Orbits in the Bar of NGC 4314

Patsis, P. A.; Athanassoula, E.; Quillen, Alice C.

doi:10.1086/304287

Cited by 79 publications

(109 citation statements)

References 18 publications

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“…For Ω bar = 25 Gyr −1 we have all the resonances inside the galaxy and corotation radius outside of the bar (see Table 2). Our selection of the sound speed value is a compromise between various realistic values adopted by other authors (Patsis & Athanassoula 2000;Englmaier & Gerhard 1997;Otmianowska-Mazur & Chiba 1995) and our model numerical abilities.…”

Section: Results For the Reference Modelmentioning

confidence: 99%

“…The observational positions of dust lanes are identified with the shock regions obtained in the numerical model. The 2D SPH simulations presented in the second paper (Patsis & Athanassoula 2000) showed that the morphology of dust lanes were similar for two slow sound speeds (10 km s −1 and 15 km s −1 ). For the experiment with the fastest sound speed (30 km s −1 ) the structure of the dust lanes has changed, but this value of the sound speed is not found in real galaxies.…”

Section: Introductionmentioning

confidence: 86%

“…This confirms that the value of the bar angular velocity is crucial not only for the gas disrtibution but also for the magnetic field evolution. Patsis & Athanassoula (2000) investigated the influence of the sound speed upon the gas distribution in their models and showed that it is an important parameter for the gas dynamics in the inner part of the bar and the bar morphological structure. Inspired by this result, we performed calculations of new models, changing the value of the sound speed c s in the range between 5 km s −1 and 10 km s −1 .…”

Section: Influence Of Bar Angular Velocity On the Magnetic Field Distmentioning

confidence: 99%

“…We will discuss our results of 3D numerical MHD simulations in the context of two papers: Athanassoula (1992), and Patsis & Athanassoula (2000). In the first one, the author made hydrodynamical numerical simulations in 2D, showing that the dynamics of gas is closely related to the configuration of orbits in the gravitational potential of the galaxy, which is influenced by the gravitational potential of the bar.…”

Section: Introductionmentioning

confidence: 99%

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3D MHD simulations of magnetic field evolution and radio polarization of barred galaxies

Kulesza-Żydzik

Kulpa-Dybeł

Otmianowska-Mazur

et al. 2010

A&A

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Aims. We study numerically the large-scale gas and magnetic field evolution of barred galaxies in the gravitational potential of a disk, bulge, halo, and bar. We solve non-linear MHD equations including the back-reaction of the magnetic field to the gas. We do not take into account any dynamo process. Methods. We apply the numerical MHD code to calculate the model of the galaxy in three dimensions. We construct realistic maps of high-frequency (Faraday rotation free) polarized radio emission on the basis of the simulated magnetic fields. The polarization model includes the effects of projection and limited resolution. Results. The main result is that our modeled polarization maps resemble the radio polarization structures observed in barred galaxies. The modeled polarization B-vectors distribution along the bar and between spiral arms resembles the observed topology of the magnetic field in barred galaxies. Our calculations for several different rotational velocities and sound speeds give the same result we got in our previous earlier published model. The reason of this behaviour is the dynamical evolution of the bar that causes gas to form spiral waves going radially outward. A gaseous spiral arms in turn generates magnetic ones, which live much longer in the inter-arm disk space than the gaseous pattern.

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Section: Results For the Reference Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 86%

Section: Influence Of Bar Angular Velocity On the Magnetic Field Distmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

3D MHD simulations of magnetic field evolution and radio polarization of barred galaxies

Kulesza-Żydzik

Kulpa-Dybeł

Otmianowska-Mazur

et al. 2010

A&A

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“…Bar dust lanes have been studied from numerical simulations (e.g. van Albada & Sanders 1982;Athanassoula 1992;Patsis & Athanassoula 2000;Patsis, Kalapotharakos & Grosbøl 2010;Kim, Seo & Kim 2012), as well as observationally (e.g. Knapen, Pérez-Ramírez & Laine 2002;Marshall et al 2008;Comerón et al 2009).…”

Section: Introductionmentioning

confidence: 99%

On the morphology of dust lanes in galactic bars

Sánchez-Menguiano¹,

Pérez²,

Zurita³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The aim of our study is to use dynamical simulations to explore the influence of two important dynamical bar parameters, bar strength and bar pattern speed, on the shape of the bar dust lanes. To quantify the shape of the dust lanes we have developed a new systematic method to measure the dust lane curvature. Previous numerical simulations have compared the curvature of bar dust lanes with the bar strength, predicting a relation between both parameters which has been supported by observational studies but with a large spread. We take into account the bar pattern speed to explore, simultaneously, the effect of both parameters on the dust lane shape.To that end, we separate our galactic bars in fast bars (1 < R < 1.4) and slow bars (R > 1.4), obtaining, as previous simulations, an inverse relation between the dust lane curvature and the bar strength for fast bars. For the first time, we extend the study to slow bars, finding a constant curvature as a function of the bar strength. As a result, we conclude that weak bars with straight dust lanes are candidates for slow bars. Finally, we have analysed a pilot sample of ten S 4 G galaxies, obtaining dust lane curvatures lying within the range covered by the simulations.

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Ordered and chaotic spiral arms

Patsis

2008

Astron Nachr

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The stellar flow at the arms of spiral galaxies is qualitatively different among different morphological types. The stars that reinforce the spiral arms can be either participating in an ordered or in a chaotic flow. Ordered flows are associated with normal (non-barred) spiral galaxies. Typically they are described with precessing ellipses corresponding to stable periodic orbits at successive energies (Jacobi constants). On the contrary, the spiral arms in barred-spiral systems may be supported by stars in chaotic motion. The trajectories of these stars are associated with the invariant manifolds of the unstable Lagrangian points (L1,2). Response and orbital models indicate that this kind of spirals either stop at an azimuth smaller than π/2, or present large gaps at about this angle. Chaotic spirals appear in strong bars having (L1,2) close to the ends of the bar. The arms of barred-spiral systems with corotation away from the end of the bar can be either as in the case of normal spirals, or supported by banana-like orbits surrounding the stable Lagrangian points (L4,5). We find also models combining ordered and chaotic flows.

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Orbits in the Bar of NGC 4314

Cited by 79 publications

References 18 publications

3D MHD simulations of magnetic field evolution and radio polarization of barred galaxies

3D MHD simulations of magnetic field evolution and radio polarization of barred galaxies

On the morphology of dust lanes in galactic bars

Ordered and chaotic spiral arms

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