Orthogonal pulsars as a key test for pulsar evolution

Novoselov, E M; Бескин, В. С.; Galishnikova, Alisa; Michael, Rashkovetskyi,; Biryukov, A. V.

doi:10.1093/mnras/staa904

Cited by 22 publications

(8 citation statements)

References 49 publications

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“…Other, more fundamental explanations may be found in the physics relating to the generation of plasma that creates the radio emission. For instance, Novoselov et al (2020) have recently suggested that the location of plasma-generating regions above the polar cap depends sensitively on P, magnetic field strength and, in particular, α. The consequence would be, in their model, that both poles may not be associated with equally strong emission, thereby creating fewer observable interpulse pulsars than otherwise expected.…”

Section: Radio Interpulsesmentioning

confidence: 99%

The Galactic population and properties of young, highly energetic pulsars

Johnston

Smith

Karastergiou

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The population of young, non-recycled pulsars with spin down energies $\dot{E} >10^{35}$ erg s−1 is sampled predominantly at γ-ray and radio wavelengths. A total of 137 such pulsars are known, with partial overlap between the sources detectable in radio and γ-rays. We use a very small set of assumptions in an attempt to test whether the observed pulsar sample can be explained by a single underlying population of neutron stars. For radio emission we assume a canonical conal beam with a fixed emission height of 300 km across all spin periods and a luminosity law which depends on $\dot{E}^{0.25}$. For γ-ray emission we assume the outer-gap model and a luminosity law which depends on $\dot{E}^{0.5}$. We synthesise a population of fast-spinning pulsars with a birth rate of one per 100 years. We find that this simple model can reproduce most characteristics of the observed population with two caveats. The first is a deficit of γ-ray pulsars at the highest $\dot{E}$ which we surmise to be an observational selection effect due to the difficulties of finding γ-ray pulsars in the presence of glitches without prior knowledge from radio frequencies. The second is a deficit of radio pulsars with interpulse emission, which may be related to radio emission physics. We discuss the implications of these findings.

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Section: Radio Interpulsesmentioning

confidence: 99%

The Galactic population and properties of young, highly energetic pulsars

Johnston

Smith

Karastergiou

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…At the same time, their evolution is still a subject of discussion. Pulsar magnetic angle is thought to be either decreasing on the spin-down time-scale (Philippov, Tchekhovskoy & Li 2014), or, alternatively, increasing toward 90 degrees (Beskin, Gurevich & Istomin 1993;Novoselov et al 2020). In any case, for an isolated pulsar, magnetic angle as a function of time is completely determined by a single process, the pulsar losses themselves.…”

mentioning

confidence: 99%

Magnetic angle evolution in accreting neutron stars

Biryukov

Abolmasov

2021

Monthly Notices of the Royal Astronomical Society

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The rotation of a magnetised accreting neutron star (NS) in a binary system is described by its spin period and two angles: spin inclination α with respect to the orbital momentum and magnetic angle χ between the spin and the magnetic moment. Magnetospheric accretion spins the NS up and adjusts its rotation axis, decreasing α to nearly perfect alignment. Its effect upon the magnetic angle is more subtle and relatively unstudied. In this work, we model the magnetic angle evolution of a rigid spherical accreting NS. We find that the torque spinning the NS up may affect the magnetic angle while both α and χ significantly deviate from zero, and the spin-up torque varies with the phase of the spin period. As the rotation axis of the NS is being aligned with the spin-up torque, the magnetic axis becomes misaligned with the rotation axis. Under favourable conditions, magnetic angle may increase by Δχ ∼ 15○ − 20○. This orthogonalisation may be an important factor in the evolution of millisecond pulsars, as it partially compensates the χ decrease potentially caused by pulsar torques. If the direction of the spin-up torque changes randomly with time, as in wind-fed high-mass X-ray binaries, both the rotation axis of the NS and its magnetic axis become involved in a non-linear random-walk evolution. The ultimate attractor of this process is a bimodal distribution in χ peaking at χ = 0 and χ = 90○.

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“…Note that other spin evolution laws have been proposed, see e.g. Novoselov et al (2020) and references therein. Both period and period derivative are measured with large precision: period is typically known with relative error of 10 −14 and period derivative with relative error of 10 −6 , which translates to negligible uncertainty in 𝐵 𝑝 when other parameters fixed.…”

Section: Magnetic Field Distribution Of Neutron Starsmentioning

confidence: 99%

Initial periods and magnetic fields of neutron stars

Igoshev,

Frantsuzova,

Gourgouliatos

et al. 2022

Preprint

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Initial distributions of pulsar periods and magnetic fields are essential components of multiple modern astrophysical models. Not enough work has been done to properly constrain these distributions using direct measurements. Here we aim to fill this gap by rigorously analysing properties of young neutron stars associated to supernova remnants. In order to perform this task, we compile a catalogue of 56 neutron stars uniquely paired to supernova remnants with known age estimate. Further, we analyse this catalogue using multiple statistical techniques. We found that distribution of magnetic fields and periods for radio pulsars are both well described using the log-normal distribution. The mean magnetic field is log 10 [𝐵/G] = 12.44 and standard deviation is 𝜎 𝐵 = 0.44. Magnetars and central compact objects do not follow the same distribution. The mean initial period is log 10 𝑃 0 [𝑃/s] = −1.04 +0.15 −0.2 and standard deviation is 𝜎 𝑝 = 0.53 +0.12 −0.08 . We show that the normal distribution does not describe the initial periods of neutron stars sufficiently well. Parameters of the initial period distribution are not sensitive to the exact value of the braking index.

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Orthogonal pulsars as a key test for pulsar evolution

Cited by 22 publications

References 49 publications

The Galactic population and properties of young, highly energetic pulsars

The Galactic population and properties of young, highly energetic pulsars

Magnetic angle evolution in accreting neutron stars

Initial periods and magnetic fields of neutron stars

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