Results 31 to 40 of about 200,989 (232)
Burning of a Hadronic Star into a Quark or a Hybrid Star [PDF]
The Astrophysical Journal, 2007 47 pages, 23 figures New version after referee's comments.
DRAGO, Alessandro +2 more
openaire +4 more sources
Properties of strange quark matter and strange quark stars
European Physical Journal C: Particles and Fields, 2021 A Polyakov chiral $$\text {SU(3)}$$ SU(3) quark mean-field (PCQMF) model is applied to study the properties of strange quark matter (SQM) and strange quark star (SQS) in $$\beta $$ β -equilibrium.
Manisha Kumari, Arvind Kumar
doaj +1 more source
Strange quark mass dependence of strange quark star properties
European Physical Journal C: Particles and Fields, 2021 The effects of strange quark mass on masses, radii, and tidal deformabilities of strange quark stars are studied via the quasiparticle model that includes the non-perturbative features of QCD in low density region. The constraints of $$M_{\mathrm {TOV}} >
Bo-Lin Li, Yan Yan, Jia-Lun Ping
doaj +1 more source
The Journal of Physiology, EarlyView., 2023 Abstract figure legend Reductions in skeletal muscle mitochondrial respiration following 60 days of bed rest explained by a decrease in mitochondrial content, but resulting in an increase in OPA1 and Drp1 mediated mitochondrial fission. Abstract It is unclear how skeletal muscle metabolism and mitochondrial function adapt to long duration bed rest and ...
John Noone +14 more
wiley +1 more source
Why can hadronic stars convert into strange quark stars with larger radii [PDF]
Phys. Rev. D 102, 063003 (2020), 2020 The total binding energy of compact stars is the sum of the gravitational binding energy $(BE)_g$ and the nuclear binding energy $(BE)_n$, the last being related to the microphysics of the interactions. While the first is positive (binding) both for hadronic stars and for strange quark stars, the second is large and negative for hadronic stars (anti ...
arxiv +1 more source
Chinese Journal of Astronomy and Astrophysics, 2006 Members of the family of pulsar-like stars are distinguished by their different manifestations observed, i.e., radio pulsars, accretion-driven X-ray pulsars, X-ray bursts, anomalous X-ray pulsars/soft gamma-ray repeaters, compact center objects, and dim thermal neutron stars. Though one may conventionally think that these stars are normal neutron stars,
openaire +2 more sources
Neutron stars and massive quark matter [PDF]
Progress in Particle and Nuclear Physics, 1996 Using the Color-Dielectric model to describe quark confinement, including strange quarks and accounting for beta--equilibrium, we get masses for a static neutron star in the range $1.3\leq M/M_{\odot}\leq 1.54 $ for a radius $R\approx 9$ km. Rapid cooling through the direct URCA mechanism is obtained.
DRAGO, Alessandro +2 more
openaire +5 more sources
Isovector properties of quark matter and quark stars in an isospin-dependent confining model [PDF]
Phys. Rev. D 96, 083019 (2017), 2017 The confining quark matter (CQM) model, in which the confinement and asymptotic freedom are modeled via the Richardson potential for quark-quark vector interaction and the chiral symmetry restoration at high density is described by the density dependent quark mass, is extended to include isospin dependence of the quark mass.
arxiv +1 more source
Quakes in solid quark stars [PDF]
Astroparticle Physics, 2004 A starquake mechanism for pulsar glitches is developed in the solid quark star model. It is found that the general glitch natures (i.e., the glitch amplitudes and the time intervals) could be reproduced if solid quark matter, with high baryon density but low temperature, has properties of shear modulus = 10^{30~34} erg/cm^3 and critical stress _c =
Zhou, A. Z. +4 more
openaire +3 more sources
Dense hadron star in quark degree of freedom
EPJ Web of Conferences, 2014 The quark degree of freedom may play an important role as one studies dense hadron stars which can help to understand the universe origin. We add a temperature dependence to the effective quark mass adopted from a quark-quark interaction on the QCD basis
Tzeng Yiharn, Tzeng S.Y.Tsay
doaj +1 more source