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Universe
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Multi-Wavelength Properties of Gamma-Ray Binaries
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Multi-Wavelength Properties of Gamma-Ray Binaries

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Solar and Stellar Physics".

Deadline for manuscript submissions: closed (30 June 2021) | Viewed by 16732

Special Issue Editors

Prof. Dr. Masha Chernyakova

E-Mail Website
Guest Editor
DCU, School of Physics, Dublin City University, 9 Dublin, Ireland
Interests: high energy astrophysics
Dr. Denys Malyshev

E-Mail Website
Guest Editor
Eberhard Karls Universität Tübingen , Institut für Astronomie und Astrophysik , Abteilungen Astronomie und Hochenergieastrophysik, Sand 1, 72076 Tübingen, Germany
Interests: high energy astrophysics

Special Issue Information

Dear Colleagues,

Gamma-ray binaries are a subclass of high-mass binary systems whose energy spectrum peaks at high energies and extends to very high energy γ-rays. In these systems, a compact object is orbiting around a young, massive, either O- or B- type star. While high-mass binaries represent a substantial fraction of galactic X-ray sources detected above 2 keV, less than ten binaries were detected in the γ-ray band by the current generation of Cherenkov telescopes. As such, γ-ray binaries represent a relatively new and unexplored class of astrophysical objects able to accelerate particles with very high efficiency.

Intensive studies during the last decade demonstrate that one should take into account all available timing and broad band information to understand physical processes governing the broad band emission of these peculiar sources. The purpose of this Special Issue is to report recent progress in the field, give an overview of the challenges and problems, to propose possible solutions and to discuss how future facilities will advance the field. We are convinced that this Special Issue will become a reference that reflects the current state-of-the-art and the progress to be made in a future.

We aim to provide the reader with an updated overview of the recent advances in the field from the theoretical and observational points of view. We would like to invite you to contribute to this Special Issue by sharing both original and review papers along any of the lines related to this fascinating area of research.

Prof. Dr. Masha Chernyakova
Dr. Denys Malyshev
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • gamma-ray binaries
  • pulsars
  • emission and acceleration processes
  • wind interaction
  • relativistic hydrodynamics and magnetohydrodynamics (MHD)
  • multi-wavelength and multi-messenger observations

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Published Papers (8 papers)

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Editorial

Jump to: Research

3 pages, 171 KiB  
Editorial
Multi-Wavelength Properties of Gamma-Ray Binaries
by Maria Chernyakova and Denys Malyshev
Universe 2022, 8(9), 439; https://doi.org/10.3390/universe8090439 - 24 Aug 2022
Viewed by 1193
Abstract
Gamma-ray binaries are a subclass of high-mass binary systems whose energy spectrum peaks at high energies ( MeV–GeV energy range) and extends to very high energy (GeV–TeV) γ-rays [...] Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)

Research

Jump to: Editorial

8 pages, 524 KiB  
Article
Fermi-LAT Observation of PSR B1259-63 during Its 2021 Periastron Passage
by Zhi Chang, Shu Zhang, Yu-Peng Chen, Long Ji, Ling-Da Kong and Peng-Ju Wang
Universe 2021, 7(12), 472; https://doi.org/10.3390/universe7120472 - 3 Dec 2021
Cited by 10 | Viewed by 2274
Abstract
PSR B1259-63 is a γ-ray binary system, where the compact object is a pulsar. The system has an orbital period of 1236.7 days and shows peculiar γ-ray flares (in 100 MeV–300 GeV) after its periastron time. We analyzed the Fermi-LAT [...] Read more.
PSR B1259-63 is a γ-ray binary system, where the compact object is a pulsar. The system has an orbital period of 1236.7 days and shows peculiar γ-ray flares (in 100 MeV–300 GeV) after its periastron time. We analyzed the Fermi-LAT observation of PSR B1259-63 during its latest periastron passage, as well as its previous three periastrons. The bright GeV flares started about 60 days after the periastron epoch in 2021. This delay is larger than that around the 2017 periastron and much larger than earlier periastrons. The delay of the GeV flux peak time in each periastron passage is apparent in our results. We discussed the possible origin of this delay and made a prediction of the GeV flux peak time in next periastron passage, based on observation of the previous delays. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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13 pages, 3136 KiB  
Article
Modeling of the Wind/Disk Outflow from Be Stars
by Sergey Bogovalov and Maxim Petrov
Universe 2021, 7(10), 353; https://doi.org/10.3390/universe7100353 - 23 Sep 2021
Cited by 5 | Viewed by 1648
Abstract
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 [...] Read more.
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. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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18 pages, 876 KiB  
Article
Optical and Near-Infrared Monitoring of Gamma-ray Binaries Hosting Be Stars
by Yuki Moritani and Akiko Kawachi
Universe 2021, 7(9), 320; https://doi.org/10.3390/universe7090320 - 30 Aug 2021
Cited by 4 | Viewed by 1993
Abstract
Optical and near-infrared observations are compiled for the three gamma-ray binaries hosting Be stars: PSR B1259−63, LSI+61 303, and HESS J0632+057. The emissions from the Be disk are considered to vary according to the changes in its structure, some of which are caused [...] Read more.
Optical and near-infrared observations are compiled for the three gamma-ray binaries hosting Be stars: PSR B1259−63, LSI+61 303, and HESS J0632+057. The emissions from the Be disk are considered to vary according to the changes in its structure, some of which are caused by interactions with the compact object (e.g., tidal forces). Due to the high eccentricity and large orbit of these systems, the interactions—and, hence the resultant observables—depend on the orbital phase. To explore such variations, multi-band photometry and linear polarization were monitored for the three considered systems, using two 1.5 m-class telescopes: IRSF at the South African Astronomical Observatory and Kanata at the Higashi–Hiroshima Observatory. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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14 pages, 13485 KiB  
Article
The Major Role of Eccentricity in the Evolution of Colliding Pulsar-Stellar Winds
by Maxim V. Barkov and Valenti Bosch-Ramon
Universe 2021, 7(8), 277; https://doi.org/10.3390/universe7080277 - 31 Jul 2021
Cited by 5 | Viewed by 1817
Abstract
Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the [...] Read more.
Binary systems that host a massive star and a non-accreting pulsar can be powerful non-thermal emitters. The relativistic pulsar wind and the non-relativistic stellar outflows interact along the orbit, producing ultrarelativistic particles that radiate from radio to gamma rays. To properly characterize the physics of these sources, and better understand their emission and impact on the environment, careful modeling of the outflow interactions, spanning a broad range of spatial and temporal scales, is needed. Full three-dimensional approaches are very computationally expensive, but simpler approximate approaches, while still realistic at the semi-quantitative level, are available. We present here the results of calculations done with a quasi three-dimensional scheme to compute the evolution of the interacting flows in a region spanning in size up to a thousand times the size of the binary. In particular, we analyze for the first time the role of different eccentricities in the large scale evolution of the shocked flows. We find that the higher the eccentricity, the closer the flows behave like a one-side outflow, which becomes rather collimated for eccentricity values ≳0.75. The simulations also unveil that the pulsar and the stellar winds become fully mixed within the grid for low eccentricity systems, presenting a more stochastic behavior at large scales than in the highly eccentric systems. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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16 pages, 347 KiB  
Article
A Precessing Jet Scenario for the Multi-Wavelength Long-Term Modulation of LS I +61°303
by Frédéric Jaron
Universe 2021, 7(7), 245; https://doi.org/10.3390/universe7070245 - 14 Jul 2021
Cited by 7 | Viewed by 2004
Abstract
The high-mass X-ray binary LS I +61°303 is detected across the electromagnetic spectrum from radio until the very high energy γ-ray regime. The emission is not only highly variable on many time scales, but is also periodic at all observed wavelengths. Periodic [...] Read more.
The high-mass X-ray binary LS I +61°303 is detected across the electromagnetic spectrum from radio until the very high energy γ-ray regime. The emission is not only highly variable on many time scales, but is also periodic at all observed wavelengths. Periodic modulation was observed on different time-scales, ranging from hours, over months to several years. The subject of this article is a super-orbital, long-term modulation of ∼4.6 years. We review the observation of this periodic modulation at multiple wavelengths and investigate systematic relationships between them. IN particular, radio observations reveal that the long-term modulation is a very stable feature of the source. Observations at other wavelengths result in a phase-shift of the modulationpattern that is a systematic function of energy. The stability of this period favors a scenario in which the long-term modulation is the result of a precessing jet giving rise to periodic changes in the Doppler factor, beating with the orbital modulation of the accretion rate. We explain the phase-shifts across energy bands in a scenario with shorter wavelengths originating closer to the base of the presessing jet. A significant deviation of the TeV emission from this trend possibly requires a different explanation related to magnetic reconnection events. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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11 pages, 600 KiB  
Communication
Multi-Wavelength Properties of the 2021 Periastron Passage of PSR B1259-63
by Maria Chernyakova, Denys Malyshev, Brian van Soelen, Shane O’Sullivan, Charlotte Sobey, Sergey Tsygankov, Samuel Mc Keague, Jacob Green, Matthew Kirwan, Andrea Santangelo, Gerd Pühlhofer and Itumeleng M. Monageng
Universe 2021, 7(7), 242; https://doi.org/10.3390/universe7070242 - 13 Jul 2021
Cited by 19 | Viewed by 2780
Abstract
PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around a O9.5Ve star, LS 2883, with a period of ∼3.4 years. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broadband emission in the radio, [...] Read more.
PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around a O9.5Ve star, LS 2883, with a period of ∼3.4 years. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broadband emission in the radio, X-ray, GeV, and TeV domains. One of the most unusual features of the system is an outburst of GeV energies around the periastron, during which the energy release substantially exceeds the spin down luminosity under the assumption of the isotropic emission. In this paper, we present the first results of a recent multi-wavelength campaign (radio, optical, and X-ray bands) accompanied by the analysis of publicly available GeV Fermi/LAT data. The campaign covered a period of more than 100 days around the 2021 periastron and revealed substantial differences from previously observed passages. We report a major delay of the GeV flare, weaker X-ray flux during the peaks, which are typically attributed to the times when the pulsar crosses the disk, and the appearance of a third X-ray peak never observed before. We argue that these features are consistent with the emission cone model proposed by us previously, in the case of a sparser and clumpier disk of the Be star. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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10 pages, 980 KiB  
Communication
Searching for Gamma-Ray Binaries in Multiwavelength Catalogs
by Josep Martí and Pedro L. Luque-Escamilla
Universe 2021, 7(7), 214; https://doi.org/10.3390/universe7070214 - 28 Jun 2021
Cited by 3 | Viewed by 1644
Abstract
The number of gamma-ray binaries currently known is still so small that even a new finding represents a significant expansion of its population. We present a possible hunting strategy based on screening different catalogs to filter potential peculiar stars consistent with gamma-ray sources [...] Read more.
The number of gamma-ray binaries currently known is still so small that even a new finding represents a significant expansion of its population. We present a possible hunting strategy based on screening different catalogs to filter potential peculiar stars consistent with gamma-ray sources whose association at lower energies is not yet certain. So far, two candidate systems have emerged from this process; we report about them here. Full article
(This article belongs to the Special Issue Multi-Wavelength Properties of Gamma-Ray Binaries)
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