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Astrophysical Constraints on Secret Neutrino Interactions

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Presentation on theme: "Astrophysical Constraints on Secret Neutrino Interactions"— Presentation transcript:

1 Astrophysical Constraints on Secret Neutrino Interactions
Shun Zhou (周顺) KTH Royal Institute of Technology, Stockholm Shanghai Particle Physics and Cosmology Symposium June 3-5, Shanghai

2 Outline Motivation and General Arguments
SN Bound on a neutrinophilic 2HDM BBN Bound on a Dark Matter Model

3 Neutrino Sources in Nature
Astrophysical Accelerators Already? Earth Atmosphere (Cosmic Rays) Sun Supernovae SN 1987A Earth Crust (Natural Radioactivity) Cosmic Big Bang (Today 330 n/cm3) Indirect Evidence Nuclear Reactors Particle Accelerators

4 Where to Test Neutrino-Matter Interactions
Discovery of neutrino oscillations New physics beyond the std. model Exotic interactions with matter Based on the SM of elementary particle physics and cosmology Compare with the precise measurements and cosmological observations Assume non-standard neutrino interactions To Derive Experimental Constraints:

5 Where to Test Neutrino-Neutrino Interactions
Secret Neutrino Interactions High neutrino number densities Neutrinos play an important role Agreement with standard theories Neutrinos in Supernovae SN 1987A Neutrino signal from SN 1987A Average energy and sig. duration Consistent with delayed-explosion Primordial abundance of light elements Cosmic microwave background Consistent with the std. cosmology Neutrinos in the Early Universe

6 Supernova 1987A 23 February 1987 Sanduleak

7 Supernova Explosions Onion structure Main-sequence star
©Raffelt ©Raffelt Onion structure Main-sequence star Hydrogen Burning Collapse (implosion) Helium-burning star Helium Burning Hydrogen Degenerate iron core: r  109 g cm-3 T  K MFe  1.5 Msun RFe  8000 km

8 Supernova Explosions Explosion Newborn Neutron Star
©Raffelt ©Raffelt Explosion Newborn Neutron Star ~ 50 km Proto-Neutron Star r  rnuc = 3  g cm-3 T  30 MeV Collapse (implosion) Neutrino Cooling

9 Neutrino Signals from SN 1987A Information from observations
Neutrino Observation of SN 1987A Neutrino Signals from SN 1987A Kamiokande (Japan) and IMB (US): Water Cerenkov Detector Intended for Proton Decays Baksan (Soviet Union): Scintillator Telescope Clock Uncertainty: + 2/-54 s Information from observations Standard Picture of Core-collapse SNe Neutrino Diffusion Time from the NS Neutrino Luminosity Lν = erg s-1

10 Spectral anti-νe Temperature [MeV]
Neutrino Observation of SN 1987A Contours at CL 68.3%, 90% and 95.4% Assumptions: 1. Thermal Spectra 2. Energy Equilibration Recent long-term simulations (Basel, Garching) Eb [1053 ergs] Jegerlehner, Neubig & Raffelt, PRD 54 (1996) 1194 Spectral anti-νe Temperature [MeV]

11 Gravitational Binding Energy
Supernova Explosions Gravitational Binding Energy outshine the host galaxy

12 Supernova Bound on secret neutrino interactions

13 Energy-loss Argument If new weakly interacting particles can be produced in the supernova core, they will steal energies from neutrino bursts, which reduces the duration of neutrino signals. Volume Emission of New Particles Neutrino Cooling Axions, Majorons, Sterile Neutrinos, … Proto-Neutron Star r  rnuc = 3  g cm-3 T  30 MeV

14 Supernova Bound on a neutrinophilic 2HDM
Wang et al., EPL 76 (2006) 388; Gabriel & Nandi, PLB 655 (2007) 141; Sher & Triola, PRD 83 (2011) Excluding a ν2HDM Tiny Dirac neutrino masses from small vev and large Yukawa coupling But …… a light scalar boson, interacting only with neutrinos----Safe? Constraints from the neutrino observation of SN 1987A

15 Supernova Bound on a neutrinophilic 2HDM
S.Z., PRD 84 (2011) Kolb-Turner Criterion D λ-1 <1 Neutrino-sphere yi <1.5 x 10-3 D = 51.4 kpc

16 Supernova Bound on a neutrinophilic 2HDM
S.Z., PRD 84 (2011) Energy-loss Argument produced in the SN core, but decay back to neutrinos yi ~ 10-4 τ = (3y2m/16π2) -1 ~ s m = 1 keV But …… T = 30 MeV, E = 3 T , leading to a Lorentz factor of 105 yi <3.5 x 10-5

17 A CDM scenario without small-scale problems
arXiv:

18 Constraints from BBN Neutrinos interact with an MeV-mass vector boson
In thermal equilibrium: Inverse decays Pair production Constraints from K and W decays Enhanced total width Two vs. three-body decays BBN bound: ΔNeff ≤ 95% C.L. Laha, Dasgupta & Beacom Mangano & Serpico ΔNeff =1 K decay W decay ΔNeff =1.3 Ahlgren, Ohlsson & S.Z. in preparation

19 Summary Neutrino signals from SNe can be used to place stringent limits on exotic neutrino interactions, as well as other weakly interacting particles. We show a neutrinophilic 2HDM has been excluded, based on the simple energy-loss argument. Using the BBN bound on extra neutrino species, we have derived very restrictive constraints on a CDM model.

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