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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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Dependency of the Bar Formation Timescale on the Halo Spin
Chen, B.-H., Kataria, S. K., Shen, J., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ae13a6 · Cited by 4
“…mass (V. P. Debattista et al. 2017; L. Beraldo e Silva et al. 2023), funneling gas into galactic centers to feed supermassive black holes (E. Athanassoula 1992; Z. Li et al. 2016, 2017, 2023; S. K. Kataria & M. Vivek 2024), heating the stellar disk (I. Minchev & B. Famaey 2010; T. Kim et…”
Davis, H., Tepper-García, T., McClure‐Griffiths, N. M., Bland‐Hawthorn, J., & Agertz, O. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf2166 · Cited by 4
The effect of mass and morphology on the mass assembly of galaxies
Camps-Fariña, A., Mérida, R. M., Sánchez–Blázquez, P., & Sánchez, S. F. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202349139 · Cited by 4
Gas Transfer between the Inner 3 kpc Disk and the Galactic Central Molecular Zone
Su, Y., Zhang, S., Sun, Y., Yang, J., Du, F., Fang, M., YAN, Q.-Z., Zhang, S., Chen, Z., Chen, X., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adc38e · Cited by 4
“Indeed, the shock features (i.e., velocity jump) on the bar region can be well reproduced in simulations (e.g., Athanassoula 1992; Kim & Stone 2012; Feng et al. 2024).”
Recovering the pattern speeds of edge-on barred galaxies via an orbit-superposition method
Jin, Y., Ling, Z., Tahmasebzadeh, B., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555378 · Cited by 4
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Ohishi, Y., Sorai, K., & Habe, A. (2012) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/64.4.74 · Cited by 4
“Gas inflow along a bar induces star formation at the leading edge due to shock (e.g., Athanassoula 1992).”
BackgroundDistinguishing between order and chaos in a simple barred galaxy model
Zotos, E. E. (2017) · Astronomische Nachrichten · doi:10.1002/asna.201713152 · Cited by 4
“Over the last decades, a huge amount of studies has been devoted on understanding the orbital structure in barred galaxy models (e.g., Athanassoula 1992; Athanassoula et al. 1983; Combes et al. 1990; Kaufmann & Contopoulos 1996; Ollé & Pfenniger 1998; Pfenniger 1984, 1996; Pichardo et al. 2004).”
BackgroundThe H i in Ring Galaxies Survey (H i -RINGS)—Effects of the bar on the H i gas in ring galaxies
Murugeshan, C., Džudžar, R., Bagge, R. S., et al. (2023) · Publications of the Astronomical Society of Australia · doi:10.1017/pasa.2023.19 · Cited by 4
Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Nilipour, A., Ott, J., Meier, D. S., Svoboda, B., Sormani, M. C., Ginsburg, A. G., Gramze, S. R., Butterfield, N., & Klessen, R. S. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8631 · Cited by 4
“Star formation may be suppressed by the aforementioned extreme processes in the Galactic bar, but also more generally in the bar regions of barred galaxies (Athanassoula 1992).”
Optimizing the analysis of emission lines in galaxies: the case of the MUSE TIMER galaxy NGC 613
Silva-Lima, L. A., Gadotti, D. A., Martins, L. P., et al. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf837 · Cited by 4
Walo-Martín, D., Pinna, F., Grand, R. J. J., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac769 · Cited by 4
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“Numerical simulations have shown that the non-axisymmetric torque exerted by a stellar bar in disk galaxies causes gas to move radially inward along dust lanes and form a ring near the centers (Athanassoula 1992; Knapen et al. 1995; Patsis & Athanassoula 2000; Kim et al. 2012).”
BackgroundDullo, B. T., Knapen, J. H., Beswick, R. J., Baldi, R. D., Williams, D. R., McHardy, I. M., Green, D. A., de Paz, A. G., Aalto, S., Alberdi, A., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1122 · Cited by 4
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Bešlić, I., Barnes, A. T., Bigiel, F., Jiménez-Donaire, M. J., Usero, A., Henshaw, J. D., Faesi, C. M., Leroy, A. K., Rosolowsky, E. W., den Brok, J. S., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347568 · Cited by 4
Akhter, S., Cunningham, M., Harvey-Smith, L., Nawaz, M. A., Jones, P. A., Walsh, A., Pino, E. M. D. G. D., & Falceta-Gonçalves, D. A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa267 · Cited by 3
Detection of Multiple Phase Space Overdensities of GSE Stars by Orbit Integration
Wu, W., Zhao, G., Chang, J., Xue, X.-X., Chen, Y., Li, C., Ye, X., & Yang, C. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acd33a · Cited by 4
“On one hand, as it is reported in the literature (Chiba et al. 2021), the pattern speed of the bar decreases in the Galaxy, which leads to an increasing of the scale length (Athanassoula 1992; Chiba et al. 2021).”
BackgroundGaseous Vortices in Barred Spiral Galaxies
England, M. N., Hunter, J. H., & Contopoulos, G. (2000) · The Astrophysical Journal · doi:10.1086/309307 · Cited by 4
Star Formation in Barred Galaxies
Phillips, A. C. (1996) · International Astronomical Union Colloquium · doi:10.1017/s025292110004940x · Cited by 4
Evolution and destruction of bars
Athanassoula, E., & Bosma, A. (2003) · Astrophysics and Space Science · doi:10.1023/a:1024004227017 · Cited by 4
Self-citationThe Effect of Bars on the Fueling of Star Formation and Nonstellar Activity in Galaxy Nuclei
Ho, L. C., Filippenko, A. V., & Sargent, W. L. W. (1996) · International Astronomical Union Colloquium · doi:10.1017/s025292110004971x · Cited by 4
Star formation and AGN fuelling
Maiolino, R., Alonso‐Herrero, A., Anders, S. W., et al. (1999) · Advances in Space Research · doi:10.1016/s0273-1177(99)00234-3 · Cited by 4
Stars and gas in the inner parts of galaxies seen in SAURON integral field observations
Peletier, R. F., Fathi, K., Allard, E. L., et al. (2006) · New Astronomy Reviews · doi:10.1016/j.newar.2006.10.013 · Cited by 4
“Athanassoula (1992) shows how gas streaming manifests itself in galaxies with strong bars.”
Stellar population gradient in lenticular galaxies: NGC 1023, NGC 3115 and NGC 4203
Bassin, M., & Bonatto, C. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20031261 · Cited by 4
“It has also been predicted by theoretical analysis and numerical simulations of the dynamics in the central regions of spiral galaxies (Athanassoula 1992a,b; Martin 1995; Piner et al. 1995; Elmegreen 1996).”
BackgroundSimulating nearby disc galaxies on the main star formation sequence
Verwilghen, P., Emsellem, É., Renaud, F., Agertz, O., Valentini, M., Fraser-McKelvie, A., Meidt, S. E., Neumann, J., Schinnerer, E., Klessen, R. S., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554056 · Cited by 3
Bar formation in disc galaxies: internal kinematics and environmental influence in MaNGA galaxies
Aquino-Ortíz, E., Sodi, B. C., & Chim-Ramirez, K. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag015 · Cited by 3
Bar-driven Shocks in NGC 1365 Revealed by the Most Luminous Extragalactic Class I Methanol Maser
Chen, X., Yang, T., Song, S., et al. (2026) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae4517 · Cited by 3
“High-velocity dispersions ( ∼ 50 km s − 1 ) and complex, multicomponent line profiles in the southern bar lane are consistent with shocks expected at the leading edge of the bar potential where gas streamlines converge ( E. Athanassoula 1992; Y. Gao et al. 2021; E. Schinnerer et al. 2023 ) .”
The Impacts of Bars, Spirals, and Bulge Size on Gas-phase Metallicity Gradients in MaNGA Galaxies
Wisz, M. E., Masters, K. L., Daniel, K. J., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adbb6f · Cited by 3
“The same internal structures that generate radial mixing of stars can also drive radial gas flows (e.g. bars; Athanassoula 1992; Fragkoudi et al. 2016 or spirals; Orr et al. 2022).”
Cao, T.-W., Lu, N. Y., Xu, C. K., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae1f4 · Cited by 3
“According to the model of Athanassoula (1992), the 2-arm dust lanes are associated with the shock fronts triggered by the presence of a bar in a rotating gas disk.”
BackgroundMethodInfluentialBezborodov, M. A., Eremin, M. A., Korolev, V. V., et al. (2020) · Journal of Imaging · doi:10.3390/jimaging6090098 · Cited by 3
Multi-scale simulations of black hole accretion in barred galaxies
Jung, M., Illenseer, T. F., & Duschl, W. J. (2016) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201731688/pdf · Cited by 3
Periodic orbits of multiplicity higher than one in an N-body barred galaxy potential
Wang, Y., Athanassoula, E., Patsis, P. A., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243699 · Cited by 3
Self-citationCool interstellar medium as an evolutionary tracer in ALMA-observed local dusty early-type galaxies
Glass, D. H. W., Sansom, A. E., Davis, T. A., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3001 · Cited by 3
López-Cobá, C., Lin, L., & Sánchez, S. F. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad152a · Cited by 3
Bagge, R. S., Foster, C., D’Eugenio, F., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1341 · Cited by 3
Hα Nuclear Geyser (Bipolar Outflow) from the Barred Galaxy NGC 1415
Garcia-Barreto, J. A., Mayya, Y. D., & Guichard, J. (2019) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ab28c3 · Cited by 3
“First, they might have been regions of density enhancement and recent star formation due to shocks when gas meets the stellar bars in NGC 1415 (Athanassoula 1992) and try to follow x1 orbits along the major axis of the bars.”
BackgroundBosma, A. (1996) · Lecture notes in physics · doi:10.1007/bfb0101966 · Cited by 3
Potential-density pairs for bent bars
Vogt, D., & Letelier, P. S. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17857.x · Cited by 3
“Furthermore, hydrodynamics simulations of the response of a gaseous disc to the imposition of a non-axisymmetric bar (Athanassoula 1992; Wada 1994; Englmaier & Gerhard 1997; Fukuda, Wada & Habe 1998; Ann & Lee 2000; Englmaier & Shlosman 2000; Patsis & Athanassoula 2000; Maciejewski et al. 2002;…”
BackgroundPatsis, P. A., Kalapotharakos, C., & Grosbol, P. J. (2010) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2010.00955.x · Cited by 3
“1 I N T RO D U C T I O N The standard picture of shocks encountered in the gas flow in the bar region of rotating barred potentials is based on the presence of a stable x1 family of periodic orbits in the underlying stellar component (Athanassoula 1992a,b).”
BackgroundThe apparent “reversed” motion of gas and stars in M 82
Greve, A. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201016069 · Cited by 3
“1a), the [S iii] (9069 Å) and P10 (9015 Å) ionized gas emission lines show the velocity features of the bar; however, spraying (Athanassoula 1992; Downes et al. 1996; Wills et al. 2000, GWNP) and shocks seem to blur the clear signature of the x2-orbits (peaks).”
BackgroundCapelo, P. R. (2019) · WORLD SCIENTIFIC eBooks · doi:10.1142/9789813227958_0001 · Cited by 4
“Several IMBH candidates have been identified in dwarf galaxies (e.g. RGG 118; ∼5 × 104 M⊙; Baldassare et al., 2015) and populations of IMBHs in dwarf galaxies have been recently detected up to z ∼ 2 (e.g. Mezcua et al., 2018).”
BackgroundMethodInfluentialDetection of CO (J = 1–0) Emission from Barred Spiral Galaxies at z$\boldsymbol{\sim}$ 0.1
matsui, K., Sorai, K., Watanabe, Y., et al. (2012) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/64.3.55 · Cited by 3
“…features is thought to influence the evolution of disk galaxies through redistributing angular momentum among the galaxy components, such as stars, gas and dark matter, and transferring gas to the central kiloparsec regions (e.g., Athanassoula 1992a, 1992b; Sellwood & Wilkinson 1993).”
BackgroundGasflows in Barred Galaxies with Big Orbital Loops—A Comparative Study of Two Hydrocodes
Pastras, S., Patsis, P. A., & Athanassoula, E. (2022) · Universe · doi:10.3390/universe8050290 · Cited by 3
“For test purposes, we carried out a complete study with the potential in [1], using all Ferrers models of that work having index n = 1, with the RAMSES code [27].”
InfluentialSelf-citationHubble Space Telescope Images of Nuclear Rings in Barred Galaxies
Barth, A. J., Ho, L. C., Filippenko, A. V., et al. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049502 · Cited by 3
Resonantly Excited Waves in Gaseous Disks: Asymptotic Theory versus Numerical Hydrodynamics
Kuo, C., & Yuan, C. (1999) · The Astrophysical Journal · doi:10.1086/306759 · Cited by 3
Bar triggered nuclear activity and the anisotropic radiation fields of Active Galactic Nuclei
Axon, D. J., & Robinson, A. (2007) · Springer eBooks · doi:10.1007/bfb0101981 · Cited by 3
Kinematics and mass modelling of NGC 1068
Dehnen, W., Bland-Hawthorn, J., Quirrenbach, A., et al. (1997) · CERN Document Server (European Organization for Nuclear Research) · Cited by 3
BARS FROM THE INSIDE OUT: AN HST STUDY OF THEIR DUSTY CIRCUMNUCLEAR REGIONSPreprint
Martini, P. (2004) · Cited by 3
Rutherford, T. H., Fraser-McKelvie, A., Emsellem, É., Sande, J. V., Croom, S. M., Poci, A., Martig, M., Gadotti, D. A., Pinna, F., Valenzuela, L. M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202556418 · Cited by 2
Molecular gas and star formation in central rings across nearby galaxies
Gleis, D. R., Stuber, S. K., Schinnerer, E., Neumann, J., Meidt, S. E., Querejeta, M., Emsellem, É., Leroy, A. K., Barnes, A. T., Bigiel, F., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557430 · Cited by 2
Bars in low-density environments rotate faster than bars in dense regions
Puczek, N., Géron, T., Smethurst, R. J., & Lintott, C. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag175 · Cited by 2
Spitoni, E., Schultheis, M., Matteucci, F., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202558155 · Cited by 2
Kinematic-distance biases in the inner Milky Way from a stellar dynamically constrained bar
Baba, J. (2026) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psag021 · Cited by 3
ALMA FACTS. III. High-resolution CO(2–1)/CO(1–0) Maps of Twelve Nearby Galaxies
Lee, A. M., Koda, J., Egusa, F., et al. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae4d39 · Cited by 2
“It has been suggested that the offset ridges are regions of strong shocks (Athanassoula 1992a,b; Sellwood & Wilkinson 1993), which should naturally increase n H 2 and T k , and hence, R 21 .”
Pan, H.-A., Kuno, N., Sorai, K., et al. (2015) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psv086 · Cited by 2
“The offset ridges trace the shocks that are associated with the crowded gas orbits, as suggested by theore - ical studies (Athanassoula 1992).”
BackgroundInfluentialAdibekyan, V., & Петросян, А. Р. (2009) · Astrophysics · doi:10.1007/s10511-009-9062-8 · Cited by 2
D’Onofrio, M., Rampazzo, R., Zaggia, S., et al. (2016) · Astrophysics and space science library · doi:10.1007/978-3-319-31006-0_4 · Cited by 2
Massive stellar systems: observational challenges and perspectives in the E-ELT era
Bono, G., Braga, V. F., Ferraro, I., et al. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921315010856 · Cited by 2
“However, photometric and spectroscopic investigations of RRLs in the Bulge stop at 2 degrees from the NB.”
BackgroundInfluentialShamir, L. (2023) · Astronomy and Computing · doi:10.1016/j.ascom.2023.100712 · Cited by 2
“Dust lanes can also make galaxies seem unusual due to the reduction of light blocked by the dust lane (Möllenhoff and Bender, 1989; Athanassoula, 1992).”
BackgroundAGN feeding along a one-armed spiral in NGC 4593
Kianfar, K., Andreani, P., Fernández-Ontiveros, J. A., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451185 · Cited by 2
Connection between Nonaxisymmetric Structures and Neutral Gas Distribution in Disk Galaxies
Liang, Z.-Z., Wang, J., Gao, H., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad87f1 · Cited by 2
“In simulations, this in fl ow could have an in fl ow rate of ∼ ( 0.01 – 100 ) M ☉ yr − 1 , depending on the bar strength and pattern speed ( E. Athanassoula 1992; M. W. Regan & P. J. Teuben 2004; W.-T. Kim et al. 2012a ) .”
InfluentialSelf-citationThe impact of radial migration on disk galaxy star formation histories
Bernaldez, J. P., Minchev, I., Ratcliffe, B., Marques, L., Sysoliatina, K., Walcher, J., Александрович, Х. С., Martig, M., de Jong, R. S., & Steinmetz, M. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557002 · Cited by 2
Ωbar in NGC 5597 from Very Large Array H i 21 cm Observations
García-Barreto, J. A., & Momjian, E. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac76be · Cited by 2
“…= 1 suggests that a plausible interpretation for the north spiral optical arm might be an outer m= 4 resonance in NGC 5597 (Contopoulos et al. 1989; Athanassoula 1992). ma (∼3.74 kpc) in NGC 5597 (see Section 3.1.5) as the corotation radius would result in Ωgas ∼ 15.3 km s −1 kpc−1; therefore,…”
BackgroundInfluentialCosmic Magnetic Fields – An Overview
Wielebinski, R., & Beck, R. (2010) · Springer eBooks · doi:10.1007/978-1-4419-7317-7_5 · Cited by 2
Infrared Emission from Barred Spiral Galaxies
Hawarden, T. G., Huang, J., & Gu, Q. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049411 · Cited by 2
Kubryk, M., Prantzos, N., & Athanassoula, E. (2014) · HAL (Le Centre pour la Communication Scientifique Directe) · doi:10.48550/arxiv.1412.4859 · Cited by 2
“Numerical simulations (Athanassoula 1992; Friedli & Benz 1993; Shlosman & Noguchi 1993) showed that the presence of a non-axisymmetric potential from a bar can drive important amounts of gas inwards of corotation (CR) fuelling star formation in the galactic nucleus, while at the same time gas is…”
BackgroundSelf-citationSlavcheva‐Mihova, L., & Mihov, B. (2011) · Astronomische Nachrichten · doi:10.1002/asna.201011489 · Cited by 2
“Generally, the PA along bars is well constrained thanks to thex1 orbits (e.g., Athanassoula 1992). c© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim www.an-journal.org As bar length,ℓ, we adopted the SMA, where the ellipticity decreases with 15% from its maximal value, after Martinez-Valpuesta,…”
MethodPhysical conditions and molecular chemistry of the Central Molecular Zone
Rodríguez-Fernández, N. J. (2006) · Journal of Physics Conference Series · doi:10.1088/1742-6596/54/1/006 · Cited by 2
On the classification of ultra-compact nuclear rings
Comerón, S., Knapen, J. H., & Beckman, J. E. (2008) · Journal of Physics Conference Series · doi:10.1088/1742-6596/131/1/012046 · Cited by 2
Stellar bars in disk galaxies: from banyans to butterflies?
Shlosman, I. (1999) · Physics Reports · doi:10.1016/s0370-1573(98)00122-7 · Cited by 2
Planetary nebulae and the chemical evolution of the galactic bulge: New abundances of older objects
Cavichia, O., Costa, R. D. D., Mollá, M., et al. (2011) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921312011258 · Cited by 2
Determining the type of orbits in the central regions of barred galaxies
Zotos, E. E., & Caranicolas, N. D. (2016) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/16/2/026 · Cited by 2
“…decades, a huge amount of research work has been devoted to understanding the orbital structure in barred galaxy models (e.g., Athanassoula et al. 1983; Pfenniger 1984; Combes et al. 1990; Athanassoula 1992; Pfenniger 1996; Kaufmann & Contopoulos 1996; Olle & Pfenniger 1998; Pichardo et al. 2004).”
BackgroundLopsided gas discs arising from mass inflow in barred spiral galaxies
Dupuy, J. L., Heitsch, F., & Cecil, G. N. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz975 · Cited by 2
Neumann, J., Gadotti, D. A., Wisotzki, L., et al. (2019) · Kölner Universitäts PublikationsServer (Universität zu Köln) · doi:10.48550/arxiv.1905.05214 · Cited by 2
Star formation history in the central region of the barred galaxy NGC 7177
Сильченко, О. К., & Smirnova, A. A. (2010) · Astronomy Letters · doi:10.1134/s1063773710050026 · Cited by 2
“According to the model results by Athanassoula (1992), the change in the orientation of the dust lanes as the center is approached is evidence for the presence of a double inner Lindblad resonance in the bar.”
BackgroundResultBarred Galaxies: Scientific Overview
Freeman, K. C. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100049356 · Cited by 2
Bars as Triggers of Gas Inflow
Athanassoula, E. (1995) · Highlights of Astronomy · doi:10.1017/s1539299600012004 · Cited by 2
Self-citationIshizuki, S. (1999) · Advances in Space Research · doi:10.1016/s0273-1177(99)00220-3 · Cited by 2
Evidence for radiation field collimation in NGC4151
Robinson, A., Axon, D. J., Pérez, E., et al. (1996) · Vistas in Astronomy · doi:10.1016/0083-6656(95)00104-2 · Cited by 2
5.16. CO mapping of barred spiral galaxies
Kuno, N., Nakai, N., Nishiyama, K., et al. (1998) · Symposium - International Astronomical Union · doi:10.1017/s0074180900084783 · Cited by 2
Fabry-Perot Observations and Hydrodynamical Simulations of the Barred Spiral NGC 4123
Weiner, B. J., Sellwood, J. A., & Williams, T. B. (1996) · International Astronomical Union Colloquium · doi:10.1017/s0252921100050302 · Cited by 2
Bar None? SQIID Observations of IC 342 Reveal Non-axisymmetric Stellar Distribution
Levine, D. A., Hurt, R. L., & Turner, J. L. (1994) · Astrophysics and space science library · doi:10.1007/978-94-011-1070-9_63 · Cited by 2
Spectral study of star-forming rings in S0 galaxies of Dorado group – NGC 1533 and NGC 1543
Proshina, I. S., Сильченко, О. К., & Kniazev, A. Y. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1314 · Cited by 1
Are Purely Gaseous Bars in Dwarf Irregulars a Myth?
Anagha, A. G., & Banerjee, A. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adbf00 · Cited by 1
“…rotates about the galactic center with a constant angular speed called the pattern speed (Aguerri et al. 2015), with the stars therein streaming along highly eccentric orbits co-aligned with its major axis (Weinberg 1985a, Contopoulos & Grosbol 1989, Athanassoula 1992,Kormendy & Kennicutt 2004).”
Discovery of a Giant Molecular Cloud at the Midpoint of the Galactic Bar Dust Lanes: M4.7–0.8
Butterfield, N., Morgan, L. K., Barnes, A. T., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adc687 · Cited by 1
“Orbital motions within the bar can create a shearing effect on the interstellar medium (ISM, Athanassoula 1992; Emsellem et al. 2015; Renaud et al. 2015).”
InfluentialGhosh, S., Kalda, T., Matteo, P. D., Green, G. M., Александрович, Х. С., Katz, D., & Haywood, M. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554692 · Cited by 1
Chemically Primitive Dwarf Accretion Reignites the Inner Disk Assembly of Malin 1
Kataria, M., & Saha, K. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae200d · Cited by 1
“The gas density is usually low within most of the bar region, with enhanced densities forming along the bar edges and in nuclear spiral-like structures (Athanassoula 1992).”
Kim, J., Leroy, A. K., Sandstrom, K. M., Meidt, S. E., Teng, Y.-H., Querejeta, M., Schinnerer, E., Clark, S. E., Chown, R., Glover, S. C. O., et al. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae4599 · Cited by 1
Bar-informed kinematic-distance mapping of molecular gas in the inner Milky Way
Baba, J. (2026) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psag045 · Cited by 1
Treß, R. G., Brucy, N., Girichidis, P., Glover, S. C. O., Göller, J., Hirschmann, M., Klessen, R. S., Peter, T., Petersson, J., Sormani, M. C., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202558503 · Cited by 1
The Radial and Vertical Structure of Molecular Gas in the Edge-on Galaxy NGC 4565
Krahm, G., Leroy, A. K., Sun, J., et al. (2026) · The Astronomical Journal · doi:10.3847/1538-3881/ae710b · Cited by 1
“In many barred galaxies, star formation in rings is attributed to bar-driven gas inflows that funnel material inward along dust lanes and deposit it near resonance radii (e.g., Athanassoula 1992; Seo & Kim 2013; Sormani et al. 2023).”
A nuclear disc at Cosmic Noon: evidence of early bar-driven galaxy evolution
Conte, Z. A. L., Gadotti, D. A., Harvey, T. E., et al. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag1122 · Cited by 1
Self-citationJolly, J.-B., Tacconi, L. J., Genzel, R., et al. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202660514 · Cited by 1
Bar Dissolution and Reformation Mechanisms
Bournaud, F., & Combes, F. (2004) · Astrophysics and space science library · doi:10.1007/978-1-4020-2862-5_13 · Cited by 1
A Molecular Face-on View of the Galactic Center Region
Sawada, T., Hasegawa, T., Handa, T., et al. (2003) · Astronomische Nachrichten · doi:10.1002/asna.200385088 · Cited by 1
Formation of nuclear rings of barred galaxies and star formation therein
Kim, W., Seo, W.-Y., & Kim, Y. (2013) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131400012x · Cited by 1
“Following Athanassoula (1992), we consider a very simple galaxy model in which the external gravitational potential responsible for disk rotation consists of a stellar disk, a bulge/halo with mass Mbul, a stellar bar with mass Mbar, and a central black hole with mass M•= 4×107 M .”
BackgroundMethodResultInfluentialThe evolution of the Galactic nuclear bulge traced by Cepheid variable stars
Matsunaga, N. (2012) · Journal of Physics Conference Series · doi:10.1088/1742-6596/372/1/012026 · Cited by 1
Star formation properties in barred galaxies
Zhou, Z., Cao, C., & Wu, H. (2011) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921312009751 · Cited by 1
Streaming Motions in the Spiral Galaxy NGC 864
Erroz-Ferrer, S. (2015) · Springer theses · doi:10.1007/978-3-319-26398-4_4 · Cited by 1
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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