[7] This density is approximately equivalent to the mass of the entire human population compressed to the size of a sugar cube.[8] In general, compact stars of less than 1.44 solar masses –the Chandrasekhar li
Neutron starsalso have a limiting mass, but it is not known as well as that forwhite dwarfsbecause thephysicsof the interior, in particular theequation of state, is not fully understood. A reasonable estimate is 2–3M⊙. If the collapsing core of a massive star exceeds this limit, the co...
4U 1820-30 is a binary system that includes a neutron star and a white dwarf approximately the same size as Earth, with a tight orbit that allows the neutron star to complete an orbit in just 11.4 minutes. The proximity of the two stars is such that the neutron star continuously siphons...
Neutron-star cores contain matter at the highest densities in our Universe. This highly compressed matter may undergo a phase transition where nuclear matter melts into deconfined quark matter, liberating its constituent quarks and gluons. Quark matter e
Higher harmonics of a lower fundamental frequency that may be possessed by a white dwarf have been mentioned; but the detailed fine structure of several short pulses repeating in each repetition cycle makes any such explanation very unlikely. Since the distances are known approximately from ...
A key motivation for finding and studying new spider pulsars is that they are one of the few types of pulsar binary system from which neutron star mass estimates can be obtained. This is because these systems have optically bright companion stars, whose radial velocities can be measured via opt...
Neutron stars (NSs) are observed with high space velocities and elliptical orbits in binaries. The magnitude of these effects points to natal kicks that originate from asymmetries during the supernova (SN) explosions. Using a growing set of long-time 3D SN simulations with the Prometheus-Vertex ...
have spotted the birth of these extreme Get great science journalism, from the most trusted source, delivered to your doorstep. It shows what we had suspected in our work from earlier Hubble observations," said Joseph Lyman, an astronomer at the University of Warwick in England, who led an ...
Heavy atomic nuclei have an excess of neutrons over protons, which leads to the formation of a neutron skin whose thickness is sensitive to details of the nuclear force. This links atomic nuclei to properties of neutron stars, thereby relating objects that differ in size by orders of magnitude...
a dead-time ofτ= 0.9 μs. However, Dushin15successfully employed the MC method introduced by Moat4to perform the dead-time correction forτ= 0.3 μs. Ideally, the electronics dead-time should be kept as short as possible. In the case of NeutronSTARS, the expected dead-time from vendor...