Results 51 to 60 of about 847,988 (312)
Correlation between the luminosity and spin-period changes during outbursts of 12 Be binary pulsars observed by the MAXI/GSC and the Fermi/GBM [PDF]
, 2017 To observationally study spin-period changes of accreting pulsars caused by the accretion torque, the present work analyzes X-ray light curves of 12 Be binary pulsars obtained by the MAXI/GSC all-sky survey and their pulse periods measured by the Fermi ...
M. Sugizaki +3 more
semanticscholar +1 more source
Structure and stability of differentially rotating compact stellar objects
Astronomische Nachrichten, Volume 344, Issue 1-2, January-February 2023., 2023 Abstract Depending on the dynamics of a binary neutron star merger, the collision may result in a differentially rotating compact object. Differentially rotating stars can sustain a total mass considerably higher than that of a uniformly rotating star, giving rise to “hypermassive” objects like hypermassive neutron stars.
Delaney Farrell +2 more
wiley +1 more source
Improving Distances to Binary Millisecond Pulsars with Gaia
The Astrophysical Journal, 2023 Pulsar distances are notoriously difficult to measure, and play an important role in many fundamental physics experiments, such as pulsar timing arrays.
Abigail Moran +4 more
doaj +1 more source
Dynamics and Interactions of Binaries and Neutron Stars in Globular Clusters [PDF]
, 1994 We model the dynamics of test binaries in isotropic, multi-mass models of galactic globular clusters. The evolution of binary orbits through the cluster potentials is modeled, including second order diffusion terms, and probabilities for close encounters
Phinney, E. S., Sigurdsson, Steinn
core +3 more sources
Gravitational radiation and the binary pulsar [PDF]
Nature, 1982 Nature Vol. 297 3 June 1982 357 NEWS AND VIEWS Tq Gravitational radiation and the binary pulsar GRAVITATIONAL radiation not only exists, but it is apparently also doing exactly what general relativity says it ought to, at least in the binary pulsar PSRl9l3 + 16. This is the conclusion drawn by J .H. Taylor and J .M.
Virginia Trimble, Virginia Trimble
openaire +3 more sources
Challenging the presence of scalar charge and dipolar radiation in binary pulsars [PDF]
, 2015 Corrections to general relativity that introduce long-ranged scalar fields which are nonminimally coupled to curvature typically predict that neutron stars possess a nontrivial scalar field profile anchored to the star.
Kent Yagi, L. Stein, N. Yunes
semanticscholar +1 more source
Super-Massive Neutron Stars and Compact Binary Millisecond Pulsars [PDF]
Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources - XIII — PoS(MULTIF2019), 2019 The maximum mass of a neutron star has important implications across multiple research fields, including astrophysics, nuclear physics and gravitational wave astronomy.
M. Linares
semanticscholar +1 more source
Binary and Other Recycled Pulsars [PDF]
Symposium - International Astronomical Union, 1992 Binary pulsars and others with weak fields and rapid rotation now number several dozen and appear to have been spun up by close binary mass transfer. Some are lineal descendents of X-ray binaries; others may result from accretion-induced collapse of binary white dwarfs or from captures, exchanges, and collisions in clusters. Seven accurate neutron star
openaire +3 more sources
Symposium - International Astronomical Union, 1981 There are now three radio frequency pulsars known to be in binary systems: PSRs 1913+16, 0820+02, and 0655+64. The first of these, discovered in 1974, moves in a tight, highly eccentric orbit with a period of approximately 7h 45m. Its companion has not yet been identified with certainty, but must be a compact object of mass comparable to that of the ...
openaire +1 more source
A Multiwavelength View of the Neutron Star Binary 1FGL J1417.7–4402: A Progenitor to Canonical Millisecond Pulsars [PDF]
Astrophysical Journal, 2018 The Fermi γ-ray source 1FGL J1417.7–4407 (J1417) is a compact X-ray binary with a neutron star primary and a red giant companion in a ∼5.4 days orbit. This initial conclusion, based on optical and X-ray data, was confirmed when a 2.66 ms radio pulsar was
S. Swihart +8 more
semanticscholar +1 more source