Neutron Star Mass Measurements. I. Radio Pulsars

Thorsett, S. E.; Chakrabarty, Deepto

doi:10.1086/306742

Cited by 626 publications

(636 citation statements)

References 64 publications

Supporting

Mentioning

580

Contrasting

Order By: Relevance

“…Unfortunately, no decisive argument has been given so far in favor of the stiff, moderate or soft equations of state. One can definitely rule out only the ultra-soft equations of state which give the maximum stellar mass lower than 1.44 M ⊙ , the accurately measured mass of the Hulse-Taylor pulsar (Thorsett and Chakrabarty 1999).…”

Section: Introductionmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

View full text Add to dashboard Cite

We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

show abstract

Section: Introductionmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

View full text Add to dashboard Cite

show abstract

“…However, modern theoretically computed equations of state (EOS) generally predict somewhat larger moments of inertia for stars more massive than 1M , a group which includes all neutron stars with measured masses (see Ref. [43]). Therefore the dependence on the moment of inertia should be considered.…”

Section: B Dependence On the Moment Of Inertiamentioning

confidence: 99%

Upper limits on gravitational wave emission from 78 radio pulsars

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

134

View full text Add to dashboard Cite

We present upper limits on the gravitational wave emission from 78 radio pulsars based on data from the third and fourth science runs of the LIGO and GEO 600 gravitational wave detectors. The data from both runs have been combined coherently to maximize sensitivity. For the first time, pulsars within binary (or multiple) systems have been included in the search by taking into account the signal modulation due to their orbits. Our upper limits are therefore the first measured for 56 of these pulsars. For the remaining 22, our results improve on previous upper limits by up to a factor of 10. For example, our tightest upper limit on the gravitational strain is 2:6 10 ÿ25 for PSR J1603 ÿ 7202, and the equatorial ellipticity of PSR J2124-3358 is less than 10 ÿ6 . Furthermore, our strain upper limit for the Crab pulsar is only 2.2 times greater than the fiducial spin-down limit.

show abstract

“…Mixing of hyperons only already leads to appreciable softening of the EOS [45,[49][50][51][52][53][54][55][56][57][58]. Hence, further development of kaon condensates in hyperonic matter would make the EOS too soft to obtain the observed neutron star masses ∼ 1.4M ⊙ [86,87] or even much larger masses∼ 2.0M ⊙ if the recent analyses from the observations of the quasi-periodic oscillations (QPO) [88] are confirmed [51]. Relativistic effects may help weaken the softness of the EOS, since it has been shown that the energy gain of kaon condensation coming from the s-wave scalar attraction is suppressed by relativistic effects [8,4]: As a kaon condensate develops, the effective nucleon mass M * decreases due to the scalar attraction, which leads to suppression of the scalar density,…”

Section: Summary and Concluding Remarksmentioning

confidence: 99%

Kaonic modes in hyperonic matter and p-wave kaon condensation

Muto

2002

Nuclear Physics A

View full text Add to dashboard Cite

Kaon excitations (kaonic modes) are investigated in hyperonic matter, where hyperons (Λ, Σ − , Ξ − ) are mixed in the ground state of neutron-star matter. P -wave kaon-baryon interactions as well as the s-wave interactions are taken into account within chiral effective Lagrangian, and the nonrelativistic effective baryon-baryon interactions are incorporated. When the hyperon Λ is more abundant than the proton at high baryon density, a proton-particle-Λ-hole mode, which has the K + quantum number, appears in addition to other particle-hole modes with the K − quantum number. It is shown that the system becomes unstable with respect to a spontaneous creation of a pair of the particle-hole modes with K + and K − quantum numbers, stemming from the p-wave kaon-baryon interaction. The onset density of this p-wave kaon condensation may be lower than that of the s-wave K − condensation.

show abstract

Neutron Star Mass Measurements. I. Radio Pulsars

Cited by 626 publications

References 64 publications

Neutrino emission from neutron stars

Neutrino emission from neutron stars

Upper limits on gravitational wave emission from 78 radio pulsars

Kaonic modes in hyperonic matter and p-wave kaon condensation

Contact Info

Product

Resources

About