James M. Lattimer

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New astrometric analysis of four WFPC2 images of the isolated neutron star RX J185635-3754 show that its distance is 117±12 pc, nearly double the originally published distance. At the revised distance, the star's age is 5×10 5 years, its space velocity is about 185 km s −1 , and its radiation radius inferred from thermal emission is R ∞ ∼ 15 km, in the(More)
Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics, and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated(More)
We investigate the possibility of kaon condensation in the dense interior of neutron stars through the s{wave interaction of kaons with nucleons. We include nucleon{nucleon interactions by using simple parametrizations of realistic forces, and include electrons and muons in {equilibrium. The equation of state above the condensate threshold is derived in the(More)
Dietary fiber and whole grains contain a unique blend of bioactive components including resistant starches, vitamins, minerals, phytochemicals and antioxidants. As a result, research regarding their potential health benefits has received considerable attention in the last several decades. Epidemiological and clinical studies demonstrate that intake of(More)
The minimal cooling paradigm for neutron star cooling assumes that enhanced cooling due to neu-trino emission from any direct Urca process, due either to nucleons or to exotica such as hyperons, Bose condensates, or deconfined quarks, does not occur. This scenario was developed to replace and extend the so-called standard cooling scenario to include(More)
We estimate that the moment of inertia of star A in the recently discovered double pulsar system PSR J0737-3039 may be determined after a few years of observation to something like 10% accuracy. This would enable accurate estimates of the radius of the star and the presure of matter in the vicinity of 1 to 2 times the nuclear saturation density, which would(More)
The main stages in the evolution of a neutron star, from its birth as a proto-neutron star, to its old age as a cold, catalyzed configuration, are described. A proto-neutron star is formed in the aftermath of a successful supernova explosion and its evolution is dominated by neutrino diffusion. Its neutrino signal is a valuable diagnostic of its internal(More)
With the aim of constraining the structural properties of neutron stars and the equation of state of dense matter, we study sudden spin-ups, glitches, occurring in the Vela pulsar and in six other pulsars. We present evidence that glitches represent a self-regulating instability for which the star prepares over a waiting time. The angular momentum(More)