A strongly magnetic neutron star in a nearly face-on binary system

Nature ◽  
1996 ◽  
Vol 382 (6587) ◽  
pp. 141-144 ◽  
Author(s):  
Pascal Daumerie ◽  
Vassiliki Kalogera ◽  
Frederick K. Lamb ◽  
Dimitrios Psaltis
Keyword(s):  
Neutron Star ◽  
Binary System

scholarly journals Spin Evolution of the Progenitors of Binary and Millisecond Pulsars

1996 ◽  
Vol 165 ◽  
pp. 57-64
Author(s):  
Pranab Ghosh
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Binary System ◽  
Neutron Stars ◽  
High Magnetic Field ◽  
Evolutionary History ◽  
Millisecond Pulsars ◽  
History Of ◽  
Low Magnetic Field ◽  
Fast Rotating

In this symposium, I have been given the task of summarizing our current understanding of the evolutionary history of spin periods of the neutron stars that we now see as binary and millisecond pulsars, i.e., recycled pulsars. We believe that a newborn, fast-spinning neutron star (with a rather high magnetic field ∼1011–1013 G) in a binary system first operates as a spin-powered pulsar, subsequently as an accretion-powered pulsar when accretion begins after the pulsar has been spun down adequately, and finally as a spin-powered pulsar for the second time after having been recycled to become a very fast-rotating neutron star (with a rather low magnetic field ∼108–1011 G) (see Ghosh 1994a, b, hereafter G94a, b).

scholarly journals Torque Reversals in Disk Accreting Pulsars

1998 ◽  
Vol 15 (2) ◽  
pp. 250-253
Author(s):  
Jianke Li ◽  
Dayal T. Wickramasinghe
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Recent Work ◽  
Time Scale ◽  
Accretion Rate ◽  
Future Studies ◽  
X Ray ◽  
The Past ◽  
X Ray Binaries ◽  
Coherent Picture

AbstractX-ray binaries in which the accreting component is a neutron star commonly exhibit significant changes in their spin. In the system Cen X-3, a disk accreting binary system, the pulsar was observed to spin up at a rate ḟ = 8 × 10−13 Hz s−1 when averaged over the past twenty years, but significant fluctuations were observed above this mean. Recent BASTE observations have disclosed that these fluctuations are much larger than previously noted, and appeared to be a system characteristic. The change in the spin state from spin-up to spin-down or vice-versa occurs on a time scale that is much shorter than the instrument can resolve (≤1 d), but appears always to be a similar amplitude, and to occur stochastically. These observations have posed a problem for the conventional torque–mass accretion relation for accreting pulsars, because in this model the spin rate is closely related to the accretion rate, and the latter needs to be finely tuned and to change abruptly to explain the observations. Here we review recent work in this direction and present a coherent picture that explains these observations. We also draw attention to some outstanding problems for future studies.

scholarly journals SPECTRAL AND TIMING NATURE OF THE SYMBIOTIC X-RAY BINARY 4U 1954+319: THE SLOWEST ROTATING NEUTRON STAR IN AN X-RAY BINARY SYSTEM

2014 ◽  
Vol 786 (2) ◽  
pp. 127 ◽  
Author(s):  
Teruaki Enoto ◽  
Makoto Sasano ◽  
Shin'ya Yamada ◽  
Toru Tamagawa ◽  
Kazuo Makishima ◽  
...  
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
X Ray

On the formation of a neutron star in a close binary system

1971 ◽  
Vol 10 (3) ◽  
pp. 464-470 ◽  
Author(s):  
George E. McCluskey ◽  
Yoji Kondo
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Close Binary System ◽  
Close Binary

Electromagnetic bursting of a rapidly rotating magnetized neutron star in a close binary system

1995 ◽  
Vol 231 (1-2) ◽  
pp. 437-440
Author(s):  
A. Treves ◽  
E. Szuszkiewicz ◽  
M. Tavani
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Close Binary System ◽  
Close Binary

Accretion of matter by a neutron star in a binary system. I

Astrophysics ◽  
1970 ◽  
Vol 6 (3) ◽  
pp. 214-217
Author(s):  
P. R. Amnuél' ◽  
O. Kh. Guseinov
Keyword(s):  
Neutron Star ◽  
Binary System

scholarly journals Binary evolution leading to the formation of the very massive neutron star in the J0740+6620 binary system

2020 ◽  
Vol 495 (2) ◽  
pp. 2509-2514
Author(s):  
M Echeveste ◽  
M L Novarino ◽  
O G Benvenuto ◽  
M A De Vito
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Effective Temperature ◽  
Binary Systems ◽  
Close Binary ◽  
Normal Donor ◽  
Millisecond Pulsar ◽  
Massive Neutron Star ◽  
Binary Evolution ◽  
Age Of The Universe

ABSTRACT 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. In order to find a progenitor for this object we compute the evolution of several binary systems composed by a neutron star and a normal donor star employing our stellar code. We assume conservative mass transfer. We also explore the effects of irradiation feedback on the system. We find that irradiated models also provide adequate models for the millisecond pulsar and its companion, so both irradiated and non irradiated systems are good progenitors for PSR J0740+6620. Finally, we obtain a binary system that evolves and accounts for the observational data of the system composed by PSR J0740+6620 (i.e. orbital period, mass, effective temperature and inferred metallicity of the companion, and mass of the neutron star) in a time scale smaller than the age of the Universe. In order to reach an effective temperature as low as observed, the donor star should have an helium envelope as demanded by observations.

scholarly journals Common envelope binaries and mass loss

1979 ◽  
Vol 83 ◽  
pp. 415-420
Author(s):  
A. Delgado
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Mass Loss ◽  
Free Parameter ◽  
Mass Ratio ◽  
Initial State ◽  
Helium Burning ◽  
Common Envelope ◽  
The Core ◽  
Before And After

In this work we calculate the evolution of a binary system with a common envelope, which consists of a blue supergiant and a neutron star. We consider as a free parameter the effectivity with which the energy liberated at the orbit produces mass loss from the system.The evolutionary calculations were made, using various values of this parameter, for a system with mass ratio 25:1. As initial state we choose a model in the phase of Hydrogen-shell burning, before and after the begin of Helium-burning in the core.We found that, under certain conditions, it is possible for the radius of the orbit and the period of the system to increase; the time scale for the “spiral-in” would be of the order of 104-105 years. Mass loss rates are between 10−3 M⊙/y and 10−4 M⊙/y.

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