Time-Dependent Corotation Resonance in Barred Galaxies

Wu, Yu-Ting; Pfenniger, D.; Taam, Ronald E.

doi:10.3847/0004-637x/830/2/111

Cited by 19 publications

(23 citation statements)

References 12 publications

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“…To further elaborate upon the short time scale variations of the barred structure in a disk galaxy model reported in Wu et al (2016), three methods are used to measure the instantaneous and local mode/pattern speed rather than the time-averaged mode/pattern speed as often done in other works. Using the Fourier mode method (which measures a mode speed), the Jacobi integral method (which measures the potential rotation speed), and the moment of inertia method (which measures the rotation speed of the second order mass moment tensor), we have investigated the instantaneous variations of the bar size, strength, and pattern speed of the bars.…”

Section: Discussionmentioning

confidence: 99%

“…When adjacent bar or spiral structures rotate with different speeds, their mutual torques cause the intermediate region to be strongly time-dependent in any rotating frame. This point was investigated quantitatively by Wu et al (2016) who demonstrated that bars and spiral arms in a double barred galaxy model are actually flexible structures especially in the vicinity of the corotation region. This results from the fact that the equilibrium points within the corotation region are time-dependent in any rotating frame due to the mutual interaction with their adjacent structure (bar-bar or bar-spiral structures).…”

Section: Introductionmentioning

confidence: 99%

“…as described in Wu et al (2016). The time-derivative of the angle φ M yields the angular speed of the principal axis,…”

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confidence: 99%

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Time-dependent Pattern Speeds in Barred Galaxies

Pfenniger

Taam

2018

ApJ

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Based on a high quality N -body simulation of a double bar galaxy model, we investigate the evolution of the bar properties, including their size, strength and instantaneous pattern speed derived by using three distinct methods: the Fourier, Jacobi integral, and moment of inertia methods. The interaction of the two bars, which rotate at distinct speeds, primarily affects the size, strength and pattern speed of the inner bar. When the two bars are perpendicular to each other, the size and the pattern speed of the inner bar decrease and its strength increases. The emergence of a strong Fourier m = 1 mode increases the oscillation amplitude of the size, strength and pattern speed of the inner bar. On the other hand, the characteristics of the outer bar are substantially influenced by its adjacent spiral structure. When the spiral structure disappears, the size of the outer bar increases and its strength and pattern speed decrease. Consequently, the ratio of the pattern speed of the outer bar with respect to the inner bar is not constant and increases with time. Overall, the double bar and disk system displays substantial high frequency semi-chaotic fluctuations of the pattern strengths and speeds both in space and time, superposed on the slow secular evolution, which invalidates the assumption that the actions of individual stars should be well conserved in barred galaxies, such as the Milky Way.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Time-dependent Pattern Speeds in Barred Galaxies

Pfenniger

Taam

2018

ApJ

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“…The pattern speed is obtained from an angle of the rotation of the ellipsoid's main axes (e.g. Wu et al 2016). In panel (b) of Fig.…”

Section: Isolated Simulation B-0 Of the Host Galaxymentioning

confidence: 99%

Effects of galaxy–satellite interactions on bar formation

Moetazedian

Polyachenko

Berczik

et al. 2017

A&A

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Aims. We aim to show how encounters with low-mass satellite galaxies may alter the bar formation in a Milky Way-like disc galaxy. Methods. We use high-resolution N-body simulations of a disc galaxy prone to mild bar instability. For realistic initial conditions of satellites, we take advantage of cosmological simulations of Milky Way-like dark matter haloes. Results. The satellites may have a significant impact on the time of bar formation. Some runs with satellites demonstrate a delay, while others show an advancement in bar formation compared to the isolated run, with such time differences reaching ∼ 1 Gyr. Meanwhile, the final bar configuration, including its very appearance and the bar characteristics such as the pattern speed and the exponential growth rate of its amplitude are independent of the number of encounters and their orbits. The contribution of satellites with masses below 10 9 M ⊙ is insignificant, unless their pericentre distances are small. We suggest that the encounters act indirectly via inducing perturbations across the disc that evolve to delayed waves in the central part and interfere with an emerging seed bar. The predicted effect for the present-day host galaxy is expected to be even more significant at redshifts z 0.5.

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“…Debattista & Shen (2007) for the first time successfully generated a long-lived S2B structure in Nbody simulations. The systematic study of Du et al (2015) demonstrated that a short (inner) bar can form spontaneously without involving gas from an initially dynamically cool, nuclear stellar disk due to its own bar instability (see also Wu et al 2016). The addition of gas was considered by Wozniak (2015).…”

Section: Introductionmentioning

confidence: 99%

A New Channel of Bulge Formation via the Destruction of Short Bars

Guo

et al. 2020

ApJ

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Short (inner) bars of sub-kiloparsec radius have been hypothesized to be an important mechanism for driving gas inflows to small scales, thus feeding central black holes. Recent numerical simulations have shown that the growth of central black holes in galaxies can destroy short bars, when the black hole reaches a mass of ∼ 0.1% of the total stellar mass of the galaxy. We study N -body simulations of galaxies with single and double bars to track the long-term evolution of the central stellar mass distribution. We find that the destruction of the short bar contributes significantly to the growth of the bulge. The final bulge mass is roughly equal to the sum of the masses of the initial pseudo bulge and short bar. The initially boxy/peanut-shaped bulge of Sérsic index n 1 is transformed into a more massive, compact structure that bears many similarities to a classical bulge, in terms of its morphology (n ≈ 2), kinematics (dispersion-dominated, isotropic), and location on standard scaling relations (Kormendy relation, mass-size relation, and correlations between black hole mass and bulge stellar mass and velocity dispersion). Our proposed channel for forming classical bulges relies solely on the destruction of short bars without any reliance on mergers. We suggest that some of the less massive, less compact classical bulges were formed in this manner.

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Time-Dependent Corotation Resonance in Barred Galaxies

Cited by 19 publications

References 12 publications

Time-dependent Pattern Speeds in Barred Galaxies

Time-dependent Pattern Speeds in Barred Galaxies

Effects of galaxy–satellite interactions on bar formation

A New Channel of Bulge Formation via the Destruction of Short Bars

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