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The existence and shapes of dust lanes in galactic bars
Abstract
I study the flow of gas in and around the bars or ovals of model barred galaxies and show that it is intimately linked to the properties of the periodic orbits. Simulations show that the density of the gas in and around the bar region is low, except for the centre and two narrow lanes which are the loci of shocks. Such shocks form if the x1 periodic orbits have either loops or large curvature values at their apocentres. The form of the shock loci depends on a number of parameters characterizing the bar and disc potentials. In order for shocks to be offset from the bar major axis towards its leading side, the x2 and x3 families must not only exist but also cover a sufficient extent along the bar major axis. The shapes of the shock loci are then understood by the gradual shift of the orientation of the flow lines from that of the x1 orbits to that of x2. Along the shock there is also substantial shear, opposing star formation. The existence of offset shock loci of the observed shape puts strict constraints on the values the various model parameters may take. This should be most useful for deriving bar parameters for observed galaxies. For example, the Lagrangian radius has to lie in the interval (1.2 ± 0.2)a, where a is the length of the bar semimajor axis. For low values of the bar axial ratio or the bar quadrupole moment the shock loci are curved, with their concave sides towards the bar major axis. Substantial inflow is found in models with strong shocks.
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“While an intersecting set of orbits can remain stable in a collisionless system, the gas undergoes a shock at the intersection and loses angular momentum. The gas then flows towards the center and finally settles into a ring-like structure closely following the x 2 orbits and thus forming the CMZ-like rings in galaxies (Binney et al. 1991; Athanassoula 1992; Sormani et al. 2015).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Athanassoula 1992
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Revealing Gas Inflows Toward the Galactic Central Molecular Zone
Su, Y., Zhang, S., Sun, Y., Yang, J., YAN, Q.-Z., Zhang, S., Chen, Z., Chen, X., Zhou, X., & Yuan, L. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad656d · Cited by 12
“In this way, the moving gas driven by the rotation bar (e.g., Athanassoula 1992; Fux 1999; Sormani & Barnes 2019) can be roughly described by Here, v // is the gas velocity towards the CMZ region along the bar (i.e., ⃗v = ⃗v // + ⃗v rot in the inertial frame of the Galaxy) and v LOS is the measured…”
BackgroundPhysical condition of the molecular gas at the centre of NGC 1097
Piñol-Ferrer, N., Fathi, K., Lundgren, A. A., et al. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18419.x · Cited by 10
“In the presence of a bar, the overdensity of a gas may occur in resonances, like the inner Lindblad resonance (ILR) for an inner ring (e.g. Combes & Gerin 1985; Athanassoula 1992; Wada 1994).”
BackgroundLuo, R., Hao, L., Blanc, G. A., Jogee, S., van den Bosch, R. C. E., & Weinzirl, T. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/823/2/85 · Cited by 10
“The inflowing gas is usually shocked and can be traced by dust lanes (Athanassoula 1992).”
BackgroundRahna, P. T., Das, M., Murthy, J., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2250 · Cited by 10
“The nuclear rings in barred galaxies are sites of intense massive star formation and are produced by the infall of gas from large radii caused by the bar (Combes & Gerin 1985; Shlosman et al. 1990; Athanassoula 1992; Heller & Shlosman 1994; Knapen et al. 1995; Buta & Combes 1996).”
BackgroundRings and Bars: Unmasking Secular Evolution of Galaxies
Knapen, J. H. (2010) · Springer eBooks · doi:10.1007/978-1-4419-7317-7_18 · Cited by 10
“Dust lanes have been recognised in relation to shocks in the flow of gas in barred galaxies now almost 50 yearsago (Prendergast 1962), and Athanassoula (1992) in fact predicted from numerical modelling that the degree of curvature of the main dust lanes in a bar should decrease as the bar gets…”
Background3D MHD simulations of magnetic field evolution and radio polarization of barred galaxies
Kulesza-Żydzik, B., Kulpa-Dybeł, K., Otmianowska-Mazur, K., et al. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201015036 · Cited by 10
“3 we show that the basic dynamical features of our barred galaxies are very similar to those constructed by Athanassoula (1992).”
BackgroundMethodResultInfluentialWhat triggers star formation in galaxies?
Elmegreen, B. G. (2011) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921312009350 · Cited by 10
“Inside this, the gas hits the bar from behind and shocks, forming a dustlane (Athanassoula 1992).”
BackgroundRole of galactic bars in the formation of spiral arms: a study through orbital and escape dynamics—I
Mondal, D., & Chattopadhyay, T. (2021) · Celestial Mechanics and Dynamical Astronomy · doi:10.1007/s10569-021-10037-5 · Cited by 10
“We use a fast bar (Athanassoula 1992) in both of the bar models.”
MethodMorphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data
Wu, Y.-T., Trejo, A., Espada, D., & Miyamoto, Y. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1087 · Cited by 10
“This implies that the velocity deviation from circular motion is larger after crossing the dust lanes and there is gas streaming motion along the dust lanes as predicted by hydrodynamic models (Athanassoula 1992).”
BackgroundInfluentialStar formation in the warped outer pseudoring of the spiral galaxy NGC 3642
Verdes–Montenegro, L., Bosma, A., & Athanassoula, E. (2002) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20020680 · Cited by 10
“While barred galaxies tend to show bisymmetrical patterns (Athanassoula 1992) non barred ones can have more irregular structures.”
BackgroundSelf-citationThe morphology of galactic rings exterior to evolving bars: test-particle simulations
Bagley, M. B., Minchev, I., & Quillen, A. C. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14575.x · Cited by 10
Companions of Bright Barred Shapley-Ames Galaxies
García-Barreto, J. A., Carrillo, R., & Vera-Villamizar, N. (2003) · The Astronomical Journal · doi:10.1086/378359 · Cited by 10
“The issue of the role of bars may play on this process has been the subject of several investigations (Combes 1988, Shlosman et al. 1989, Athanassoula 1992, Phinney 1994, Athanassoula 1994, Wada & Habe 1995, Ho, Filippenko & Sargent 1996, Mulchaey, Regan & Kundu 1997, Sakamoto et al. 1999,…”
BackgroundMolecular Gas in the Central Regions of Barred Galaxies
Kenney, J. D. P. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049654 · Cited by 10
“Hydrodynamic simulations by Athanassoula (1992) pro duced circumnuclear spiral features near ILRs, and from simple dynamical con siderations, Combes (1988) and Wada (1994) described why spiral gas patterns are sometimes expected near ILRs.”
Bars and the connection between dark and visible matter
Athanassoula, E. (2004) · Symposium - International Astronomical Union · doi:10.1017/s0074180900183330 · Cited by 10
“A gaseous component could increase further the central concentration of the disc material (e.g. Athanassoula 1992, Heller & Shlosman 1994) and thus make its inwards pull on the halo material yet stronger.”
BackgroundSelf-citationNexus : a framework for controlled simulations of idealized galaxies
Tepper-García, T., Bland‐Hawthorn, J., Vasiliev, E., Agertz, O., Teyssier, R., & Federrath, C. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2372 · Cited by 10
Maeda, F., Ohta, K., Egusa, F., Fujimoto, Y., Kobayashi, M. I. N., Inoue, S., & Habe, A. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adb41e · Cited by 9
On the Spiral Structure of NGC 5248: An Analytic Approach
Yuan, C., & Yang, C. (2006) · The Astrophysical Journal · doi:10.1086/503519 · Cited by 9
The flow in the spiral arms of slowly rotating bar-spiral models
Patsis, P. A., & Tsigaridi, L. (2017) · Astrophysics and Space Science · doi:10.1007/s10509-017-3109-9 · Cited by 9
How Nested Bars Enhance, Modulate, and Are Destroyed by Gas Inflows
Li, Z., Du, M., Debattista, V. P., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acffb3 · Cited by 9
The universal variability of the stellar initial mass function probed by the TIMER survey
Martín-Navarro, I., de Lorenzo-Cáceres, A., Gadotti, D. A., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348060 · Cited by 9
Pseudo bulges in galaxy groups: the role of environment in secular evolution
Mishra, P. K., Wadadekar, Y., & Barway, S. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx247 · Cited by 9
CHANG-ES. XXIV. First Detection of a Radio Nuclear Ring and Potential LLAGN in NGC 5792
Yang, Y., Irwin, J., Li, J., Wiegert, T., Wang, Q. D., Sun, W., Damas-Segovia, A., Li, Z., Shen, Z. Q., Walterbos, R. A. M., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac4ae7 · Cited by 9
“…and the ring, where the accumulated gas proceeds to move in nearly circular orbits and forms a luminous, compact ring around the galactic center (Athanassoula 1992; Heller & Shlosman 1994, 1996; Piner et al. 1995; Buta & Combes 1996; Regan et al. 1997; Benedict et al. 2002; Kim et al. 2012;…”
BackgroundBosma, A. (1998) · Celestial Mechanics and Dynamical Astronomy · doi:10.1023/a:1008366614769 · Cited by 9
Ongoing star formation in AGN host galaxy discs: a view from core-collapse supernovae
Wang, J., Deng, J. S., & Wei, J. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16629.x · Cited by 9
Comparison between 2D and 3D codes in dynamical simulations of gas flow in barred galaxies
Pérez, I. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20078180 · Cited by 9
“A change in the parameters such as the pattern speed and the M/L would have caused the velocity field and the shock strength,location and shape to be significantly different (see Athanassoula (1992); Weiner et al. (2001a); Pérez et al. (2004)) to the results obtained here.”
BackgroundMethodResultInfluentialThe study of two barred galaxies with curious kinematical features
Saburova, A. S., Katkov, I. Y., Khoperskov, S., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1200 · Cited by 9
“A number of numerical simulations suggest that bars induce torques which force the gas to shock, subsequently losing angular momentum and funneling to the centre (Athanassoula 1992; Regan & Teuben 2004; Kim et al. 2012).”
BackgroundHYDRODYNAMIC SIMULATIONS FOR THE NUCLEAR MORPHOLOGY OF NGC 4314Preprint
Ann, H. B. (2001) · Cited by 9
The Central Region of M83 ⋆Preprint
Houghton, R. C. W., & Thatte, N. (2012) · Cited by 9
Bar-driven Gas Dynamics of M31
Feng, Z., Li, Z., Shen, J., Gerhard, O., Saglia, R. P., Blaña, M., Li, H., & Jing, Y. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad13ee · Cited by 8
“The overall gas patterns of our models are similar to the previous studies (Athanassoula 1992; Kim et al. 2012b; Li et al. 2015).”
BackgroundResultInfluentialBernet, M., Ramos, P., Antoja, T., Monari, G., & Famaey, B. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348410 · Cited by 8
Bottom’s Dream and the Amplification of Filamentary Gas Structures and Stellar Spiral Arms
Meidt, S. E., & van der Wel, A. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad12c5 · Cited by 8
“Stellar bars, for example, shape the gas within them into narrow ‘dust lane’ features (e.g. Athanassoula 1992; Kim et al. 2012) and set up spirals in the exterior gas (Combes & Gerin 1985).”
BackgroundRathore, H., Besla, G., Daniel, K. J., & Silva, L. J. B. E. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ade0ae · Cited by 8
“…in gas rich Corresponding author: Himansh Rathore himansh@arizona.edu galaxies, bars drive gas inflows through angular momentum transport (e.g. Athanassoula 1992; Kim et al. 2012; Beane et al. 2023; Romeo et al. 2023; Liang et al. 2024), which is observable as streaming motions in the spatial…”
Pastras, S., Genzel, R., Tacconi, L. J., Schuster, K.-F., Neri, R., Schreiber, N. M. F., Naab, T., Barfety, C., Burkert, A. M., Cao, Y., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555430 · Cited by 9
Bar properties and photometry of barred low surface brightness disc galaxies
Peters, W., & de Naray, R. K. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3505 · Cited by 8
“Bars are considered ‘fast’ rotators if R < 1.4 and ‘slow’ rotators if R > 1.4 (Athanassoula 1992; Elmegreen et al. 1996; Debattista & Sellwood 2000).”
BackgroundInfluentialStar formation in extreme environments: A 200 pc high velocity gas stream in the Galactic centre
Veena, V. S., Kim, W.-J., Sánchez-Monge, Á., Schilke, P., Menten, K. M., Fuller, G. A., Sormani, M. C., Wyrowski, F., Banda-Barragán, W. E., Riquelme, D., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450902 · Cited by 8
Chen, Q., Grasha, K., Battisti, A. J., Wisnioski, E., Li, Z., Park, H.-J., Groves, B. A., Torrey, P., Mendel, J. T., Madore, B. F., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2119 · Cited by 8
The Nuclear Ring in the Barred Spiral Galaxy IC 4933
Ryder, S. D., Illingworth, S., Sharp, R., et al. (2010) · Publications of the Astronomical Society of Australia · doi:10.1071/as09016 · Cited by 8
“As shown in the simulations of Athanassoula (1992), such offset curved dust lanes mark the loci of shocks at the leading edge of a relatively fat bar.”
Magnetic fields and gas flows around circumnuclear starbursts
Beck, R. (2012) · Journal of Physics Conference Series · doi:10.1088/1742-6596/372/1/012051 · Cited by 8
Characterizing bars in low surface brightness disc galaxies
Peters, W., & de Naray, R. K. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty441 · Cited by 8
“Bars are classified as ‘fast’ if R < 1.4 or ‘slow’ if R > 1.4 (Athanassoula 1992; Elmegreen et al. 1996; Debattista & Sellwood 2000).”
BackgroundInfluentialThe Net Radial Flow Velocity of the Neutral Hydrogen in the Oval Distortion of NGC 4736
Speights, J. C., Godwin, C., Reimer, R., Benton, A., & Lemaire, R. (2019) · Astrophysical Journal · doi:10.3847/1538-4357/ab3b54 · Cited by 6
“The expected values for the net radial flow velocities vary from as small as ≈−0.1 km s−1 to as large as ≈−10 km s−1 (e.g., Lacey & Fall 1985; Struck-Marcell 1991; Athanassoula 1992; Quillen et al. 1995; Struck & Smith 1999; Bilitewski & Schönrich 2012; Schmidt et al. 2016).”
BackgroundInfluentialChemical abundances in Seyfert galaxies – VIII. Argon abundance estimates
Monteiro, A. F., & Dors, O. L. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2750 · Cited by 8
Large-scale Hydrodynamical Shocks as the Smoking-gun Evidence for a Bar in M31
Feng, Z., Li, Z., Shen, J., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac7964 · Cited by 8
“One of the most characteristic gaseous features in typical barred galaxies is a pair of dust-lanes on the leading side of the bar (Athanassoula 1992).”
BackgroundResultInfluentialOn the Tremaine–Weinberg method: how much can we trust gas tracers to measure pattern speeds?
Borodina, O., Williams, T. G., Sormani, M. C., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2068 · Cited by 8
Basis function expansions for galactic dynamics: Spherical versus cylindrical coordinates
Wang, Y., Athanassoula, E., & Mao, S. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038225 · Cited by 8
“…Dehnen & Binney 1998b; Fux 2001), the origin of hypervelocity stars (e.g. Zheng et al. 2014; Kenyon et al. 2014; Erkal et al. 2019), the flow of gas in bars (Athanassoula 1992a,b) and the formation and structure of bars, including their boxy and peanut bulges (e.g. Patsis et al. 1997, 2002, 2003).”
BackgroundSelf-citationSpiral galaxies with a central plateau \n in the gas velocity curve along the major axis
Coccato, L., Corsini, E. M., Pizzella, A., et al. (2005) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20042228/pdf · Cited by 8
The Morphology of Barred Galaxies
Buta, R. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049368 · Cited by 8
“The morphology of bar dust lanes has been considered by Athanassoula (1992), who demonstrated how bar strength and the existence of an ILR help to shape these features.”
BackgroundDynamics of the Bar at the Galactic Centre
Gerhard, O. (1996) · Springer eBooks · doi:10.1007/978-94-009-1687-6_11 · Cited by 8
“This is independent of whether the simulations use sticky particles (Schwarz 1981, 1984; Habe & Ikeuchi 1985) or smooth uids (Sanders & Huntley 1976; van Albada 1985; Mulder & Liem 1986; Athanassoula 1992).”
BackgroundMethodColombo, D., Kalinova, V., Bazzi, Z., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453217 · Cited by 7
“…dispersions are higher compared to the discs, e.g. Colombo et al. 2014; Leroy et al. 2016; Sun et al. 2018; Duarte-Cabral et al. 2021), bars (e.g. Athanassoula 1992; Hogarth et al. 2024; Scaloni et al. 2024), but even within strong spiral structure (e.g Meidt et al. 2013; Dobbs & Baba 2014), and…”
Querejeta, M., Pety, J., Schruba, A., Leroy, A. K., Herrera, C. N., Chiang, I.-D., Meidt, S. E., Rosolowsky, E. W., Schinnerer, E., Schuster, K.-F., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202143023 · Cited by 7
Dynamical resonances in PHANGS galaxies
Ruiz-García, M., Querejeta, M., García‐Burillo, S., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450935 · Cited by 7
An Improved Method for Determining the Integrated Properties of Nuclear Rings: NGC 1512
Ma, C., de Grijs, R., & Ho, L. C. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa709e · Cited by 7
“…the ring region at the two ‘contact points’ between the dust lanes and the ring, where the accumulated gas proceeds to move in nearly circular orbits and forms a luminous, compact ring around the galactic center (e.g., Athanassoula 1992; Buta & Combes 1996; Maciejewski 2004; Kim et al. 2012b).”
BackgroundCuomo, V., Debattista, V. P., Racz, S., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3047 · Cited by 7
Central Spiral Structure of Molecular Gas in Maffei 2
Kuno, N., Nakanishi, K., Sorai, K., et al. (2008) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/60.3.475 · Cited by 7
“Many numerical simulations of gas motion in the bar potential show that bars can accumulate gas toward the central region (e.g., Athanassoula 1992).”
BackgroundComparing gaseous and stellar orbits in a spiral potential
Gómez, G. C., Pichardo, B., & Martos, M. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt107 · Cited by 7
“In resonant regions, it has been suggested that shocks occur close to the intersections of stable periodic orbits (Schwarz 1981; van Albada & Sanders 1982; Athanassoula 1992b).”
BackgroundEvidence for a Bar at the Centre of the Milky Way
Binney, J. J. (1994) · Springer eBooks · doi:10.1007/978-94-011-0752-5_8 · Cited by 7
Global Rotational Properties of Barred Galaxies
Bosma, A. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049630 · Cited by 7
Kohno, K., Vila-Vilaró, B., Sakamoto, S., et al. (2003) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/55.1.103 · Cited by 7
“We propose that a small nuclear bar lies along a position angle of −50◦±−10◦ and a possible semi-major radius of Rbar ∼ 1.1 – 1.4 kpc (12 ′′ – 15′′).”
BackgroundMethodInfluentialCan gas dynamics in centres of galaxies reveal orbiting massive black holes?
Etherington, J., & Maciejewski, W. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10016.x · Cited by 7
Internal Secular Evolution in Disk Galaxies: The Growth of PseudobulgesPreprint
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The dynamical state of bars in cluster dwarf galaxies: the cases of NGC 4483 and NGC 4516
Cuomo, V., Morelli, L., Aguerri, J. A. L., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3945 · Cited by 6
Are all starbursts equal? Star-formation-rate profiles in merger versus secular starbursts
Thorp, M., Ellison, S. L., & Galicia, A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451662 · Cited by 6
Do Strong Bars Exhibit Strong Noncircular Motions?
Kim, T., Gadotti, D. A., Lee, Y. H., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8573 · Cited by 6
“Athanassoula (1992b) find that the velocity jump increases as a function of the bar axis ratio and the quadrupole moment of the bar (see their figure 12).”
InfluentialThe Impact of Bar-induced Noncircular Motions on the Measurement of Galactic Rotation Curves
Liu, J., Li, Z., & Shen, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adabe0 · Cited by 6
“The elliptical nuclear ring is almost perpendicular to the bar (Athanassoula 1992b,a; Ma-ciejewski 2004a,b; Kim et al. 2012a,b; Li et al. 2015).”
SDSS-IV MaNGA: Spatial Evolution of Gas-phase Metallicity Changes Induced by Galaxy Interactions
Pan, H.-A., Lin, L., Sánchez, S. F., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adbbd2 · Cited by 6
“Galactic bars, for example, can redistribute metal-enriched gas through radial flows driven by their non-axisymmetric gravitational potential (Athanassoula 1992).”
Asymmetric Star Formation Triggered by Gas Inflow in a Barred Lenticular Galaxy PGC 34107
Lu, S., Gu, Q., Ge, X., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac4be1 · Cited by 6
“Bars have been proven to trigger the secular evolution of disk galaxies by theory and numerical simulations (Athanassoula 1992; Sellwood & Wilkinson 1993; Piner et al. 1995; Knapen et al. 2000; Athanassoula 2003).”
BackgroundPeriodic changes in the morphology of the Galactic resonance rings
Melnik, A. M., Podzolkova, E. N., & Dambis, A. K. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2520 · Cited by 6
Bars from the Inside Out: An HST Study of Their Dusty Circumnuclear Regions
Martini, P. (2004) · Astrophysics and space science library · doi:10.1007/978-1-4020-2862-5_18 · Cited by 6
“…to larger-scale spirals: SB(s) and SB(r) galaxies GD structure is preferentially found in galaxies with large ; and in many cases appears to be the continuation of the dust lanes along the leading edges of large scale bars, dust lanes that models show are formed by strong bars (Athanassoula 1992).”
BackgroundTHE BULGELESS SEYFERT/LINER GALAXY NGC 3367: DISK, BAR, LOPSIDEDNESS, AND ENVIRONMENT
Hernández-Toledo, H. M., Cano-Díaz, M., Valenzuela, O., et al. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/142/6/182 · Cited by 6
“The dust lane curvature observed in Figure 4 when compared with the results of Athanassoula (1992), suggests that the bar in NGC 3367 might be either weak or not as fast as the ones found in early type galaxies which are lines parallel to the bar major axis.”
BackgroundMethodResultInfluentialUnveiling kinematic structure in the starburst heart of NGC 253
Cohen, D. P., Turner, J. L., & Consiglio, S. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa292 · Cited by 6
“…the form of nuclear rings of super star clusters (SSCs; e.g., Athanassoula 1984; Buta & Combes 1996; Buta 1999; Böker et al. 2008; Comerón et al. 2010), as predicted by simulations (Athanassoula 1992; Shlosman 2002; Regan & Teuben 2003; Li et al. 2015; Sormani et al. 2018; Seo et al. 2019).”
BackgroundMultiwavelength study of the star-formation in the bar of NGC 2903
Popping, G., Pérez, I., & Zurita, A. (2010) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201014183/pdf · Cited by 6
Basis function expansions for galactic dynamics: Spherical versus cylindrical coordinates
Wang, Y., Athanassoula, E., & Mao, S. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202038225/pdf · Cited by 6
Self-citationThe Two Pattern Speeds of NGC 3359
Boonyasait, V., Patsis, P. A., & Gottesman, S. T. (2005) · Annals of the New York Academy of Sciences · doi:10.1196/annals.1350.015 · Cited by 6
Stellar populations in the central region of the barred spiral galaxy NGC 4900
Cantin, S., Robert, C., Mollá, M., & Pellerin, A. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16343.x · Cited by 6
Toyouchi, D., & Chiba, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/810/1/18 · Cited by 8
“Such radial redistributions of metals can actually occur via radial gas flow associated with gravitational disk instabilities (e.g., Athanassoula 1992; Noguchi 1998) or re-accretion of metal-enriched gas ejected from the galactic disk as outflow (e.g., Oppenheimer & Davé 2008).”
BackgroundStar formation in the warped outer pseudoring of the spiral \ngalaxy NGC 3642
Verdes-Montenegro, L. L., Bosma, A., & Athanassoula, E. (2002) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20020680/pdf · Cited by 6
Self-citationSecular evolution in barred galaxies
Sellwood, J. A., & Debattista, V. P. (2007) · Springer eBooks · doi:10.1007/bfb0101964 · Cited by 6
“The best such evidence comes from the locations and shapes of dust lanes; the extensive survey of hydrodynamical bar flows by Athanassoula (1992) led her to conclude that DL/aB = 1.1 ± 0.1 would best account for the dust lane morphology in galaxies.”
BackgroundInfluentialEFFECT OF CENTRAL MASS CONCENTRATION ON THE FORMATION OF NUCLEAR SPIRALS IN BARRED GALAXIESPreprint
Thakur, P., Ann, H. B., & Jiang, I. (2012) · Cited by 6
Bar-driven Streaming Motions Mimic a Massive Bulge in the Inner Milky Way
Baba, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adf2a3 · Cited by 5
The Dependency of Bar Formation Timescale on Disk Mass Fraction, Toomre Q, and Scale Height
Chen, B.-H., & Shen, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adf966 · Cited by 5
Nuclear discs in disc galaxies: structural properties and scaling relations
Gadotti, D. A., & de Sá-Freitas, C. (2025) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slaf099 · Cited by 5
Gas dynamics in the central molecular zone and its connection with the galactic bar
Chaves-Velasquez, L., Gómez, G. C., & Pérez-Villegas, Á. (2024) · Publications of the Astronomical Society of Australia · doi:10.1017/pasa.2024.130 · Cited by 5
Chemical evolution in nuclear stellar discs
Friske, J. K. S., & Schönrich, R. A. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554932 · Cited by 5
MHD Simulation in Galactic Center Region with Radiative Cooling and Heating
Kakiuchi, K., Suzuki, T. K., Inutsuka, S., Inoue, T., & Shimoda, J. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad3638 · Cited by 5
“…potential based on the basic theory of Binney et al. (1991), several intersecting orbits are formed, and the orbits near the Galactic center, called X1 and X2 orbits, reproduce the elongated orbits of the gas in and around the CMZ and the gas accretion flow along the dust lanes (Athanassoula 1992).”
BackgroundChoi, W., Bureau, M., Liu, L., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1394 · Cited by 5
Self-consistent modelling of the Milky Way structure using live potentials
Durán-Camacho, E., Duarte-Cabral, A., Pettitt, A. R., Treß, R. G., Clark, P. C., Klessen, R. S., Bogue, K. R. J., Smith, R. J., & Sormani, M. C. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1469 · Cited by 5
Gas Dynamics in the Galactic Bar Region from N-Body and SPH Simulations
Fux, R. (2001) · Astrophysics and Space Science · doi:10.1023/a:1017510224571 · Cited by 5
Stellar Populations in the Galactic Center
Bono, G., Matsunaga, N., Inno, L., Lagioia, E. P., & Genovali, K. (2013) · Astrophysics and space science proceedings · doi:10.1007/978-3-642-35410-6_9 · Cited by 6
How to recover both velocity components in discs of barred galaxies with integral-field spectroscopy
Maciejewski, W., Emsellem, É., & Krajnović, D. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.22040.x · Cited by 5
“Gas flows on the two sides of the major axis of the bar differ considerably (e.g. Athanassoula 1992), and with our method one cannot retrieve two velocity components of gas flow in a bar, and thus explicitly derive the inflow rate.”
MethodTricolor Technique for Visualization of Spatial Variations of Polydisperse Dust in Gas-Dust Flows
Korolev, V. V., Bezborodov, M. A., Kovalenko, I. G., et al. (2018) · Journal of Imaging · doi:10.3390/jimaging4050061 · Cited by 5
Salak, D., Noma, Y., Sorai, K., et al. (2019) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psz004 · Cited by 5
“In the bar region, gas clouds lose angular momentum and gradually (on Gyr timescale) inflow toward the galactic center (Athanassoula 1992).”
BackgroundInfluentialAssessing Disk Galaxy Stability through Time
Valencia-Enríquez, D., Puerari, I., & Rodrigues, I. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab100f · Cited by 5
“This parameterization permits a classification of bars into “fast” ( < <1.0 1.4) or “slow” ( > 1.4; Athanassoula 1992; Debattista & Sellwood 2000).”
BackgroundInfluentialA SINFONI view of circum-nuclear star-forming rings in spiral galaxies
Falcón‐Barroso, J., Böker, T., Schinnerer, E., et al. (2007) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921308017584 · Cited by 5
“The basic picture of how these rings form seems well established, both theoretically and observationally, and is usually associated to the interplay between bar-driven inflow and bar resonances (e.g. Schwarz 1984; Combes & Gerin 1985; Athanassoula 1992; Knapen et al. 1995).”
BackgroundIntrinsic properties of the bars formed by the bar instability in flat stellar discs
Hozumi, S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3704 · Cited by 5
Intrinsic nonaxisymmetric instabilities in galaxy rings
Christodoulou, D. M., Cazes, J. E., & Tohline, J. E. (1997) · New Astronomy · doi:10.1016/s1384-1076(97)00004-3 · Cited by 5
Internal secular evolution in disk galaxies: the growth of pseudobulges
Kormendy, J. (2007) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921308017407 · Cited by 5
Multi-scale simulations of black hole accretion in barred galaxies
Jung, M., Illenseer, T. F., & Duschl, W. J. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731688 · Cited by 5
Molecular Gas in Candidate Double Barred Galaxies III. A Lack of Molecular Gas?
Petitpas, G., & Wilson, C. (2004) · CERN Document Server (European Organization for Nuclear Research) · Cited by 5
Kinematics and Mass Modelling of NGC 1068
Dehnen, W., Bland-Hawthorn, J., Quirrenbach, A., et al. (1997) · Astrophysics and Space Science · doi:10.1023/a:1000524016349 · Cited by 5
“However, theoretical studies also revealed a sensitive dependence of position and strength of the shocks to overall quantities such as pattern speed, bar strength, central mass concentration, and sound speed of the gas (Athanassoula, 1992; Englmaier & Gerhard, 1997).”
BackgroundDynamics of inner galactic disks: The striking case of M 100
Shlosman, I. (2007) · Springer eBooks · doi:10.1007/bfb0101973 · Cited by 5
“…low resolution of numerical schemes and to a common belief that the inner ILR (IILR) is probably located too close to the center to be observationally resolved, most e orts have been devoted to the study of gas dynamics between the OILR and outer Lindblad resonance (OLR; e.g. Athanassoula 1992).”
BackgroundMethodCan gas dynamics in centres of galaxies reveal orbiting massive black holes?Preprint
Etherington, J., & Maciejewski, W. (2006) · Cited by 5
Metadata
- Authors
- Athanassoula, E.
- Corresponding author
- Athanassoula, E.
- ORCID
- Athanassoula, E.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 1992-11-15
- Volume
- 259
- Issue
- 2
- Pages
- 345-364
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2050371636
- Cited by
- 1,011
- References
- 0
- Citations by year
- 2026: 27 · 2025: 46 · 2024: 52 · 2023: 33 · 2022: 37 · 2021: 32 · 2020: 36 · 2019: 41 · 2018: 22 · 2017: 33 · 2016: 46 · 2015: 42 · 2014: 31 · 2013: 41 · 2012: 25
- FWCI
- 6.58
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- galactic bars, dust lanes, periodic orbits, shock, gas flow, shear, star formation, barred galaxies, gas inflow
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