Kenta Kiuchi Collaboration with Y Sekiguchi K Kyutoku M Shibata Ref 11055035 Introduction Our research target high energy astrophysical phenomena e g Supernova energy ID: 350509
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Slide1
Gravitational waves and neutrino emission from the merger of binary neutron stars
Kenta KiuchiCollaboration with Y. Sekiguchi, K. Kyutoku, M. Shibata
Ref.)
1105.5035Slide2
Introduction
Our research target = high energy astrophysical phenomenae.g., Supernova energy ≈ 1.5*10
46J
= energy the Sun consumes for 1.2 trillion years !!
SN1054
（
Crab Nebula
）
r
～
1000km
～
10km
～
Solar mass
Energy source =
gravitational potential energy
∝ r
-1Slide3
Products of high energy astrophysical phenomena
～10km
～3km
（1 Solar mass）
✓
Density
～
10
15g/cm
3 (1.41 g/cm3)
⇒ General Relativity, Strong
interaction✓Temperature～
1011K
(15.7×106K)⇒
Weak interaction✓Magnetic fields～1015
Gauss (Sunspot：several thousand Gauss)⇒Electromagnetic force
All of fundamental interaction play an essential role.Slide4
Physical aspects of high energy astrophysical phenomena
✓Highly dynamical✓No special symmetry, e.g., spherical symmetry⇒Numerical modeling including four kinds of forcesNumerical RelativityFiguring out high energy astrophysical phenomena
by numerically solving the Einstein equations Slide5
Importance of Numerical Relativity
○ Gravitational waves✓imprinting “raw” information of sources✓extremely weak signal, hc∼10
-22 = the change of (Size of H atoms)/(Distance to Sun)
GW detectors
Need to prepare
theoretical templates of
GWsSlide6
Today’s topic =
Coalescence of binary neutron stars✓Promising source of GWs✓Theoretical candidate of Short-Gamma-Ray Burst✓High-end laboratory for Nuclear theoryA nuclear theory ⇒ Mass-Radius relation for Neutron Star
Image of GRB
Black hole + disk?
Mass-RadiusSlide7
Overview of binary neutron star merger
NS
G.Ws.
imprint
only information of mass
G.Ws.
imprint
information of radius
Rapidly rotating massive NS
BH and torus
M
total
<
M
crit
M
total
>
M
crit
✓
M
crit
depends
on the Equation of State
, i.e.
M
crit
= 1.2-1.7
M
max
✓
Final massive NS or torus around BH are extremely hot,
T
∼
O(10)
MeV
⇒
Neutrino cooling plays an importance roleSlide8
Set up of binary neutron star
○ Shen or Shen-Hyperon
EOS based on RMF theory (Shen+,98, Sumiyoshi+,11) ⇒
Mcrit = 2.8-2.9 Solar mass for Shen, 2.3-2.4 Solar mass for Shen-Hyperon EOS○
Neutrino cooling
based on GR leakage scheme
(Sekiguchi,10)
○ Equal mass model with
1.35
Solar mass, i.e., M
tot=2.7
Solar mass
O
bserved BNSs (Lattimer &
Paraksh 06)
Mass-Radius
Observation constraint by PSR J1614-2230 Slide9
Result
Density color contour on equatorial (x-y) plane = orbital plane
In units of Kilometer
In units of millisecond
Log
10
(
ρ
[g/cc])Slide10
Gravitational Waveforms
Shen
Shen-Hyperon
NSs orbit around each other
BH formation
Massive NS oscillatesSlide11
Gravitational Wave
SpectrumfrequencyAmplitude
Sensitivity curves for GW detectors
Shen
Shen
-
Hyperon
GWs could be detected if the merger happens within 30
Mpc
.Slide12
○
○ Neutrino cooling timescale ∼ 2-3 second
○ Huge luminosity ∼ 10
53 erg/s○ Could be detected if it happened within 10 Mpc for HK
Neutrino Luminosity
Shen
Shen
+
Hyperon
Anti electron neutrino
E
lectron neutrino
μ,
τ
neutrino
BH formationSlide13
Summary
○ Binary neutron star merger Numerical Relativity simulations with microphysical process for the first time ○ GWs could be detected if it happened within 30 Mpc○ Neutrino could be detected if it happened within 10
Mpc⇒
Multi messenger astronomy is coming soon !!Thanks to SR16000 in YITP
Thank you for your attention