Supernova Neutrinos Georg G. Raffelt Max-Planck-Institut fr Physik, - - PowerPoint PPT Presentation

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Supernova Neutrinos Georg G. Raffelt Max-Planck-Institut fr Physik, - - PowerPoint PPT Presentation

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Crab Nebula Supernova Neutrinos Georg G. Raffelt Max-Planck-Institut fr Physik, Mnchen, Germany Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012 Sanduleak -69 202 Sanduleak 69 202 Tarantula

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Crab Nebula

Supernova Neutrinos

Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Sanduleak -69 202 Sanduleak −69 202

Large Magellanic Cloud Distance 50 kpc (160.000 light years) Tarantula Nebula

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Sanduleak -69 202 Sanduleak −69 202

Large Magellanic Cloud Distance 50 kpc (160.000 light years) Tarantula Nebula

Supernova 1987A

23 February 1987

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Crab Nebula

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

The Crab Pulsar

Chandra x-ray images

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Supernova Remnant in Cas A (SN 1667?)

Non-pulsar compact remnant

Chandra x-ray image

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Baade and Zwicky

Baade and Zwicky were the first to speculate about a connection between supernova explosions and neutron-star formation [Phys. Rev. 45 (1934) 138] Walter Baade (1893–1960) Fritz Zwicky (1898–1974)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Stellar Collapse and Supernova Explosion

Hydrogen Burning Main-sequence star Helium-burning star Helium Burning Hydrogen Burning

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Stellar Collapse and Supernova Explosion

Hydrogen Burning Main-sequence star Helium-burning star Helium Burning Hydrogen Burning Onion structure

Degenerate iron core: ρ ≈ ρ ≈ 109 g cm−3 T ≈ 1010 K MFe≈ 1.5 Msun RFe ≈ 3000 km

Collapse (implosion)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Stellar Collapse and Supernova Explosion

Collapse (implosion) Explosion Newborn Neutron Star

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Stellar Collapse and Supernova Explosion

Newborn Neutron Star

Neutrino cooling by diffusion

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Neutrino Signal of Supernova 1987A

Kamiokande-II (Japan) Water Cherenkov detector 2140 tons Clock uncertainty ±1 min Irvine-Michigan-Brookhaven (US) Water Cherenkov detector 6800 tons Clock uncertainty ±50 ms Within clock uncertainties, all signals are contemporaneous

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Interpreting SN 1987A Neutrinos

Jegerlehner, Neubig & Raffelt, PRD 54 (1996) 1194 Contours at CL 68.3%, 90% and 95.4%

Recent long-term simulations (Basel, Garching)

Theory

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Predicting Neutrinos from Core Collapse

  • Phys. Rev. 58:1117 (1940)
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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Explosion Mechanism

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Why No Prompt Explosion?

Dissociated Material (n, p, e, ν)

  • 0.1 Msun of iron has a

nuclear binding energy ≈ 1.7 × 1051 erg

  • Comparable to

explosion energy

  • Shock wave forms

within the iron core

  • Dissipates its energy

by dissociating the remaining layer of iron

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Neutrinos Rejuvenating Stalled Shock

Neutrino heating increases pressure behind shock front Picture adapted from Janka, astro-ph/0008432

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Delayed Explosion

Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys. (1982) Bethe & Wilson, ApJ 295 (1985) 14

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Exploding Models (8–10 Solar Masses)

Kitaura, Janka & Hillebrandt: “Explosions of O-Ne-Mg cores, the Crab supernova, and subluminous type II-P supernovae”, astro-ph/0512065

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

3D Simulation (Garching group)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Standing Accretion Shock Instability (SASI)

Mezzacappa et al., http://www.phy.ornl.gov/tsi/pages/simulations.html

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Gravitational Waves from Core-Collapse Supernovae

Müller, Rampp, Buras, Janka, & Shoemaker, astro-ph/0309833 “Towards gravitational wave signals from realistic core collapse supernova models”

Bounce GWs from asymmetric neutrino emission GWs from convective mass flows

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Three Phases of Neutrino Emission

Prompt νe burst Accretion Cooling

  • Shock breakout
  • De-leptonization of
  • uter core layers

Cooling on neutrino diffusion time scale

  • Spherically symmetric model (10.8 M⊙) with Boltzmann neutrino transport
  • Explosion manually triggered by enhanced CC interaction rate

Fischer et al. (Basel group), A&A 517:A80, 2010 [arxiv:0908.1871]

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Neutrinos from Next Nearby SN

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Operational Detectors for Supernova Neutrinos

Super-K (104) KamLAND (400) MiniBooNE (200)

In brackets events for a “fiducial SN” at distance 10 kpc

LVD (400) Borexino (100) IceCube (106) Baksan (100) HALO (tens) Daya Bay (100)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Super-Kamiokande Neutrino Detector

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Simulated Supernova Burst in Super-Kamiokande

Movie by C. Little, including work by S. Farrell & B. Reed, (Kate Scholberg’s group at Duke University) http://snews.bnl.gov/snmovie.html

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

IceCube as a Supernova Neutrino Detector

Pryor, Roos & Webster (ApJ 329:355, 1988), Halzen, Jacobsen & Zas (astro-ph/9512080) SN signal at 10 kpc 10.8 Msun simulation

  • f Basel group

[arXiv:0908.1871]

Accretion Cooling

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Variability seen in Neutrinos

Luminosity Detection rate in IceCube Lund, Marek, Lunardini, Janka & Raffelt, arXiv:1006.1889 Using 2-D model of Marek, Janka & Müller, arXiv:0808.4136 Probably smaller in realistic 3D models

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Quark-Matter Phase Transition Signature in IceCube

Dasgupta, Fischer, Horiuchi, Liebendörfer, Mirizzi, Sagert & Schaffner-Bielich arXiv:0912.2568

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Next Generation Large-Scale Detector Concepts

Memphys Hyper-K DUSEL LBNE Megaton-scale water Cherenkov 5-100 kton liquid Argon 100 kton scale scintillator LENA HanoHano

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

SuperNova Early Warning System (SNEWS)

http://snews.bnl.gov Early light curve of SN 1987A

Coincidence Server @ BNL Super-K

Alert

Borexino LVD IceCube

  • Neutrinos arrive several hours

before photons

  • Can alert astronomers several

hours in advance

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Supernova Rate

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Local Group of Galaxies

Current best neutrino detectors sensitive out to few 100 kpc With megatonne class (30 x SK) 60 events from Andromeda

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Core-Collapse SN Rate in the Milky Way

References: van den Bergh & McClure, ApJ 425 (1994) 205. Cappellaro & Turatto, astro-ph/0012455. Diehl et al., Nature 439 (2006) 45. Strom, Astron. Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekseev et al., JETP 77 (1993) 339 and my update.

Gamma rays from

26Al (Milky Way)

Historical galactic SNe (all types) SN statistics in external galaxies No galactic neutrino burst Core-collapse SNe per century 1 2 3 4 5 6 7 8 9 10

van den Bergh & McClure (1994) Cappellaro&Turatto (2000) Diehl et al. (2006) Tammann et al. (1994) Strom (1994) 90 % CL (30 years) Alekseev et al. (1993)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

High and Low Supernova Rates in Nearby Galaxies

M31 (Andromeda) D = 780 kpc NGC 6946 D = (5.5 ± 1) Mpc

Last Observed Supernova: 1885A Observed Supernovae: 1917A, 1939C, 1948B, 1968D, 1969P, 1980K, 2002hh, 2004et, 2008S

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

The Red Supergiant Betelgeuse (Alpha Orionis)

First resolved image of a star

  • ther than Sun

Distance (Hipparcos) 130 pc (425 lyr) If Betelgeuse goes Supernova:

  • 6×107 neutrino events in Super-Kamiokande
  • 2.4×103 neutrons /day from Si burning phase

(few days warning!), need neutron tagging [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012]

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Diffuse SN Neutrino Background

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Diffuse Supernova Neutrino Background (DSNB)

Beacom & Vagins, PRL 93:171101,2004

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Supernova vs. Star Formation Rate in the Universe

Horiuchi, Beacom, Kochanek, Prieto, Stanek & Thompson arXiv:1102.1977 Measured SN rate about half the prediction from star formation rate Many “dark SNe” ?

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Neutron Tagging in Super-K with Gadolinium

200 ton water tank Selective water & Gd filtration system Transparency measurement Mark Vagins Neutrino 2010

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Average spectral properties from DSNB

Adapted from Yüksel, Ando & Beacom, astro-ph/0509297 90% CL sensitivity to average SN spectrum from DSNB after 5 years

  • f Gd enhanced Super-K
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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Particle-Physics Constraints

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Do Neutrinos Gravitate?

Early light curve of SN 1987A

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Millisecond Bounce Time Reconstruction

Super-Kamiokande IceCube

Halzen & Raffelt, arXiv:0908.2317 Pagliaroli, Vissani, Coccia & Fulgione arXiv:0903.1191 Onset of neutrino emission

  • Emission model adapted to

measured SN 1987A data

  • “Pessimistic distance” 20 kpc
  • Determine bounce time to

a few tens of milliseconds

10 kpc

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Neutrino Limits by Intrinsic Signal Dispersion

Time of flight delay by neutrino mass “Milli charged” neutrinos

  • Barbiellini & Cocconi,

Nature 329 (1987) 21

  • Bahcall, Neutrino Astrophysics (1989)

Loredo & Lamb Ann N.Y. Acad. Sci. 571 (1989) 601 find 23 eV (95% CL limit) from detailed maximum-likelihood analysis Assuming charge conservation in neutron decay yields a more restrictive limit of about 3×10−21 e

  • G. Zatsepin, JETP Lett. 8:205, 1968

Path bent by galactic magnetic field, inducing a time delay SN 1987A signal duration implies SN 1987A signal duration implies

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Supernova 1987A Energy-Loss Argument

SN 1987A neutrino signal Late-time signal most sensitive observable Emission of very weakly interacting particles would “steal” energy from the neutrino burst and shorten it. (Early neutrino burst powered by accretion, not sensitive to volume energy loss.)

Neutrino diffusion Neutrino sphere

Volume emission

  • f new particles
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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Axion Bounds and Searches

Direct searches Too much CDM (misalignment) Tele

scope

Experiments

Globular clusters (a-γ-coupling) SN 1987A Too many events Too much energy loss Too much hot dark matter CAST ADMX (Seattle & Yale)

103 106 109 1012 [GeV] fa eV keV meV

µeV

ma neV 1015

Globular clusters (helium ignition) (a-e coupling) Too much cold dark matter (misalignment with Θi = 1) String/DW decay Anthropic Range

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Diffuse Supernova Axion Background (DSAB)

Raffelt, Redondo & Viaux work in progress (2011)

  • Neutrinos from all core-collapse SNe comparable to photons from all stars
  • Diffuse Supernova Neutrino Background (DSNB) similar energy density as

extra-galactic background light (EBL), approx 10% of CMB energy density

  • DSNB probably next astro neutrinos to be measured
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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Dirac Neutrino Constraints by SN 1987A

Right-handed currents Dirac mass Dipole moments Milli charge e p n N N p p

  • If neutrinos are Dirac particles, right-handed states

exist that are “sterile” (non-interacting)

  • Couplings are constrained by SN 1987A energy-loss
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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Degenerate Fermi Seas in a Supernova Core

Trapped lepton number is stored in e− and νe

n p e- νe νµ ντ

Particles Anti- particles

In true thermal equilibrium with flavor mixing, only one chemical potential for charged leptons and one for neutrinos. No chemical potential for Majorana neutrinos (lepton number violation)

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Degenerate Fermi Seas in a Supernova Core

n p e- νe νµ ντ

Equilibration by flavor lepton number violation, but flavor oscillations ineffective (matter effect) Non-standard interactions could be effective, most sensitive environment Equilibration by lepton number violation, but Majorana masses too small R-parity violating SUSY interactions? TeV-scale bi-leptons? Consequences in core collapse should be studied numerically

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Bi-Leptons and Core Collapse

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

Neutrino Flavor Oscillations

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations in Core-Collapse Supernovae

Neutrino sphere MSW region Neutrino flux Flavor eigenstates are propagation eigenstates Neutrino-neutrino refraction causes a flavor instability, flavor exchanged between different parts of spectrum

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Georg Raffelt, MPI Physics, Munich ITN Invisibles, Training Lectures, GGI Florence, June 2012

Flavor Oscillations

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