ﻻ يوجد ملخص باللغة العربية
We present upper limits on the X-ray emission for three neutron stars. For PSR J1840$-$1419, with a characteristic age of 16.5 Myr, we calculate a blackbody temperature upper limit (at 99% confidence) of $kT_{mathrm{bb}}^{infty}<24^{+17}_{-10}$ eV, making this one of the coolest neutron stars known. PSRs J1814$-$1744 and J1847$-$0130 are both high magnetic field pulsars, with inferred surface dipole magnetic field strengths of $5.5times10^{13}$ and $9.4times10^{13}$ G, respectively. Our temperature upper limits for these stars are $kT_{mathrm{bb}}^{infty}<123^{+20}_{-33}$ eV and $kT_{mathrm{bb}}^{infty}<115^{+16}_{-33}$ eV, showing that these high magnetic field pulsars are not significantly hotter than those with lower magnetic fields. Finally, we put these limits into context by summarizing all temperature measurements and limits for rotation-driven neutron stars.
The pulsar PSR J1756$-$2251 resides in a relativistic double neutron star (DNS) binary system with a 7.67-hr orbit. We have conducted long-term precision timing on more than 9 years of data acquired from five telescopes, measuring five post-Keplerian
The rapid-neutron-capture (r) process is responsible for synthesizing many of the heavy elements observed in both the solar system and Galactic metal-poor halo stars. Simulations of r-process nucleosynthesis can reproduce abundances derived from obse
We report the discovery of a very cool, isolated brown dwarf, UGPS 0722-05, with the UKIDSS Galactic Plane Survey. The near-infrared spectrum displays deeper H2O and CH4 troughs than the coolest known T dwarfs and an unidentified absorption feature a
We study the evolution of close binary systems in order to account for the existence of the recently observed binary system containing the most massive millisecond pulsar ever detected, PSR J0740+6620, and its ultra-cool helium white dwarf companion.
Two low mass neutron stars, J0737-3039B and the companion to J1756-2251, show strong evidence of being formed from the collapse of an ONeMg core in an electron capture supernova (ECSN) or in an ultra-stripped iron core collapse supernova (FeCCSN). Us