Modelling the interaction between relativistic and non-relativistic winds in binary pulsar systems: strong magnetization of the pulsar wind

Bogovalov, S. V.; Khangulyan, D.; Koldoba, A. V.; Ustyugova, G. V.; Aharonian, F.

doi:10.1093/mnras/stz2815

Cited by 20 publications

(13 citation statements)

References 92 publications

(144 reference statements)

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“…A natural improvement of the developed model could consist in a further extension of Cronos to incorporate SRMHD. As it was suggested by various works including this one, the magnetisation of the pulsar wind is significant and should no longer be neglected in the dynamics of the wind interaction Bogovalov et al, 2019). Such an extension can be integrated seamlessly into the existing framework, as the respective interfaces have already been foreseen.…”

Section: Future Prospectsmentioning

confidence: 98%

“…The relevant interfaces have already been foreseen while implementing the current version of the code. With this, we will be able to additionally investigate the influence of the pulsar and stellar magnetic fields on the fluid flow (see also Bogovalov et al, 2019).…”

Section: Relativistic Hydrodynamicsmentioning

confidence: 99%

“…In this work, we extend this approach to gamma-ray binaries by translating the previous simulations into a relativistic framework, but we neglect the possible effect of the pulsar and stellar magnetic field on the fluid flow at this stage Bogovalov et al 2019). This allows a production of emitting particle distributions that is consistent with the dynamics of the wind interaction; this has not been attempted in the case of gamma-ray binaries before.…”

Section: Introductionmentioning

confidence: 99%

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Relativistic fluid modelling of gamma-ray binaries

Huber

Kissmann

Reimer

et al. 2021

A&A

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Context. Gamma-ray binaries are systems that radiate the dominant part of their non-thermal emission in the gamma-ray band. In a wind-driven scenario, these binaries are thought to consist of a pulsar orbiting a massive star, accelerating particles in the shock arising in the wind collision. Aims. We develop a comprehensive numerical model for the non-thermal emission of shock-accelerated particles including the dynamical effects of fluid instabilities and orbital motion. We demonstrate the model on a generic binary system. Methods. The model was built on a dedicated three-dimensional particle transport simulation for the accelerated particles that were dynamically coupled to a simultaneous relativistic hydrodynamic simulation of the wind interaction. In a post-processing step, a leptonic emission model involving synchrotron and inverse-Compton emission was evaluated based on resulting particle distributions and fluid solutions, consistently accounting for relativistic boosting and γγ-absorption in the stellar radiation field. The model was implemented as an extension to the CRONOS code. Results. In the generic binary, the wind interaction leads to the formation of an extended, asymmetric wind-collision region distorted by the effects of orbital motion, mixing, and turbulence. This gives rise to strong shocks terminating the pulsar wind and secondary shocks in the turbulent fluid flow. With our approach it is possible for the first time to consistently account for the dynamical shock structure in particle transport processes, which yields a complex distribution of accelerated particles. The predicted emission extends over a broad energy range, with significant orbital modulation in all bands.

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Section: Future Prospectsmentioning

confidence: 98%

Section: Relativistic Hydrodynamicsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Relativistic fluid modelling of gamma-ray binaries

Huber

Kissmann

Reimer

et al. 2021

A&A

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“…To account for the shocked region of the e ± -wind between the termination shock and the CD, the e ± -wind was terminated at ≈2/3 of the distance from the pulsar to the CD (see Bogovalov et al 2008 for cases with η 0.01, although if B were strong it would largely modify the overall interaction structure, see Bogovalov et al 2019). In the presence of orbital motion, analytical and numerical calculations show that a strong shock should terminate the pulsar wind due to Coriolis forces in the directions away from the star (see, e.g., Bosch-Ramon & Barkov 2011;Bosch-Ramon et al 2012Huber et al 2020).…”

Section: Modelmentioning

confidence: 99%

Properties of a hypothetical cold pulsar wind in LS 5039

Bosch‐Ramon

2021

A&A

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Context. LS 5039 is a powerful high-mass gamma-ray binary that probably hosts a young non-accreting pulsar. However, despite the wealth of data available, the means by which the non-thermal emitter is powered are still unknown. Aims. We use a dynamical-radiative numerical model, and multiwavelength data, to constrain the properties of a hypothetical pulsar wind that would power the non-thermal emitter in LS 5039. Methods. We ran simulations of an ultrarelativistic (weakly magnetized) cold e±-wind that Compton scatters stellar photons and that dynamically interacts with the stellar wind. The effects of energy losses on the unshocked e±-wind dynamics, and the geometry of the two-wind contact discontinuity, are computed for different wind models. The predicted unshocked e±-wind radiation at periastron, when expected to be the highest, is compared to LS 5039 data. Results. The minimum possible radiation from an isotropic cold e±-wind overpredicts the X-ray to gamma-ray fluxes at periastron by a factor of ∼3. In the anisotropic (axisymmetric) wind case X-ray and ≳100 MeV data are not violated by wind radiation if the wind axis is at ≲20−40° from the line of sight (chance probability of ≲6−24%), depending on the anisotropic wind model, or if the wind Lorentz factor ∈102 − 103, in which case the wind power can be higher, but it requires e±-multiplicities of ∼106 and 109 for a 10−2 s and 10 s pulsar period, respectively. Conclusions. The studied model predicts that a weakly magnetized cold pulsar e±-wind in LS 5039 should be strongly anisotropic, with either a wind Lorentz factor ∈102 − 103 and very high multiplicities or with a fine-tuned wind orientation. A weakly magnetized, cold baryon-dominated wind would be a possible alternative, but then the multiplicities should be rather low, while the baryon-to-e± energy transfer should be very efficient at wind termination. A strongly magnetized cold wind seems to be the most favorable option as it is consistent with recent research on pulsar winds and does not require fine-tuning of the pulsar wind orientation, and the wind multiplicity and Lorentz factor are less constrained.

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“…GeV flares 30 days after the passage of the periastron in 2010 [14], 2014 [13] and 2017 [15,16] are one of the most mysterious phenomena in this system. So far, the problem of the flares has not been solved [17,18]. One of the reasons for this could be our poor understanding of the physics of the outflow from Be stars.…”

Section: Introductionmentioning

confidence: 99%

Modeling of the Wind/Disk Outflow from Be Stars

Bogovalov

Petrov

2021

Universe

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The objective of this work is to reproduce the formation of the fast polar wind and viscous disk outflow from Be stars in a unified physical picture. Numerical modeling of the plasma outflow from fast rotating stars was performed taking into account the acceleration of the plasma due to scattering of the radiation of the star in lines of plasma ions and excitation of the hydrodynamic turbulence in the outflow. The fast polar wind naturally arises in this picture with an expected flow rate. For the first time, it is shown that a disk-like outflow with a relatively high level of turbulence is formed at the equator of fast rotating stars emitting radiation-driven wind. However, the level of turbulent viscosity is well below the level necessary for the formation of a Keplerian disk.

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Modelling the interaction between relativistic and non-relativistic winds in binary pulsar systems: strong magnetization of the pulsar wind

Cited by 20 publications

References 92 publications

Relativistic fluid modelling of gamma-ray binaries

Relativistic fluid modelling of gamma-ray binaries

Properties of a hypothetical cold pulsar wind in LS 5039

Modeling of the Wind/Disk Outflow from Be Stars

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