Astrophysical Neutrino Probes - Miami
Miami 2016Astrophysical Neutrino ProbesIna SarcevicUniversity of Arizona
Origin of High Energy Neutrinos:Cosmic Accelerators Particles (electrons, protons, etc) areaccelerated to high energies via Fermishock acceleration High energy protons collide withambient protons and photons Hadronic production of pions, kaonsand D-mesons which decay intoneutrinos
Cosmic AcceleratorsPhysics Today 2009
Observed High Energy Particlesfrom the Sky Cosmic Rays (energy up to 1021 eV) Gamma - rays (energy up to 1013 eV) Atmospheric Neutrinos (energy up to 109 eV ) Astrophysical Neutrinos (30GeV – 2 PeV)
Active Galaxy
High Energy Gamma Rays Active Galactic Nuclei (AGNs) areprodigious particle accelerators and themost powerful radiation sources known inthe Universe, with luminosities rangingfrom 1042 – 1048 erg/s. Over 50 AGNs observed by EGRET in MeVenergy range, and about 15 AGNs in TeVrange.
Cosmic Neutrinos Solar Neutrinos (MeV energies) SN 1987A (MeV energies) Atmospheric Neutrinos (GeV to TeVenergies) Astrophysical Neutrinos (AGN, GRB,cosmogenic, etc; GeV to EeV energies) Neutrinos from Dark Matter Decay orDark Matter Annihilation?
Neutrino fluxes
First Observation of HE Cosmic Neutrinos
Mechanism for particle production inastrophysical source Electrons and protons are accelerated tovery high energy in internal shocks viaFermi shock acceleration. Electrons cooldown rapidly via synchrotron radiation inthe presence of the magnetic field In an optically thin envirement, theserelativistic electrons emit synchrotronphotons which are observed as gamma-rayson Earth
Could Observed Astrophysical Neutrinosbe Due to Charm from Slow-jetSupernovae?
A. Bhattacharya, R. Enberg, M.H. Reno and I. Sarcevic,JCAP 06 (2015) 034"
Additional Neutrino Flux fromHeavy Dark Matter DecayA. Bhattacharya, M.H. Reno and I. Sarcevic,JHEP 1406 (2014) 110"Atri Bhattacharya, Arman Esmaili, Sergio Palmarez-Ruizand I. Sarcevic, December 2016"Galactic:Extragalactic:Decay modes: DM ! DM ! Z 0 Z 0DM ! µ µDM ! W W
A. Bhattacharya, M.H. Reno and I. Sarcevic, JHEP 1406 (2014) 110
Likelihood Analysis to determine the bestfit to HESE data The combined neutrino flux from an astrophysicalpower-law and DM decays can be represented interms of 4 parameters:DM massDM lifetimeAstrophysical spetral indexAstrophysical normalization
Best fit parametersA. Bhattacharya, A. Esmaili,S. Palomares-Ruiz and I. Sarcevic"
Best fit parametersA. Bhattacharya, A. Esmaili,S. Palomares-Ruiz and I. Sarcevic"
Prompt Neutrino Flux Constrained by LHC dataA. Bhattacharya, R. Enberg, Y.S. Jeon, M.H.Reno, I. Sarcevic and A. Stasto,JHEP 1611 (2016) 167 "
Dominant components of the atmosphericneutrino flux (schematic view)
Theoretical issues with charm production
Theoretical uncertainties
Reducing theoretical uncertainties Use total charm cross section measured up toLHC energies (ALICE, LHCb) Use differential charm distributons (transversemomentum and rapidity distributions measuredby LHCb at 7TeV and 13TeV Evaluate charm production in severalperturbative QCD approached: NLO pQCD, dipolemodel and k T factorization approach.
Total charm cross section
Transverse momentum distribution at theLHC compared to LHCb dataA. Bhattacharya, R. Enberg, Y.S. Jeon, M.H.Reno, I. Sarcevic and A. Stasto,JHEP 1611 (2016) 167 "
Prompt Neutrino FLuxA. Bhattacharya, R. Enberg, Y.S. Jeon, M.H.Reno, I. Sarcevic and A. Stasto,JHEP 1611 (2016) 167 "
Summary Astrophysical neutrinos are valuable probes of newphysics (solar and atmospheric neutrinos haveprovided us with the very first indication thatneutrinos have mass).Ultrahigh energy cosmic neutrinos (from AGNs,GRB, SJS, etc,) probe physics at energiesbeyond the LHC Dark matter which decays into neutrinos givesunique signatures in observed neutrino spectrum(explains excess in IceCube data?) Understanding of astrophysical neutrino fluxproduced in pp collisions at energies close orabove the LHC is very important – charmcontribution dominant at high energies.
Back-up Slides
Dipole Cross Sections
Factorization approach
A. Bhattacharya, A. Esmaili,S. Palomares-Ruiz and I. Sarcevic"
Reno, I. Sarcevic and A. Stasto, JHEP 1611 (2016) 167 "Dominant components of the atmospheric neutrino flux (schematic view) Theoretical issues with charm production . Theoretical uncertainties . Reducing theoretical uncertainties
Jeff Hyde Bowdoin College Resonant neutrino self-interactions in astrophysical spectra Work w/ Cyril Creque-Sarbinowski & Marc Kamionkowski CCS, JH, MK, Phys. Rev. D 103, 023527, arXiv:2005.05332
Ina Sarcevic University of Arizona Models of Neutrino Mass with a Low Scale Symmetry Breaking New Interactions of Supernova Relic Neutrinos Probing Neutrino Properties with Supernova Neutrinos Experimental Detection of the New Interactions via Light Scalar (HyperK, GADZOOKS, UNO, MEMPHYS) BBN and SN1987A Constraints on the Parameter Space of the
Study of Acoustic Ultra-high-energy Neutrino Detection (SAUND) J. Vandenbroucke et al. ApJ 2005 7 hydrophones at undersea Navy array in Bahamas Searched for neutrino signals in 195-day exposure First acoustic neutrino limit, not competitive with radio but new technique SAUND-II now underway, 49 hydrophones (103 km2)
Atmospheric Neutrino Oscillation In the simplest, two-flavor, oscillation case, the survival probability depends on m2 L/E ν The various atmospheric neutrino sub-samples span a range of five decades in neutrino energy Eν From 100 MeV to 10 TeV Depending on the neutrino's arrival direction, L spans a range of three decades From 15 km .
This catalog shows Olympus standard phased array probes, which are divided into three types: angle beam probes, integrated wedge probes, and immersion probes. Other types of probes can be designed to suit the needs of your application.File Size: 1MB
Seminario Internacional de Miami Miami International Seminary 14401 Old Cutler Road. Miami, FL 33158. 305-238-8121 ext. 315 INTRODUCCIÓN A LA BIBLIA REVISIÓN VERANO 2005 VARIOS AUTORES Un curso del Seminario Internacional de Miami / Miami International Seminary - Instituto Bíblico Reformado 14401 Old Cutler Road Miami, FL 33158. 305-238-
in stellar astrophysical fluid dynamics, and marks the 60th birthday of Douglas Gough, Professor of Theoretical Astrophysics at the University of Cambridge and leading contributor to stellar astrophysical fluid dynamics. Topics include proper-ties of pulsating stars, helioseismology, convection and mixing in stellar interiors,
The Asset Management Strategy supports our strategic priority to: To provide quality, well maintained homes that are fit for the future . Page 5 of 10 Asset Management Strategy 2018 The strategy supports our growth aspirations and development strategy. A key principle is that any development decision will complement and enhance our current asset portfolio. Our aim is that: We invest in our .
