On the bar formation mechanism in galaxies with cuspy bulges
Evgeny Polyachenko, Peter Berczik, Andreas Just

TL;DR
Numerical simulations demonstrate that Milky Way-like galaxies with cuspy bulges can develop bars through standard instability mechanisms, with bar properties consistent with observed features like the Hercules stream.
Contribution
This study shows that bar formation in galaxies with cuspy bulges can occur via classical instability, even with inner Lindblad resonances, and compares live versus rigid halo effects.
Findings
Bar formation occurs despite inner Lindblad resonance.
Bar pattern speed aligns with the Hercules stream observations.
Bar growth timescales suggest recent formation in Milky Way-like galaxies.
Abstract
We show by numerical simulations that a purely stellar dynamical model composed of an exponential disc, a cuspy bulge, and an NFW halo with parameters relevant to the Milky Way Galaxy is subject to bar formation. Taking into account the finite disc thickness, the bar formation can be explained by the usual bar instability, in spite of the presence of an inner Lindblad resonance, that is believed to damp any global modes. The effect of replacing the live halo and bulge by a fixed external axisymmetric potential (rigid models) is studied. It is shown that while the e-folding time of bar instability increases significantly (from 250 to 500 Myr), the bar pattern speed remains almost the same. For the latter, our average value of 55 km/s/kpc agrees with the assumption that the Hercules stream in the solar neighbourhood is an imprint of the bar--disc interaction at the outer Lindblad…
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