Astroparticles I
O. L. G. Peres1
1Instituto de Fisica Gleb Wataghin UNICAMP
Fifth Class 16 January 2009 XV Jorge André Swieca Summer School-Particles and Fields
Orlando Luis Goulart Peres Astroparticles I Supernova Seminar’s plan
1 Supernova
Orlando Luis Goulart Peres Astroparticles I Supernova Supernova
Supernova: An energetic outburst resulting in the disruption of a star
Orlando Luis Goulart Peres Astroparticles I Supernova Supernovae produces γ and neutrinos
99 % of SN energy to neutrinos and < 1% go to photons and kinetic energy.
Orlando Luis Goulart Peres Astroparticles I Supernova Supernovae produces γ and neutrinos
99 % of SN energy to neutrinos and < 1% go to photons and kinetic energy.
Orlando Luis Goulart Peres Astroparticles I Supernova Some facts about supernova
Evolution time scale: ∼ 107 years; Collapse: < second Explosion brightness: ∼ 109 stars ( 1 average galaxy) Typical 2 2 3GN M 53 M 10km values: Eb ∼ ∼ 1.6 10 ergs . 5R M R Density range: 10−8 < ρ < 1014 g/cm3. High Energy Cosmic Ray Injection in Intergalactic Medium
Orlando Luis Goulart Peres Astroparticles I Supernova Some facts about supernova
Evolution time scale: ∼ 107 years; Collapse: < second Explosion brightness: ∼ 109 stars ( 1 average galaxy) Typical 2 2 3GN M 53 M 10km values: Eb ∼ ∼ 1.6 10 ergs . 5R M R Density range: 10−8 < ρ < 1014 g/cm3. High Energy Cosmic Ray Injection in Intergalactic Medium
Orlando Luis Goulart Peres Astroparticles I Supernova Some facts about supernova
Evolution time scale: ∼ 107 years; Collapse: < second Explosion brightness: ∼ 109 stars ( 1 average galaxy) Typical 2 2 3GN M 53 M 10km values: Eb ∼ ∼ 1.6 10 ergs . 5R M R Density range: 10−8 < ρ < 1014 g/cm3. High Energy Cosmic Ray Injection in Intergalactic Medium
Orlando Luis Goulart Peres Astroparticles I Supernova Some facts about supernova
Evolution time scale: ∼ 107 years; Collapse: < second Explosion brightness: ∼ 109 stars ( 1 average galaxy) Typical 2 2 3GN M 53 M 10km values: Eb ∼ ∼ 1.6 10 ergs . 5R M R Density range: 10−8 < ρ < 1014 g/cm3. High Energy Cosmic Ray Injection in Intergalactic Medium
Orlando Luis Goulart Peres Astroparticles I Supernova Known Supernova
Supernova Name Distance (kpc) SN 1006 3,3 SN 1054 Crab 2,0 SN 1181 3C58 8 SN 1572 Tycho 5 SN 1604 Kepler 7 SN 1680 Cas A 2,8
Orlando Luis Goulart Peres Astroparticles I Supernova How often does a galactic core collapse occur
Estimatives vary for the mean interval in yr Core collapse All SNae Visible SNae in history 30-60 Extragalactic SNae 35-60 30-50 γ ray remnants 16-25 Radio remnants < 18 − 42 Pulsars 4-120 Iron abundance > 19 >16 Stellar death rates 20-125 Overal can expect 3 ± 1 per century.
Orlando Luis Goulart Peres Astroparticles I Supernova SN1987A
In 1987A was seen the light from supernova explosion. At this time there was a experiment Kamiokande that measured the rate. The measured total energy and duration was in agreement with expectations. Totsuka, chairman of experiment win the NobeL Prize.
Orlando Luis Goulart Peres Astroparticles I Supernova Evolution of supernova
Orlando Luis Goulart Peres Astroparticles I Supernova Neutrino trapping
In the innermost region we have ρ ∼ 6 × 1011 g/cm3, that correspond for a typical neutrino cross section to a mean free path of 1 km.
Orlando Luis Goulart Peres Astroparticles I Supernovas have the highSupernova densities where neutrinos can cross. Density of supernova
Orlando Luis Goulart Peres Astroparticles I Supernova Spectrum for supernova
For stars with masses between 8 < M < 70M we have a
spectrum like
Orlando Luis Goulart Peres Astroparticles I Supernova Neutrino Spectrum
From simulation (Woosley and Janka, Nature), predicted a quasi-thermal spectrum −η dN (E) (ρ )ρw E w e−(E/Ew )(ρw ) ρw = w dE Γ(ρw ) Ew Ew
where Ew are the different temperatures.
Eνe ∼ 9 − 16 MeV Eν¯e ∼ 12 − 18 MeV
Eνµντ ∼ 15 − 22 MeV ρw ∼ 4 , ..., 5 and ηw = 1 + ρw . Large variation: different simulations did not agree and most of simulations cannot explode a supernova
Orlando Luis Goulart Peres Astroparticles I Supernova Rates for supernova formation
The rate of supernovas change along the time. We have few information about direct supernova rate.
Orlando Luis Goulart Peres Astroparticles I Supernova Relic supernova
The rate of supernovas that explode in the past is called diffuse neutrinos from relic supernova. Due the universe behaviour the spectrum of neutrinos in this ways it is redshifted.
Orlando Luis Goulart Peres Astroparticles I Supernova History of supernova
TIME AXIS
TODAY Physics involved z=0
1. Neutrino spectrum from each supernova
2. Neutrino oscillation during propagation ν inside SN envelope ν ν ν 3. Supernova rate formation z=1
ν
z=5
Orlando Luis Goulart Peres Astroparticles I Supernova Past supernova rate
We need to compute
dφ R dz P dNρw (E(1 + z)) ∼ RSN (z) Pxe(E, z) p 3 x 0 dE Ωm(1 + z) + ΩΛ dE
where E’=E(1+z), H0 = 70 Km/(s*Mpc), Ωm = 0.3, ΩΛ = 0.7 RSN (z) is the past supernova rate. Pxe(E, z)(z) is the survival probability for the neutrino at redshift z
Orlando Luis Goulart Peres Astroparticles I Supernova Spectrum for relic supernova
Due the Universe expansion the neutrino supernova spectrum
is displaced to lower energies.
Orlando Luis Goulart Peres Astroparticles I
Supernova N Fluxes from past supernovae ¦
10 7 6 Constant SN rate (Totani et al., 1995) 10 Population synthesis (Totani et al., 1996) 5 10 Cosmic gas infall (Malaney, 1997) Cosmic chemical evolution (Hartmann et al, 1997) 10 4 Heavy metal abundance (Kaplinghat et al., 2000) 3 10 LMA neutrino oscillation (Ando et al., 2002) 10 2 -2 -1 10 1 -1 10 -2 10 -3 10 -4 10 Neutrino Flux (cm second MeV ) -5 10 -6 10 -7 10 0 10 20 30 40 50 60 70 80 90 100
Neutrino Energy (MeV)
Sf)WcMA/.- ¦ £PN § @E- - Og -0N91.-0< CE\ o XM¥ ¡©N 3GHWN0MAH+351;-9<Zb/.6GF *,) 1;@A-96/.-d1;)WN 3GH Fa6j J )+*gE/.-0*,-07:1;-9<¤£ @E- CO\ho XM¥ gA/.-9 J /.-03GN91.6/1! 5 s #.$ #%$ #.$ H+)W7A-17 ¡A3G7E Orlando Luis Goulart Peres Astroparticles I Typical fluxes: 2 - 54 cm−2 s−1 Fluxes used by Super-Kamiokande experiment. Supernova SuperKamiokande as a supernova detector Orlando Luis Goulart Peres Astroparticles I Supernova SK limit for ν¯e + ν¯e: σ(¯νep → e n) no charge ID Orlando Luis Goulart Peres Astroparticles I