Formation of Scorpius X-1 induced by anomalous magnetic braking of Ap/Bp stars

Chen, Wen-Cong

doi:10.1051/0004-6361/201630239

Cited by 7 publications

(1 citation statement)

References 39 publications

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“…Subsequently, there is a period of mass transfer as an intermediate-mass X-ray binary (IMXB), during which the secondary loses some mass through ac-cretion and ablation processes. Such an IMXB phase has also been suggested to have occurred during the evolution of Sco X-1 (Chen 2017). Towards the end of the IMXB phase, Roche lobe overflow can lead to a period of dynamically unstable mass transfer and the creation of a CE (Lazarus et al 2013).…”

Section: Nature Of the Companion Starmentioning

confidence: 89%

X-ray Eclipse Mapping Constrains the Binary Inclination and Mass Ratio of Swift J1858.6-0814

Knight,

Ingram,

Middleton

2022

Preprint

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X-ray eclipse mapping is a promising modelling technique, capable of constraining the mass and/or radius of neutron stars (NSs) or black holes (BHs) in eclipsing binaries and probing any structure surrounding the companion star. In eclipsing systems, the binary inclination, 𝑖, and mass ratio, 𝑞 relate via the duration of totality, 𝑡 e . The degeneracy between 𝑖 and 𝑞 can then be broken through detailed modelling of the eclipse profile. Here we model the eclipses of the NS low-mass X-ray binary Swift J1858.6-0814 utilising archival NICER observations taken while the source was in outburst. Analogous to EXO 0748−676, we find evidence for irradiation driven ablation of the companion's surface by requiring a layer of stellar material to surround the companion star in our modelling. This material layer extends ∼ 7000 − 14000 km from the companion's surface and is likely the cause of the extended, energy-dependent and asymmetric ingress and egress that we observe. Our fits return an inclination of 𝑖 ∼ 81 • and a mass ratio 𝑞 ∼ 0.14. Using Kepler's law to relate the mass and radius of the companion star via the orbital period (∼ 21.3 hrs), we subsequently determine the companion to have a low mass in the range 0.183 𝑀 ≤ 𝑀 cs ≤ 0.372 𝑀 and a large radius in the range 1.02 𝑅 ≤ 𝑅 cs ≤ 1.29 𝑅 . Our results, combined with future radial velocity amplitudes measured from stellar absorption/emission lines, can place precise constraints on the component masses in this system.

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Section: Nature Of the Companion Starmentioning

confidence: 89%

X-ray Eclipse Mapping Constrains the Binary Inclination and Mass Ratio of Swift J1858.6-0814

Knight,

Ingram,

Middleton

2022

Preprint

View full text Add to dashboard Cite

show abstract

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

Chen

Tauris

Han

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Close-orbit low-mass X-ray binaries (LMXBs), radio binary millisecond pulsars (BMSPs) with extremely low-mass helium WDs (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.

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X-ray eclipse mapping constrains the binary inclination and mass ratio of Swift J1858.6−0814

Knight¹,

Ingram²,

Middleton³

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

X-ray eclipse mapping is a promising modelling technique, capable of constraining the mass and/or radius of neutron stars (NSs) or black holes (BHs) in eclipsing binaries and probing any structure surrounding the companion star. In eclipsing systems, the binary inclination, i, and mass ratio, q relate via the duration of totality, te. The degeneracy between i and q can then be broken through detailed modelling of the eclipse profile. Here we model the eclipses of the NS low-mass X-ray binary Swift J1858.6-0814 utilising archival NICER observations taken while the source was in outburst. Analogous to EXO 0748−676, we find evidence for irradiation driven ablation of the companion’s surface by requiring a layer of stellar material to surround the companion star in our modelling. This material layer extends ∼7000 − 14000 km from the companion’s surface and is likely the cause of the extended, energy-dependent and asymmetric ingress and egress that we observe. Our fits return an inclination of i ∼ 81○ and a mass ratio q ∼ 0.14. Using Kepler’s law to relate the mass and radius of the companion star via the orbital period (∼21.3 hrs), we subsequently determine the companion to have a low mass in the range 0.183 M⊙ ≤ Mcs ≤ 0.372 M⊙ and a large radius in the range 1.02 R⊙ ≤ Rcs ≤ 1.29 R⊙. Our results, combined with future radial velocity amplitudes measured from stellar absorption/emission lines, can place precise constraints on the component masses in this system.

show abstract

Formation of Scorpius X-1 induced by anomalous magnetic braking of Ap/Bp stars

Cited by 7 publications

References 39 publications

X-ray Eclipse Mapping Constrains the Binary Inclination and Mass Ratio of Swift J1858.6-0814

X-ray Eclipse Mapping Constrains the Binary Inclination and Mass Ratio of Swift J1858.6-0814

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

X-ray eclipse mapping constrains the binary inclination and mass ratio of Swift J1858.6−0814

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