scholarly journals Erratum: Formation of millisecond pulsars with helium white dwarfs, ultra-compact X-ray binaries, and gravitational wave sources

2021 ◽  
Vol 506 (3) ◽  
pp. 4446-4446
Author(s):  
Hai-Liang Chen ◽  
Thomas M Tauris ◽  
Zhanwen Han ◽  
Xuefei Chen
Keyword(s):  
Gravitational Wave ◽  
White Dwarfs ◽  
Millisecond Pulsars ◽  
X Ray ◽  
X Ray Binaries

scholarly journals Formation of millisecond pulsars with helium white dwarfs, ultra-compact X-ray binaries, and gravitational wave sources

2021 ◽  
Vol 503 (3) ◽  
pp. 3540-3551 ◽  
Author(s):  
Hai-Liang Chen ◽  
Thomas M Tauris ◽  
Zhanwen Han ◽  
Xuefei Chen
Keyword(s):  
Gravitational Wave ◽  
White Dwarfs ◽  
Fine Tuning ◽  
Period Range ◽  
Millisecond Pulsars ◽  
X Ray ◽  
Close Orbit ◽  
Low Mass ◽  
Magnetic Braking ◽  
X Ray Binaries

ABSTRACT Close-orbit low-mass X-ray binaries (LMXBs), radio binary millisecond pulsars (BMSPs) with extremely low-mass helium white dwarfs (ELM He WDs) and ultra-compact X-ray binaries (UCXBs) are all part of the same evolutionary sequence. It is therefore of uttermost importance to understand how these populations evolve from one specie to another. Moreover, UCXBs are important gravitational wave (GW) sources and can be detected by future space-borne GW observatories. However, the formation and evolutionary link between these three different populations of neutron star (NS) binaries are not fully understood. In particular, a peculiar fine-tuning problem has previously been demonstrated for the formation of these systems. In this investigation, we test a newly suggested magnetic braking prescription and model the formation and evolution of LMXBs. We compute a grid of binary evolution models and present the initial parameter space of the progenitor binaries which successfully evolve all the way to produce UCXBs. We find that the initial orbital period range of LMXBs, which evolve into detached NS + ELM He WD binaries and later UCXBs, becomes significantly wider compared to evolution with a standard magnetic braking prescription, and thus helps to relieve the fine-tuning problem. However, we also find that formation of wide-orbit BMSPs is prohibited for strong versions of this new magnetic braking prescription, which therefore calls for a revision of the prescription. Finally, we present examples of the properties of UCXBs as Galactic GW sources and discuss their detection by the LISA, TianQin, and Taiji observatories.

scholarly journals Super-Eddington Accretion in the Formation of Low-Mass X-ray Binaries and Millisecond Pulsars

1997 ◽  
Vol 163 ◽  
pp. 828-829 ◽  
Author(s):  
R. F. Webbink ◽  
V. Kalogera
Keyword(s):  
Mass Transfer ◽  
Initial Phase ◽  
Transfer Rate ◽  
Birth Rate ◽  
Mass Transfer Rate ◽  
Millisecond Pulsars ◽  
X Ray ◽  
Low Mass ◽  
Orbital Periods ◽  
X Ray Binaries

AbstractConsiderations of donor star stability, age, and mass transfer rate show that low-mass X-ray binaries and binary millisecond pulsars with orbital periods longer than a few days must have survived an initial phase of super-Eddington mass transfer. We review the physical arguments leading to this conclusion, and examine its implications for the apparent discrepancy between the death rate for low-mass X-ray binaries and the birth rate of binary millisecond pulsars.

From X-ray binaries to binary and millisecond pulsars

1988 ◽  
Vol 8 (2-3) ◽  
pp. 355-365 ◽  
Author(s):  
E.P.J. van den Heuvel
Keyword(s):  
Millisecond Pulsars ◽  
X Ray ◽  
X Ray Binaries

scholarly journals Recycling Pulsars: spins, masses and ages

2012 ◽  
Vol 8 (S291) ◽  
pp. 137-140 ◽  
Author(s):  
T. M. Tauris ◽  
M. Kramer ◽  
N. Langer
Keyword(s):  
White Dwarf ◽  
Formation Process ◽  
Intermediate Mass ◽  
Millisecond Pulsars ◽  
X Ray ◽  
Spin Period ◽  
X Ray Binaries

AbstractAlthough the first millisecond pulsars (MSPs) were discovered 30 years ago we still do not understand all details of their formation process. Here, we present new results from Tauris, Langer & Kramer (2012) on the recycling scenario leading to radio MSPs with helium or carbon-oxygen white dwarf companions via evolution of low- and intermediate mass X-ray binaries (LMXBs, IMXBs). We discuss the location of the spin-up line in the PṖ–diagram and estimate the amount of accreted mass needed to obtain a given spin period and compare with observations. Finally, we constrain the true ages of observed recycled pulsars via calculated isochrones in the PṖ–diagram.

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