Neutron star constraints on the H dibaryon

Glendenning, Norman K.; Schaffner-Bielich, J.

doi:10.1103/physrevc.58.1298

Cited by 37 publications

(49 citation statements)

References 43 publications

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“…Since its first prediction in 1977, the H-dibaryon has been the subject of many theoretical and experimental studies as a possible candidate for a strongly bound exotic state. In neutron stars, which may contain a significant fraction of Λ hyperons, the Λ's could combine to form H-dibaryons, which could give way to the formation of H-dibaryon matter at densities somewhere above ∼ 3 ǫ 0 [200,201,202] depending on the in-medium properties of the H-dibaryon. For an attractive optical potential, U H , of the H-dibaryon at normal nuclear density the equation of state is softened considerably, as shown in Fig.…”

Section: H-dibaryonsmentioning

confidence: 99%

“…H-dibaryon matter could thus exist in the cores of moderately dense neutron stars. Hdibaryons with a vacuum mass of about 2.2 GeV and a moderately attractive potential in the medium of about U H = −30 MeV, for instance, could go into a boson condensate in the cores of neutron stars if the limiting star mass is about that of the Hulse-Taylor pulsar PSR 1913+16, M = 1.444 M ⊙ [202]. Conversely, if the medium potential were moderately repulsive, around U H = +30 MeV, the formation of H-dibaryons may only take place in heavier neutron stars of mass M > ∼ 1.6 M ⊙ .…”

Section: H-dibaryonsmentioning

confidence: 99%

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Strange quark matter and compact stars

Weber

2005

Progress in Particle and Nuclear Physics

664

280

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Astrophysicists distinguish between three different types of compact stars. These are white dwarfs, neutron stars, and black holes. The former contain matter in one of the densest forms found in the Universe which, together with the unprecedented progress in observational astronomy, make such stars superb astrophysical laboratories for a broad range of most striking physical phenomena. These range from nuclear processes on the stellar surface to processes in electron degenerate matter at subnuclear densities to boson condensates and the existence of new states of baryonic matter-like color superconducting quark matter-at supernuclear densities. More than that, according to the strange matter hypothesis strange quark matter could be more stable than nuclear matter, in which case neutron stars should be largely composed of pure quark matter possibly enveloped in thin nuclear crusts. Another remarkable implication of the hypothesis is the possible existence of a new class of white dwarfs. This article aims at giving an overview of all these striking physical possibilities, with an emphasis on the astrophysical phenomenology of strange quark matter. Possible observational signatures associated with the theoretically proposed states of matter inside compact stars are discussed as well. They will provide most valuable information about the phase diagram of superdense nuclear matter at high baryon number density but low temperature, which is not accessible to relativistic heavy ion collision experiments.

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Section: H-dibaryonsmentioning

confidence: 99%

Section: H-dibaryonsmentioning

confidence: 99%

Strange quark matter and compact stars

Weber

2005

Progress in Particle and Nuclear Physics

664

280

View full text Add to dashboard Cite

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“…This effect provides a constraint on the property of the H-dibaryon in dense matter as the maximum mass can not be lower than M = 1.44M ⊙ . A deeply bound H-dibaryon with an attractive nuclear potential turns out to be not compatible with this constraint [29].…”

Section: Strange Hadrons In Compact Starsmentioning

confidence: 99%

The role of strangeness in astrophysics$mdash$an odyssey through strange phases

Schaffner-Bielich¹

2002

J. Phys. G: Nucl. Part. Phys.

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Abstract. The equation of state for compact stars is reviewed with special emphasis on the role of strange hadrons, strange dibaryons and strange quark matter. Implications for the properties of compact stars are presented. The importance of neutron star data to constrain the properties of hypothetic particles and the possible existence of exotic phases in dense matter is outlined. We also discuss the growing interplay between astrophysics and heavy-ion physics.

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“…Neutron star constraints on the H-dibaryon from the mass of the Hulse-Taylor pulsar. A deeply bound H-dibaryon feeling an attractive potential in matter can be ruled out as the corresponding neutron stars have a too small maximum mass (from [18]). …”

Section: Hyperons and Dibaryons In Neutron Starsmentioning

confidence: 99%

“…we set g ωH = 4/3g ωN . We fix the scalar coupling to an optical potential at normal nuclear matter density in the range Figure 1 shows the resulting equation of state when using the parameter set TM1 and including effects from hyperons (see [18] for details). The equation of state turns out to be quite sensitive to the choice of the optical potential of the H-dibaryon.…”

Section: Hyperons and Dibaryons In Neutron Starsmentioning

confidence: 99%

Strange dibaryons in neutron stars and in heavy-ion collisions

Schaffner-Bielich¹

2001

Nuclear Physics A

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The formation of dibaryons with strangeness are discussed for the interior of neutron stars and for central relativistic heavy-ion collisions. We derive limits for the properties of H-dibaryons from pulsar data. Signals for the formation of possible bound states with hyperons at BNL's Relativistic Heavy-Ion Collider (RHIC) are investigated by studying their weak decay patterns and production rates. HYPERONS AND DIBARYONS IN NEUTRON STARSThere has been a lot of speculations about the appearance of new particles in the interior of neutron stars. A traditional neutron star consists of neutrons, protons, and leptons only. Cameron suggested first in 1959, that hyperons will also appear at high baryon density [1]. A possible phase transition to quark matter was conjectured shortly after the quark model was introduced [2]. Pion condensation [3] as well as kaon condensation were considered later [4]. Finally, strange stars, built out of absolutely stable strange quark matter, have been studied within the MIT bag model [5,6]. The appearance of one or the other exotic phase in the core of neutron stars is still a matter of active debates. Nevertheless, recent developments in the field indicate, that hyperons are probably the first exotic particle to appear in neutron star matter at twice normal nuclear density. This result was consistently derived within various, different models: nonrelativistic potential models [7], quark-meson coupling model [8], relativistic mean-field models [9-11], relativistic Hartree-Fock [12], Brueckner-Hartree-Fock models [13,14], and chiral effective Lagrangians [15]. Hence, the onset of hyperons at 2ρ 0 seems to be rather insensitive to the underlying details of the hyperon-nucleon interaction used.If there are a lot of hyperons in the interior of neutron stars, then it might be also possible to form dibaryons with strangeness. Besides the famous H-dibaryon proposed by Jaffe [16] built out of six quarks, the most recent version of the Nijmegen potential predicts the existence of deeply bound states of two hyperons, involving the Σ's and Ξ's with maximum isospin [17]. Their results can be understood in terms of the underlying SU(3) symmetry for the baryon-baryon interactions (see [17]).Let us assume in the following, that there exist bound states with hyperons. What would be the consequences for the properties of dense matter, as present in the interior of neutron stars? Bound systems in dense matter have been discussed before in connection * I thank RIKEN, BNL, and the U.S. Department of Energy for providing the facilities essential for the completion of this work.

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Neutron star constraints on the H dibaryon

Cited by 37 publications

References 43 publications

Strange quark matter and compact stars

Strange quark matter and compact stars

The role of strangeness in astrophysics$mdash$an odyssey through strange phases

Strange dibaryons in neutron stars and in heavy-ion collisions

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