ay250: neutrino transients wherein “the most tiny quantities of reality ever imagined by a human...
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AY250: Neutrino Transients
Wherein
“The Most Tiny Quantities of Reality Ever Imagined by a Human Being”--
Fred Raines Meet “The Most Powerful Explosions in the Universe (Since the Big Bang)”
Neutrino
Disclaimer !
• I am not a weak physicist; I am a weak astrophysicist; sort of. I don’t study neutrinos.
• I am a OoM theorist (cover your wallet).• I am discussing a field with 19 particles detected.• Stop me to ask questions. I probably stopped you.
!
Discussion Overview• Neutrino Physics Review (Astrophysics Perspective)
– Why Neutrinos as Probes of the Universe?– Gamma-Ray/Cosmic-Ray/Neutrino Connection
• Transient Neutrino Sources– Stellar Core-Collapse (Neutron Star Formation)*– Gamma-Ray Bursts*, Giant Magnetar Flares*– Neutron Star X-Ray Binaries– Blazars*, Microquasars, Supernova Remnants
• Neutrino Observatories– Past: Kamiokande I/II*, IMB*, AMANDA*, SNO, LVD– Present: IceCube*, KamLAND, Baikal(NT-200), Super-K– Future: SNO+, ANTARES, NEMO, NESTOR, UNO?
Low or “Nuclear” or “Human Accelerator” Energies High or “Nature Accelerator” Energies
Neutrino Review for Astrophysicists
• Postulated by Pauli (1930), “Popularized” by Fermi (1933), Experimentally Confirmed by Cowan/Reines (1950s)– “ghost” particle invented to carry away energy in decay
• Only Confirmed Solely Weakly Interacting Particles– “Fundamental” Leptons (spin 1/2)
• Fermi-Dirac Statistics with ~ 0 mass threshold
– 3 Flavors (Electron, Muon, Tau)
• e, , (and corresponding antineutrinos)
• Flavor Oscillations (Vacuum or Matter)– Observed ≠ Source-Produced Flavor – Mostly Ignored in Astrophysics
• Probably Smoothes to 1:1:1 Ratio
€
n ⇒ p + e− + ν e
Why Neutrinos? Physics & Astrophysics!
Physics-Solar Model (Nuclear Physics/Convection/B Fields, ENUC ~ 1-10 MeV)
-Beyond Standard Model (e.g., Neutrino Oscillations, Sterile Neutrinos)
-Dark Matter (Primordial WIMP Annihilation, EWIMP ~ 10 GeV-10 TeV)
-Tests of Special/General Relativity (e.g., weak equivalence principle)
Both Low and High Neutrino Energies Interesting!
Why Neutrinos? Physics & Astrophysics!
Physics-Solar Model (Nuclear Physics/Convection/B Fields, ENUC ~ 1-10 MeV)
-Beyond Standard Model (e.g., Neutrino Oscillations, Sterile Neutrinos)
-Dark Matter (Primordial WIMP Annihilation, EWIMP ~ 10 GeV-10 TeV)
-Tests of Special/General Relativity (e.g., weak equivalence principle)
Astrophysics-Probe Photo-Inaccessible Environments (e.g., Core-Collapse SNe) -
*Complementary to Gravitational Wave Detectors
-In Principle Observable STRAIGHT to the End of the Universe *Cosmology/AGN/GRB *Gamma Rays Absorbed, Cosmic Rays Deflected and Absorbed
-Tracks Particle Acceleration (Cosmic Ray Connection, ECR > GeV)
*Where do the ultra-high energy cosmic rays come from?
Both Low and High Neutrino Energies Interesting!
Relevant Neutrino-Matter Interactions: In Earth Detectors, Core Collapse Supernovae &
Astrophysical Particle Accelerators • Electron Scattering
•Directional Information
€
(e,μ ,τ ) + e− →ν (e,μ ,τ ) + e−
ν (μ ,τ ) + e− → (μ,τ ) + ν e
€
σe /σ T ~ 10−20 Eν
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
Relevant Neutrino-Matter Interactions: In Earth Detectors, Core Collapse Supernovae &
Astrophysical Particle Accelerators
€
σn /σ T ~ 10−20 Eν
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟2
, MeV < Eν < GeV
• Electron Scattering•Directional Information
• Nucleon Absorption (Core Collapse)
€
(e,μ ,τ ) + e− →ν (e,μ ,τ ) + e−
ν (μ ,τ ) + e− → (μ,τ ) + ν e
€
e + n → p + e−
ν e + p → n + e+€
σe /σ T ~ 10−20 Eν
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
Relevant Neutrino-Matter Interactions: In Earth Detectors, Core Collapse Supernovae &
Astrophysical Particle Accelerators
€
σn /σ T ~ 10−20 Eν
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟2
, MeV < Eν < GeV
• Electron Scattering•Directional Information
• Nucleon Absorption (Core Collapse)
• Photohadronic Pion Cascade (Shocks)
•Threshold Energy: e.g.
€
(e,μ ,τ ) + e− →ν (e,μ ,τ ) + e−
ν (μ ,τ ) + e− → (μ,τ ) + ν e
€
e + n → p + e−
ν e + p → n + e+
€
E p Eγ ' > 12 mΔ
2 − mp2
( ) ~ (500 MeV)2
€
σe /σ T ~ 10−20 Eν
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
Cosmic Ray Acceleration => Neutrino Flux
The Neutrino Sky
Taken from Smoot Online
• Thermal BB Relic Neutrinos (E ~10-4 eV) – Hopelessly Undetectable (Z-Bursts?)
• SN Core Collapse Relic Neutrinos (E ~1 MeV)
– Bound Supernova / Star Formation Rate– Constrain Cosmology?
– Still ~ 1 OoM Below Detection Ability
The Neutrino Sky
Taken from Smoot Online
• Thermal BB Relic Neutrinos (E ~10-4 eV) – Hopelessly Undetectable (Z-Bursts?)
• SN Core Collapse Relic Neutrinos (E ~1 MeV)
– Bound Supernova / Star Formation Rate– Constrain Cosmology?
– Still ~ 1 OoM Below Detection Ability • Atmospheric Neutrinos • “Diffuse” CR Interaction Emission
– Cosmogenic Emission– Gas (Galactic, Star-Forming Galaxies)
• Big Bang Relics– Primordial Black Holes, Topological Defects– WIMP Annihilation
The Neutrino Sky
Taken from Smoot Online
• Thermal BB Relic Neutrinos (E ~10-4 eV) – Hopelessly Undetectable (Z-Bursts?)
• SN Core Collapse Relic Neutrinos (E ~1 MeV)
– Bound Supernova / Star Formation Rate– Constrain Cosmology?
– Still ~ 1 OoM Below Detection Ability • Atmospheric Neutrinos • “Diffuse” CR Interaction Emission
– Cosmogenic Emission– Gas (Galactic, Star-Forming Galaxies)
• Big Bang Relics– Primordial Black Holes, Topological Defects– WIMP Annihilation
• SN Core Collapse Point Sources (E ~ 10 MeV)
– Limited to Local Universe
• Potential Cosmic Ray Acceleration Sites• What We Haven’t Thought Of
Part I: Low Energy Core Collapse Neutrinos
Core-Collapse Supernovae Theory: A Brief Pre-History (Before Neutrinos, <1960)
• Neutron Stars Might Exist! - Landau, 1932, 1937: NS Core Powers the Sun?
- Gulag-Saving Measure?
- Got Oppenheimer et al. Interested
Cas A (Chandra)
Core-Collapse Supernovae Theory: A Brief Pre-History (Before Neutrinos, <1960)
• Neutron Stars Might Exist! - Landau, 1932, 1937: NS Core Powers the Sun?
- Gulag-Saving Measure?
- Got Oppenheimer et al. Interested
• SNe Beget Neutron Stars? - Baade & Zwicky, 1934: ESN ~ GMCH
2/RN ??
- All SN Types Clumped
- No Neutrino Connection
Cas A (Chandra)
Core-Collapse Supernovae Theory: A Brief Pre-History (Before Neutrinos, <1960)
• Neutron Stars Might Exist! - Landau, 1932, 1937: NS Core Powers the Sun?
- Gulag-Saving Measure?
- Got Oppenheimer et al. Interested
• SNe Beget Neutron Stars? - Baade & Zwicky, 1934: ESN ~ GMCH
2/RN ??
- All SN Types Clumped
- No Neutrino Connection
• B2FH Onion Skin Model- Widely Popularized Non Big-Bang Nucleosynthesis
- No Iron Core Emphasis, Connection to MCH
- 254Cf Powers Light?
Cas A (Chandra)
Core-Collapse Supernova Neutrinos: Modeling & The Standard Model (>1960)
• Chiu (1961): Neutrinos Control Collapse Dynamics– Weak Interaction Controls MacroDynamics!
• Colgate & White (1961): First Numerical Simulations - Neutrino Transport Ad Hoc (1053 erg SNe!)- >100 MeV Neutrinos (~Gravitational Binding Energy), ~10 ms Infall Timescale
PNS
Core-Collapse Supernova Neutrinos: Modeling & The Standard Model (>1960)
• Chiu (1961): Neutrinos Control Collapse Dynamics– Weak Interaction Controls MacroDynamics!
• Colgate & White (1961): First Numerical Simulations - Neutrino Transport Ad Hoc (1053 erg SNe!)- >100 MeV Neutrinos (~Gravitational Binding Energy), ~10 ms Infall Timescale
• Improved Physics! Glashow,Salam,& Weinberg (1968): Neutral Current Weak Interactions
• Neutrinos are Trapped! (1970s) - Optically Thick ProtoNeutron Star Forms- ~10 MeV, ~1-100 s Diffusion Timescale- Dynamics Independent of Supernova Mechanism
PNS
Neutrinos are Trapped in HERE!
Core-Collapse Supernova Neutrinos: Modeling & The Standard Model (>1960)
• Chiu (1961): Neutrinos Control Collapse Dynamics– Weak Interaction Controls MacroDynamics!
• Colgate & White (1961): First Numerical Simulations - Neutrino Transport Ad Hoc (1053 erg SNe!)- >100 MeV Neutrinos (~Gravitational Binding Energy), ~10 ms Infall Timescale
• Improved Physics! Glashow,Salam,& Weinberg (1968): Neutral Current Weak Interactions
• Neutrinos are Trapped! (1970s) - Optically Thick ProtoNeutron Star Forms- ~10 MeV, ~1-100 s Diffusion Timescale- Dynamics Independent of Supernova Mechanism
• SNe Don’t Explode! (1980s-NOW) - ProtoNeutron Star Neutrinos May Re-Energize Supernova Shock (Bethe & Wilson 1985)???
PNS
Neutrinos are Trapped in HERE!
The Theoretical Argument for ~10 seconds of Detectable ~10 MeV Neutrinos
€
Kelvin - Helmholtz ProtoNeutron Star Cooling
Egrav ~ GM 2 /R, tdiffuse ~ (R /c)τ nν
Lν ~ Egrav / tdiffuse ~ 4πR2σTS4
Radiative Transfer ⇒ Ts4τ ν ~ TC
4
TC ~ 60M1.4 M sun
1/ 2R30km−1 MeV
σ nν ~ 10−44 (Eν ,C /mec2)2cm2, Eν ,C ~ 3kT, M ~ (4π /3)R3ρ
τ ν ~ ρ /mn( )σ nν R ~ 104 −105 M1.4 M sun
2R30km−4
Eν ,S ~ 3kTS ~ 3kTC /τ ν1/ 4 ~ 15 MeV
Lν ~ 3×1052 R30km2 erg/s
tdiffuse ~ (R /c)τ ν ~ 10R30kms
F⊕ ~ Lν /4πD2, Ne,H20 ~ (Vρ H 20 /mp )
N⊕ ~ tdiffuse (F⊕ / Eν )σ νnNe,H20 /6 ~
~ Ebind /6(σ νn / Eν )Ne,H20 ~ 20(V /kton)M1.4 M sun
2R30km−1 D50kpc
−2
“The Supernova is only a sideshow to the main event: Neutron Star Birth” - A. Burrows
The Theoretical Argument for ~10 seconds of Detectable ~10 MeV Neutrinos
€
Kelvin - Helmholtz ProtoNeutron Star Cooling
Egrav ~ GM 2 /R, tdiffuse ~ (R /c)τ nν
Lν ~ Egrav / tdiffuse ~ 4πR2σTS4
Radiative Transfer ⇒ Ts4τ ν ~ TC
4
TC ~ 60M1.4 M sun
1/ 2R30km−1 MeV
σ nν ~ 10−44 (Eν ,C /mec2)2cm2, Eν ,C ~ 3kT, M ~ (4π /3)R3ρ
τ ν ~ ρ /mn( )σ nν R ~ 104 −105 M1.4 M sun
2R30km−4
Eν ,S ~ 3kTS ~ 3kTC /τ ν1/ 4 ~ 15 MeV
Lν ~ 3×1052 R30km2 erg/s
tdiffuse ~ (R /c)τ ν ~ 10R30kms
F⊕ ~ Lν /4πD2, Ne,H20 ~ (Vρ H 20 /mp )
N⊕ ~ tdiffuse (F⊕ / Eν )σ νnNe,H20 /6 ~
~ Ebind /6(σ νn / Eν )Ne,H20 ~ 20(V /kton)M1.4 M sun
2R30km−1 D50kpc
−2
“The Supernova is only a sideshow to the main event: Neutron Star Birth” - A. Burrows
Detectable with 1000 tons of water!
1980s Water Cerenkov “Proton Decay Experiments”
• Japanese Zinc Mine (Shielding from Cosmic Ray Muons)
• Volume: ~2 ktons• 1000 PMTs• Detector Efficiency:
– ~66% at 10 MeV, ~90% at 15 MeV
• Salt Mine in Ohio• Volume: ~6 ktons• 2048 PMTs• Detector Efficiency:
– ~10% at 20 MeV, ~60% at 40 MeV
Kamiokande (I & II)
Irvine. Michigan. Brookhaven (IMB)
Core Collapse Neutrino Predictions on Feb 22., 1987
•Stage 1: Prompt Deneutronization (~30 ms, ~1051 ergs of e’s)
•Stage 2: Shock Breakout (~10 ms, ~1051 ergs of e’s)
•Stage 3: Accretion Luminosity (<1 s, Depends on SN Mechanism)
•Stage 4: ProtoNeutron Star Cooling (~10 s, ~1053 ergs; all flavors) Log t (ms)
“On Detecting Stellar Collapse with
Neutrinos” (A. Burrows 1984)
Core Collapse Neutrino Predictions on Feb 22., 1987
•Stage 1: Prompt Deneutronization (~30 ms, ~1051 ergs of e’s)
•Stage 2: Shock Breakout (~10 ms, ~1051 ergs of e’s)
•Stage 3: Accretion Luminosity (<1 s, Depends on SN Mechanism)
•Stage 4: ProtoNeutron Star Cooling (~10 s, ~1053 ergs; all flavors) Log t (ms)
IMB Upgrades PMTs Late 1986
"The chances of a neutrino actually hitting something as it travels through all this howling emptiness are roughly comparable to that of
dropping a ball bearing at random from a cruising 747 and hitting, say, an egg
sandwich.” --Douglas Adams
SN1987A in LMC!
SN1987A in LMC!
~3 Hours Before Robert McNaught’s LMC Plates (20 Hours Before Ian Shelton’s Discovery)
Neutrinos from SN1987A•19 Neutrinos Total
•11 Kamiokande, 8 IMB, (5 Mt. Blanc?)
•Probably All Electron Antineutrinos
•No Directional Information
•One Scattering Event?
•Fermi-Dirac Black Body T~3-5 MeV
•Diffusion Process Confirmed (R~20 km)
•Definite Proof of Neutron Star Birth
•No Black Hole Signature (No Pulsar to Date Though!)
•Insufficient to Extract SN Mechanism
•Constraints on Electron Neutrino Mass (<14 eV, 95%)
•No KII/IMB Synchronization!!!, Still Limited by Intrinsic Emission Time
€
e + p → n + e+
The Future of Core Collapse Neutrino Detection• Present/Future Detectors
LARGER CERENKOV VOLUME = BETTER STATISTICS– Super-K (32 kton volume)
• ~4,000 Neutrinos for Galactic SN at 10 kpc
– Amanda (Only Because Short Timescale)• ~20,000 Neutrinos for Galactic SN at 10 kpc• Galactic SN Rate Upper Limit ~4/year
– Enough Scattering Events for Direction?MULTI-FLAVOR– e.g., KamLand (~70 NC Reactions), OMNIS?
The Future of Core Collapse Neutrino Detection• Present/Future Detectors
LARGER CERENKOV VOLUME = BETTER STATISTICS– Super-K (32 kton volume)
• ~4,000 Neutrinos for Galactic SN at 10 kpc
– Amanda (Only Because Short Timescale)• ~20,000 Neutrinos for Galactic SN at 10 kpc• Galactic SN Rate Upper Limit ~4/year
– Enough Scattering Events for Direction?MULTI-FLAVOR– e.g., KamLand (~70 NC Reactions), OMNIS?
• New Tools– SUNG (Supernova Neutrino Generation Tool) – SNEWS (Lets Get Organized)
• Things to Learn– SN Explosion Mechanism (Accretion Shock Luminosity) – Breakout Signature? Currently Unlikely– With Next SN Will We Learn More About SNe or Neutrino Physics?
SNEWS: Supernova Neutrino Early Warning System
International Collaboration of SN Neutrino-Sensitive InstrumentsSuper-K, LVD, SNO(+), AMANDA(IceCube)
GOALS: (1) Act as a Prompt Alert (and Localization) for Galactic SNe (2) Improve Sensitivity Through Multiple Telescopes
- Improve Small-Number Statistics- Eliminate Costly False Warnings
MEANS: (1) Computer Correlates “Warnings” from SNEWs Members
- “Warning” Designation on Group-to-Group Basis, > 1 False Warning/Week ==> Elimination from SNEWs
(2) Emails Astronomical Community (Sign Up Online!)- Optical/X-ray/Radio Pointings Hours Earlier than any SN to Date- < 1 False Warning / Century
Part II: High Energy, “Nature Accelerator” Neutrinos
Antartic Muon And Neutrino Detector Array• 677 PMTs in Cylinder (D = 200m)
1500 - 1900 m Depth Under Ice• Primarily Looks “Down” For Muons
Created by Muon Neutrinos (~20 Reconstruction)– Huge “Down-Going” CR Muons
Background– Electrons, Taus Produce Cascades– Water Vs. Ice:
Scattering/Absorption Length
• Energy Threshold ~50 GeV– But ~1 MeV For Huge Brief Flux (SNe)– Calibrated To Atmospheric Neutrinos– Low Background at E > TeV
• No Astrophysical Detections (Diffuse or Point Source)– Mostly Atmospheric Neutrinos Observed– BATSE GRB Coincidence Search -
None Observed/None Expected
• Integrated to IceCube in 2005
L. Kopke
AMANDA RESULTS
Hardtke et al.
Cosmic Beam Dumps & the Gamma-Ray/Cosmic-Ray Connection
,Neutron Stars, and any Shocks
CR + -Ray ==> Neutrino
-Ray ==> CR Acceleration
Neutrino ==> CR Acceleration!
, baryons
Halzen & Hooper
4:3, E=4E
Cosmic Beam Dumps & the Gamma-Ray/Cosmic-Ray Connection
,Neutron Stars, and any Shocks,
CR + -Ray ==> Neutrino
-Ray ==> CR Acceleration
Neutrino ==> CR Acceleration!
, baryons
Halzen & Hooper
TWO APPROACHES TO FINDING SOURCES OF HIGH ENERGY NEUTRINOS:
(1) Follow the Gamma-Ray Photons
(2) Look Where YOU THINK Particle Acceleration is Happening In the Universe and Test Your Hypothesis
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Good Bet; Bright TeV Sources. Bet on Radio Quasars
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Good Bet; Bright TeV Sources. Bet on Radio Quasars
Maybe; Only PWNe (TeV Sources) If Ion Component
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Good Bet; Bright TeV Sources. Bet on Radio Quasars
Maybe; Only PWNe (TeV Sources) If Ion Component
Probably; If CRs Really Accelerated as Advertised
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Good Bet; Bright TeV Sources. Bet on Radio Quasars
Maybe; Only PWNe (TeV Sources) If Ion Component
Probably; If CRs Really Accelerated as Advertised
Good Bet; TeV Flux Plausibly Hadronic
Chuck Dermer’s “Best-Bet Astrophysical Neutrino Sources”
• Solar Flares
• Blazars: PKS 0208-512, PKS 0528+134, NRAO 530, 3C279, PKS
1622-297
• Pulsars/PWNe: 1706-44, Crab, Vela, Geminga • SN Remnants: W44, IC 443, Gamma Cygni
• Microquasars: LS 5039, LSI +61 303
• GRBs (Successful and “Failed”)
• Giant Magnetar Flares• Unidentified EGRET Sources (In and Out of Galactic Plane)
The Universe is NOT Transparent to > TeV Energies, So Extrapolate Known SEDs (Compton GRO-TeV)
Gamma-Ray Fluences > 10-4 ergs cm-2
NO; Spectrum Too Soft
Good Bet; Bright TeV Sources. Bet on Radio Quasars
Maybe; Only PWNe (TeV Sources) If Ion Component
Probably; If CRs Really Accelerated as Advertised
Good Bet; TeV Flux Plausibly Hadronic
Good Bet; Depends Sensitively on Baryon Fraction/Lorentz Factor
Whipple Detection of Blazar TeV Photon Bursts
Kerrick et al. 1995
But Are These The Result of 0 Decay?
The Cosmic Ray Spectrum
UHECRs Only Directional for 1019 eV < E < EGZK, D < 100 Mpc
OMG Particles!
Are AGN the Source of UHECRs?
SMBH Jets ==> E > EGZK Cosmic Rays ==> AGN Source!€
EMAX ~ eΓGMBH
κ es
~ 1021 Γ
10
⎛
⎝ ⎜
⎞
⎠ ⎟
L
LED
⎛
⎝ ⎜
⎞
⎠ ⎟
1/ 2MBH
109 Msun
⎛
⎝ ⎜
⎞
⎠ ⎟
1/ 2
eV
•Nature’s Particle Accelerators Must Be Able To Confine Particles Inside Larmor Radius
GRBs or “Failed GRBs” Also Can Produce UHECRs
Neutrino-Cooled Accretion
Narayan & Quataert
•Black Hole Mass ~109 Smaller
• Mass/Energy Accretion Rate ~1010-15 Larger
•Lorentz Factor ~10 Larger
•EMAX ~102-5 Larger
GRBs’ More Powerful Explosions Make Up For Smaller Size
Neutrinos (or Lack Thereof) Would Tell Us About “Fireball” Content of GRBs or AGN Jets
The Case for Kilometer-Scale Neutrino Observatories• At km3 ~100 TeV Atmospheric Neutrinos Don’t Limit Detection• Threshold For Detecting Neutrino Sources with Luminosities ~ Largest in
Universe (AGN / GRBs)• Detectable Fluences Match High Energy Gamma-Ray ~10-100 Point Sources• Sensitive to Waxman-Bahcall “Diffuse” Limit in ~1 Year
IceCube
• AMANDA’s BIG BROTHER: 1 km3 of Ice • 4800 PMTs on 80 Strings• ~10 Angular Resolution to Muon Neutrinos • IceTop Air Shower Array to
Veto Downgoing Muons• Digitized/Time-Stamped at
Each PMT • Easily Reach Waxman/Bahcall
Diffuse Bounds & Begin to
Probe Point Sources• ~10 GRB Neutrinos Predicted
(Borderline!)
• Started Deploying 2005;• Construction Finished ~2011
L. Kopke
TeV-PeV Neutrinos from Giant Magnetar Flares?
-Ray Energetic Burst (~1044-1047 ergs)
• Durations: ~0.1-1 s (Longer Soft Tail)
• Rate: ~1/Decade • A Young Galactic
Magnetar’s Crustal Failure?
• “mini-GRB”
Courtesy K. Hurley/ S. Boggs (RHESSI)
SGR 1806-20 December 27,2004 Flare: “Brightest Cosmic Transient Ever”
(Ioka et al. 2005)
But how much like a GRB? - Bulk Acceleration and Shocks???
SGR Giant Flares
TeV-PeV Neutrinos from Giant Magnetar Flares? Critical Question: Baryon-Loaded or Not?
• Adiabatic Expansion, Acceleration, Non-Thermal Shocks
• Radio Emission Calorimetry ==> Baryons in Outflow
• Some Previous Flares May Be Nonthermal
• Short GRBs are Non-Thermal - Some may be SGRs
• MAYBE DETECTABLE
• Prompt Emission Just a Thermal Photospheric Breakout
• Also Consistent with Radio Calorimetry?
• Hurley et al. Claim Thermal Emission
• NOT DETECTABLE
If < 30, AMANDA saw 1 neutrino; IceCube should see 1 from even weak SGR Giant Flare => Test Baryon-Loaded Hypothesis!
Baryon Rich Baryon Poor
Optical Follow-Up of Neutrino Transients• Some Astrophysical Neutrino Sources May Be Burst-Like
– Long-Duration GRBs and “Failed GRB” SNe (dt ~ 1-100 s)– Probable Electromagnetic Counterparts
• IceCube & other km3 arrays => Marginal Detections Expected– Need to Extract Signal from Atmospheric Neutrino Background
(~100 day-1 total, but only 1000(10) year-1 above 10(100) TeV)
Kowalski & Mohr (2007)
Optical Follow-Up of Neutrino Transients• Some Astrophysical Neutrino Sources May Be Burst-Like
– Long-Duration GRBs and “Failed GRB” SNe (dt ~ 1-100 s)– Probable Electromagnetic Counterparts
• IceCube & other km3 arrays => Marginal Detections Expected– Need to Extract Signal from Atmospheric Neutrino Background
(~100 day-1 total, but only 1000(10) year-1 above 10(100) TeV)
• Look for Temporal (~100s), Angular Coincidences (~20)– 3 Neutrino Coincidence Rate: ~10-4 year-1(Own-Merit Detection- Identify Source)– 2 Neutrino Coincidence Rate: ~2 year-1 (Many False Positives)$$$
– 1 Neutrino: Only Meaningful If Identified with SNe < 20 Mpc
• Single High Energy GRB Neutrinos Rare***
Kowalski & Mohr (2007)
Optical Follow-Up of Neutrino Transients• Some Astrophysical Neutrino Sources May Be Burst-Like
– Long-Duration GRBs and “Failed GRB” SNe (dt ~ 1-100 s)– Probable Electromagnetic Counterparts
• IceCube & other km3 arrays => Marginal Detections Expected– Need to Extract Signal from Atmospheric Neutrino Background
(~100 day-1 total, but only 1000(10) year-1 above 10(100) TeV)
• Look for Temporal (~100s), Angular Coincidences (~20)– 3 Neutrino Coincidence Rate: ~10-4 year-1(Own-Merit Detection- Identify Source)– 2 Neutrino Coincidence Rate: ~2 year-1 (Many False Positives)$$$
– 1 Neutrino: Only Meaningful If Identified with SNe < 20 Mpc
• Single High Energy GRB Neutrinos Rare***• PROBLEM: Neutrino Detector Monitors ~ Full Hemisphere ---
Electromagnetic Telescopes Have Limited FOV– Few Expected Detectable Sources - Can’t be Picky!
Kowalski & Mohr (2007)
Optical Follow-Up of Neutrino Transients• Some Astrophysical Neutrino Sources May Be Burst-Like
– Long-Duration GRBs and “Failed GRB” SNe (dt ~ 1-100 s)– Probable Electromagnetic Counterparts
• IceCube & other km3 arrays => Marginal Detections Expected– Need to Extract Signal from Atmospheric Neutrino Background
(~100 day-1 total, but only 1000(10) year-1 above 10(100) TeV)
• Look for Temporal (~100s), Angular Coincidences (~20)– 3 Neutrino Coincidence Rate: ~10-4 year-1(Own-Merit Detection- Identify Source)– 2 Neutrino Coincidence Rate: ~2 year-1 (Many False Positives)$$$
– 1 Neutrino: Only Meaningful If Identified with SNe < 20 Mpc
• Single High Energy GRB Neutrinos Rare***• PROBLEM: Neutrino Detector Monitors ~ Full Hemisphere ---
Electromagnetic Telescopes Have Limited FOV– Few Expected Detectable Sources - Can’t be Picky!
• SOLUTION: ToO Optical Follow-Up to Neutrino Trigger– 2 m Class Telescope, 10 FOV, – SNe$$$ (~2-3 Times Sensitivity - Might Make a Big Difference)– GRBs*** (Even Bigger Payoff, Meaningful Provided You Look >100 TeV)
Kowalski & Mohr (2007)
Neutrinos, they are very small.
They have no charge and have no (sic) mass
And do not interact at all.
The earth is just a silly ball
To them, through which they simply pass,
Like dustmaids down a drafty hall
Or photons through a sheet of glass.
They snub the most exquisite gas,
Ignore the most substantial wall, . . .
—From John Updike’s “Cosmic Gall”
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