pith. machine review for the scientific record. sign in

arxiv: 2604.08175 · v1 · submitted 2026-04-09 · 🌌 astro-ph.HE · hep-ph

Recognition: 2 theorem links

· Lean Theorem

How many VHE gamma-ray binaries with young pulsars can be observed?

A. M. Bykov (Ioffe PTI , StPetersburg) , A. G. Kuranov (Sternberg Astronomical Institute , Moscow) , A. E. Petrov (Ioffe PTI , SPb) , K. A. Postnov (SAI Moscow)
Authors on Pith no claims yet

Pith reviewed 2026-05-10 18:38 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-ph
keywords gamma-ray binariesyoung pulsarsVHE gamma rayspopulation synthesisparticle accelerationstellar windsanisotropic emission
0
0 comments X

The pith

Stellar and pulsar wind collisions in binaries accelerate particles to PeV energies in some orbital phases, with anisotropy shaping how many systems are visible as VHE gamma-ray sources.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper performs population synthesis of Galactic binaries pairing a young massive OB or Be star with a pulsar to estimate the number of systems capable of producing observable very high energy gamma rays. It incorporates distributions of eccentricities, orbital periods, Be-disk inclinations, and pulsar braking losses while modeling conditions for particle acceleration, radiation, and photon absorption. The interaction between the star's strongly magnetized wind and the pulsar's relativistic outflow creates a zone that can reach PeV energies at favorable configurations. Anisotropy in this zone affects emission direction and absorption, thereby influencing the count of detectable gamma-ray loud binaries.

Core claim

The stellar winds with strong (~ Gauss) magnetic fields at ~ AU distances colliding with powerful pulsar outflows are capable of accelerating particles up to PeV energies at some orbital configurations and phases. The strong magnetic field in the interaction region produces a highly anisotropic structure of the particle accelerator and emitter in the pulsar outflow. The anisotropic radiation pattern may affect the gamma-ray photon absorption and the number of the observed gamma-ray loud systems.

What carries the argument

The anisotropic structure of the interaction zone between the relativistic pulsar wind and the strongly magnetized massive star's wind, which enables PeV particle acceleration and directional emission.

If this is right

  • Certain orbital periods and eccentricities allow particle acceleration to PeV energies during specific phases of the orbit.
  • Anisotropy in the emission and absorption reduces the fraction of systems that appear as gamma-ray loud to a distant observer.
  • The synthesis yields an estimate for the total number of potentially observable VHE gamma-ray binaries in the Galaxy.
  • Multi-wavelength data on known binaries can test the modeled conditions for acceleration and visibility.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Targeted observations at predicted orbital phases could raise detection rates of new VHE sources beyond current blind surveys.
  • The same wind-collision physics could apply to black-hole companions, broadening the census of gamma-ray binaries.
  • PeV acceleration in these systems offers a possible contribution to the high-energy end of the Galactic cosmic-ray spectrum.

Load-bearing premise

The assumed distributions of binary eccentricities, orbital periods, Be-disk inclinations, and pulsar braking energy losses, together with the modeled conditions for VHE particle acceleration and anisotropic emission in the wind-interaction zone, correctly capture the physics that determines observability.

What would settle it

A statistical mismatch between the predicted number and phase-dependent detectability of VHE gamma-ray binaries and the actual count or variability patterns found in observations of known pulsar systems would falsify the central claim.

Figures

Figures reproduced from arXiv: 2604.08175 by A. E. Petrov (Ioffe PTI, A. G. Kuranov (Sternberg Astronomical Institute, A. M. Bykov (Ioffe PTI, K. A. Postnov (SAI Moscow), Moscow), SPb), StPetersburg).

Figure 1
Figure 1. Figure 1: Simulated Galactic populations of massive binary systems with pulsars for the assumed Galactic star formation rate 2 M⊙/yr. Left and right panels show, respectively, the differential distribution of the Be+PSR and OB+PSR binaries over the optical star mass M2 and the orbital period Porb (top row) and over Porb (bottom row). For Be+PSR systems (left columns), blue and red curves show differential distributi… view at source ↗
Figure 2
Figure 2. Figure 2: Simulated population of Galactic pulsar+Be-type star binaries for the neutron star surface magnetic field distributed according to Eq. (3) with log B0 = 12.6 and σµ = 0.55. Shown are model distributions of Be+PSR systems over the optical companion mass M2 and the orbital period Porb (top row) and over Porb (bottom row). Left panels: distribution of the Galactic formation rate of Be+PSR binaries (per year).… view at source ↗
Figure 3
Figure 3. Figure 3: Model distribution of Galactic number of binary systems with pulsars over the spin-down power of pulsars (in units E˙ 30 = 1030 erg s−1 ) and the neutron star spin period PNS for Be+PSR (top panels) and OB+PSR (bottom panels) binaries. 9 [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Estimate of the magnetic field amplitude in the gamma-ray binary LS 5039. Color curves show a typical energy of synchrotron photons produced by electrons of different energies E cw f max (fixed for each curve) as a function of the magnetic field in the emission site B. E cw f max is the maximum energy available in particle acceleration in colliding winds of the binary. Different colors correspond to differ… view at source ↗
Figure 5
Figure 5. Figure 5: Model distributions of Galactic Be+PSR binaries over eccentricity e and orbital periastron distance Rmin = a (1 − e) (a is the orbital semi￾major axis in units of solar radius). As in Fig.2, the left columns show the distribution of Be+PSR formation rate (per year), the middle columns show the average time the systems spent in the particular parameter bin (in Myrs), and the right columns is the number dist… view at source ↗
Figure 6
Figure 6. Figure 6: Model distributions of pulsar+Be-star binaries over angle µ between the spin axis of the massive star and the orbital angular momentum. Top panel: the kick velocity produced in the parent supernova explosion is distributed isotropically for 0◦ < θ0 < 180◦ , where θ0 is measured from the pre-supernova spin axis. Bottom panel: the kick is isotropic within a narrow cone with 0◦ < θ0 < 10◦ . The distributions … view at source ↗
Figure 7
Figure 7. Figure 7: Relativistic MHD simulations of the collision zone of two winds in a gamma-ray binary (performed using code PLUTO [71]). Shown is the structure of the magnetic field B (in Gauss) produced in modeling of the pulsar wind nebula inflation in a strongly magnetized locally uniform stellar wind flow. The results of 3D simulation are shown in two cuts: meridional (left columns) and equatorial (right columns). The… view at source ↗
Figure 8
Figure 8. Figure 8: Estimates of particle’s mean free path (mfp) in the simu￾lated structure of the bubble of a pulsar wind nebula blown in a dense magnetized stellar wind in a binary system. Shown is the map of mfp calculated in the Bohm diffusion approximation λ = Rg = E/eB for particles with energy E = 50 TeV. The map is calculated using the simulated map of the magnetic field amplitude, the mfp in each point is computed u… view at source ↗
Figure 9
Figure 9. Figure 9: Typical times of radiative energy losses for leptons acceler￾ated in the collision winds zone in a gamma-ray binary and propagat￾ing in the stellar wind. Shown is the dependence of loss times on the particle energy for synchrotron (red curves), inverse Compton (blue curves) and synchrotron + inverse Compton radiation (black curves). Note that estimates are calculated for averaged fields – magnetic field an… view at source ↗
Figure 10
Figure 10. Figure 10: Top: sketch of acceleration and escape from the accelerator of leptons accelerated in the magnetized structure of a PWN bubble inflated in a strongly magnetized stellar wind in a massive binary system. The results of rMHD-PIC simulation of particle transport are superimposed on the gray-color map of the simulated magnetic structure. Middle: the result of rMHD-PIC simulation of propagation of PeV protons a… view at source ↗
read the original abstract

A population of Galactic gamma-ray binaries is currently emerging due to ever increasing sensitivity of gamma-ray observatories. The detection of very high energy (VHE) photons with energies well above 10 TeV from a dozen of sources and the estimated power of those sources make them potentially interesting cosmic ray accelerators. Multi-wavelength observations of gamma-ray binaries revealed that most of them include a young massive star in pair with a relativistic companion, either a black hole or energetic pulsar. Fast stellar winds interacting with powerful relativistic outflows from pulsars or the black hole jets in microquasars are favorable sites for VHE particle acceleration. To estimate the expected number of gamma-ray binaries, we present results of population synthesis calculations of Galactic binaries in which a young massive OB- or Be-star is accompanied by a pulsar capable of producing a powerful relativistic outflow. The distributions over the binary eccentricities, orbital periods, Be-disk inclinations, and the pulsar braking energy losses are taken into account. Conditions for a binary to accelerate VHE particles, radiate and absorb the non-thermal photons that may reach the observer are discussed. We model the anisotropic structure of the zone of interaction of the relativistic pulsar wind with the strongly magnetized massive star's wind. The stellar winds with strong ($\sim$ Gauss) magnetic fields at $\sim$ AU distances colliding with powerful pulsar outflows are capable of accelerating particles up to PeV energies at some orbital configurations and phases. The strong magnetic field in the interaction region produces a highly anisotropic structure of the particle accelerator and emitter in the pulsar outflow. The anisotropic radiation pattern may affect the gamma-ray photon absorption and the number of the observed gamma-ray loud systems.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript performs population synthesis calculations for Galactic binaries consisting of a young massive OB- or Be-star paired with a pulsar to estimate the number of observable VHE gamma-ray binaries. It incorporates distributions over binary eccentricities, orbital periods, Be-disk inclinations, and pulsar braking energy losses, models the anisotropic interaction zone between the relativistic pulsar wind and the strongly magnetized stellar wind, and argues that ~Gauss magnetic fields at ~AU distances enable particle acceleration to PeV energies at certain orbital phases, with anisotropy affecting gamma-ray absorption and the count of detectable systems.

Significance. If the quantitative results hold, the work would supply a falsifiable prediction for the size of the VHE gamma-ray binary population detectable by current and future instruments (H.E.S.S., MAGIC, VERITAS, CTA), directly informing the interpretation of the dozen known sources and the role of wind-collision zones as cosmic-ray accelerators. The explicit treatment of anisotropic particle acceleration and emission is a strength that could be tested against multi-wavelength data.

major comments (2)
  1. Abstract: the central population estimate (the expected number of observable VHE gamma-ray binaries) is not reported, nor are any numerical outcomes, uncertainties, or direct comparisons to the dozen known sources supplied; without these the synthesis calculation cannot be verified or assessed for robustness.
  2. The modeling of VHE acceleration and anisotropic emission relies on the assumed distributions for eccentricity, orbital period, Be-disk inclination, and pulsar braking losses (listed as free parameters); no justification, observational priors, or sensitivity tests for these choices are visible in the provided text, which directly affects the reliability of the observability prediction.
minor comments (2)
  1. The abstract refers to 'a dozen of sources' without citing specific objects or references; adding a brief list or reference would improve context.
  2. Clarify the precise functional forms or parameter ranges used for the magnetic field strength at AU scales and the conditions for PeV acceleration in the interaction zone.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We address each major comment below and have revised the manuscript to improve clarity and completeness.

read point-by-point responses

  1. Referee: Abstract: the central population estimate (the expected number of observable VHE gamma-ray binaries) is not reported, nor are any numerical outcomes, uncertainties, or direct comparisons to the dozen known sources supplied; without these the synthesis calculation cannot be verified or assessed for robustness.

    Authors: We agree that the abstract should report the key quantitative outcome. In the revised manuscript we have updated the abstract to state the estimated number of observable VHE gamma-ray binaries, the associated uncertainties, and a direct comparison with the dozen known sources. revision: yes

  2. Referee: The modeling of VHE acceleration and anisotropic emission relies on the assumed distributions for eccentricity, orbital period, Be-disk inclination, and pulsar braking losses (listed as free parameters); no justification, observational priors, or sensitivity tests for these choices are visible in the provided text, which directly affects the reliability of the observability prediction.

    Authors: The referee is correct that explicit justifications and sensitivity tests were not detailed in the submitted text. We have added a dedicated subsection describing the observational priors for each distribution (drawn from pulsar binary surveys and Be-star studies) with appropriate references, and we have included sensitivity tests that vary the parameters within observationally motivated ranges to show the robustness of the predicted count. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper conducts population synthesis of Galactic binaries using externally supplied input distributions for eccentricities, orbital periods, Be-disk inclinations, and pulsar braking losses, combined with a standard model of anisotropic particle acceleration and photon absorption in the pulsar-wind/stellar-wind interaction zone. No equations, fitted parameters, or results are presented that reduce the predicted number of observable VHE systems to a self-defined quantity, a renamed fit, or a load-bearing self-citation chain. The central estimate therefore rests on independent assumptions and external physics rather than internal redefinition or circular closure.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The estimate depends on input distributions for orbital and pulsar parameters plus domain assumptions about wind magnetization and particle acceleration efficiency; no new entities are postulated and no parameters are fitted to the output count itself.

free parameters (4)
  • binary eccentricity distribution
    Used as input to the population synthesis
  • orbital period distribution
    Used as input to the population synthesis
  • Be-disk inclination distribution
    Used as input to the population synthesis
  • pulsar braking energy losses distribution
    Used as input to the population synthesis
axioms (2)
  • domain assumption Stellar winds with strong magnetic fields at AU distances can accelerate particles to PeV energies when colliding with pulsar outflows
    Invoked to justify VHE emission capability at certain orbital phases
  • domain assumption The anisotropic structure of the wind-interaction zone governs gamma-ray absorption and observability
    Central to the modeling of detectable systems

pith-pipeline@v0.9.0 · 5647 in / 1487 out tokens · 56502 ms · 2026-05-10T18:38:29.275361+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

79 extracted references · 67 canonical work pages · 1 internal anchor

  1. [2]

    Bosch-Ramon, D

    V . Bosch-Ramon, D. Khangulyan, Under- standing the V ery-High Emission from Micro- quasars, International Journal of Modern Physics D 18 (2009) 347–387. doi: 10.1142/ S0218271809014601. arXiv:0805.4123

    work page arXiv 2009

  2. [3]

    doi: 10.48550/arXiv.2410

    LHAASO Collaboration, Ultrahigh-Energy Gamma-ray Emission Associated with Black Hole-Jet Systems, arXiv e-prints (2024) arXiv:2410.08988. doi: 10.48550/arXiv.2410. 08988. arXiv:2410.08988

    work page doi:10.48550/arxiv.2410 2024

  3. [4]

    Dubus, Gamma-ray binaries: pul- sars in disguise?, A&A 456 (2006) 801–

    G. Dubus, Gamma-ray binaries: pul- sars in disguise?, A&A 456 (2006) 801–

    2006

  4. [5]

    arXiv:astro-ph/0605287

    doi: 10.1051/0004-6361:20054779. arXiv:astro-ph/0605287

    work page doi:10.1051/0004-6361:20054779

  5. [6]

    Dubus, Gamma-ray binaries and re- lated systems, Astron

    G. Dubus, Gamma-ray binaries and re- lated systems, Astron. Astroph. Reviews 21 (2013) 64. doi: 10.1007/s00159-013-0064-5 . arXiv:1307.7083

    work page doi:10.1007/s00159-013-0064-5 2013

  6. [7]

    G. E. Romero, M. Boettcher, S. Marko ff, F. Tavec- chio, Relativistic Jets in Active Galactic Nuclei and Microquasars, Space Sci. Rev. 207 (2017) 5–61. doi: 10.1007/s11214-016-0328-2 . arXiv:1611.09507

    work page doi:10.1007/s11214-016-0328-2 2017

  7. [9]

    S. S. Kimura, K. Tomida, M. I. N. Kobayashi, K. Kin, B. Zhang, Isolated Black Holes as Po- tential PeV atrons and Ultrahigh-energy Gamma- Ray Sources, ApJ 981 (2025) L36. doi: 10.3847/ 2041-8213/adb841. arXiv:2412.08136

    work page arXiv 2025

  8. [10]

    Lhaaso Collaboration, Z. Cao, F. Aharonian, Q. An, Axikegu, L. X. Bai, Y . X. Bai, Y . W. Bao, D. Bastieri, X. J. Bi, Y . J. Bi, H. Cai, J. T. Cai, 21 Z. Cao, J. Chang, J. F. Chang, B. M. Chen, E. S. Chen, J. Chen, L. Chen, L. Chen, L. Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. L. Chen, Y . Chen, N. Cheng, Y . D. Chen...

    work page arXiv 2021

  9. [11]

    Amato, B

    E. Amato, B. Olmi, The Crab Pulsar and Nebula as Seen in Gamma-Rays, Universe 7 (2021) 448. doi: 10.3390/universe7110448. arXiv:2111.07712

    work page doi:10.3390/universe7110448 2021

  10. [12]

    Aleksi ´c, S

    J. Aleksi ´c, S. Ansoldi, L. A. Antonelli, P . An- toranz, A. Babic, P . Bangale, J. A. Barrio, J. Becerra González, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. Carosi, P . Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P . Da V ela, F. Dazzi, A. De Angelis, G. D...

    work page doi:10.1051/0004-6361/201424261 2014

  11. [13]

    A. M. Bykov, A. E. Petrov, M. E. Kalyashova, S. V . Troitsky, PeV Photon and Neutrino Flares from Galactic Gamma-Ray Binaries, ApJ 921 (2021) L10. doi: 10.3847/2041-8213/ac2f3d. arXiv:2110.11189

    work page doi:10.3847/2041-8213/ac2f3d 2021

  12. [14]

    Arons, Pulsar Wind Nebulae as Cosmic Pevatrons: A Current Sheet’s Tale, Space Sci

    J. Arons, Pulsar Wind Nebulae as Cosmic Pevatrons: A Current Sheet’s Tale, Space Sci. Rev. 173 (2012) 341–367. doi: 10.1007/ s11214-012-9885-1 . arXiv:1208.5787. 22

    work page arXiv 2012

  13. [15]

    G., Yuan, W., Macri, L

    E. de Oña Wilhelmi, R. López-Coto, E. Amato, F. Aharonian, On the Potential of Bright, Y oung Pulsars to Power Ultrahigh Gamma-Ray Sources, ApJ 930 (2022) L2. doi: 10.3847/2041-8213/ ac66cf. arXiv:2204.09440

    work page doi:10.3847/2041-8213/ 2022

  14. [16]

    Rivinius, A

    T. Rivinius, A. C. Carciofi, C. Martayan, Clas- sical Be stars. Rapidly rotating B stars with vis- cous Keplerian decretion disks, Astron. As- troph. Reviews 21 (2013) 69. doi: 10.1007/ s00159-013-0069-0 . arXiv:1310.3962

    work page arXiv 2013

  15. [17]

    F. C. Michel, Rotating Magnetospheres: an Ex- act 3-D Solution, ApJ 180 (1973) L133. doi: 10. 1086/181169

    1973

  16. [18]

    S. V . Bogovalov, On the physics of cold MHD winds from oblique rota- tors, A&A 349 (1999) 1017–1026. doi:10.48550/arXiv.astro-ph/9907051. arXiv:astro-ph/9907051

    work page doi:10.48550/arxiv.astro-ph/9907051 1999

  17. [19]

    A. M. Bykov, A. E. Petrov, G. A. Ponomaryov, K. P . Levenfish, M. Falanga, PeV proton acceler- ation in gamma-ray binaries, Advances in Space Research 74 (2024) 4276–4289. doi: 10.1016/j. asr.2024.01.021. arXiv:2401.06271

    work page doi:10.1016/j 2024

  18. [20]

    A. M. Bykov, A. E. Petrov, K. P . Levenfish, Rela- tivistic Astrospheres of Pulsars and Gamma-Ray Binaries: Modeling of Non-thermal Processes, Fluid Dynamics 59 (2024) 2377–2391. doi: 10. 1134/S0015462824605059

    2024

  19. [21]

    Lemoine, E

    M. Lemoine, E. Waxman, Anisotropy vs chemi- cal composition at ultra-high energies, JCAP 2009 (2009) 009. doi: 10.1088/1475-7516/2009/11/

    work page doi:10.1088/1475-7516/2009/11/ 2009

  20. [22]

    Bykov, N

    A. Bykov, N. Gehrels, H. Krawczynski, M. Lemoine, G. Pelletier, M. Pohl, Particle Acceleration in Relativistic Outflows, Space Sci. Rev. 173 (2012) 309–339. arXiv:1205.2208

    work page arXiv 2012

  21. [24]

    S.-S. Weng, L. Qian, B.-J. Wang, D. F. Tor- res, A. Papitto, P . Jiang, R. Xu, J. Li, J.-Z. Y an, Q.-Z. Liu, M.-Y . Ge, Q.-R. Y uan, Ra- dio pulsations from a neutron star within the gamma-ray binary LS I +61° 303, Nature Astronomy 6 (2022) 698–702. doi: 10.1038/ s41550-022-01630-1 . arXiv:2203.09423

    work page arXiv 2022

  22. [25]

    Zabalza, J

    V . Zabalza, J. M. Paredes, V . Bosch-Ramon, On the origin of correlated X-ray /VHE emission from LS I +61 303, A&A 527 (2011) A9. doi:10.1051/ 0004-6361/201015373. arXiv:1011.4489

    work page arXiv 2011

  23. [26]

    Y oneda, K

    H. Y oneda, K. Makishima, T. Enoto, D. Khangulyan, T. Matsumoto, T. Taka- hashi, Sign of Hard-X-Ray Pulsation from the γ -Ray Binary System LS 5039, Phys. Rev. Lett. 125 (2020) 111103. doi:10.1103/PhysRevLett.125.111103. arXiv:2009.02075

    work page doi:10.1103/physrevlett.125.111103 2020

  24. [28]

    J. R. Hurley, O. R. Pols, C. A. Tout, Com- prehensive analytic formulae for stellar evolution as a function of mass and metal- licity, MNRAS 315 (2000) 543–569. doi:10.1046/j.1365-8711.2000.03426.x. arXiv:astro-ph/0001295

    work page doi:10.1046/j.1365-8711.2000.03426.x 2000

  25. [29]

    J. R. Hurley, C. A. Tout, O. R. Pols, Evolu- tion of binary stars and the e ffect of tides on binary populations, MNRAS 329 (2002) 897–

    2002

  26. [30]

    doi: 10.1046/j.1365-8711.2002.05038. x. arXiv:astro-ph/0201220

    work page doi:10.1046/j.1365-8711.2002.05038 2002

  27. [31]

    Chomiuk, M

    L. Chomiuk, M. S. Povich, Toward a Uni- fication of Star Formation Rate Determinations in the Milky Way and Other Galaxies, AJ 142 (2011) 197. doi: 10.1088/0004-6256/142/ 6/197. arXiv:1110.4105

    work page doi:10.1088/0004-6256/142/ 2011

  28. [32]

    T. C. Licquia, J. A. Newman, Improved Esti- mates of the Milky Way’s Stellar Mass and Star Formation Rate from Hierarchical Bayesian Meta- Analysis, ApJ 806 (2015) 96. doi: 10.1088/ 0004-637X/806/1/96. arXiv:1407.1078

    work page arXiv 2015

  29. [33]

    H. Sana, S. E. de Mink, A. de Koter, N. Langer, C. J. Evans, M. Gieles, E. Gosset, R. G. Izzard, J.- B. Le Bouquin, F. R. N. Schneider, Binary Inter- action Dominates the Evolution of Massive Stars, Science 337 (2012) 444. doi: 10.1126/science. 1223344. arXiv:1207.6397. 23

    work page doi:10.1126/science 2012

  30. [35]

    K. A. Postnov, L. R. Y ungelson, The Evolution of Compact Binary Star Systems, Living Re- views in Relativity 17 (2014) 3. doi: 10.12942/ lrr-2014-3. arXiv:1403.4754

    work page arXiv 2014

  31. [36]

    R. F. Webbink, Double white dwarfs as progeni- tors of R Coronae Borealis stars and Type I super- novae, ApJ 277 (1984) 355–360. doi: 10.1086/ 161701

    1984

  32. [37]

    Iben, Jr., A

    I. Iben, Jr., A. V . Tutukov, Supernovae of type I as end products of the evolution of binaries with com- ponents of moderate initial mass (M not greater than about 9 solar masses), ApJS 54 (1984) 335–

    1984

  33. [38]

    A. J. Loveridge, M. V . van der Sluys, V . Kalogera, Analytical Expressions for the Envelope Binding Energy of Giants as a Function of Basic Stellar Parameters, ApJ 743 (2011) 49. doi: 10.1088/ 0004-637X/743/1/49. arXiv:1009.5400

    work page arXiv 2011

  34. [40]

    J. S. Vink, Winds from stripped low-mass helium stars and Wolf-Rayet stars, A&A 607 (2017) L8. doi: 10.1051/0004-6361/201731902. arXiv:1710.02010

    work page doi:10.1051/0004-6361/201731902 2017

  35. [41]

    2005 , month = sep, journal =

    G. Hobbs, D. R. Lorimer, A. G. Lyne, M. Kramer, A statistical study of 233 pulsar proper motions, MNRAS 360 (2005) 974–992. doi:10.1111/j.1365-2966.2005.09087.x. arXiv:astro-ph/0504584

    work page doi:10.1111/j.1365-2966.2005.09087.x 2005

  36. [43]

    Miyaji, K

    S. Miyaji, K. Nomoto, K. Y okoi, D. Sugimoto, Su- pernova triggered by electron captures., PASJ 32 (1980) 303–329

    1980

  37. [44]

    A. G. Kuranov, S. B. Popov, K. A. Postnov, Pulsar spin-velocity alignment from single and binary neutron star progenitors, MNRAS 395 (2009) 2087–2094. doi: 10.1111/j.1365-2966. 2009.14595.x. arXiv:0901.1055

    work page doi:10.1111/j.1365-2966 2009

  38. [45]

    V . M. Lipunov, K. A. Postnov, M. E. Prokhorov, The Scenario Machine: restrictions on key param- eters of binary evolution., A&A 310 (1996) 489– 507

    1996

  39. [46]

    Sce- nario Machine

    V . M. Lipunov, K. A. Postnov, M. E. Prokhorov, A. I. Bogomazov, Description of the “Sce- nario Machine”, Astronomy Reports 53 (2009) 915–940. doi: 10.1134/S1063772909100047. arXiv:0704.1387

    work page doi:10.1134/s1063772909100047 2009

  40. [47]

    M., 2006, @doi [ ] 10.1086/501516 , https://ui.adsabs.harvard.edu/abs/2006ApJ...643..332F 643, 332

    C.-A. Faucher-Giguère, V . M. Kaspi, Birth and Evolution of Isolated Radio Pulsars, ApJ 643 (2006) 332–355. doi: 10.1086/501516. arXiv:astro-ph/0512585

    work page doi:10.1086/501516 2006

  41. [48]

    A. P . Igoshev, S. B. Popov, Indication of rapid magnetic field decay in X-ray dim iso- lated neutron star RX J0720.4-3125, MNRAS 535 (2024) L54–L57. doi: 10.1093/mnrasl/ slae094. arXiv:2409.03573

    work page doi:10.1093/mnrasl/ 2024

  42. [49]

    T. M. Tauris, E. P . J. van den Heuvel, Physics of Binary Star Evolution. From Stars to X-ray Binaries and Gravitational Wave Sources, 2023. doi:10.48550/arXiv.2305.09388

    work page doi:10.48550/arxiv.2305.09388 2023

  43. [50]

    Paczynski, A Polytropic Model of an Accre- tion Disk, a Boundary Layer, and a Star, ApJ 370 (1991) 597

    B. Paczynski, A Polytropic Model of an Accre- tion Disk, a Boundary Layer, and a Star, ApJ 370 (1991) 597. doi: 10.1086/169846

    work page doi:10.1086/169846 1991

  44. [51]

    Popham, R

    R. Popham, R. Narayan, Does Accretion Cease When a Star Approaches Breakup?, ApJ 370 (1991) 604. doi: 10.1086/169847

    work page doi:10.1086/169847 1991

  45. [52]

    G. S. Bisnovatyi-Kogan, A self-consistent solution for an accretion disc structure around a rapidly ro- tating non-magnetized star, A&A 274 (1993) 796

    1993

  46. [53]

    W. C. G. Ho, C. Y . Ng, A. G. Lyne, B. W. Stappers, M. J. Coe, J. P . Halpern, T. J. John- son, I. A. Steele, Multiwavelength monitoring and X-ray brightening of Be X-ray binary PSR J2032+4127/MT91 213 on its approach to peri- astron, MNRAS 464 (2017) 1211–1219. doi: 10. 1093/mnras/stw2420. arXiv:1609.06328

    work page arXiv 2017

  47. [55]

    Matchett, B

    N. Matchett, B. van Soelen, New insight into the orbital parameters of the gamma-ray binary HESS J0632 + 057, MNRAS 536 (2025) 166–173. doi:10.1093/mnras/stae2597. arXiv:2411.12499

    work page doi:10.1093/mnras/stae2597 2025

  48. [56]

    2005 , month = sep, journal =

    J. Casares, M. Ribó, I. Ribas, J. M. Pare- des, J. Martí, A. Herrero, A possible black hole in the γ-ray microquasar LS 5039, MNRAS 364 (2005) 899–908. doi:10.1111/j.1365-2966.2005.09617.x. arXiv:astro-ph/0507549

    work page doi:10.1111/j.1365-2966.2005.09617.x 2005

  49. [57]

    The origin of the formalism intrinsic degeneracies and their influence on H 0

    B. van Soelen, S. Mc Keague, D. Malyshev, M. Chernyakova, N. Komin, N. Matchett, I. M. Monageng, Improved binary solution for the gamma-ray binary 1FGL J1018.6-5856, MNRAS 515 (2022) 1078–1085. doi: 10.1093/mnras/ stac1754. arXiv:2206.11647

    work page doi:10.1093/mnras/ 2022

  50. [58]

    van Soelen, N

    B. van Soelen, N. Komin, A. Kniazev, P . Väisä- nen, The orbital parameters of the gamma- ray binary LMC P3†, MNRAS 484 (2019) 4347–4351. doi:10.1093/mnras/stz289. arXiv:1901.08911

    work page doi:10.1093/mnras/stz289 2019

  51. [61]

    D. D. Dzhappuev, Y . Z. Afashokov, I. M. Dza- parova, T. A. Dzhatdoev, E. A. Gorbacheva, I. S. Karpikov, M. M. Khadzhiev, N. F. Klimenko, A. U. Kudzhaev, A. N. Kurenya, A. S. Lidvansky, O. I. Mikhailova, V . B. Petkov, E. I. Podlesnyi, V . S. Romanenko, G. I. Rubtsov, S. V . Troitsky, I. B. Unatlokov, I. A. V aiman, A. F. Y anin, Y . V . Zhezher, K. V . Z...

    work page arXiv 2021

  52. [62]

    J. H. Grunhut, G. A. Wade, C. Neiner, M. E. Oksala, V . Petit, E. Alecian, D. A. Bohlen- der, J. C. Bouret, H. F. Henrichs, G. A. J. Hussain, O. Kochukhov, MiMeS Collaboration, The MiMeS survey of Magnetism in Massive Stars: magnetic analysis of the O-type stars, MNRAS 465 (2017) 2432–2470. doi: 10.1093/ mnras/stw2743. arXiv:1610.07895

    work page arXiv 2017

  53. [63]

    M. E. Shultz, G. A. Wade, T. Rivinius, E. Ale- cian, C. Neiner, V . Petit, S. Owocki, A. ud- Doula, O. Kochukhov, D. Bohlender, Z. Keszthe- lyi, MiMeS Collaboration, BinaMIcS Collab- oration, The magnetic early B-type stars - III. A main-sequence magnetic, rotational, and magnetospheric biography, MNRAS 490 (2019) 274–295. doi: 10.1093/mnras/stz2551. arXi...

    work page doi:10.1093/mnras/stz2551 2019

  54. [64]

    A. M. Bykov, E. Amato, A. E. Petrov, A. M. Krassilchtchikov, K. P . Levenfish, Pulsar Wind Nebulae with Bow Shocks: Non-thermal Ra- diation and Cosmic Ray Leptons, Space Sci. Rev. 207 (2017) 235–290. doi: 10.1007/ s11214-017-0371-7 . arXiv:1705.00950

    work page arXiv 2017

  55. [65]

    Aharonian, A

    F. Aharonian, A. G. Akhperjanian, A. R. Bazer- Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, C. Boisson, O. Bolz, V . Bor- rel, I. Braun, A. M. Brown, R. Bühler, I. Büsching, S. Carrigan, P . M. Chadwick, L. M. Chounet, R. Cornils, L. Costamante, B. Degrange, H. J. Dickinson, A. Djannati-Ataï, L. O’C. Drury, G. Dubus, K. Egberts, D. Em- manoulopou...

    work page doi:10.1051/0004-6361: 2006

  56. [66]

    J. S. Vink, Theory and Diagnostics of Hot Star Mass Loss, ARA&A 60 (2022) 203–246. doi: 10. 1146/annurev-astro-052920-094949 . arXiv:2109.08164

    work page arXiv 2022

  57. [67]

    R. M. Shannon, S. Johnston, R. N. Manchester, The kinematics and orbital dynamics of the PSR B1259-63/LS 2883 system from 23 yr of pulsar timing, MNRAS 437 (2014) 3255–3264. doi: 10. 1093/mnras/stt2123. arXiv:1311.0588

    work page arXiv 2014

  58. [68]

    Cognitive Science36(5), 757–798 (2012).https://doi.org/10.1111/j

    M. Chernyakova, A. Neronov, F. Aharonian, Y . Uchiyama, T. Takahashi, X-ray observations of PSR B1259-63 near the 2007 periastron passage, MNRAS 397 (2009) 2123–2132. doi: 10.1111/j. 1365-2966.2009.15116.x

    work page doi:10.1111/j 2007

  59. [69]

    Chernyakova, A

    M. Chernyakova, A. A. Abdo, A. Neronov, M. V . McSwain, J. Moldón, M. Ribó, J. M. Paredes, I. Sushch, M. de Naurois, U. Schwanke, Y . Uchiyama, K. Wood, S. Johnston, S. Chaty, A. Coleiro, D. Malyshev, I. Babyk, Multi- wavelength observations of the binary sys- tem PSR B1259-63 /LS 2883 around the 2010-2011 periastron passage, MNRAS 439 (2014) 432–445. doi...

    work page doi:10.1093/mnras/stu021 2010

  60. [70]

    Chernyakova, D

    M. Chernyakova, D. Malyshev, B. van Soelen, A. Finn Gallagher, N. Matchett, T. D. Russell, J. van den Eijnden, M. E. Lower, S. Johnston, S. Tsygankov, A. Salganik, I. Shebalkova, Mul- tiwavelength coverage of the 2024 periastron pas- sage of PSR B1259-63 /LS 2883, MNRAS 536 (2025) 247–253. doi:10.1093/mnras/stae2621. arXiv:2411.02128

    work page doi:10.1093/mnras/stae2621 2024

  61. [71]

    H. E. S. S. Collaboration, F. Aharonian, F. Ait Benkhali, J. Aschersleben, H. Ashkar, M. Backes, V . Barbosa Martins, R. Batzofin, Y . Becherini, D. Berge, K. Bernlöhr, M. Böttcher, C. Boisson, J. Bolmont, M. de Bony de Lavergne, J. Borowska, M. Bouyahiaoui, R. Brose, A. Brown, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, S. Caro ff, S. Casanova, J. Ce...

    work page doi:10.1051/0004-6361/202449612 2021

  62. [72]

    Bosch-Ramon, Properties of a hypothetical cold pulsar wind in LS 5039, A&A 645 (2021) A86

    V . Bosch-Ramon, Properties of a hypothetical cold pulsar wind in LS 5039, A&A 645 (2021) A86. doi: 10.1051/0004-6361/202039666. arXiv:2012.11578

    work page doi:10.1051/0004-6361/202039666 2021

  63. [73]

    2007, The Astrophysical Journal Supplement Series, 170, 228–242, doi: 10.1086/513316

    A. Mignone, G. Bodo, S. Massaglia, T. Matsakos, O. Tesileanu, C. Zanni, A. Ferrari, PLUTO: A Numerical Code for Computational Astrophysics, ApJS 170 (2007) 228–242. doi: 10.1086/513316. arXiv:astro-ph/0701854. 26

    work page doi:10.1086/513316 2007

  64. [74]

    Mbarek and D

    A. Mignone, G. Bodo, B. V aidya, G. Mat- tia, A Particle Module for the PLUTO Code. I. An Implementation of the MHD-PIC Equations, ApJ 859 (2018) 13. doi: 10.3847/1538-4357/ aabccd. arXiv:1804.01946

    work page doi:10.3847/1538-4357/ 2018

  65. [75]

    Klement, A

    R. Klement, A. C. Carciofi, T. Rivinius, L. D. Matthews, R. G. Vieira, R. Ignace, J. E. Bjorkman, B. C. Mota, D. M. Faes, A. D. Bratcher, M. Curé, S. Štefl, Revealing the structure of the outer disks of Be stars, A&A 601 (2017) A74. doi: 10.1051/ 0004-6361/201629932. arXiv:1703.07321

    work page arXiv 2017

  66. [76]

    Nikishov, Absorption of high-energy photons in the Universe, Sov

    A. Nikishov, Absorption of high-energy photons in the Universe, Sov. Phys. JETP 14 (1962) 393

    1962

  67. [77]

    Dubus, B

    G. Dubus, B. Cerutti, G. Henri, The modulation of the gamma-ray emission from the binary LS 5039, A&A 477 (2008) 691–700. doi: 10.1051/ 0004-6361:20078261. arXiv:0710.0968

    work page arXiv 2008

  68. [78]

    Neronov, M

    A. Neronov, M. Ribordy, Neutrino signal from γ- ray-loud binaries powered by high energy protons, Phys. Rev. D 79 (2009) 043013. doi: 10.1103/ PhysRevD.79.043013. arXiv:0812.0306

    work page arXiv 2009

  69. [79]

    Takata, P

    J. Takata, P . H. T. Tam, C. W. Ng, K. L. Li, A. K. H. Kong, C. Y . Hui, K. S. Cheng, High- energy Emissions from the Pulsar /Be Binary Sys- tem PSR J2032 +4127/MT91 213, ApJ 836 (2017) 241. doi: 10.3847/1538-4357/aa5c80. arXiv:1702.04446

    work page doi:10.3847/1538-4357/aa5c80 2017

  70. [80]

    T. J. Johnson, K. S. Wood, M. Kerr, R. H. D. Cor- bet, C. C. Cheung, P . S. Ray, N. Omodei, A Luminous and Highly V ariable Gamma-Ray Flare Following the 2017 Periastron of PSR B1259- 63/LS 2883, ApJ 863 (2018) 27. doi: 10.3847/ 1538-4357/aad185. arXiv:1805.03537

    work page arXiv 2017

  71. [81]

    Chernyakova, D

    M. Chernyakova, D. Malyshev, S. Mc Keague, B. van Soelen, J. P . Marais, A. Martin-Carrillo, D. Murphy, New insight into the origin of the GeV flare in the binary system PSR B1259-63 /LS 2883 from the 2017 periastron passage, MNRAS 497 (2020) 648–655. doi:10.1093/mnras/staa1876. arXiv:2005.14060

    work page doi:10.1093/mnras/staa1876 2017

  72. [82]

    Chernyakova, D

    M. Chernyakova, D. Malyshev, B. van Soelen, S. O’Sullivan, C. Sobey, S. Tsygankov, S. Mc Keague, J. Green, M. Kirwan, A. Santangelo, G. Pühlhofer, I. M. Monageng, Multi-Wavelength Properties of the 2021 Periastron Passage of PSR B1259-63, Universe 7 (2021) 242. doi: 10.3390/ universe7070242. arXiv:2106.03759

    work page arXiv 2021

  73. [83]

    Hubrig, A

    S. Hubrig, A. F. Kholtygin, L. Sidoli, M. Schöller, S. P . Järvinen, Studying the presence of mag- netic fields in a sample of high-mass X-ray bi- naries, in: L. M. Oskinova, E. Bozzo, T. Bu- lik, D. R. Gies (Eds.), High-mass X-ray Bina- ries: Illuminating the Passage from Massive Bina- ries to Merging Compact Objects, volume 346 of IAU Symposium, 2019, pp...

    2019

  74. [84]

    Hubrig, M

    S. Hubrig, M. Schöller, Magnetic Fields in O, B, and A Stars, IOP ebooks, 2021. doi: 10.1088/ 2514-3433/abefcc

    2021

  75. [87]

    Perego, A

    S. del Palacio, V . Bosch-Ramon, G. E. Romero, Gamma-ray binaries beyond one-zone mod- els: an application to LS 5039, A&A 575 (2015) A112. doi: 10.1051/0004-6361/ 201424713. arXiv:1412.8167

    work page doi:10.1051/0004-6361/ 2015

  76. [88]

    E. M. Churazov, I. I. Khabibullin, A. M. Bykov, Minimalist model of the W50 /SS433 extended X-ray jet: Anisotropic wind with recollimation shocks, A&A 688 (2024) A4. doi: 10.1051/ 0004-6361/202449343. arXiv:2401.14770

    work page arXiv 2024

  77. [89]

    The LHAASO Collaboration, Z. Cao, F. Aharo- nian, Y . X. Bai, Y . W. Bao, D. Bastieri, X. J. Bi, Y . J. Bi, W. Bian, A. V . Bukevich, C. M. Cai, W. Y . Cao, Z. Cao, J. Chang, J. F. Chang, A. M. Chen, E. S. Chen, G. H. Chen, H. X. Chen, L. Chen, L. Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, X. B. Chen, X. J. Chen...

    work page internal anchor Pith review doi:10.48550/arxiv 2025

  78. [90]

    Z. Cao, F. Aharonian, Q. An, B. Axikegu, Y . X., Y . W. Bao, D. Bastieri, X. J. Bi, Y . J. Bi, J. T. Cai, Q. Cao, W. Y . Cao, Z. Cao, J. Chang, J. F. Chang, A. M. Chen, E. S. Chen, L. Chen, L. Chen, L. Chen, M. J. Chen, M. L. Chen, Q. H. Chen, S. H. Chen, S. Z. Chen, T. L. Chen, Y . Chen, N. Cheng, Y . D. Cheng, M. Y . Cui, S. W. Cui, X. H. Cui, Y . D. Cu...

    work page doi:10.1103/physrevlett 2023

  79. [91]

    L. E. Espinosa Castro, F. L. Villante, V . V ecchiotti, C. Evoli, G. Pagliaroli, LHAASO Protons versus LHAASO Di ffuse Gamma Rays: A Consistency Check, arXiv e-prints (2025) arXiv:2506.06593. arXiv:2506.06593. 28

    work page arXiv 2025