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From Tides to Waves: Understanding the Formation Mechanisms of Galactic...
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From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals

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

Deadline for manuscript submissions: 15 September 2025 | Viewed by 1852

Special Issue Editor

Dr. Aleksandr Mosenkov

E-Mail Website
Guest Editor
Department of Physics and Astronomy, Brigham Young University, Provo, UT 84602, USA
Interests: galaxy formation and evolution; interstellar medium; cosmology

Special Issue Information

Dear Colleagues,

The formation mechanisms of galactic spiral structures remain one of the most captivating topics in modern astrophysics. Recent advancements have significantly deepened our understanding of these prominent galaxy features, from the gravitational effects of tidal interactions to the intricate wave-like processes within galactic disks. This Special Issue, titled "From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals", aims to collate the latest research and insights into the dynamic processes that shape spiral galaxies.

We invite contributions that explore the diverse origins and evolutionary paths of spiral structures. Topics of interest include, but are not limited to, the role of density waves, the impact of dark matter on spiral arm formation, the influence of galactic interactions, and the correlation between the morphology of spiral arms and star formation rates. We are particularly keen to publish studies utilizing advanced observational data, such as those from the James Webb Space Telescope, the Hubble Space Telescope, and other space- and ground-based observatories, alongside cutting-edge simulations and theoretical models.

By bringing together experts in the field, this Special Issue aims to foster a comprehensive understanding of the physical processes driving the formation and evolution of spiral arms in galaxies. We look forward to your valuable contributions that will undoubtedly enrich our collective knowledge and inspire future research in this dynamic area of astronomy.

Yours faithfully,

Dr. Aleksandr Mosenkov
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

  • spiral arms
  • density waves
  • galactic dynamics
  • star formation
  • tidal interactions
  • pitch angle
  • dark matter
  • galactic morphology
  • radial profiles
  • secular evolution

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Published Papers (5 papers)

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Research

34 pages, 2012 KiB  
Article
Numerical Study of Bar Suppression in Galaxy Models Due to Disc Heating
by Alejandro López Gómez, Ruslan Gabbasov and Isaura Luisa Fuentes-Carrera
Galaxies 2025, 13(2), 45; https://doi.org/10.3390/galaxies13020045 - 21 Apr 2025
Viewed by 120
Abstract
The process of bar formation, evolution and destruction is still a controversial topic regarding galaxy dynamics. Numerical simulations show that these phenomena strongly depend on physical and numerical parameters. In this work, we study the combined influence of the softening parameter, ϵ and [...] Read more.
The process of bar formation, evolution and destruction is still a controversial topic regarding galaxy dynamics. Numerical simulations show that these phenomena strongly depend on physical and numerical parameters. In this work, we study the combined influence of the softening parameter, ϵ and disc mass fraction, md, on the formation and evolution of bars in isolated disc-halo models via N-body simulations with different particle resolutions. Previous studies indicate that the bar strength depends on md as ∝md−1, which is seen as a delay in bar formation. However, the distorsion parameter, η, which measures the bar’s momentum through time, shows that an increase in md does not always induce a delay in bar formation. This suggests that ϵ interact to either enhance or weaken the bar. Moreover, numerical heating dominates in models with small softening values, creating highly accelerated particles at the centre of discs, regardless of md or resolution. These enhanced particle accelerations produce chaotic orbits for ϵ≤5 pc, resulting in bar suppression due to collisional dynamics in the centre. In our high-resolution models (N≈107), small softening values are incapable of reproducing the bar instability. The role of disc mass is as follows: increasing md for moderate ϵ (≥10 pc) reduces the amount of drift in the acceleration profile, without affecting the bar’s behaviour. Models with lower md values, coupled with small softening values, have an excess of highly accelerated particles, introducing unwanted effects into otherwise reliable simulations. Finally, we show that the evolution of the disc’s vertical acceleration profile is a reliable indicator of numerical heating introduced by ϵ and the bar. Full article
(This article belongs to the Special Issue From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals)
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35 pages, 6349 KiB  
Article
Examination of the Functional Form of the Light and Mass Distribution in Spiral Arms
by Ilia V. Chugunov, Alexander A. Marchuk and Sergey S. Savchenko
Galaxies 2025, 13(2), 44; https://doi.org/10.3390/galaxies13020044 - 19 Apr 2025
Viewed by 121
Abstract
Spiral arms are a common feature of local galaxies, but the exact form of the distribution of mass and light in them is not well known. In this work, we aim to measure this distribution as accurately as possible, focusing on individual spiral [...] Read more.
Spiral arms are a common feature of local galaxies, but the exact form of the distribution of mass and light in them is not well known. In this work, we aim to measure this distribution as accurately as possible, focusing on individual spiral arms and using the so-called slicing method. The sample consists of 19 well-resolved, viewed face-on spiral galaxies from the S4G survey. We work primarily with infrared images at 3.6 μm from the same survey and, secondarily, with ultraviolet data from the GALEX telescope. We derive the properties of the spiral arms step by step, starting from their overall shape, then measuring their brightness profile and width variation along the arm and then examining the fine structure of the profile across the arm, namely, its skewness and Sérsic index. We construct a 2D photometric function of the spiral arm that can be used in further decomposition studies, validate it and identify the most and least important parameters. Finally, we show how our results can be used to unravel the nature of the spiral arms, supporting the evidence that NGC 4535 has a density wave in its disc. Full article
(This article belongs to the Special Issue From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals)
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31 pages, 4553 KiB  
Article
Accurate Decomposition of Galaxies with Spiral Arms: Dust Properties and Distribution
by Alexander A. Marchuk, Ilia V. Chugunov, Frédéric Galliano, Aleksandr V. Mosenkov, Polina V. Strekalova, Sergey S. Savchenko, Valeria S. Kostiuk, George A. Gontcharov, Vladimir B. Il’in, Anton A. Smirnov and Denis M. Poliakov
Galaxies 2025, 13(2), 39; https://doi.org/10.3390/galaxies13020039 - 9 Apr 2025
Viewed by 415
Abstract
We analyze three nearby spiral galaxies—NGC 1097, NGC 1566, and NGC 3627—using images from the DustPedia database in seven infrared bands (3.6, 8, 24, 70, 100, 160, and 250 μm). For each image, we perform photometric decomposition and construct a multi-component model, including [...] Read more.
We analyze three nearby spiral galaxies—NGC 1097, NGC 1566, and NGC 3627—using images from the DustPedia database in seven infrared bands (3.6, 8, 24, 70, 100, 160, and 250 μm). For each image, we perform photometric decomposition and construct a multi-component model, including a detailed representation of the spiral arms. Our results show that the light distribution is well described by an exponential disk and a Sérsic bulge when non-axisymmetric components are properly taken into account. We test the predictions of the stationary density wave theory using the derived models in bands, tracing both old stars and recent star formation. Our findings suggest that the spiral arms in all three galaxies are unlikely to originate from stationary density waves. Additionally, we perform spectral energy distribution (SED) modeling using the hierarchical Bayesian code HerBIE, fitting individual components to derive dust properties. We find that spiral arms contain a significant (>10%) fraction of cold dust, with an average temperature of approximately 18–20 K. The estimated fraction of polycyclic aromatic hydrocarbons (PAHs) declines significantly toward the galactic center but remains similar between the arm and interarm regions. Full article
(This article belongs to the Special Issue From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals)
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16 pages, 310 KiB  
Article
Non-Zero Coriolis Field in Ehlers’ Frame Theory
by Federico Re and Oliver F. Piattella
Galaxies 2025, 13(2), 38; https://doi.org/10.3390/galaxies13020038 - 5 Apr 2025
Viewed by 245
Abstract
Ehlers’ Frame Theory is a class of geometric theories parameterized by λ:=1/c2 and identical to the General Theory of Relativity for λ≠0. The limit λ→0 does not recover Newtonian gravity, as one [...] Read more.
Ehlers’ Frame Theory is a class of geometric theories parameterized by λ:=1/c2 and identical to the General Theory of Relativity for λ≠0. The limit λ→0 does not recover Newtonian gravity, as one might expect, but yields the so-called Newton–Cartan theory of gravity, which is characterized by a second gravitational field ω, called the Coriolis field. Such a field encodes at a non-relativistic level the dragging feature of general spacetimes, as we show explicitly for the case of the (η,H) geometries. Taking advantage of the Coriolis field, we apply Ehlers’ theory to an axially symmetric distribution of matter, mimicking, for example, a disc galaxy, and show how its dynamics might reproduce a flattish rotation curve. In the same setting, we further exploit the formal simplicity of Ehlers’ formalism in addressing non-stationary cases, which are remarkably difficult to treat with the General Theory of Relativity. We show that the time derivative of the Coriolis field gives rise to a tangential acceleration which allows for studying a possible formation in time of the rotation curve’s flattish feature. Full article
(This article belongs to the Special Issue From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals)
30 pages, 10621 KiB  
Article
A Comprehensive Analysis on the Nature of the Spiral Arms in NGC 3686, NGC 4321, and NGC 2403
by Valeria Kostiuk, Alexander Marchuk, Alexander Gusev and Ilia V. Chugunov
Galaxies 2025, 13(2), 27; https://doi.org/10.3390/galaxies13020027 - 24 Mar 2025
Cited by 1 | Viewed by 282
Abstract
In theoretical investigations, various mechanisms have been put forward to explain the emergence of spiral patterns in galaxies. One of the few ways to find out the nature of spirals in a particular galaxy is to consider the so-called corotation radius, or corotation [...] Read more.
In theoretical investigations, various mechanisms have been put forward to explain the emergence of spiral patterns in galaxies. One of the few ways to find out the nature of spirals in a particular galaxy is to consider the so-called corotation radius, or corotation resonance. A distinctly defined corotation resonance is likely to indicate the existence of a spiral density wave, while the chaotic distribution of their positions may suggest a dynamic nature to the spiral structure. In this study, we analyzed measurements of the corotation radius obtained using several methods for three galaxies (NGC 3686, NGC 4321, and NGC 2403) that exhibit different morphologies of spiral structures. We also performed independent measurements to estimate the location of the resonance, which allowed us to determine whether each galaxy has a clear corotation radius position. This examination, along with other tests such as stellar age gradient, interlocking resonances, and the radial distribution of metallicity, enables us to understand the mechanism that may be responsible for the formation of spiral arms in the studied galaxies. Full article
(This article belongs to the Special Issue From Tides to Waves: Understanding the Formation Mechanisms of Galactic Spirals)
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