constraints on the nuclear equation of state. hyperon...
TRANSCRIPT
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Constraints on the Nuclear Equation of State. Hyperon Puzzle of Neutron Stars
Evgeni KolomeitsevMatej Bel University, Banska Bystrica
In collaboration with K.A. Maslov and D.N. Voskresensky (MEPhI, Moscow)
[PLB 748 (2015) 369; PRC 92 (2015) 052801(R), NPA 950 (2016) 64]
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• Constraints on the nuclear EoS:maximum neutron-star massbaryon mass vs. gravitational massmass-radius relationparticle flow in heavy-ion collisions
• Making RMF model flexible
• Hyperon puzzle
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>1400 neutron stars in isolated rotation-powered pulsars
~ 30 millisecond pulsars
>1400 neutron stars in isolated rotation-powered pulsars
~ 30 millisecond pulsars
>100 neutron stars in accretion-powered X-ray binaries ~ 50 x-ray pulsar
intense X-ray bursters
(thermonuclear flashes)
>100 neutron stars in accretion-powered X-ray binaries ~ 50 x-ray pulsar
intense X-ray bursters
(thermonuclear flashes)
short gamma-ray bursts neutron star --
neutron star, neutron star --
black-hole mergers
short gamma-ray bursts neutron star --
neutron star, neutron star --
black-hole mergers
soft gamma-ray repeaters –
magnetars
(super-strong magnetic fields)
soft gamma-ray repeaters –
magnetars
(super-strong magnetic fields)
Neutron Star Zoo
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Pulsar mass can be measured only in binary systems
Measuring pulsar mass
m1 m2
Newton gravity 5 Keplerian
orbital parameters: orbital period, semi-major axis length,excentricity, …
direction of observation
Do not determine individual masses of stars and the orbital inclination.
Einstein gravity 5 potentially measurable post-Keplerian
parameters:orbit precession, Shapiro delay, gravitational redshift, ….
Measurement of any 2 post-Keplerian
parameters allows to determine the massof each star.
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White dwarf --
neutron star binaries
For 28 pulsars of this type the masses are measured
Lattimer
ARNPS62 (2012)
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X-ray binaries
Measuring pulsar mass
Low mass14 masses are measured
Lattimer
ARNPS62 (2012)
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Double neutron star binaries
1974 PSR B1913+16 Hulse-Taylor pulsar
First precise test of Einstein gravitation theory
2003 J0737-3039 first double pulsar system
Pulsar A: P(A)=22.7 ms, M(A)=1.338 MsolPulsar B: P(B)=2.77 ms, M(A)=1.249±0.001
MsolOrbiting period 2.5 hours
[Nature 426, 531 (2003), Science 303, 1153 (2004)]
Measuring pulsar mass
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Double neutron star binaries
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Pulsar J1614-2230
P.Demorest et al., Nature 467, 1081-1083 (2010)
Measured Shapiro delay with high precision
Time signal is getting delayed when passing near massive object.
Highest well-known
masses of NS
there are heavier, but far less precisely measured candidates
Pulsar J03448+0432
Antonadis
et al., Science 340,448
radio-timing observations of pulsar+phase-resolved optical spectroscopy of WD
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first double pulsar system J0737-3039
(John Rowe animation)
Pulsar A: P(A)=22.7 ms, M(A)=1.338 MsolPulsar B: P(B)=2.77 ms, M(A)=1.249±0.001
MsolOrbiting period 2.5 hours
[Nature 426, 531 (2003), Science 303, 1153 (2004)]
Pulsar B:
progenitor ONeMg
white dwarf, driven hydrodyn. unstable by e−
captures on Mg & Ne; [Podsiadlowski
et al., MNRAS 361, 1243 (2005)]
observed NSs gravitational mass (remnant star): 1.248—1.250 Msol
critical baryon mass of progenitor white dwarf: 1.366—1.375 Msol
assume no mass-loss during collapse…
Gravitational mass -- baryon number constraint
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Mass-radius relation
BPA: Bayesian probability analysis [Lattimer,Steiner
…]
msp
PSRJ0437-4715: 3
confidence Bogdanov
ApJ
762, 96 (2013)
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• EoS•
Cooling scenario [neutrino production]
Given:
Cooling curve
Mass of NS
Neutron star cooling data
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neutron star is transparent for neutrino
CV -
specific heat, L -
luminosityemissivity
standard: modified Urca
exotic:
direct Urca
starts at some critical density, i.e. in stars with M>MDUcrit
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[Blaschke, Grigorian, Voskresensky A&A 424 (2004) 979]
DU process schould be „exotics“
(if DU starts it is dificult to stop it)
EoS should produce a large DU threshold in NS matter ![EEK, Voskresensky
NPA759 (2005) 373]
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[Danielewicz, Lacey, Lynch, Science 298, 1592 (2002)]
-
Boltzmann kinetic equation
-
Mean-field potential
fitted to directed & elliptic flow
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~10 km
crust
outer core
inner core
Nuclei and electronsNeutron-rich nuclei and electronsNuclei, electrons and neutrons
neutrons, protons, electrons, muons
Exotics:hyperons,meson-condensates,quark matter
Cross section of a neutron star
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Crust
Nucleus melting
Pasta structure
interplay of Coulomb energy and surface tension Negele
& Vautherin
(1973)
dens
ity g
row
th
saturation density
Mcrust
~0.1Msol
Rcrust
~102—103
m
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Equilibrium condition for a shell in a non-rotating neutron star
Newton’s Law
boundary conditions:
OUTPUT:
relativistic corrections
INPUT: equation of state (EoS)
neutron star density profile, radius R and mass M
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stable unstable
limitting
masslimitting
mass
nlim
=0.1n0
nlim
~10-5
n0
HHJ EoS
uncertainty in R~103 m
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Ab inito calculations of the EoS starting from NN potential
[Akmal, Pandharipande, Ravenhall PRC58(98)1804]
variational
chain-summation methods (Urbana)
matters is superluminalat higher densities
auxiliary field diffusion Monte Carlo technique
[Gandolfi
et al PRC 79, 054005 (2009)]non-relativistic EoS!
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Relativistic mean-field models
vacuum: one boson-exchange for NN-potential + Lippmann-Schwinger equations
nucleon-nucleon interaction
medium: mean-field approximation
pion
dynamics falls out completely in this approx.
a model
[Serot, Walecka]
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Energy-density functional
evaluated for σ
field followed from the equation
If we add gradient terms this energy density functional can be used for a description of properties of atomic nuclei.
nucleon spectrum in MF approximation
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(pure) Walecka model U()=0
Hardest EoS
among all RMF models
modified Walecka U()=a3+b4
maximal mass of NS
weak dependence on K !strong dependence on m*N
PSR J1614-2230
non-linear Walecka model (NLW)
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T. Gaitanos, M. Di Toro, S. Typel, V. Baran,C. Fuchs, V. Greco, H.H. Wolter
E.N.E. van Dalen, C. Fuchs, A. Faessler
S. Typel
E.E. Kolomeitsev, D.N.Voskresensky
Relativistic Mean Field Models
[Nucl. Phys. A 759, 373 (2005)]
Dirac- Bruekner-Hartree-Fock
NL, NL
KVR, KVOR
[Nucl. Phys. A 732, 24 (2004)]
[Phys. Rev. C 71, 064301 (2005) ]DD, D3C, DD-Fdensity dependent couplings
Nuclear EoS:Nuclear EoS:
scalar-field dependent couplings
DBHF
reduction of hadron
masses in dense medium is included
Examples for illustrations
[Klaehn
et al., PRC
74 (2006) 035802.]
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HIC
atomicnuclei
ab
initio
Urbana Argonne
smallsmalllargelarge
similarsimilar
within empirical rangewithin empirical range surface in atomic nucleisurface in atomic nuclei
similarsimilar
isospin
diffusion in HIC62 MeV
< L < 107 MeVB.A. Li, A.W. Steiner
nucl-th/0511064
isospin
diffusion in HIC62 MeV
< L < 107 MeVB.A. Li, A.W. Steiner
nucl-th/0511064
spin-orbit splittingRMF Models
spin-orbit splittingRMF Models
single nucleon spectrasingle nucleon spectra
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[Klaehn
et al., PRC
74 (2006) 035802.]
isospin symmetrical matter neutron matter
symmetryenergy
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Dots indicate star masses and corresponding central densities, at whichdirect Urca reaction starts.
Only nucleons!
[Klaehn
et al., PRC
74 (2006) 035802.]
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[Klaehn
et al., PRC
74 (2006) 035802.]
baryon massgr
avita
tiona
l mas
s
no mass lo
1% Msol
lost
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Making RMF EoS flexible
Non-linear Walecka model: Play with a scalar-field potential
Scaling of meson masses and coupling constants
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The standard non-linear Walecka (NLW) model
nucleons
scalar field
vector fields
maximum NS mass
Maximum mass strongly depends on m*N
(n0
) and weakly on K.
For better description of atomic nuclei one Includes no-linear terms
Input parameters
softening of EoS
and Mmax
reduction
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K.A. Maslov
et al., PRD92 (2015) 052801(R)
If we modify the scalar potential so that the m*N
(n) levels off then the EoS
stiffens
soft core:
hard core:
NLWcut
model
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maximum NS mass
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EEK and D.Voskresensky
NPA 759 (2005) 373
KVOR EoS successfully tested in Klaehn
at al., PRC74 (2006) 035802
Aim: Construct a better parameterization which satisfies new constraints on the nuclear EoSInclusion of hyperons. “Hyperon
puzzle”.Increase of hyperon-hyperon
repulsion due to phi-meson exchange (phi-mass reduction)
Lattice QCD (SC-QCD): common drop of meson masses [Ohnishi Miura Kawamoto Mod.Phys.Lett
A23, 2459]
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Generalized RMF Model
Nucleon and meson Lagrangians
effective masses:
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Energy-density functional
effective densities:
with coupling constant ratios
The standard sigma potential can be introduced as
mass scaling: scaling functions
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KVORcut
model Apply cut-scheme to
function
2
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C, C2, C2 and parameters of are fitted to reproduce
scaling functions for coupling constants vs
scalar field:
increase repulsionto stiffen EoS
suppress symmetry energyDU constraint
saturate f growth
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Scalar field in dense matter
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BM: Brockmann
–
MachleidtPRC42 (1990)
KS: Katayama-Saito PRC88 (2013)
Scalar and vector potentials in KVOR and MKVOR models vs. DBHF calculations
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Neutron matter EoS
--
(AIS) analog isobar states [Danielewicz, Lee NPA 922 (2014) 1]
--
D
electric dipole polarizability
208Pb[Zhang, Chen 1504.01077]
empirical constraints on symmetry energy
microscopic calculations
--
(APR) Akmal, Pandharipande, Ravenhall --
(AFDMC) Gandolfi
et al.MNRAS
404 (2010) L35--(EFT) Hebeler, Schwenk
EPJA 50 (2014) 11
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Constraints on EoS from HICs
Particle flow: Danielewicz, Lacey
and Lynch, Science 298 (2002) 1592
Kaon
production: Fuchs, Prog. Part. Nucl. Phys. 56 (2006) 1
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Gravitational vs baryon mass of PSR J0737-3039(B)PSR J0737-3039(B): double pulsar system 1.
Podsiadlowski
et al., MNRAS 361 (2005) 12432.
Kitaura
et al., A&A 450 (2006) 345possible mass loss in explosion
BPS crust is included
sensitive to proton concentration Ypthe smaller Yp
-
the better;smaller L are preferred.
Crust matching, see talk by C. Providencia
LKVOR
=71 MeVLMKVOR
=41 MeV
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Hyperon puzzle
nucleonic stars
hyperonic
stars
[Weissenborn et al., NPA 881 (2012) 62]
various RMF models
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Inclusion of hyperons
Vector coupling constants from SU(6) symmetry:
Scalar coupling constants from hyperon
binding energiesdata on hypernuclei
1) standard. extension: H
2) +phi mesons. extension: H
Phi meson mediated repulsion among hyperons is enhanced
3) + hyperon-sigma couplings reduced. extension: H
but
hyperon-nucleon mass gap grows with densityQMC model: Guichon, Thomas
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Strangeness concentration
KVOR: nDU
=3.96 MDU
=1.77 Msol
KVORH: n
=2.81n0
, M
=1.37Msol
, n
=3.13n0 M
=1.48 Msol
MKVORH: n
=2.63n0
, M
=1.43Msol
, n
=2.93n0, M
=1.65Msol
MKVORH: n
=3.61n0, M
=2.07Msol
no Lambdas!fulfill DU constraint
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Maximum NS mass and the strangeness concentration
fS –# strange quarks / # all quarks
0
3.4%
3.5%
0.92%
Weissenborn, Chatterjee
Schafner-Bielich
0
2.3%
0.62%
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Mass-radius constraints
BPA: Bayesian probability analysis [Lattimer,Steiner
…]
msp
PSRJ0437-4715: 3
confidence Bogdanov
ApJ
762, 96 (2013)
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RMF model with with scaled meson masses and coupling constants
Universal scaling of hadron masses. Not universal scaling of coupling constants
The model is flexible enough to satisfy many astrophysical constraints, constraints from HIC and microscopic calculations.
Hyperon puzzle can be partially resolved if the reduction of phi meson mass is taken into account
Compact stars do provide some constraints on the nuclear EoS