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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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3D Modeling of the Molecular Gas Kinematics in Optically Selected Jellyfish Galaxies
Bacchini, C., Mingozzi, M., Poggianti, B. M., Moretti, A., Gullieuszik, M., Marasco, A., Sodi, B. C., Sánchez-García, O., Vulcani, B., Werle, A., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acc9b9 · Cited by 17
“Both features are typical of barred galaxies (e.g., Athanassoula 1992a; Bureau & Freeman 1999; Merrifield & Kuijken 1999; Kormendy & Kennicutt 2004; Hogarth et al. 2021).”
BackgroundThe robustness in identifying and quantifying high-redshift bars using JWST observations
Liang, X., Yu, S.-Y., Fang, T., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348539 · Cited by 17
Impacts of Bar-driven Shear and Shocks on Star Formation
Kim, T., Gadotti, D. A., Querejeta, M., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad410e · Cited by 17
“Gas fl ows inward along the bar dust lanes, which are found at locations of hydrodynamic shocks based on simulations ( e.g., Roberts et al. 1979; Athanassoula 1992; Sormani et al. 2015; Fragkoudi et al. 2017 ) .”
BackgroundInfluentialThe effect of projection on the observed gas velocity fields in barred galaxies
Moisseev, A. V., & Mustsevoi, V. V. (2000) · Astronomy Letters · doi:10.1134/1.1307890 · Cited by 17
“Such an arrangement of shock fronts is consistent with both the observations of dust lanes in bars and with the results of earlier numerical simulations (Athanassoula 1992a, 1992b).”
BackgroundResultValenzuela, O., Hernández-Toledo, H. M., Cano-Díaz, M., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/147/2/27 · Cited by 17
“CO Intensity maps It is well established in galaxy dynamics that a galaxy bar produces interstellar medium schocks wich can be traced by dust lanes (Athanassoula 1992; Prendergast 1983).”
BackgroundKinematics of Arp 270: gas flows, nuclear activity and two regimes of star formation
Zaragoza-Cardiel, J., Font-Serra, J., Beckman, J. E., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt527 · Cited by 17
“The velocity profiles are strongly reminiscent of the simulated profiles in Athanassoula (1992), in which gas is shocked as it collides with the bar, forming dust lanes, with their characteristic morphology.”
BackgroundBoxy/peanut and discy bulges: formation, evolution and properties
Athanassoula, E. (2007) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921308017389 · Cited by 17
“This inflow is due to the torques exerted by a nonaxisymmetric component, usually a large-scale bar, as witnessed in hydrodynamic simulations (e.g. Athanassoula 1992; Friedli & Benz 1993; Heller & Shlosman 1994; Wada & Habe 1995).”
BackgroundSelf-citationThe Effect of Bars on the Ionized ISM: Optical Emission Lines from Milky Way Analogs
Krishnarao, D., Tremonti, C., Fraser-McKelvie, A., Kraljic, K., Boardman, N. F., Masters, K. L., Benjamin, R. A., Haffner, L. M., Jones, A. M., Pace, Z. J., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9fa3 · Cited by 17
“Inflowing material along the bar can fuel central mass concentrations (such as the CMZ in the Milky Way) or AGN, as observed in other galaxies (e.g., George et al. 2019) and in simulations (e.g., Athanassoula 1992).”
BackgroundZhang, C., Peng, Y., Ho, L. C., Maiolino, R., Renzini, A., Mannucci, F., Dekel, A., Guo, Q., Li, D., Yuan, F., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abd723 · Cited by 17
“A strong bar is able to drive gas inflows toward galactic center (Athanassoula 1992; Sheth et al. 2005) and produce a gas-deficient region on the scale of several kiloparsecs (Gavazzi et al. 2015; Spinoso et al. 2017).”
BackgroundBayesian inference of three-dimensional gas maps
Mertsch, P., & Vittino, A. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141000 · Cited by 17
Englmaier, P., & Gerhard, O. (2006) · Celestial Mechanics and Dynamical Astronomy · doi:10.1007/s10569-006-9003-3 · Cited by 17
“2 times the radius of the bar ends (Athanassoula 1992). Larger values would be possible if the bar were able to slow down (Debattista and Sellwood 2000). Our corotation derived above is consistent with the condition RCR/Rbar = 1.2 ± 0.2, however, if the bar length turns out to be underestimated, we would need to incre…”
BackgroundResultInfluentialCircumnuclear star-forming activities along the Hubble sequence
Shi, L., Gu, Q., & Peng, Z. (2005) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20054045/pdf · Cited by 17
The Molecular Gas in the Circumnuclear Region of Seyfert Galaxies
Schinnerer, E., Eckart, A., & Tacconi, L. J. (1999) · The Astrophysical Journal · doi:10.1086/312288 · Cited by 17
“The bar model requires highly elliptical orbits inside the ring, thus making the ILR interpretation of the 2 kpc stellar near-IR bar (Scoville et al. 1988) very unlikely since it is expected that the orbits become more circular inside the ILR (e.g., Athanassoula 1992).”
BackgroundMethodValenzuela, O., Hern, H., Puerari, I., et al. (2016) · Cited by 17
Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Otter, J. A., Rowlands, K., Alatalo, K., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9dee · Cited by 16
“It is also possible that the WHAN and BPT-classified AGN spaxels away from the center of this galaxy are from shocks that could be driven by the rotation of the bar, as has been observed in other strongly barred galaxies (e.g., Athanassoula 1992).”
BackgroundThe most luminous, merger-free AGNs show only marginal correlation with bar presence
Garland, I. L., Fahey, M. J., Simmons, B. D., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad966 · Cited by 16
Choi, W., Liu, L., Bureau, M., Cappellari, M., Davis, T. A., Gensior, J., Liang, F.-H., Lu, A., Williams, T. G., & Chung, A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1211 · Cited by 16
FIRST VIEWS OF A NEARBY LIRG: STAR FORMATION AND MOLECULAR GAS IN IRAS 04296+2923
Meier, D. S., Turner, J. L., Beck, S. C., et al. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/140/5/1294 · Cited by 16
“For more expected net inflow rates of a few percent of the orbital velocity (Athanassoula 1992), Ṁinf ∼ 1 M yr −1.”
BackgroundInfluentialMetallicities in the Outer Regions of Spiral Galaxies
Bresolin, F. (2017) · Astrophysics and space science library · doi:10.1007/978-3-319-56570-5_5 · Cited by 16
“While stellar bars can affect the chemical evolution in the inner regions of galaxies (Athanassoula 1992; Cavichia et al. 2014), the overlap of spiral and bar resonances (Minchev et al. 2011) can affect the distribution and metallicity of stars at large galactocentric distances.”
BackgroundRapid Formation of Black Holes in Galaxies: A Self-limiting Growth Mechanism
Li, Z., Sellwood, J. A., & Shen, J. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9377 · Cited by 16
“A gaseous “inner ring” that lies on the edge of the bar is commonly seen in the simulations using a prolate spheroid (e.g., Athanassoula 1992; Kim et al. 2012a), while such a feature has not been found in observations.9 In addition, Fragkoudi et al. (2016) argued that boxy/peanut (B/P) bulges…”
BackgroundMethodA slow bar in the lenticular barred galaxy NGC 4277
Buttitta, C., Corsini, E. M., Cuomo, V., Aguerri, J. A. L., Coccato, L., Costantin, L., Bontà, E. D., Debattista, V. P., Iodice, E., Méndez‐Abreu, J., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244297 · Cited by 15
Determination of the Pattern Speed of Barred Spiral Galaxies
Hirota, A., Kuno, N., Sato, N., et al. (2009) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/61.3.441 · Cited by 16
“The parameters describing each component are the same as those of run066 in Athanassoula (1992), which is widely used for studies of the dynamical response of the ISM to the barred potential.”
MethodInfluentialBars as seen byHerscheland Sloan
Consolandi, G., Dotti, M., Boselli, A., et al. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629213 · Cited by 16
“We conclude that the FIR morphologies are similar to the Hα morphologies (consistent with Verley et al. 2007) and that both are consistent with bar-driven inflows of gas inside the corotation radius as predicted by simulations (Sanders & Huntley 1976; Athanassoula 1992).”
BackgroundMethodThe complex multi-component outflow of the Seyfert galaxy NGC 7130
Comerón, S., Knapen, J. H., Almeida, C. R., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039382 · Cited by 16
“In non-interacting galaxies, and at scales larger than 1 kpc, inwards gas transportation can be efficiently triggered by energy dissipation at shocks and gravitational torques associated with bars (Schwarz 1984; Athanassoula 1992) and spiral arms (Lubow et al. 1986; Kim & Kim 2014).”
BackgroundThe Molecular Gas in the Circumnuclear Region of Seyfert Galaxies
Schinnerer, E., Eckart, A., Tacconi, L. J., et al. (1999) · OpenGrey (Institut de l'Information Scientifique et Technique) · Cited by 16
Knapen, J. H. (2004) · Astrophysics and space science library · doi:10.1007/978-1-4020-2862-5_16 · Cited by 16
“along the leading edges of the bar, whereas the dust lanes will be more curved in weak bars (Athanassoula 1992).”
BackgroundOuter dynamics and escapes in barred galaxies
Contopoulos, G., & Patsis, P. A. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10388.x · Cited by 16
Hydrodynamic Simulations for the Nuclear Morphology of NGC 4314
Ann, H. B. (2001) · The Astronomical Journal · doi:10.1086/320374 · Cited by 16
“Because the shape and orientation of a nuclear ring depend on the dynamical properties of a galaxy (Combes & Gerin 1985 ; Athanassoula 1992 ; Piner, Stone, & Teuben 1995 ; Ann & Lee 2000), we can use the morphology of a nuclear ring, combined with hydrodynamic simulations, as a probe of the…”
BackgroundMethodFUELLING STARBURSTS AND AGNPreprint
Knapen, J. H. (2004) · Cited by 16
On the 3D dynamics and morphology of inner ringsPreprint
Patsis, P. A., Skokos, C., & Athanassoula, E. (2003) · Cited by 16
Self-citationUnveiling the origins of galactic bars: insights from barred and unbarred galaxies
López, P. D., Scannapieco, C., Cora, S. A., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae576 · Cited by 15
Discovery of ~2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy
Li, J., Kreckel, K., Sarbadhicary, S. K., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450730 · Cited by 15
ADF22-WEB: A giant barred spiral starburst galaxy in the z = 3.1 SSA22 protocluster core
Umehata, H., Steidel, C. C., Smail, I. R., et al. (2025) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psaf010 · Cited by 15
“…of the ISMs is a common feature seen in local barred spiral galaxies and have been reproduced by numerical and analytical calculations, including the cloud-orbit and hydrodynamical shock wave models (Contopoulos & Papayannopoulos 1980, Binney et al. 1991, Athanassoula 1992, Schinnerer et al. 2023).”
Oka, T., & Geballe, T. R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb1b5 · Cited by 16
“…orbit with high eccentricity The interpretation of the gas in the CMZ as having a largely circular distribution, as suggested by the EMR and GCR, was drastically modified by Binney et al. (1991), who developed a theory of gas motion in the Galactic barred potential (see also Athanassoula 1992a,b).”
MethodOn the morphology of dust lanes in galactic bars
Sánchez-Menguiano, L., Pérez, I., Zurita, A., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv782 · Cited by 15
“Athanassoula (1992), analysing simulations for fast bars, deduced that curved dust lanes result from weak bars and straight ones originate from strong bars.”
BackgroundResultInfluentialEFFECT OF CENTRAL MASS CONCENTRATION ON THE FORMATION OF NUCLEAR SPIRALS IN BARRED GALAXIES
Thakur, P., Ann, H. B., & Jiang, I.-G. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/693/1/586 · Cited by 15
“If the ILR is absent, the x2-orbits do not exist, and strong gas inflow to the center can take place (Athanassoula 1992; Piner et al. 1995).”
BackgroundSpiral galaxies with a central plateau in the gas velocity curve along the major axis
Coccato, L., Corsini, E. M., Pizzella, A., et al. (2005) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20042228 · Cited by 15
“Qualitatively, the minor-axis gas kinematics can be explained as due to non-circular (e.g., Athanassoula 1992) or off-plane (e.g., Friedli & Benz 1993) motions induced on the gaseous component by the tumbling triaxial potential of the bar.”
BackgroundPan, H.-A., Lim, J., Matsushita, S., Wong, T., & Ryder, S. D. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/768/1/57 · Cited by 15
“2) exhibits an S-shaped asymmetry characteristic of periodic orbits predicted theoretically for barred galaxies (e.g., Athanassoula 1992, and references therein).”
BackgroundExamining the Seyfert - Starburst Connection with Arcsecond Resolution Radio Continuum Observations
Laine, S., Kotilainen, J. K., Reunanen, J., et al. (2005) · CERN Document Server (European Organization for Nuclear Research) · Cited by 15
Dynamical modelling of a remarkable four-armed barred spiral galaxy ESO 566-24
Rautiainen, P., Salo, H., & Buta, R. (2003) · CERN Document Server (European Organization for Nuclear Research) · Cited by 15
Shibatsuka, T., Matsushita, S., Kohno, K., et al. (2003) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/55.1.87 · Cited by 15
Structure and Kinematics of COJ= 2–1 Emission in the Central Region of NGC 4258
Sawada‐Satoh, S., Ho, P. T. P., Müller, S., et al. (2007) · The Astrophysical Journal · doi:10.1086/511762 · Cited by 15
“Here we discuss the possibility that Component 1 and 3 are molecular gas produced by bar driven shocks, and that they flow in and around the bars into the periodic orbit perpendicular to the arms (e.g. Athanassoula 1992; Downes et al. 1996).”
BackgroundGalactic Bar/Spiral Arm Interactions in NGC3627Preprint
Beuther, H., Meidt, S. E., Schinnerer, E., et al. (2016) · arXiv (Cornell University) · doi:10.48550/arxiv.1609.06448 · Cited by 15
Large gas inflow driven by a matured galactic bar in the early Universe
Huang, S., Kawabe, R., Umehata, H., et al. (2025) · Nature · doi:10.1038/s41586-025-08914-2 · Cited by 14
“Then, a plausible explanation for the observed velocity is that the gas flows from pericenter to apocenter along elongated orbits in bar potential 16 (Figure 4) and appears to move outward.”
CO(2–1)/CO(1–0) Line Ratio on a ∼100 Parsec Scale in the Nearby Barred Galaxy NGC 1300
Maeda, F., Egusa, F., Ohta, K., Fujimoto, Y., Habe, A., & Asada, Y. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac4505 · Cited by 14
“…of GMCs in the bar regions; the strong shock or/and shear, which would make GMCs stripped, shredded, and finally destroyed (e.g., Tubbs 1982; Athanassoula 1992; Reynaud & Downes 1998; Emsellem et al. 2015), the presence of gravitationally unbound GMCs (Sorai et al. 2012; Nimori et al.…”
BackgroundGASP. XLV. Stellar Bars in Jellyfish Galaxies: Analysis of Ionized Gas and Stellar Populations
Sánchez-García, O., Sodi, B. C., Fritz, J., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb269 · Cited by 14
Disc galaxies are still settling
de Sá-Freitas, C., Gadotti, D. A., Fragkoudi, F., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347028 · Cited by 14
Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Gramze, S. R., Ginsburg, A. G., Meier, D. S., Ott, J., Shirley, Y. L., Sormani, M. C., & Svoboda, B. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ad01be · Cited by 16
“X 1 orbits are nested, elongated ellipses that make up the main body of the bar, but become self-intersecting as material loses angular momentum due to crossing orbits ( Athanassoula 1992 ) .”
BackgroundWhy does the Milky Way have a bar?
Александрович, Х. С., Minchev, I., Steinmetz, M., Ratcliffe, B., Walcher, C. J., & Libeskind, N. I. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1902 · Cited by 16
Large velocity dispersion of molecular gas in bars of strongly barred galaxies NGC 1300 and NGC 5383
Maeda, F., Ohta, K., Fujimoto, Y., et al. (2018) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psy028 · Cited by 14
“Athanassoula (1992) argued that strong shear motion in a bar region prevents molecular cloud formation.”
BackgroundThe Evolution of NGC 7465 as Revealed by Its Molecular Gas Properties
Young, L. M., Meier, D. S., Bureau, M., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abe126 · Cited by 14
“In a bar model, this would imply that either dense gas is present beyond the inner Lindblad resonance (ILR), contrary to expectation (e.g., Athanassoula 1992), or alternatively that the radius of the ILR is much larger than is usual in early-type disk galaxies, and it extends to almost the end of…”
Iles, E. J., Pettitt, A. R., & Okamoto, T. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3330 · Cited by 14
HOT DIFFUSE EMISSION IN THE NUCLEAR STARBURST REGION OF NGC 2903
Yukita, M., Swartz, D. A., Tennant, A. F., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/758/2/105 · Cited by 14
“The gas forms thin “centered” dust lanes along the bar (Athanassoula 1992).”
BackgroundMultiwavelength study of the star-formation in the bar of NGC 2903
Popping, G., Pérez, I., & Zurita, A. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014183 · Cited by 14
“Dust lanes can be used as tracers of shocks in the gas flow (Athanassoula 1992).”
BackgroundAre galactic disks dynamically influenced by dust?
Theis, C., & Orlova, N. (2004) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20034047 · Cited by 14
“This, however, might change when strongly barred nuclei are investigated as the simulations by Athanassoula (1992) have revealed.”
Regular motions in double bars - II. Survey of trajectories and 23 models
Maciejewski, W., & Athanassoula, E. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13418.x · Cited by 14
“This shows limitations of the axisymmetric approximation,already pointed out for a single bar, when the x2 orbits can be absent dspite the presence of the azimuthally-averaged Inner Lindblad Resonance (e.g. Athanassoula 1992a).”
BackgroundMethodInfluentialSelf-citationPan, H.-A., Lim, J., Matsushita, S., Wong, T., & Ryder, S. D. (2013) · Cited by 14
Nuclear starburst-driven evolution of the central region in NGC 6764
Léon, S., Eckart, A., Laine, S. J., et al. (2007) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20066075/pdf · Cited by 14
Potential Black Hole Seeding of the Spiral Galaxy NGC 4424 via an Infalling Star Cluster
Graham, A. W., Soria, R., Ciambur, B. C., Davis, B. L., & Swartz, D. A. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac235b · Cited by 14
“One can also see that the dust lane, associated with obscuration in Figure 3, and a studied feature in some spiral galaxy bars (e.g., Athanassoula 1992), also appears red.”
BackgroundH i and CO observations of Arp 104: a spiral-elliptical interacting pair
Cullen, H., Alexander, P. E., Green, D. A., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11506.x · Cited by 14
“Assuming co-rotation is at 1.2× R (Athanassoula 1992, 1994) yields a co-rotation radius of 17.”
BackgroundInfluentialOnodera, S., Koda, J., Sofue, Y., et al. (2004) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/56.3.439 · Cited by 14
“Bars are thought to be the most viable candidates for fueling the central activity, transferring mass from large to small scales (e.g. Simkin et al. 1980; Shlosman et al. 1989; Athanassoula 1992).”
BackgroundNuclear Rings in Galaxies - A Kinematic PerspectivePreprint
Mazzuca, L. M., Swaters, R. A., Knapen, J. H., et al. (2016) · Cited by 14
The bar rotation rate as a diagnostic of dark matter content in the centre of disc galaxies
Buttitta, C., Corsini, E. M., Aguerri, J. A. L., Coccato, L., Costantin, L., Cuomo, V., Debattista, V. P., Morelli, L., & Pizzella, A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad646 · Cited by 12
Kolcu, T., Maciejewski, W., Gadotti, D. A., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1896 · Cited by 13
“…cause starbursts in nuclear rings (Heller & Shlosman 1994; Mazzuca et al. 2008) and change the morphology of the central regions by creating substructures (e.g., gaseous and stellar disks, rings) (Shlosman et al. 1989; Athanassoula 1992; Martini et al. 2003; Kim et al. 2012; Sormani et al. 2015).”
BackgroundInfluentialOrbital analysis of stars in the nuclear stellar disc of the Milky Way
Nieuwmunster, N., Schultheis, M., Sormani, M. C., Fragkoudi, F., Nogueras-Lara, F., Schödel, R., McMillan, P. J., Smith, L. C., & Sanders, J. L. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202349000 · Cited by 13
Piñol-Ferrer, N., Lindblad, P. O., & Fathi, K. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.20367.x · Cited by 13
“Athanassoula 1992), as well as the mechanisms which trigger starbursts and nuclear activity in the centers of galaxies (e.g., Shlosman et al. 1989).”
BackgroundDo nuclear rings in barred galaxies form at the shear minimum of the rotation curve?
Sormani, M. C., & Li, Z. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1139 · Cited by 13
“In order to avoid transients, we introduce the bar gradually, as is common practice in this type of simulations (e.g. Athanassoula 1992).”
How the bar properties affect the induced spiral structure
Garma-Oehmichen, L., Martinez-Medina, L. A., Hernández-Toledo, H. M., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab333 · Cited by 13
“Numerical simulations with steady bar potentials have found that the gas particles settle in steady-state trailing spirals (Sanders &Huntley 1976; Athanassoula 1992;Wada 1994; Rodriguez-Fernandez & Combes 2008).”
BackgroundZhang, C., Peng, Y., Ho, L. C., Maiolino, R., Renzini, A., Mannucci, F., Dekel, A., Guo, Q., Li, D., Yuan, F., et al. (2021) · Apollo (University of Cambridge) · doi:10.17863/cam.72494 · Cited by 13
THE CENTRAL REGION OF THE NEARBY SEYFERT 2 GALAXY NGC 4945: A PAIR OF SPIRALS
Lin, L., Taam, R. E., Yen, C.-C., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/731/1/15 · Cited by 13
“Ωp takes a value between 213 ≤ Ωp ≤ 249 km s −1 kpc−1, corresponding to a radial interval for the radius of the OILR of 0.17 kpc ≤ ROILR ≤ 0.22 kpc.”
BackgroundInfluentialFast cloud–cloud collisions in a strongly barred galaxy: suppression of massive star formation
Fujimoto, Y., Maeda, F., Habe, A., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa840 · Cited by 13
“It has been proposed that a strong shock and/or shear along the bar would inject turbulence into the dense gas to prevent star formation (Tubbs 1982; Athanassoula 1992; Downes et al. 1996; Reynaud & Downes 1998; Sorai et al. 2012; Meidt et al. 2013).”
BackgroundMaeda, F., Ohta, K., Fujimoto, Y., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab130 · Cited by 13
“Some hydrodynamic simulations and observations argued that existence of a high shear probably suppresses the molecular cloud formation (e.g. Athanassoula 1992; Zurita et al. 2004; Emsellem et al. 2015).”
BackgroundOn the relation between orbital structure and observed bar morphology
Patsis, P. A. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.08768.x · Cited by 13
“2 in Athanassoula 1992a).”
BackgroundMethodInfluentialGas Distribution and Starburst Activity in the Widely Separated Interacting Galaxy Pair NGC 6670
Wang, W.-H., Lo, K. Y., Gao, Y., et al. (2001) · The Astronomical Journal · doi:10.1086/321112 · Cited by 13
“Theoretical studies have shown that stellar and gaseous bars may play an important role in driving gas into the central regions of galaxies (Schwarz 1984 ; Athanassoula 1992 ; Barnes & Hernquist 1991).”
BackgroundThe circumnuclear environment of the peculiar galaxy NGC 3310
Hägele, G. F., Díaz Beltrán, Á. I., Cardaci, M. V., et al. (2010) · LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) · Cited by 13
Dynamical Evolution Driven by Bars and Interactions: Input from Numerical Simulations
Athanassoula, E. (2002) · Astrophysics and Space Science · doi:10.1023/a:1019595111382 · Cited by 13
“As a response to the bar forcing, the region in and around the bar is depleted of its gas, which concentrates in two narrow lanes along the leading edges of the bar (e.g. Athanassoula, 1992).”
BackgroundResultInfluentialSelf-citationCO Observations of the Interacting Galaxy Pair NGC 5394/95
Kaufman, M., Sheth, K., Struck, C., et al. (2002) · The Astronomical Journal · doi:10.1086/338433 · Cited by 13
“Straight dust lanes are the signature of a bar that extends between an inner Lindblad resonance and corotation (Athanassoula 1992a,b).”
BackgroundThe impact of bar origin and morphology on stellar migration
Iles, E. J., Pettitt, A. R., Okamoto, T., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3377 · Cited by 12
IllustrisTNG insights: Factors affecting the presence of bars in disk galaxies
Lu, S., Du, M., & Debattista, V. P. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453143 · Cited by 12
Zhou, Z., Cao, C., Meng, X., et al. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/142/2/38 · Cited by 12
“…may be a result of the concentration of gas inflowing from the disk under the influence of the bar, because the gravitational torque of the large-scale bar can make the gas lose angular momentum, and then drive it down inward through the stellar bar (Athanassoula 1992; Sellwood & Wilkinson 1993).”
BackgroundThe central region of the enigmatic Malin 1
Saha, K., Dhiwar, S., Barway, S., et al. (2021) · Journal of Astrophysics and Astronomy · doi:10.1007/s12036-021-09715-5 · Cited by 12
“It can funnel gas inwards (Combes, 2004) and ignite star-formation activity in the central region of a galaxy and lead to the formation of a pseudobulge (Athanassoula, 1992; ?”
BackgroundPhotometric Signature of Ultraharmonic Resonances in Barred Galaxies
Krishnarao, D., Pace, Z. J., D’Onghia, E., Aguerri, J. A. L., McClure, R. L., Peterken, T., Fernández-Trincado, J. G., Merrifield, M. R., Masters, K. L., Garma-Oehmichen, L., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac5d55 · Cited by 13
“This would be in contradiction with the classical view of bars supported by the orbits of the x1-family (e.g. Contopoulos & Papayannopoulos 1980; Athanassoula 1992).”
ResultUnderstanding the secular evolution of NGC 628 using UltraViolet Imaging Telescope
Ujjwal, K., Kartha, S. S., Subramanian, S., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2285 · Cited by 12
Kinematics of ionized gas in the barred Seyfert galaxy NGC 4151
Asif, M. W., Mundell, C. G., & Pedlar, A. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.08910.x · Cited by 12
“…1979; Schwarz 1985; Shlosman, Frank & Begelman 1989; Sakamoto et al. 1997), for example when gas streamlines associated with different orbit families converge and form shocks that dissipate angular momentum, thereby allowing gas to move to smaller radii (Prendergast 1983; Athanassoula 1992a,b).”
BackgroundSchultheis, M., Sormani, M. C., & Gadotti, D. A. (2025) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-025-00163-6 · Cited by 20
Bar properties as a function of wavelength: a local baseline with S4G for high-redshift studies
Menéndez‐Delmestre, K., Gonçalves, T. S., Sheth, K., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3662 · Cited by 11
Self-citationvan Donkelaar, F., Mayer, L., Capelo, P. R., Tamfal, T., Quinn, T., & Madau, P. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae804 · Cited by 11
Zheng, Y., & Shen, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad9bae · Cited by 11
“Analyses of the shapes of dust lanes predict the parameter to fall within a range of 1.2 ± 0.2 ( E. Athanassoula 1992 ) .”
InfluentialRediscovering the Milky Way with an orbit superposition approach and APOGEE data
Александрович, Х. С., Steinmetz, M., Haywood, M., van de Ven, G., Krajnović, D., Ratcliffe, B., Minchev, I., Matteo, P. D., Kacharov, N., Marques, L., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453305 · Cited by 20
Explaining two circumnuclear star forming rings in NGC 5248
van der Laan, T. P. R., Schinnerer, E., Emsellem, É., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321572 · Cited by 11
“Jogee et al. (2002b) estimate that the pattern speed for their 5.9 kpc large scale stellar bar must be close to 30 km s−1 kpc given the semi-major axis of that bar; a bar’s CR radius is typically at 1.2 ± 0.2 times the semi-major axis of the bar (Athanassoula 1992a).”
BackgroundInfluentialDíaz, R., Dottori, H., Vera-Villamizar, N., et al. (2003) · The Astrophysical Journal · doi:10.1086/381215 · Cited by 11
“Farther out, up to r 3:5 kpc, non-Keplerian motions begin to be evident in the rotation curve because the shape of the rotation curve in this region is strongly affected by the non-axisymmetric potential of the large-scale bar (e.g., Athanassoula 1992; Piner et al. 1995).”
BackgroundA slow lopsided bar in the interacting dwarf galaxy IC 3167
Cuomo, V., Corsini, E. M., Morelli, L., et al. (2022) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slac064 · Cited by 11
Kalinova, V., Colombo, D., Sánchez, S. F., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243541 · Cited by 11
Molecular Gas in Candidate Double‐Barred Galaxies. III. A Lack of Molecular Gas?
Petitpas, G. R., & Wilson, C. D. (2004) · The Astrophysical Journal · doi:10.1086/381569 · Cited by 11
“The two important ones are the x1 family that runs parallel to the bar major axis, and the x2 family that runs perpendicular to it (e.g., Athanassoula 1992).”
BackgroundRapid Formation of Black Holes in Galaxies: A Self-limiting Growth Mechanism
Li, Z., Sellwood, J. A., & Shen, J. (2018) · Cited by 11
NH3 in the Galactic Center is Formed under Cool Conditions
Nagayama, T., Omodaka, T., Handa, T., Toujima, H., Sofue, Y., Sawada, T., Kobayashi, H., & Koyama, Y. (2009) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/61.5.1023 · Cited by 12
“In such a case, a strong shock is expected at the leading edge of the bar (e.g., Sorensen et al. 1976; Athanassoula 1992).”
BackgroundHCN(1–0) enhancement in the bar of NGC 2903
Léon, S., Jeyakumar, S., Pérez-Ramírez, D., et al. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200810162 · Cited by 11
“Shocks are expected to trace the dust lane in the bar (Athanassoula 1992).”
BackgroundInfluentialSignificance of bar quenching in the global quenching of star formation
George, K., Subramanian, S., & Paul, K. T. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935207/pdf · Cited by 11
Petitpas, G., & Wilson, C. (2003) · CERN Document Server (European Organization for Nuclear Research) · Cited by 11
The effect of dust on Tremaine-Weinberg measurementsPreprint
Gerssen, J., & Debattista, V. P. (2007) · Cited by 11
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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