Holographic Mesons in D4/D6 Model Revisited

Jo, Kwanghyun; Kim, Youngman; Sin, Sang-Jin

doi:10.3938/jkps.59.2984

Cited by 5 publications

(4 citation statements)

References 24 publications

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“…It is defined as Σ KN ≈ 1 2 (m + m s ) N |ūs +ss|N and in medium, the nucleon matrix element of the bilinear quark fields will undergo medium modification. Therefore what it can be in (19) is known neither theoretically nor experimentally. Even in matter-free space, the sigma term has evolved from ∼ 400 MeV to ∼ 200 MeV, the latest result coming from lattice QCD measurements.…”

Section: Three-layer Compact Starsmentioning

confidence: 99%

Cold Dense Baryonic Matter and Compact Stars

Lee

Rho

Sin

2011

Int. J. Mod. Phys. A

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Probing dense hadronic matter is thus far an uncharted field of physics. Here we give a brief summary of the highlights of what has been so far accomplished and what will be done in the years ahead by the World Class University III Project at Hanyang University in the endeavor to unravel and elucidate the multifacet of the cold dense baryonic matter existing in the interior of the densest visible stable object in the Universe, i.e., neutron stars, strangeness stars and/or quark stars, from a modest and simplified starting point of an effective field theory modeled on the premise of QCD as well as from a gravity dual approach of hQCD. The core of the matter of our research is the possible origin of the ∼ 99% of the proton mass that is to be accounted for and how the "vacuum" can be tweaked so that the source of the mass generation can be uncovered by measurements made in terrestrial as well as space laboratories. Some of the issues treated in the program concern what can be done -both theoretically and experimentally -in anticipation of what's to come for basic physics research in Korea. 15:15 WSPC/INSTRUCTION FILE MPLA-LRSCold Dense Baryonic Matter and Compact Stars 3 such hot (but not so dense) matter revealing what takes place at high temperature. However the situation with high density at low temperature is totally different. It is nearly completely unknown what happens to cold hadronic system when it is squeezed to a very high density, other than that one is observing compact stars with an interior density estimated to be as high as or even higher than, say, ∼ 10 times, that of nuclear matter. This is because cold dense hadronic matter is a strongly correlated system inaccessible to theoretical tools relying on standard perturbation theory, and furthermore the only reliable non-perturbative approach to QCD, i.e., lattice QCD, cannot handle, because of the famous sign problem, the density regime involved. In this paper, we describe the approach initiated by the WCU3-Hanyang team, what (little) has been so far accomplished and what remains to be done in the future. The earlier part of this development was summarized in 1 .

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Section: Three-layer Compact Starsmentioning

confidence: 99%

Cold Dense Baryonic Matter and Compact Stars

Lee

Rho

Sin

2011

Int. J. Mod. Phys. A

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“…The holographic approaches have been applied to the investigation of the hadron physics such as hadron spectra [344][345][346][347][348][349], hadron-hadron interactions [350], atomic nuclei [351,352] and quark-gluon plasma [353,354]. It has also been attempted to investigate the heavy flavor physics [349,355,356]. In the top-down approaches, however, the presence of the heavy quark symmetry in the holographic model is not clear [357], because the pseudoscalar and vector mesons belong always to the same multiplet in the gauge theory possessing the SUSY.…”

Section: Summary and Future Prospectsmentioning

confidence: 99%

Heavy hadrons in nuclear matter

Hosaka

Hyodo

Sudoh

et al. 2017

Progress in Particle and Nuclear Physics

119

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Current studies on heavy hadrons in nuclear medium are reviewed with a summary of the basic theoretical concepts of QCD, namely chiral symmetry, heavy quark spin symmetry, and the effective Lagrangian approach. The nuclear matter is an interesting place to study the properties of heavy hadrons from many different points of view. We emphasize the importance of the following topics: (i) charm/bottom hadron-nucleon interaction, (ii) structure of charm/bottom nuclei, and (iii) QCD vacuum properties and hadron modifications in nuclear medium. We pick up three different groups of heavy hadrons, quarkonia (J/ψ, Υ), heavy-light mesons (D/D,B/B) and heavy baryons (Λ c , Λ b ). The modifications of those hadrons in nuclear matter provide us with important information to investigate the essential properties of heavy hadrons. We also give the discussions about the heavy hadrons, not only in infinite nuclear matter, but also in finite-size atomic nuclei with finite baryon numbers, to serve future experiments. but it is "renormalized" to the low energy degrees of freedom such as the collective modes (e.g. surface vibration, rotation, nucleon pairings) [9].2 We notice that, for the light u and d flavors, the first excited state of the nucleon, N (1535) with spin-parity J P = 1/2 − , is well explained as an orbital excitation of valence quarks (P-wave excitation), but with an s quark the corresponding state, Λ(1405) with J P = 1/2 − , shows up with very different structure governed by theKN -πΣ dynamics.4 See for example Ref. [28]. 5 This is an example of the quantum fluctuations, which are important in the state with finite baryon number density.Such fluctuation effect is suppressed at finite temperature. 6 The Kondo effect is a known phenomena caused by the Fermi instability when the heavy impurity particle with non-Abelian interaction exists (see Sect. 4).(j ) J with total spin J and brown muck spin j decays to the final heavy hadron Ψ (j) J with total spin J and brown muck spin j by emitting a light hadron, e.g. a pion π with relative angular momentum L. Due to the independent conservations of the heavy quark spin S and the brown muck spin j, we see that the strength of the decay widths is parametrized as(2.2.45) by neglecting the corrections with the heavy hadron mass M [57]. Here J ( ) = j ( ) ± 1/2. In realistic application to experimental data, we need to include the phase space factor due to the different mass thresholds. Including this factor, we can reproduce the branching ratios of the known decay patterns of 8 We notice the conservation of J is valid only when the vacuum is rotationally invariant. If the rotational symmetry is broken, we cannot apply the following discussion. For example, such situation can happen when the external field (e.g. a magnetic field [56]) breaks the rotational symmetry.11 Note that the notations are different from those in Sect. 2.3.1 as fπ = √ 2F , ξ = u, V µ = −a µ , A µ = −a µ ⊥ and Uq = h. 12 We note that the covariant derivative forqQ meson is defined by D µ Hv = ∂ µ Hv + iHvV µ [26]...

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“…One may determine the values of λ and M KK by using the quark mass and meson mass as inputs into two basic relations: m q = λM KK y ∞ /(2 2/3 9π) and M 2 η ′ = 0.46M 2 KK y ∞ with our coordinate choice. From the the non-anomalous η ′ mass, ∼ 390 MeV [20], and the quark mass, M q ∼ 41 MeV, 1 we can determine the parameters of the D4/D6 model: M KK = 1.04 GeV [22] and λ = 6. In this case,Q ∼ 1.2 corresponds to the normal nuclear matter density ρ 0 .…”

Section: )mentioning

confidence: 99%