Formation of the binary pulsars J1141-6545 and B2303+46

@article{Davies2002FormationOT,
  title={Formation of the binary pulsars J1141-6545 and B2303+46},
  author={Melvyn B Davies and Hans Georg Ritter and Andrew Levan University of Leicester and UK. and Max-Planck-Institut fuer Astrophysik and H Germany},
  journal={Scopus},
  year={2002}
}
The binaries PSR J1141-6545 and PSR B2303+46 each appear to contain a white dwarf that formed before the neutron star. We describe an evolutionary pathway to produce these two systems. In this scenario, the primary transfers its envelope on to the secondary, which is then the more massive of the two stars, and indeed sufficiently massive later to produce a neutron star via a supernova. The core of the primary produces a massive white dwarf, which enters into a common envelope with the core of… Expand
Detailed models of the binary pulsars J1141−6545 and B2303+46
We have modelled the formation of the eccentric double-degenerate binaries J1141-6545 and B2303+46 using the Henyey-type full stellar evolution code STARS and the population synthesis code BSE. WeExpand
A pre-explosion optical transient event from a white dwarf merger with a giant supernova progenitor
We examine rare evolutionary routes of binary systems where the initially more massive primary star of ~5.5-8.5Mo, forms a white dwarf (WD), while the secondary star of 4Mo < M_2,0 < M_1,0 accretesExpand
Compact binaries, hypernovae, and GRBs
The collapse of a massive stellar core may lead to the production of a black hole surrounded by a torus of material. Such a system is a potential source for the so-called long gamma-ray burstsExpand
PSR J1755-2550: A young radio pulsar with a massive, compact companion
Radio pulsars found in binary systems with short orbital periods are usually fast spinning as a consequence of recycling via mass transfer from their companion stars; this process is also thought toExpand
The demographics of neutron star – white dwarf mergers
Context. The mergers of neutron stars (NSs) and white dwarfs (WDs) could give rise to explosive transients, potentially observable with current and future transient surveys. However, the expectedExpand
Double‐core evolution and the formation of neutron star binaries with compact companions
We present the results of a systematic exploration of an alternative evolutionary scenario to form double neutron star (DNS) binaries, first proposed by Brown (1995), which does not involve a neutronExpand
Stability of Mass Transfer in Eccentric Compact Binaries
Compact binaries, which consist of a white dwarf and a neutron star, are interesting in several respects. Formed at the rate 10−4 – 10−5 yr−1, most of them will come into contact in less than aExpand
A white dwarf companion to the relativistic pulsar PSR J1141−6545
Pulsars with compact companions in close eccentric orbits are unique laboratories for testing general relativity and alternative theories of gravity. Moreover, they are excellent targets for futureExpand
Type Ia supernovae and the formation of single low-mass white dwarfs
Context. There is still considerable debate over the progenitors of type Ia supernovae (SNe Ia). Likewise, it is not agreed how single white dwarfs with masses less than or similar to 0.5 M(circleExpand
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction
Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a populationExpand
...
1
2
3
...

References

SHOWING 1-10 OF 15 REFERENCES
Cygnus X-2, super-Eddington mass transfer, and pulsar binaries
TLDR
It is shown that this star closely resembles a remnant of early massive Case B evolution, during which the neutron star ejected most of the mass transferred from the donor, and thus strongly supports the idea that a neutron star efficiently ejects the excess inflow during super-Eddington mass transfer. Expand
A Massive White Dwarf Companion to the Eccentric Binary Pulsar System PSR B2303+46
Pulsars in close, eccentric binary systems are usually assumed to have another neutron star as a companion. These double neutron star binaries have proven to be the best laboratories for experimentalExpand
The violent past of Cygnus X-2
Cygnus X-2 appears to be the descendant of an intermediate-mass X-ray binary (IMXB). Using Mazzitelli's stellar code we compute detailed evolutionary sequences for the system and find that itsExpand
Double white dwarfs as progenitors of R Coronae Borealis stars and type I supernovae
Close double white dwarfs should arise from the second phase of mass exchagne in close binaries which first encountered mass exchange while the more massive star was crossing the Hertzprung gap.Expand
Discovery of a Young Radio Pulsar in a Relativistic Binary Orbit
We report on the discovery of PSR J1141-6545, a radio pulsar in an eccentric, relativistic 5 hr binary orbit. The pulsar shows no evidence of being recycled, having a pulse period P = 394 ms, aExpand
The possible companions of young radio pulsars
We discuss the formation of pulsars with massive companions in eccentric orbits. We demonstrate that the probability for a non-recycled radio pulsar to have a white dwarf as a companion is comparableExpand
Research Note On the binding energy parameter of common envelope evolution - Dependency on the definition of the stellar core boundary during spiral-in
According to the standard picture for binary interactions, the outcome of binaries surviving the evolution through a common envelope (CE) and spiral-in phase is determined by the internal structureExpand
Evolution of Neutron Star, Carbon-Oxygen White Dwarf Binaries
We consider the evolution of neutron-star (ns), carbon-oxygen white-dwarf (co) binaries, using both the Bethe & Brown (1998) schematic analytic evolutions and the Portegies Zwart & Yungelson (1998)Expand
Formation of Low-Mass X-ray Binaries. I. Constraints on Hydrogen-Rich Donors at the Onset of the X-ray Phase
We identify and quantify the set of constraints that neutron star-normal star binaries must satisfy in order to become observable LMXBs. These constraints are related to (i) the thermal andExpand
The Pulsar kick velocity distribution
We analyse the sample of pulsar proper motions, taking detailed account of the selection effects of the original surveys. We treat censored data using survival statistics. From a comparison of ourExpand
...
1
2
...