Galaxy models have long predicted that galactic bars slow down by losing angular momentum to their postulated dark haloes. When the bar slows down, resonance sweeps radially outwards through the galactic disc while growing in volume, thereby sequentially capturing new stars at its surface/separatrix. Since trapped stars conserve their action of libration, which measures the relative distance to the resonance centre, the order of capturing is preserved: the surface of the resonance is dominated by stars captured recently at large radius, while the core of the resonance is occupied by stars trapped early at small radius. The slow down of the bar thus results in a rising mean metallicity of trapped stars from the surface towards the centre of ...
Using data from the Gaia satellite’s Radial Velocity Spectrometer Data Release 3 (RVS, DR3), we find...
We show that bars in galaxy models having halos of moderate density and a variety of velocity dis- t...
We construct and evolve three one-parameter families and one two-parameter family of steady-state mo...
Galaxy models have long predicted that galactic bars slow down by losing angular momentum to their p...
We provide the first quantitative evidence for the deceleration of the Galactic bar from local stell...
This thesis provides a novel dynamical evidence for dark matter by measuring for the first time the ...
Elongated bar-like features are ubiquitous in galaxies, occurring at the centers of approximately tw...
We have used Spitzer images of a sample of 68 barred spiral galaxies in the local universe to make s...
We test the idea that bar pattern speeds decrease with time owing to angular momentum exchange with ...
Bars are remarkable stellar structures, which play an essential role in driving the secular evolutio...
The length and pattern speed of the Milky Way bar are still controversial. Photometric and spectrosc...
The pattern speed with which galactic bars rotate is intimately linked to the amount of dark matter ...
Funding: IB was supported by a ‘Pathways to Research’ fellowship from the University of Bonn. He ack...
We show that bars in galaxy models having halos of moderate density and a variety of velocity distri...
Bars may induce morphological features, such as rings, through their resonances. Previous studies su...
Using data from the Gaia satellite’s Radial Velocity Spectrometer Data Release 3 (RVS, DR3), we find...
We show that bars in galaxy models having halos of moderate density and a variety of velocity dis- t...
We construct and evolve three one-parameter families and one two-parameter family of steady-state mo...
Galaxy models have long predicted that galactic bars slow down by losing angular momentum to their p...
We provide the first quantitative evidence for the deceleration of the Galactic bar from local stell...
This thesis provides a novel dynamical evidence for dark matter by measuring for the first time the ...
Elongated bar-like features are ubiquitous in galaxies, occurring at the centers of approximately tw...
We have used Spitzer images of a sample of 68 barred spiral galaxies in the local universe to make s...
We test the idea that bar pattern speeds decrease with time owing to angular momentum exchange with ...
Bars are remarkable stellar structures, which play an essential role in driving the secular evolutio...
The length and pattern speed of the Milky Way bar are still controversial. Photometric and spectrosc...
The pattern speed with which galactic bars rotate is intimately linked to the amount of dark matter ...
Funding: IB was supported by a ‘Pathways to Research’ fellowship from the University of Bonn. He ack...
We show that bars in galaxy models having halos of moderate density and a variety of velocity distri...
Bars may induce morphological features, such as rings, through their resonances. Previous studies su...
Using data from the Gaia satellite’s Radial Velocity Spectrometer Data Release 3 (RVS, DR3), we find...
We show that bars in galaxy models having halos of moderate density and a variety of velocity dis- t...
We construct and evolve three one-parameter families and one two-parameter family of steady-state mo...