Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang...
-
Upload
alvin-bradford -
Category
Documents
-
view
216 -
download
2
Transcript of Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang...
![Page 1: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/1.jpg)
Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation
Hyun Kyu LeeHanyang University
Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167 (2011)
![Page 2: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/2.jpg)
I. IntroductionCompact Stars - neutron stars, quark stars, ….., (black
hole) mass ~ solar mass size ~ 10km neutral object in weak equilibrium - higher density 1057 / (10km)3 ~ 1/ fm3 > n0
![Page 3: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/3.jpg)
A. Constituents of compact star Hadrons responsible for mass of star neutrons, protons, hyperons pions, kaons, ……. Quarks(deconfined phase) Leptons electrons, muons, neutrinos(e-, mu-) Exotics ?
![Page 4: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/4.jpg)
B. Stars and GravityGravity Pressure
TOV(Tolmann-Oppenheimer-Volkov) Equation
![Page 5: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/5.jpg)
Equation of state for hadronic mater: Fermi pressure of hadrons + Strong in-
teraction
Strong interaction appears in different forms
in nuclei, neutron star and quark star
Much more complicated than cosmological EoS
C. EoS of compact stars: pressure and energy
![Page 6: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/6.jpg)
• Heavier nuclei
• Nuclear matter
Symmetry energy: measure of n-p asymmetry in nuclear
matter
![Page 7: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/7.jpg)
• Up to nuclear density , n0 = 0.16 fm-3
• Compact star, n > n0 with central den-sity ncenter > 3 n0
• Simple extrapolation of what are known at low density nuclear matter(?)
Nucleon Interaction : S(n) and V(n)
![Page 8: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/8.jpg)
D. Mass of neutron stars
![Page 9: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/9.jpg)
![Page 10: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/10.jpg)
• A two-solar mass neutron star measured using Shapiro delay, Nature 467, 1081-1083(2010)
• Neutron stars are composed of the densest form of matter known to exist in our Universe, the composition and properties of which are still theoreti-cally uncertain. Measurements of the masses or radii of these objects can strongly constrain the neutron star matter equation of state and rule out theoretical models of their composition1, 2. The observed range of neutron star masses, however, has hitherto been too narrow to rule out many pre-dictions of ‘exotic’ non-nucleonic components3, 4, 5, 6. The Shapiro delay is a general-relativistic increase in light travel time through the curved space-time near a massive body7. For highly inclined (nearly edge-on) binary mil-lisecond radio pulsar systems, this effect allows us to infer the masses of both the neutron star and its binary companion to high precision8, 9. Here we present radio timing observations of the binary millisecond pulsar J1614-223010, 11 that show a strong Shapiro delay signature. We calculate the pulsar mass to be (1.97 ± 0.04)M⊙, which rules out almost all currently proposed2, 3, 4, 5 hyperon or boson condensate equations of state (M⊙, solar mass). Quark matter can support a star this massive only if the quarks are strongly interacting and are therefore not ‘free’ quarks12.
PSR J1614-2230(1.97 ± 0.04)M⊙
![Page 11: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/11.jpg)
• Higher nucleon number density inside n =0 n_0 6n_0 1. nucleon-nucleon interaction with density 2. Emerging of new hadrons with density kaons, hyperons(strange hadrons), quarks, ..
• Dense Hadronic Matter at the Core Change of EOS with density• Lattice QCD, Effective theory for hadrons, Many body inetractions, …
E. EoS at high density : open problem
![Page 12: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/12.jpg)
• QCD phase diagram
![Page 13: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/13.jpg)
• What is the role of symmetry energy(n-p asymmetry ) in compact star?
• Symmetry energy provides a channel for new degrees of freedom in n-p system via weak interaction:
electron, muon, strange particles(kaon, hyperon) ,..
II. Symmetry energy in compact star
Composition of compact star
![Page 14: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/14.jpg)
Npe(mu)-weak equilibrium: :
When neutrino escaped and equilibrium is frozen
with zero neutrino chemical potential : (1)• Hadron interaction: (2)• Charge neutrality condition: (3)
• Eq(1,2,3) solved for neutron, proton and electron(muon) densities
equation of state
![Page 15: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/15.jpg)
• Balance between symmetry energy and weak interaction
Proton abundance
![Page 16: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/16.jpg)
• Compact stars with Npe(mu)
(example)
![Page 17: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/17.jpg)
• Change of effective theory with density (1) n_0< n < n_t (2) n_t < n < n_c (3) n_c < n
• Degree of freedom(new): strange parti-cle
(1) nucleon (2) nucleon and kaon (3) quark (u,d,s)
• Continuous change (1) (2) (3)
III. Strategy(simple-minded)
![Page 18: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/18.jpg)
• When the difference between chemical po-tentials of proton and neutron becomes comparable to kaon mass in medium or nucleon-hyperon mass difference in medium, the corresponding strange parti-cles begin populating and the EOS get changed significantly.
• Kaon condensation Kaplan and Nelson,
Bethe and Brown, Brown, Rho and Kubodera, …
A. Nuclear matter with kaon condensationNPKe(mu) system
![Page 19: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/19.jpg)
• Equation of state
• Hadron interaction nucleon-nucleon interaction kaon-nucleon interaction
![Page 20: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/20.jpg)
• S-wave condensed kaon
![Page 21: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/21.jpg)
• Effective kaon mass(chemical potential)
• Kaon energy density
• Kaon pressure
• negative pressure for off-shell condensation: soft EOS smaller mass
![Page 22: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/22.jpg)
• For a hadron system, where kaon chemi-cal potential becomes smaller than electron mass, there is no leptons to balance the positive charge of protons but kaons.
• This is equivalent to strange quark mat-ter with high enough density.
• It defines the transition surface between hadronic phase with kaon condensation and strange quark matter
B. Strange quark matter driven by kaon condensation
![Page 23: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/23.jpg)
Quark MatterHadronic Matter
Kaon condensationat zero chemical potential
SQM
![Page 24: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/24.jpg)
• Quantum Chromodynamics(QCD)
![Page 25: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/25.jpg)
• Boundary condition at NM-SQM inter-phase
• With kaon condensation at critical density
Strange Quark Matter(SQM)
![Page 26: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/26.jpg)
• SQM (massless limit)
perturbative correction
bag constant: confinement
![Page 27: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/27.jpg)
IV. Triple-layered neutron star
SQM
KMNM
![Page 28: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/28.jpg)
• Numerical results
- Nucleon interaction
- Kaon -nucleon interaction
- SQM
![Page 29: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/29.jpg)
![Page 30: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/30.jpg)
Discussion• Higher density, n > n0 at the core of compact
star new physics• Emergence of strangeness at the core kaon condensation, hyperon, quarks Mass, radius and compositions,.... Cooling, GW, GRB, …..
• Triple-layered star with SQM driven by kaon condensation : , ,
PSR J1614-2230(1.97 ± 0.04)M⊙
![Page 31: Dense Stellar Matter Strange Quark Matter driven by Kaon Condensation Hyun Kyu Lee Hanyang University Kyungmin Kim HKL and Mannque Rho arXiv:1102.5167.](https://reader030.fdocuments.net/reader030/viewer/2022032606/56649ea05503460f94ba29da/html5/thumbnails/31.jpg)
• Vacuum property under extreme condition: high T and density
• Probed by experiments : High T frontier: RHIC and LHC High density frontier: LHC, FAIR,
RIB’s• Quest for origin of hadron mass
Remarks