Strange stars

Alcock, C.; Farhi, Edward; Olinto, Angela V.

doi:10.1086/164679

Cited by 1,249 publications

(1,668 citation statements)

References 0 publications

Supporting

Mentioning

1,612

Contrasting

Unclassified

Order By: Relevance

“…Some of the mechanisms for the production of the strange quark matter in neutron stars have been investigated by Alcock et al [14]. These authors have assumed that…”

Section: Introductionmentioning

confidence: 99%

Strangeness production in neutron stars

Ghosh¹,

Phatak²,

Sahu³

1996

Nuclear Physics A

View full text Add to dashboard Cite

Production of strange quarks in neutron stars is investigated in this work.Three cases, one in which the energy and neutrinos produced in the strangeness production reactions are retained in the reaction region, second in which the neutrinos are allowed to escape the reaction region but the energy is retained and the third in which both the energy and neutrinos escape the reaction region are considered. It is shown that the nonleptonic weak process dominates strange quark production while semileptonic weak processes, which produce neutrinos, lead to the cooling if the neutrinos escape the reaction region. It is found that the time required for the saturation of the strangeness fraction is between 10 −7 and 10 −5 sec, with the shorter time corresponding to the first two cases. About 0.2 neutrinos/baryon are emitted during the process in the first two cases where as the neutrino emission is somewhat suppressed in the last case. The average energy of the neutrinos produced in all the three cases is found to be several hundred M eV . 0We also find that a large amount of energy is released during the strangeness production in the first two cases and this leads to the heating of the reaction region.Implications of the neutrino production are investigated.

show abstract

“…Some of the mechanisms for the production of the strange quark matter in neutron stars have been investigated by Alcock et al [14]. These authors have assumed that…”

Section: Introductionmentioning

confidence: 99%

Strangeness production in neutron stars

Ghosh¹,

Phatak²,

Sahu³

1996

Nuclear Physics A

View full text Add to dashboard Cite

show abstract

“…In the present letter, we have not considered the possibility of having a thin crust of nuclear material, suspended from contact with the high density mixed phase by an electric dipole field [11,17]. The introduction of this thin crust would modify significantly the M-R relationship only for extremely small values of the mass (M ≈ 0.1M ⊙ ) [7].…”

mentioning

confidence: 93%

“…The latter consists of an approximately equal number of up, down and strange quarks having energy per baryon E/A smaller than that of iron (E F e ≈ 930 MeV), at zero temperature and pressure [10]. Stars entirely composed of matter in such ultra-stable state are self-bound [11,12] and could rotate with a period well below one millisecond [13,14].…”

mentioning

confidence: 99%

From quark stars to hybrid stars

Drago

Lavagno

2001

Physics Letters B

View full text Add to dashboard Cite

We show the possible existence of compact stars having a surface composed of a mixed phase of quarks and hadrons. This scenario can be realized both for self-bound stars, satisfying the so-called Witten-Bodmer hypothesis, and for gravitationally bound stars. Recently several analysis of observational data have emphasized the possible existence of compact stars having very small radii, of the order of 9 kilometers or less [1]. To account theoretically for the existence of such a star, one would need to use of very soft Equations of State (EOSs), that can be obtained, in principle, introducing kaon condensation [2-4], or hyperonic degrees of freedom [5][6][7]. Another possibility is to consider quark stars, where the density of the surface is above nuclear matter saturation density. These objects have been obtained till now assuming the validity of the hypothesis introduced independently by Bodmer [8] and Witten [9], which states that the true and absolute ground state of the strong interaction is a state of deconfined quark matter. The latter consists of an approximately equal number of up, down and strange quarks having energy per baryon E/A smaller than that of iron (E F e ≈ 930 MeV), at zero temperature and pressure [10]. Stars entirely composed of matter in such ultra-stable state are self-bound [11,12] and could rotate with a period well below one millisecond [13,14].A possible problem in interpreting neutron stars as strange quark stars is the difficulty of having glitches in the latter, since the most widely accepted model for the glitches require the existence of a crystallized phase trapping magnetic

show abstract

“…Witten (1984) pointed out that the true ground state of hadrons may be strange matter, which contains roughly equal numbers of up, down and strange quarks. It is then realized that a quark star or strange star (SS) might be the ground state of NSs (Alcock et al 1986;Haensel et al 1986). NSs may convert to SSs.…”

Section: Introductionmentioning

confidence: 99%

The missing compact star of SN1987A: a solid quark star?

Liu¹,

Liang

Xu³

et al. 2012

Proc. IAU

View full text Add to dashboard Cite

To investigate the missing compact star of Supernova 1987A, we analyzed both the cooling and the heating processes of a possible compact star based on the upper limit of observational X-ray luminosity. From the cooling process we found that a solid quark-cluster star, which has a stiffer equation of state than that of conventional liquid quark star, has a heat capacity much smaller than a neutron star. It can cool down quickly, which can naturally explain the nondetection of a point source (neutron star or quark star) in X-ray band. On the other hand, we consider the heating process from magnetospheric activity and possible accretion, and obtain some constraints to the parameters of a possible pulsar. We conclude that a solid quark-cluster star can be fine with the observational limit in a large and acceptable parameter space. A pulsar with a short period and a strong magnetic field (or with a long period and a weak field) would has luminosity higher than the luminosity limit if the optical depth is not large enough to hide the compact star. The constraints of the pulsar parameters can be tested if the central compact object in 1987A is discovered by advanced facilities in the future.

show abstract

Strange stars

Cited by 1,249 publications

References 0 publications

Strangeness production in neutron stars

Strangeness production in neutron stars

From quark stars to hybrid stars

The missing compact star of SN1987A: a solid quark star?

Contact Info

Product

Resources

About