Secular Public

Stellar Dynamics in Galactic Nuclei

Astrophysical Context

Supermassive black holes (BHs) are ubiquitous in external galaxies, while their active feedback plays a critical role in regulating galaxy formation through cosmic age. Yet, the details of their diet and their impact on the stellar cluster orbiting it remains a very much open and challenging equation. Indeed, galactic nuclei are fascinating dynamical systems, in particular because the steep potential well defined generated by the central supermassive BH guarantees the existence of a wide range of dynamical timescales in the system.

As such, the dynamical evolution of the stellar cluster surrounding the BH comprises numerous evolution processes acting on radically different timescales. These include: (i) the dynamical time, sourced by the fast Keplerian motion around the central BH, which, following an orbit-average, amounts then to replacing stars by their underlying Keplerian ellipses; (ii) the precession time, during which stars undergo an in-plane precession of their pericentre generated by the cluster's mean potential and the BH's relativistic corrections; (iii) the vector resonant relaxation time, during which stellar orbital orientations undergo stochastic random walks as a result of finite-N perturbations; (iv) the scalar resonant relaxation time, during which resonant torques between the precessing ellipses lead to the relaxation of their eccentricities; (v) the non-resonant relaxation time that sources the relaxation of the ellipses' energies and is driven by local pairwise scatterings among the stars.

Because of its large number of constituents (~1 Million stars within the sphere of influence of the Milky Way's central BH), and the very significant range of timescales ranging from 1yr for the fast dynamical time of the innermost stars up to 10Gyr for the galactic nucleus' overall lifespan, direct numerical explorations of a galactic nucleus' long-term evolution are systematically bound to fail.

Upshot

This is where the heart of the present PhD project lies. Its goal is to tackle the long-term evolution of galactic nuclei using a novel and innovative framework stemming from kinetic theory.

As such, the PhD candidate will develop, tailor, and apply the framework of long-range and long-term kinetic theories in the context of stellar dynamics around supermassive BHs. Once completed, this project will have truly highlighted the versatility of secular theory to describe the long-term evolution of galactic nuclei.

Objectives

• Building upon Giral et al. (2020), the PhD candidate will characterise the efficiency with which stars with similar orientations get slowly separated through potential fluctuations. In particular, the PhD candidate will use the recent observation of a clockwise stellar disc in the centre of the Milky-Way to constrain the properties of the old stellar cluster that may drive the disc's spontaneous dissolution.
• Because of their gigantic range of timescales, numerical simulations of galactic nuclei are very challenging, and require appropriate and tailored orbital averages. Following upon Fouvry et al. (2020), the PhD candidate will design an efficient multipole method to directly track the evolution of stellar orientations during the process of vector resonant relaxation.
• Following Szolgyen & Kocsis (2018), the PhD candidate will investigate the long-term thermodynamical equilibria of stellar orientations in galactic nuclei. Can one predict the presence of discs of intermediate mass BHs in galactic nuclei?

Requirement

Strong interest in theoretical astronomy, dynamics, analytical and numerical work.

Framework

The PhD will be co-supervised by Jean-Baptiste Fouvry and Christophe Pichon, as part of the SEGAL ANR (www.secular-evolution.org).