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Kate ScholbergMITNEPPSR 2003
Fundamental Physics with Cosmic Rays
OUTLINE
Cosmic rays in particle physics history
SUSY dark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relic big bang neutrinos
Questions of Fundamental PhysicsWhat are the elementary particles and their interactions?
Is nature supersymmetric?
What are the neutrino masses and mixings?
Why is there a matter-antimatter asymmetry?
What is the Universe made of, and how did it all come about?
What is the dark matter?
"Cosmic Ray" ≡ "a particle from space"� naturally occurring� various sources (Sun, supernovae, AGN, GRB)
� many species, charged and neutral
� wide energy range
(Are photons CR? Depends...)p, n, A, e±, γ, µ±, ν, ...
Cosmic Ray Primer
PRIMARY CR: directly from outer space (stable, charged component mostly protons)
More terminology:
SECONDARY CR: created in collisions with atmosphere
(c) 1999 K. Bernlohr
(includes muons,short-livedcomponent)
Charged cosmic ray fluxes for different species
Dominatedby protonsup to~ TeV
(compositionless wellknown at higherenergies)
Charged cosmic rays:affected by Earth's dipole magnetic field
Many interesting trapping and bouncing effects...
Low energy primary CR cannot enter geomagnetic field
Cutoff rigidity ~1-10 GeV per nucleon, depending on latitude
Rigidity≡ p/(Ze)
solar windeffects at <~ 1 GeV
Another comment: charged cosmic rays don't point back to where they came from!
Gyromagnetic radius:
R= 3.3 x 1012 p/(ZB) R in cm, E in GeV, B in µG
For Galactic field of 3 µG, R=1012 cm(<0.1 A.U.) for 1 GeV/c proton
R~ diameter of Galaxy at ~ 1019 eV/c
Charged CR follow tangled path, nearly isotropic
Neutral CR (γ,ν) point back to source
Charged Primary Cosmic Ray Energy Spectrum
Sun Supernovae Other sources ???
geo magnetic cutoff
higher energies preferentially escape Galaxy
OUTLINE
Cosmic rays in particle physics history
SUSYdark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relic big bang neutrinos
Cosmic rays have figured prominently in the history of particle physics...
Victor Hess, 1912: gold leaf electroscope to 5000 m altitude
First identification of "cosmic radiation"
Years of high drama ensue...
Anderson's discovery of the positron, 1932
Wilsoncloud chamberphoto
The antimatterpredictedby Dirac!
Neddermeyer and Anderson, 1937: discovery of the muon in cloud chamber
"Mesotron": mass intermediate between electron and proton
Late 1940's: Powell and others
Mountaintop observatories and photographic emulsion: discovery of the pion
π→ µ + ν µ → e + ν + ν
Discovery of strangeness: "V particles"
Rochester andButler, 1946
First kaon
The "particle zoo" followed...
Over the next ~40 years,accelerators dominated newdiscoveries in particle physics...
...but, now since the 1990's, cosmic rays have again come tothe forefront as a tool for fundamentalphysics, complementing accelerators!
Cosmic ray physicists mostly focused on understanding sources, composition, propagation, ...
Cosmic rays answer whereaccelerators can't reach...
SUSY dark matter: annihilation signals, direct detection
Ultrahigh energy cosmic rays:exotic matter,Z-bursts,cosmic ν's
Matter-antimatter asymmetry: antimatter searches
Relic big bang neutrinos
Neutrino mass & oscillations:Atmospheric, solar, and supernova ν's
Strange matter, QCD Gravitational waves
Primordial black holes Neutrino astrophysics
OUTLINE
Cosmic rays in particle physics history
SUSY dark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relicbig bang neutrinos
Cosmic Ray Spectrum
1 per sq km per century above 1020 eV
extragalacticcomponent
M G T Peta Exa Zetta
Greisen-Zatsepin-Kuzmin (GZK) cutoffCosmic rays with energies greater than 5 x 1019 eV will be absorbed by the Cosmic Microwave Background
p + γ → N + π
Mean free path 50 Mpc at 1020 eV
Galaxy: 20 kpcAndromeda: 0.7 Mpc
But some CR observed above the GZK cutoff...
What are they??
"Bottom up" mechanisms: particles accelerated to high energies
Any observed anisotropy should lead to sources
How? SN can only accelerate up to 1015 eV
Origin in AGN, GRB, magnetars?
Need very large fields,confinedspaces
→ not clear how it works...
"Top-down": source is something exotic, involving new fundamental physics?
e.g. Superheavy (1013-1013 GeV) particles decay to UHE Standard Model particles...
BB relic long-lived dark matter?
No cutoff because Galactic origin
Expect excess toward Galactic center
� Topological defects? � Other exotic primaries?
� Violation of Lorentz invariance?� Strong neutrino interactions?� "Z-bursts"?
uhecrons (light SUSY hadrons), glueballinos,...
Again, we need to look at anisotropy, correlations with objects, spectrum, composition to distinguish the models
Other ideas:
Detection Techniquesobserve gigantic air showers
Requires huge area!
Air Fluorescence: glow of excited N molecules
Air shower array: observe particles on ground
Fly's Eye, Hi-Res, TA
AGASA
1 per sq km per century above 1020 eV
Recent results
Exp'tsdon't agree?
Hi-Res: fluorescenceAGASA: air shower
Is GZKcutoffthere ornot?
The Pierre Auger Experiment
air fluorescence and air shower array
Argentina
3000 km2, expect 50-100 UHE events per year
EUSO for ISS
OWL/Airwatch stereo view satellites
air fluorescence from above to view huge area!
And the farther future: site a detector in space
Summary of UHECR
Nucleons are absorbed by the CMB above ~1020 eV within 50 Mpc...
Observed post-GZK events have a mysterious origin
"Bottom-up": exotic astrophysics"Top-down": exotic physics
Need to characterize anisotropy, spectrum
Gigantic area detectors required...AGASA, Hi-Res→ Auger → EUSO, OWL
OUTLINE
Cosmic rays in particle physics history
SUSY dark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relic big bang neutrinos
The DARK MATTER Mystery
Baryonic matter (ordinary stuff) only ~5%!
Non-baryonicdark matter
~25% !!
Many independent measurements� Galactic rotation curves� Gravitational lensing, microlensing� Cosmic microwave background� Large scale structure� Nucleosynthesis� High z redshift surveys
"DARK ENERGY"
One appealing hypothesis toexplain non-baryonic dark matter:
Weakly Interacting Massive Particles (WIMPs) that froze out after the Big Bang
NEUTRALINO χ lightest stable supersymmetric particle
50 GeV/c2< mχ < 3 TeV/c2
accelerator bound (LEP)
cosmological bound
e.g.
Neutralinos couldmake up the Galactic halo
χ
χ
χ
χ
χχ
χ
χχ
χ χ
χ
Local halo density ~ 0.3 GeV cm-3
(but could be clumpy)
Signature of neutralino dark matter:Look for ANNIHILATION PRODUCTS
χχ gauge bosonsquarksleptons
e+
pdγ...
Here, have background of SECONDARIES from CR collisions
⇒ look for ANOMALIESin the energy distribution
"bump in the spectrum"
Look for anomalous POSITRONS
χχ annihilationwould givebump around ~10-100 GeVbackground
from secondaries should be smooth
A hint from a balloon experiment, HEAT? hep-ph/9902162
Bump at ~10 GeV seen with different instruments
Positron fraction vs energy
N
Interpretation in terms of SUSY DMBaltz et al. astro-ph/0109318
Fits require "boost factor" to enhance signal (plausible for clumpy DM)
SUSY parameter space dots represent allowed models
Look for anomalous ANTIPROTONS
In this case, low energiesmay have less background
backgroundfrom secondaries
But:geomagnetic cutoff, solar wind effects
AAlso: antideuterons
Can also look for χχ annihilation via γ-ray products
χχ gauge bosonsquarksleptons
γ's inshowers
hadronize
Continuum emission at ~1/10 mχ
Or, spectral line from direct χχ -> γ's
The Alpha Magnetic Spectrometer for ISS
Sensitivity to charged cosmicrays up to 1 TeV, and γ's 10-100 GeV
Summary of Dark Matter SearchNon-baryonic dark matter (e.g. χ) indirect signature: χχ annihilation products
in >~ 10 GeV range
in ~< 1 GeV range
in 10-100 GeV range from Galactic center, halo
Positrons
Antiprotons
Gamma rays
from Earth center, sun, Galactic center (trapped WIMPs)
Neutrinos
OUTLINE
Cosmic rays in particle physics history
SUSY dark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relic big bang neutrinos
Core Collapse Supernovae: Copious producers of ν's
Expect ~3 ±1 /century in our Galaxy
The Supernova Neutrino Signal
< 1% in em radiation, k.e., 99% in ν's of all flavors
~1% νe from 'breakout', 99% νν from cooling
Energies: <Eνe > ~ 12 MeV
<Eνe > ~ 15 MeV
<Eνµ,τ
> ~ 18 MeV( )
Deeperν-sphere => hotter ν's
Timescale: prompt after core collapse ∆t~10's of seconds (possible sharp cutoff if BH forms)
�Eb~GMcore
2
Rnstar
~2 × 1053 ergs
Neutrino Luminosity: Generic Features
1 s
50 s
Burrows et al. 1992
very short (ms) νe spike at
shock breakout
cooling →
sum ofν
µ,τ and
anti-ν's
roughlyequalluminosityper flavor
luminositydecreaseover 10'sof seconds
SN1987A
Confirmed baseline model... but still many questions
Type II in LMC (~55 kpc)
Water Cherenkov: IMB Eth~ 29 MeV, 6 kton 8 events
Kam II Eth~ 8.5 MeV, 2.4 kton 11 events
Liquid Scintillator: Baksan Eth~ 10 MeV, 130 ton 3-5 events
Mont Blanc Eth~ 7 MeV, 90 ton 5 events??
What Can We Learn from a Galactic Supernova Neutrino Signal?
NEUTRINO PHYSICS� ν absolute mass from time of flight delay� ν oscillations from spectra (flavor conversion in supernova core, in Earth)
CORE COLLAPSE PHYSICS� explosion mechanism� proto nstar cooling, quark matter� black hole formation
from flavor, energy, time structure of burst
ASTRONOMY FROM EARLY ALERT~hours of warning before visible SN, + some pointing with ν's� progenitor and environment info� unknown early effects?
sin2 2θ
∆m2
10−11
10−10
10−9
10−8
10−7
10−6
10−5
10−4
10−3
10−2
10−1
1
10
10−4
10−3
10−2
10−1
1 �e � �x
��� �
�
��� �e
LSND signal still there: wait for BooNE
Atmospheric signal confirmed by K2K beam suppression + spectrum Solar ν oscillation
confirmed by SNO NC; only LMA now allowed; and now KamLAND confirms with reactor ν's!
Neutrinos: What Do We Now Know?2-flavor oscillation signals
"Standard" 3-flavor picture: Parameters: 2 ∆m2, 3 angles, δ
CP, (2 δ
M)
or
U=1 0 00 C23 S23
0 �S23 C23
C13 0 S13 ei �
0 1 0�S13 ei � 0 C13
C12 S12 0�S12 C12 0
0 0 1
MNSmixingmatrix
∆m12
2
∆m23
2
µτ
ee µ
τ
τ{
{ ∆m12
2
∆m23
2 τ
{
{µ
µ
"Normal" hierarchy "Inverted" hierarchy
Absolute mass scale?
µτ
ee
τ
(solar)
(atm.)
µ
Kinematic limits: mν< 2.2 eV
0νββ limits: <mν> < 0.35 eV
Cosmology (WMAP): mν < 0.23 eV
{
Remaining Questions (that supernova neutrinos might shed light on)
What is the mass hierarchy?
What is Ue3
? Is it non-zero?
or∆m
122
∆m23
2
µτ
ee µ
τ
τ{
{ ∆m12
2
∆m23
2 τ
{
{µ
µ
"Normal" hierarchy "Inverted" hierarchy
µτ
ee
τ
(solar)
(atm.)
µ
What is the absolute mass scale?
Neutrino Absolute Mass:
� energy-dependent time spread � flavor-dependent delay
∆t(E) = 0.515(mν/E)2D
t=0 from black hole collapse? grav wave signal?
Look for:
Expect time of flight delay
SN1987A: mν< 20 eV for ν
e
...no longer relevant?
Example: νe signal for black hole cutoff
Beacom et al. hep-ph/9806311
Current detectors: ~few eV level limits possible, at best
energy-dependent delay for ν
e
Neutrino Oscillations, Mass Hierarchy
⇒ compare NC, νe, ν
e rates and spectra
Perhaps more promising:
Energies: <Eνe > ~ 12 MeV
<Eνe > ~ 15 MeV
<Eνµ,τ
> ~ 18 MeV( )
Flavor-energy hierarchy is robust
Flavor transformations in stellar matter ⇒ spectral distortion e.g. expect hot ν
e or ν
e
Also: matter effects in Earth can modify signal
Some signatures
� νe in neutronization peak
completely transformed� hard ν
e during cooling
� Earth matter effects for νe
Some SN model-dependence...
Sensitivity to |Ue3
|2 as low as 10-4 to 10-5
� νe in neutronization peak
partly transformed� hard ν
e during cooling
� Earth matter effects for νe
}}
Normalhierarchy
Invertedhierarchy
(assuming LMA, |Ue3
|2 relatively
large, 3-flavor picture)
Supernova Neutrino DetectorsNeed ~ 1kton for ~100 interactions
Must have bg rate << rate in burst
Also want: � Timing� Energy resolution� Pointing� Flavor sensitivity (neutral current)
Detector Types
� Scintillator CnH
2n
�
Water Cherenkov H
2O
� Heavy Water D2O
� Long string water Cherenkov H2O
� 'High Z' Pb, Fe
Example: Super-Kamiokande Mozumi, Japan
50 kton of water(32 kton inner + outer detector)Now resumed operation after 2001 accident
νe + p e+ + n
νe + 16,18O 16,18F + e-
νx + 16O ν
x +
16O*
νx + e- → ν
x + e-
νe + 16O 16N + e+
7000
53005060
200
Pointing: ~4o at 8.5 kpc
Events expected for collapse at 8.5 kpc, > 5 MeV:
(5-10 from breakout)
Summary of Types of SN Neutrino Detectors
� Primary sensitivity is to νe, NC for heavy water, high Z
� Pointing for water Cherenkov, heavy water, argon� All real-time except radiochemical� All have energy resolution except long string, radiochemical
Distance for 90% CL detection, 1/month threshold
Far side of GalaxyLMC
Andromeda
Detector Mass (kton)
Dis
tan
ce s
ensi
tivi
ty (
kpc)
λ=0.01 Hz/kton
λ=0.001 Hz/kton
λ=0.0001 Hz/kton
0
200
400
600
800
1000
1200
0 100 200 300 400 500 600
Distancesensitivitydepends on:
� Mass� Background rate λ
Eth~ 5 MeV
∆T = 10 s
Summary of Future SN Neutrino Detectors
Galactic sens- itivity
ExtraGalactic
Summary of Supernova Neutrinos
A Galactic core collapse will yielda vast quantity ofinformation...
� Neutrino absolute mass: few eV sensitivity from time of flight delay (not better than lab?) � Oscillation info: mass hierarchy, θ
13
from spectral distortion, Earth matter effect
Many detectors with Galactic sensitivity online now... next generation extra-Galactic?
OUTLINE
Cosmic rays in particle physics history
SUSY dark matter
Ultrahigh energy cosmic rays
Supernova neutrinos
A few selections from the smorgasbord:
Introduction to cosmic rays
Relic big bang neutrinos
Relic neutrinos which froze out after the Big Bang, t ~ 1 sec
Expect T=1.95 K, sub-eV ! Nonrelativistic? Number density 113/cm3 per family
Very very very hard to detect...
A experimental Holy Grail...
One idea: Z-bursts
Ultra-high energy neutrinos interact with relic BB ν background at Z-pole ⇒ produce UHE CR
Eres
= MZ
2/2mν= 4.2 x 1021 eV (m
ν/1 eV)
SummaryCosmic rays have a venerable history, and are in vogue again!
The next progress in fundamental physics may come from a non-standard approach...
Sumptuous dining ahead!