Towards an extended meta-modeling of dense matter including phase transitions: the case of quarkyonic matter - Indico
←
→
Page content transcription
If your browser does not render page correctly, please read the page content below
NewMAC on-line seminar, Sept. 2020
Towards an extended meta-modeling of
dense matter including phase transitions: Jérôme Margueron
iP2i Lyon
the case of quarkyonic matter
In collaboration with A. Pfaff, P. Proust, R. Stiele, R. Somasundaram & G. Chanfray, H. Hansen.
Probing extreme matter physics with GW
Heavy Ion collision
ear
c l
nu
a nd
r $ cle tors
Pa lera
e
acc a l
ic
ys s
Dubna p h
NI C A@
stro a$on
A er v
obs [Hades, Nature phys. 2019]
Neutron stars,
BNS merger supernovae,
kilonovae… Probe limits of
extreme ma/er
Questions to What is the nuclear interaction in dense, isospin asymmetric matter, hot?
be answered: Which new particles appear at supra-saturation densities?
At which density occurs the deconfinement from hadrons to Quarks-Gluons Plasma (QGP)?
How neutrinos propagate and what are the transport properties of extreme matter?
Are BNS the main astrophysical site for the r-process?
EoS [nuclear] (M,R) [astro]
Tolmann-Oppenheimer-
Volkov (TOV) GR equations
P(n) (M,R)(nc)
[A. Watts et al., PoD (AASKA 14) 043]
Reverse engineering,
Bayesian statistics
Neutron star radii
(my own) classification:
Radius estimation: R1.4 ∈ [10 : 14] km for a 1.4 M⊙ NS
low radii (10-11 km),
average radii (12-13 km),
How to extract a radius?
large radii (>14 km).
+ Thermal emission from qLMXB (quiescient Low-Mass X-ray
binaries) [Raaijmakers 2019 - NICER]
[Guillot 2013, Ozel 2016, Bogdanov 2016, Steiner 2018]
+ X-ray bursts
[Poutanen 2013, Ozel 2016, Nattila 2017]
+ Gravitational waves from binary NS mergers
[LVC PRL 2017, Bauswein 2017, Tews PRC 2018, …]
+ NICER mission
[Miller 2019, Raaijmakers 2019, Bogdanov 2019, Guillot 2019]
+ Future: ATHENA mission
[Barcons 2017]A few anomalous results…
Thermal emission from qLMXB
qLMXB: quiescent Low Mass X-ray binaries
Chandra observation
Black body like emission: F # T4(Rinf/D)2 of U24 in NGC6397
[Rutledge et al. 1999]
7 sources in globular clusters:
- constant flux, purely H atmosphere,
- Low magnetic fields —> almost pure thermal components,
- In globular clusters —> accurate distances.
Simultaneous analysis assuming a single EoS for all qLMXB.
[Guillot Rutledge Brown 2011]
Exemple: constant radius model [Guillot 2013]
[Baillot d’Étivaux+, ApJ 2019]
With latest X-ray spectra
model and new data :
—> very low radii (8-11 km)
RNS ≈ 11.0(5) kmMulti-messenger GW analysis
Direct comparison of the GW waveforms to the raw/whitened data, with EoS modeling
+ Mtotal ≤ Mthresh( ≈ 2.3M⊙).
ntr = nsat ntr = 2nsat
Capano, Tews et al. 2019
—> Low NS radii also seems to be preferred.GW analysis from the Λ PDF
0,004
Impact of 2 analyses from raw data: TD-LVC-2018
TD-De-2018
GW170817
LVC, PRX 9 (2019) 0,003
Mtot=2.73M
Mchirp=1.186M
De et al., PRL 121 (2019)
PDF
0,002
Impact of 2 prior sets:
#1: small ranges defined from global nuclear physics analysis (JM 2018) 0,001
#2: large ranges (included non-zero probabilities) 0,000
0 100 200 300 400 500 600 700 800
Λ
Marginalization over R1.4 H. Güven et al., PRC 102 (2020)
(a) TD-LVC-2018+χEFT+GMR (b) TD-LVC-2018+χEFT+GMR
1,2 1,2
TD-De-2018+χEFT+GMR TD-De-2018+χEFT+GMR
TD-LVC-2018 TD-LVC-2018
TD-De-2018 TD-De-2018
χEFT χEFT
0,9 GMR 0,9 GMR
Prior set #1 Prior set #2
PDF
PDF
0,6 0,6
0,3 0,3
0,0 0,0
11 12 13 14 11 12 13 14
R1.4 (km) 1.4M⊙ NS radius R1.4 (km)Quarkyonic matter
Quarkyonic matter
Idea:
• As a result of the non-perturbative regime of
QCD at low energy, baryons emerge as « Cooper
pairs » of quarks around the Fermi energy.
• The associated gap Δ defines the baryon region,
on top of the deeply bound free quark states.
Baryon density:
nucleons quarks
The gap result from the unknown solution of
Connection between nucleon and quark
QCD in dense matter. In the present model, it
s.p. energies: ϵ (k − Δ) = N μ
B FB c Q is given by the following prescription:
where Λ is the QCD scale (~300 MeV).Quarkyonic matter
Equation of state:
only cross- quark
nucleons over dominance
+ shallow gap
of nucleons
M-R relation at equilibrium:Extension to asymmetric matter
Work in preparation with P. Proust and H. Hansen.
From 2 Fermi seas (SM and NM) to 4:
p n
u
d
Isoscalar
2 Fermi seas: 4 Fermi seas: dynamical
symmetry
1 variable: nB 2 variables: nB and δB
Nucleons are constructed
1 constraint: 2 constraints: from quarks (p: uud; n:
ϵB(kFB − Δ) = Nc μQ ϵB(kFB − Δ) = Nc μQ and δQ = δN /Nc udd) and quarks are
released from the
destruction of nucleons
(dynamical symmetry).
Construct the 2 densities. Construct the 4 densities.Quarkyonic (asymmetric) matter
800
3000 QCD=300 MeV
600
EB/A (MeV)
µn (MeV)
2000 400
200
1000 sym. matter
asym. matter 0
neut. matter
0
1000 1
0.8
PB (MeV.fm-3)
(vs,B/c)2 0.6
500
0.4
0.2
0
0
0 500 1000 1500 2000 0 0.5 1 1.5 2
2 -3 nB (fm-3)
Bc (MeV.fm )Quarkyonic beta-eq. Matter
800
3000
600
EB/A (MeV)
µn (MeV)
2000 400
nucl. matter 200
1000 Q. matt. 300
Q. matt. 320 0
Q. matt. 340
0
1000 1
0.8
PB (MeV.fm-3)
(vs,B/c)2 0.6
500
0.4
0.2
0
0
0 500 1000 1500 2000 0 0.5 1 1.5 2
2 -3 nB (fm-3)
Bc (MeV.fm )Quarkyonic stars
3 3
nucl. matter
Q. matt. 300
Q. matt. 320
2 2
M (Msun)
M (Msun)
Q. matt. 340
1 1
0 0
10 12 14 16 18 200 400 600 800 1000
R (km) GW
1000 3
800
2
M (Msun)
600
GW
400
1
200
0 0
10 12 14 16 18 0.3 0.6 0.9 1.2
R (km) nc (fm-1)In summary
Possible tensions between nuclear physics expectation and some observations.
—> it may signal that nucleonic matter changes its nature soon after saturation density.
We have explored the newly suggested quarkyonic model for dense matter.
We have suggested an extension to asymmetric matter assuming an isoscalar dynamical symmetry
among baryons and quarks:
• Asymmetric matter has same features as SM: cross-over, peak in the sound speed, etc…
• Quarkyonic stars have an interesting path in the MR plot. They have higher maximal mass
than NS (built on top of the same meta-model).
In the future: extension to finite T, neutrino scattering, inclusion of strangeness, etc… (with also
A. Pfaff, R. Stiele, R. Somasundaram)Conclusion and outlook
Multi-messenger observation: The BNS GW + kilonovae EM signal + GRB (+ neutrinos?).
Variety of GW sources: BNS, BH-NS, CCSN, continuous emission, etc…
(Futur) post-merger GW signal: investigation of phase transitions.
Future upgrades and new telescopes (a lot of new data):
GW interferometers: upgrades of LIGO-Virgo (KAGRA, LIGO India).
E-M follow-up: GRANDMA, ZTF à (future) LSST.
3rd generation (~2030-2040): Cosmic explorer, Einstein telescope.
Space interferometer (LISA ~2035): low frequencies (trigger future mergers).
ET
LSSTYou can also read
