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Galaxies
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X-ray Binary Formation and Evolution
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X-ray Binary Formation and Evolution

A special issue of Galaxies (ISSN 2075-4434).

Deadline for manuscript submissions: closed (13 May 2022) | Viewed by 6570

Special Issue Editor

Dr. Antara R. Basu-Zych

E-Mail Website
Guest Editor
1. University of Maryland, Baltimore County (UMBC), Baltimore, MD 21250, USA
2. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD 20771, USA
Interests: galaxy evolution; multi-wavelength astronomy; X-ray binaries; starburst galaxies; high-redshift galaxy analogs; star formation; compact objects; X-rays

Special Issue Information

Dear Colleagues,

Over the past decade, the X-ray binary research community has dedicated significant research to addressing: How do X-ray binaries form and evolve in different galaxy host environments?

As the predecessors of gravitational wave sources and millisecond pulsars and as sources which are potentially relevant in the early universe for heating the intergalactic medium preceding the epoch of reionization, understanding how X-ray binaries form and evolve has become more relevant also to the broader scientific community. The emission from X-ray binary (XRB) populations within nearby and distant galaxies, based on stacking analyses to study the average emission, has seen marked refinement over these years by adding additional parameters and more nuanced studies of the relationships between XRBs and their host galaxy properties (e.g., star formation rates, stellar masses, metallicities, and stellar ages). Additionally, studies of the XRB luminosity functions in spatially resolved galaxies have probed the XRB populations deeper by investigating different types of galaxies (i.e., early-types, spirals, irregular) and galaxy environments, such as interacting galaxies. By comparing observations with XRB population synthesis models, we have gained deeper insight into the drivers of these correlations. Additionally, both theoretical and observational studies of detailed physics, including accretion mechanisms, within XRB systems have offered important constraints for these models. Therefore, the growth of our collective understanding and access to better data has opened up new vistas and the exploration of new questions.

Here, we are soliciting papers from the science community related to XRB populations, their formation, and evolution. Particularly, we would like this Special Issue to cover topics that span XRBs within nearby galaxies (including population studies within the Milky Way, LMC, SMC, and local group) to scaling relations in distant galaxies. We welcome papers that cover both theoretical work and observational studies on this general topic and outline specific areas that we hope this Special Issue can address:

  • XRBs populations in nearby galaxies—the Milky Way, LMC, SMC;
  • XRBs in interacting galaxies;
  • Scaling relations of XRB emission with host galaxy properties (including evolution of these relations with redshift);
  • XRB luminosity functions in nearby and spatially resolved galaxies;
  • Comparison of observations with theoretical models of XRB formation and evolution, including via dynamical channels (e.g., within globular clusters);
  • Impact of XRBs on high-z IGM studies;
  • Accretion physics models and observations using galactic or nearby XRBs;
  • Ultraluminous X-ray sources and unique classes of XRBs (e.g., Wolf–Rayet XRBs, supergiant fast X-ray transients) and their relationship to other XRBs and/or their host galaxies.

Dr. Antara R. Basu-Zych
Guest Editor

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. Galaxies is an international peer-reviewed open access semimonthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 1400 CHF (Swiss Francs). 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

  • X-ray binaries
  • galaxies
  • evolution
  • X-ray observations

Published Papers (3 papers)

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Research

23 pages, 16928 KiB  
Article
Synthetic Neutrino Imaging of a Microquasar
by Theodoros Smponias
Galaxies 2021, 9(4), 80; https://0-doi-org.brum.beds.ac.uk/10.3390/galaxies9040080 - 19 Oct 2021
Cited by 2 | Viewed by 1234
Abstract
Microquasar binary stellar systems emit electromagnetic radiation and high-energy particles over a broad energy spectrum. However, they are so far away that it is hard to observe their details. A simulation offers the link between relatively scarce observational data and the rich theoretical [...] Read more.
Microquasar binary stellar systems emit electromagnetic radiation and high-energy particles over a broad energy spectrum. However, they are so far away that it is hard to observe their details. A simulation offers the link between relatively scarce observational data and the rich theoretical background. In this work, high-energy particle emission from simulated twin microquasar jets is calculated in a unified manner. From the cascade of emission within an element of jet matter to the dynamic and radiative whole jet model, the series of physical processes involved are integrated together. A programme suite assembled around model data produces synthetic images and spectra directly comparable to potential observations by contemporary arrays. The model is capable of describing a multitude of system geometries, incorporating increasing levels of realism depending on need and available computational resources. As an application, the modelling process is applied to a typical microquasar, which is synthetically observed from different angles using various imaging geometries. Furthermore, the resulting intensities are comparable to the sensitivity of existing detectors. The combined background emission from a potential distribution of microquasars is also modelled. Full article
(This article belongs to the Special Issue X-ray Binary Formation and Evolution)
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10 pages, 460 KiB  
Article
The Origin of Radio Emission in Black Hole X-ray Binaries
by Xiang Liu, Ning Chang, Xin Wang and Qi Yuan
Galaxies 2021, 9(4), 78; https://0-doi-org.brum.beds.ac.uk/10.3390/galaxies9040078 - 17 Oct 2021
Cited by 3 | Viewed by 1598
Abstract
We studied the relation of accretion-jet power and disk luminosity, especially the jet efficiencies and disk radiative efficiencies for different accretion disks as well as black hole (BH) spin, in order to explore the origin of radio emission in black hole X-ray binaries [...] Read more.
We studied the relation of accretion-jet power and disk luminosity, especially the jet efficiencies and disk radiative efficiencies for different accretion disks as well as black hole (BH) spin, in order to explore the origin of radio emission in black hole X-ray binaries (BHXBs). We found that jet efficiency increases more rapidly (efficient) than the nearly constant disk radiative efficiency for thin disk component in high accretion regime, which could account for the steep track (μ>1) in the observed radio and X-ray luminosity relations (LR∝LXμ), but the thin disk component may not be able to explain the standard track (μ≈0.6) in the BHXBs. For hot accretion flows (HAF), the resulting jet efficiency changes along with the large range of accretions from quiescent state to nearly Eddington state, which could account for the standard track in the BHXBs. The BH spin-jet is discussed for the magnetic arrested disk (MAD) state; in this state, the spin-jet power might contribute to a linear correlation between jet power and mass accretion rate for a given source. More accurate observations are required to test the results. Full article
(This article belongs to the Special Issue X-ray Binary Formation and Evolution)
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17 pages, 517 KiB  
Article
Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets
by Theodora Papavasileiou, Odysseas Kosmas and Ioannis Sinatkas
Galaxies 2021, 9(3), 67; https://0-doi-org.brum.beds.ac.uk/10.3390/galaxies9030067 - 13 Sep 2021
Cited by 6 | Viewed by 2102
Abstract
Recently, microquasar jets have aroused the interest of many researchers focusing on the astrophysical plasma outflows and various jet ejections. In this work, we concentrate on the investigation of electromagnetic radiation and particle emissions from the jets of stellar black hole binary systems [...] Read more.
Recently, microquasar jets have aroused the interest of many researchers focusing on the astrophysical plasma outflows and various jet ejections. In this work, we concentrate on the investigation of electromagnetic radiation and particle emissions from the jets of stellar black hole binary systems characterized by the hadronic content in their jets. Such emissions are reliably described within the context of relativistic magneto-hydrodynamics. Our model calculations are based on the Fermi acceleration mechanism through which the primary particles (mainly protons and electrons) of the jet are accelerated. As a result, a small portion of thermal protons of the jet acquire relativistic energies, through shock-waves generated into the jet plasma. From the inelastic collisions of fast (non-thermal) protons with the thermal (cold) ones, secondary charged and neutral particles (pions, kaons, muons, η-particles, etc.) are created, as well as electromagnetic radiation from the radio wavelength band to X-rays and even very high energy gamma-rays. One of our main goals is, through the appropriate solution of the transport equation and taking into account the various mechanisms that cause energy losses to the particles, to study the secondary particle concentrations within hadronic astrophysical jets. After assessing the suitability and sensitivity of the derived (for this purpose) algorithms on the Galactic MQs SS 433 and Cyg X-1, as a concrete extragalactic binary system, we examine the LMC X-1 located in the Large Magellanic Cloud, a satellite galaxy of our Milky Way Galaxy. It is worth mentioning that, for the companion O star (and its extended nebula structure) of the LMC X-1 system, new observations using spectroscopic data from VLT/UVES have been published a few years ago. Full article
(This article belongs to the Special Issue X-ray Binary Formation and Evolution)
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