Exploring N eutron S tar Equation of S tate via F ailed Supernova N eutrino
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Exploring Neutron Star Equation of State via Failed Supernova Neutrino collaborators: Grant J. Mathews (Notre Dame), Toshitaka Kajino (Univ. of Tokyo), Jyutaro Suzuki Jun Hidaka (NAOJ)
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Exploring N eutron S tar Equation of S tate via F ailed Supernova N eutrino. Jun Hidaka (NAOJ). collaborators: Grant J. Mathews (Notre Dame), Toshitaka Kajino (Univ. of Tokyo), Jyutaro Suzuki. (stiff). (soft). Supernova Relic Neutrinos. Failed SNe. - PowerPoint PPT Presentation
Transcript of Exploring N eutron S tar Equation of S tate via F ailed Supernova N eutrino
Exploring Neutron Star Equation of State
viaFailed Supernova Neutrino
collaborators: Grant J. Mathews (Notre Dame), Toshitaka Kajino (Univ. of Tokyo), Jyutaro Suzuki
Jun Hidaka (NAOJ)
Failed SNe
Supernova Relic Neutrinos
(soft) (stiff)
Evaluate Supernova Relic Neutrino Flux
High-z SNe
Middle-z SNe
Redshifted
Expanding Universe
Z=5For Flux
Parameterized by
Fermi-Dirac Distribution
SRN Energy Spectrum : # flux per unit energy
SupernovaRate at z
SNe-type?
SNe-type?
Lunardini (2009)Totani et al (1996)
Lunardini&Tomborra (2012)
Initial mass function
IMF (Initial Mass Function)
Salpeter(1955)
( # of SNe )
( total gas inside all stellar objects )
IMF
Our mass range of luminous CC-SNe
Observation : SNII + SNIb,c
(SFR)
Star FormationRate
(mass consumptionrate)
Supernova Rate
Supernova Rate
Star Formation Rate (obs.)
Smaller by factor 1.4 – 2 : Supernova Rate Problem How to reduce RSN ?
IMF ( e.g., Salpeter )
Theory
Observation
Horiuchi, S. et al. 2011, ApJ, 738, 154
Supernova Rate
Star Formation Rate (obs.)
Increase
IncreaseDecrease
How they look like ?
??
Classification of SNe Luminous CCSN (SNII + SNIb,c)
ONeMg
Failed SN : BH forming
Dim SNe
GRB
Shen EOS LS EOS
Our Choice of parameters
Sumiyoshi et al. (2008)
Hudepohl et al. (2010)
Harikae et al. (2009)
Luminous CCSN
Failed SN
ONeMg-SN
GRB
LS EOS
Shen EOS
Difference ← EOS
Atmospheric neutrino background
Noise from reactors
* Hyper-Kamiokande 10 years run
Shen EoS
LS EoS
Shen EoS
LS EoS
Shen EoS
LS EoS
Summary
Reduce RSN
νfSN
Shen EoS
LS EoS
Supernova
Rate Problem
Enhance IMF
: more fSNe
EoS dependence
in SRN spectrum !
