Determination of wind-fed model parameters of neutron stars in high-mass X-ray binaries

Taani, Ali; Karino, Shotaro; Song, Liming; Zhang, Chengmin; Chaty, S.

doi:10.1017/pasa.2022.32

Cited by 4 publications

(2 citation statements)

References 81 publications

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“…Based on these interesting results, Nagakura, Burrows, & Vartanyan (2021) estimated the amount of the gravitational mass of the NS, which is ∼ 1.2M ⊙ . This result is consistent with the NS observations made by Özel & Freire (2016); Taani, Karino, Song, Zhang, & Chaty (2022).…”

Section: The Companionsupporting

confidence: 93%

The binding energy produced within the framework of the accretion of millisecond pulsars

Taani¹

2023

Preprint

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The role and implication of binding energy through the accretion-induced collapse (AIC) of accreting white dwarfs (WDs) for the production of millisecond pulsars (MSPs) are investigated. I examine the binding energy model due to the dynamical process in close binary systems and investigating the possible mass of the companion sufficient to induce their orbital parameters. The deterministic nature of this interaction has a strong sensitivity to the equation of state of the binary systems (where the compactness of a neutron star is proportional to the amount of binding energy) associated with their initial conditions. This behavior will mimic the commonly assumed mass and amount of accreted matter under the instantaneous mass loss (Δ ∼ 0.18 ⊙ ). As a result, this will indicate an increase in the MSP's gravitational mass due to angular momentum losses. The outcome of such a system will then be a circular binary MSP in which the companion is a low-mass WD, thus distinguishing the binary formation scenarios. In addition, the results of this work could provide constraints on the expected mass and binding energy of a neutron star based on the accretion rate.

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Section: The Companionsupporting

confidence: 93%

The binding energy produced within the framework of the accretion of millisecond pulsars

Taani¹

2023

Preprint

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“…[49] estimated the amount of the gravitational mass of the NS, which is . This result is consistent with the NS observations made by [50,51].…”

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confidence: 93%

Binding energy produced within the framework of the accretion of millisecond pulsars

Taani¹

2023

Chinese Phys. C

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The role and implication of binding energy through the accretion-induced collapse (AIC) of accreting white dwarfs (WDs) for the production of millisecond pulsars (MSPs) are investigated. I examine the binding energy model due to the dynamical process in close binary systems and investigate the possible mass companion sufficient to induce their orbital parameters. The deterministic nature of this interaction has a strong sensitivity to the equation of state of the binary systems (where the compactness of a neutron star is proportional to the amount of binding energy) associated with their initial conditions. This behavior will mimic the commonly assumed mass and amount of accreted matter under the instantaneous mass loss (M í 0:18Mæ). As a result, this will indicate an increase in the MSP’s gravitational mass due to the angular momentum losses. The outcome of such a system will then be a circular binary MSP in which the companion is a low-mass WD, thus distinguishing the binary formation scenarios. I have shown that it is possible to add some constraints on the expected values of the mass and binding energy of a neutron star depending on the accretion rate.

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Speckle-interferometric Study of Close Visual Binary System HIP 11253 (HD 14874) using Gaia (DR2 and EDR3)

Al-jboor¹,

Taani

2023

Res. Astron. Astrophys.

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We present a comprehensive set of physical and geometrical parameters for each of the components of the close visual binary system Hip 11253 (HD14874). We present an analysis for the binary and multiple stellar systems with the aim to obtain a match between the overall observational spectral energy distribution of the system and the spectral synthesis created from model atmospheres. The epoch positions are used to determine the orbital parameters and the total mass. The parameters of both components are derived as: , , , , , , , . Our analysis shows that the spectral types of both are F9a and K3b . By combining the orbital solution with the parallax measurements of Gaia DR2 and EDR3, we estimate the individual masses using H-R diagram Ma=1.09M⨀ and Mb=0.59M⨀ for using Gaia DR2 parallax and Ma=1.10M⨀ and Mb=0.61M⨀ for using Gaia EDR3 parallax. Finally, the location of both system’s components on the stellar evolutionary tracks is presented.

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Determination of wind-fed model parameters of neutron stars in high-mass X-ray binaries

Cited by 4 publications

References 81 publications

The binding energy produced within the framework of the accretion of millisecond pulsars

The binding energy produced within the framework of the accretion of millisecond pulsars

Binding energy produced within the framework of the accretion of millisecond pulsars

Speckle-interferometric Study of Close Visual Binary System HIP 11253 (HD 14874) using Gaia (DR2 and EDR3)

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