Neutron-star measurements in the multi-messenger Era

Ascenzi, Stefano; Graber, Vanessa; Rea, Nanda

doi:10.1016/j.astropartphys.2024.102935

Cited by 6 publications

(2 citation statements)

References 442 publications

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“…Detectability of the f -mode oscillations. The f -mode is the fundamental non-radial mode of a NS with typical frequencies lying in the 1.5 − 3 kHz range, along with a damping time of 0.1 − 0.5 s [9,11,24,25,137]. The detection of gravitational waves arising from f -mode oscillations by different detectors depends on the mode energy of those oscillations.…”

Section: Jcap04(2024)065mentioning

confidence: 99%

Probing the impact of delta-baryons on nuclear matter and non-radial oscillations in neutron stars

Kalita,

Routaray,

Ghosh

et al. 2024

J. Cosmol. Astropart. Phys.

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Non-radial oscillations of Neutron Stars (NSs) provide a means to learn important details regarding their interior composition and equation of state. We consider the effects of Δ-baryons on non-radial f-mode oscillations and other NS properties within the Density-Dependent Relativistic Mean Field formalism. Calculations are performed for Δ-admixed NS matter with and without hyperons. Our study of the non-radial f-mode oscillations revealed a distinct increase in frequency due to the addition of the Δ-baryons with upto 20% increase in frequency being seen for canonical NSs. Other bulk properties of NSs, including mass, radii, and dimensionless tidal deformability (Λ) were also affected by these additional baryons. Comparing our results with available observational data from pulsars (NICER) and gravitational waves (LIGO-VIRGO collaboration), we found strong agreement, particularly concerning Λ.

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Section: Jcap04(2024)065mentioning

confidence: 99%

Probing the impact of delta-baryons on nuclear matter and non-radial oscillations in neutron stars

Kalita,

Routaray,

Ghosh

et al. 2024

J. Cosmol. Astropart. Phys.

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“…Accretion is a widespread process occurring in various neutron star (NS) systems, such as newborn NSs within supernova envelopes (e.g., Chevalier 1989), NSs in high-mass X-ray binaries (e.g., Reig 2011), and NSs in low-mass X-ray binaries (e.g., Bhattacharya & van den Heuvel 1991), among others, contributing significantly to the evolution of the mass, spin, and magnetic field properties of the NSs (e.g., Konar 2017;Igoshev et al 2021;Abolmasov et al 2024), while concurrently producing observable radiation (e.g., Mushtukov & Tsygankov 2022;Ascenzi et al 2024). Therefore, accretion plays a crucial role in the NS populations (Harding 2013).…”

Section: Introductionmentioning

confidence: 99%

Super-Eddington Magnetized Neutron Star Accretion Flows: A Self-similar Analysis

Chen,

Dai

2024

ApJ

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The properties of super-Eddington accretion disks exhibit substantial distinctions from the sub-Eddington ones. In this paper, we investigate the accretion process of a magnetized neutron star (NS) surrounded by a super-Eddington disk. By constructing self-similar solutions for the disk structure, we study in detail an interaction between the NS magnetosphere and the inner region of the disk, revealing that this interaction takes place within a thin boundary layer. The magnetosphere truncation radius is found to be approximately proportional to the Alfvén radius, with a coefficient ranging between 0.34–0.71, influenced by the advection and twisting of a magnetic field, NS rotation, and radiation emitted from an NS accretion column. Under super-Eddington accretion, the NS can readily spin up to become a rapid rotator. The proposed model can be employed to explore the accretion and evolution of NSs in diverse astrophysical contexts, such as ultraluminous X-ray binaries or active galactic nucleus disks.

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