
Particle Physics Extremely long baseline for neutrino oscillation studies
Dark Matter Searches Many dark matter candidates would leave neutrino
signatures
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The Detector
A neutrino interacts with matter in thetelescope, creating a muon or a hadronic orelectromagnetic shower
The muon (or shower) emits Cherenkovradiation as it travels through the ice
Photomultipliers pick up the Cherenkovradiation and can infer the direction of travel
To select only neutrino events, only trackscoming through the Earth are kept
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The Detector
Picture from AMANDA II Web Site: http://www.amanda.uci.edu
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Advantages ofNeutrino Astronomy
Can see through nearly anything Wide viewing angle
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Disadvantages ofNeutrino Astronomy
Need gigantic telescopes Still see very few events
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AMANDA
Many arrays (A, B10,and II) at the SouthPole
Operational sinceJanuary 1997
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ANTARES
Astronomy with a Neutrino Telescope andAbyss environmental RESearch
Currently under construction, 5/12 stringscompleted
1000 photomultipliers, 0.1 km2 planned Data will combine with AMANDA to provide
better sky coverage
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IceCube
Next generation ofneutrino telescopes
4200 photomultipliers, 1km2 telescope area
1O angular resolution formuons, 10O for showers
30% resolution in log ofenergy for muons, 20% inenergy for showers
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Astronomy
Extremely high energy protons (over 1020 eV)have been observed
Expected to come from supernova remnantsand neutron stars accreting matter fromcompanions
These processes are expected to generateneutrinos as well, which would point back totheir source
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Astronomy
Active Galactic Nuclei are the most luminousknown objects in the Universe (1035 – 1041 W)
Some emit relativistic jets with γ rays exceeding1012 eV
Theoretical models of AGNs have largeuncertainties
Any observations of these sources (such asneutrino emissions) are helpful
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Astronomy
γ ray bursts are extremely violent releases ofenergy (1045 J in ~1 sec in γ rays alone)
We don't have a good theory about themechanism of γ ray bursts
By observing the afterglow, we can determinewhat happens, but not how it starts
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Neutrino Physics
A neutrino telescope can see atmosphericneutrinos produced on the other side of theEarth
This gives a very long baseline for neutrinooscillation observations
Much more accurate neutrino oscillationmeasurements, possibly including a sterileneutrino
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Dark Matter Searches
WIMPs can get trapped in gravity wells andannihilate at great rates
γ rays would be absorbed, but neutrinos couldbe detected
Neutrinos have energies 1/3 - 1/2 of WIMPmass
Kaluza-Klein dark matter annihilates intoneutrinos at a higher rate than WIMPs
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Dark Matter Searches
Both dark matter candidates would lead to anincreased neutrino rate from the Sun:
rqR
1= 0.1
rqR
1= 0.2
rqR
1= 0.3
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Possible Exotic Results
Neutrino telescopes are essentially detectorsfor extremely high energy accelerators (10PeV)
We might see new physics at energy scales thishigh
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Quantum Gravity
Earth becomesopaque above ~100TeV
Angular distributioncan give crosssection
Don't need knownluminosity of source
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Magnetic Monopoles
Magnetic monopoles wouldhave a large equivalentcharge
Cherenkov radiation goesas charge squared
AMANDA has improved thebound on monopole fluxdensity
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References
Francis Halzen, Astroparticle Physics with HighEnergy Neutrinos: from AMANDA to IceCube
Dan Hooper, High Energy Neutrino Astronomy:Opportunities for Particle Physics
Gianfranco Bertone, Dan Hooper and JosephSilk, Particle Dark Matter: Evidence,Candidates and Constraints
ANTARES web site: http://antares.in2p3.fr