1550-7998=20 Numerical simulations of binary neutron stars by Wilson, Mathews, and Marronetti indicated that neutron stars that are stable in isolation can be made to collapse to black holes when placed in a binary. This claim was surprising as it ran counter to the Newtonian expectation that a neutron star in a binary should be more stable, not less. After correcting an error found by Flanagan...

The PSR1259−63/SS2883 binary system consists of a Be star and a radio pulsar in a highly eccentric orbit. We discuss on very-high energy and high energy emissions from the particles accelerated in the Be star flows, due to the interactions of the relativistic pulsar wind and mass outflows of the star. The outflow parameters are constrained by the TeV observation results.

The equation of state (EoS) neutron star (NS) matter is investigated considering kaon condensation. Moreover, the tidal parameters related to components binary mergers are determined and compared constraints GW170817 imposed on these quantities. In this study, we employ lowest-order constrained variational (LOCV) approach utilize {AV6$'$, AV8$'$, AV18 potentials} accompanied by three nucleon in...

Binary radio pulsars are superb tools for mapping binary orbits, because of the precision of the pulse timing method (e.g Taylor & Weisberg 1989). To date, all orbital parameters for binary pulsars have been derived from observations of the pulsar alone. We present the rst observations of the radial velocity variations due to the binary motion of a companion to a radio pulsar. Our results demon...

| Binary tree structures have been very useful in solving divide-and-conquer type of problems. Embedding binary trees into another network|the host network|helps in designing solutions for the host network using the known solutions on binary trees. Embedding arbitrary binary trees into networks, in particular into the hypercube, has been addressed in the literature. The latter was achieved with...

With the aim of investigating the binary population of the 700 Myr old Praesepe cluster, we have observed 149 G and K-type cluster members using adaptive optics. We detected 26 binary systems with an angular separation ranging from less than 0.08 to 3.3 arcsec (15–600 AU). After correcting for detection biases, we derive a binary frequency (BF) in the log P (days) range from 4.4 to 6.9 of 25.3±...