Statistics of interpulse radio pulsars: the key to solving the alignment/counter-alignment problem

Arzamasskiy, Lev; Бескин, В. С.; Pirov, Khurram K.

doi:10.1093/mnras/stw3139

Cited by 15 publications

(18 citation statements)

References 40 publications

(72 reference statements)

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“…Remember that according to Arzamasskiy et al (2017) within MHD model the distribution function NMHD(P, χ) (47) reproduces good enough the number of both aligned and orthogonal interpulse pulsars. In particular, the number of orthogonal pulsars in the range 0.03 s < P < 0.5 s is 18 ÷ 40, in good agreement with observations (see Table 1).…”

Section: Approximately Orthogonal Pulsarsmentioning

confidence: 92%

“…The analysis produced by Arzamasskiy et al (2017) have shown that the number of observable interpulse pulsars with χ ≈ 0 • can be explained within both BGI (counteralignment) and MHD (alignment) models due to considerable uncertainties in the initial pulsar distribution Q(P, χ). In turn, this approach gave us the possibility to evaluate birth functions QP (P ) and Qχ(χ) on pulsar initial periods 1 In Table 1 we use the normalization for the total number of pulsars in the corresponding range of pulsar periods P .…”

Section: Kinetic Equation Methodsmentioning

confidence: 99%

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Orthogonal pulsars as a key test for pulsar evolution

Novoselov

Бескин

Galishnikova

et al. 2020

Monthly Notices of the Royal Astronomical Society

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At present, there is no direct information about evolution of inclination angle χ between magnetic and rotational axes in radio pulsars. As to theoretical models of pulsar evolution, they predict both the alignment, i.e. evolution of inclination angle χ to 0 • , and its counter-alignment, i.e. evolution to 90 • . In this paper, we demonstrate that the statistics of interpulse pulsars can give us the key test to solve the alignment/counteralignment problem as the number of orthogonal interpulse pulsars (χ ≈ 90 • ) drastically depends on the evolution trajectory.

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Section: Approximately Orthogonal Pulsarsmentioning

confidence: 92%

Section: Kinetic Equation Methodsmentioning

confidence: 99%

Orthogonal pulsars as a key test for pulsar evolution

Novoselov

Бескин

Galishnikova

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…models of pulsar evolution predict both the alignment and counter-alignment of the magnetic and rotational axes but neither of these two possibilities has been convincingly justified by observations (see e.g. Arzamasskiy et al 2017, and references therein). We cannot discern between the two cases either.…”

Section: Spectra Of J0633 and Its Pwnmentioning

confidence: 99%

XMM–Newton observations of a gamma-ray pulsar J0633+0632: pulsations, cooling and large-scale emission

Danilenko

Карпова

Ofengeim

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report results of XMM-Newton observations of a γ-ray pulsar J0633+0632 and its wind nebula. We reveal, for the first time, pulsations of the pulsar X-ray emission with a single sinusoidal pulse-profile and a pulsed fraction of 23 ± 6 per cent in the 0.3-2 keV band. We confirm previous Chandra findings that the pulsar X-ray spectrum consists of thermal and non-thermal components. However, we do not find the absorption feature that was previously detected at about 0.8 keV. Thanks to the greater sensitivity of XMM-Newton, we get stronger constraints on spectral model parameters compared to previous studies. The thermal component can be equally well described by either blackbody or neutron star atmosphere models, implying that this emission is coming from either hot pulsar polar caps with a temperature of about 120 eV or from the colder bulk of the neutron star surface with a temperature of about 50 eV. In the latter case, the pulsar appears to be one of the coolest among other neutron stars of similar ages with estimated surface temperatures. We discuss cooling scenarios relevant to this neutron star. Using an interstellar absorption-distance relation, we also constrain the distance to the pulsar to the range of 0.7-2 kpc. Besides the pulsar and its compact nebula, we detect regions of weak large-scale diffuse non-thermal emission in the pulsar field and discuss their possible nature.

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“…As a result, the velocity of the resulting neutron star can differ significantly from the velocity of nearby stars. Therefore, a significant part of the pulsars is distributed in a disk that is about 3 times thicker than the disk of stars (Payne-Gaposchkin 1979; Arzamasskiy et al 2017).…”

Section: Other Features Of Relict Neutron Starsmentioning

confidence: 99%

Black Holes and Neutron Stars in an Oscillating Universe

Gorkavyi,

Tyul'bashev

2021

Preprint

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In recent years, hypotheses about a cyclical Universe have been again actively considered. In these cosmological theories, the Universe, instead of a "one-time" infinite expansion, periodically shrinks to a certain volume, and then again experiences the Big Bang. One of the problems for the cyclic Universe will be its compatibility with a vast population of indestructible black holes that accumulate from cycle to cycle. The article considers a simple iterative model of the evolution of black holes in a cyclic Universe, independent of specific cosmological theories. The model has two free parameters that determine the iterative decrease in the number of black holes and the increase in their individual mass. It is shown that this model, with wide variations in the parameters, explains the observed number of supermassive black holes at the centers of galaxies, as well as the relationships between different classes of black holes. The mechanism of accumulation of relict black holes during repeated pulsations of the Universe may be responsible for the black hole population detected by LIGO observations and probably responsible for the dark matter phenomenon. The number of black holes of intermediate masses corresponds to the number of globular clusters and dwarf satellite galaxies. These results argue for models of the oscillating Universe, and at the same time impose substantial requirements on them. Models of a pulsating Universe should be characterized by a high level of relict gravitational radiation generated at the time of maximum compression of the Universe and mass mergers of black holes, as well as solve the problem of the existence of the largest black hole that is formed during this merger. It has been hypothesized that some neutron stars can survive from past cycles of the Universe and contribute to dark matter. These relict neutron stars will have a set of features by which they can be distinguished from neutron stars born in the current cycle of the birth of the Universe. The observational signs of relict neutron stars and the possibility of their search in different wavelength ranges are discussed.

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Statistics of interpulse radio pulsars: the key to solving the alignment/counter-alignment problem

Cited by 15 publications

References 40 publications

Orthogonal pulsars as a key test for pulsar evolution

Orthogonal pulsars as a key test for pulsar evolution

XMM–Newton observations of a gamma-ray pulsar J0633+0632: pulsations, cooling and large-scale emission

Black Holes and Neutron Stars in an Oscillating Universe

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