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Thermodynamics of Plasmas workshop

5–7 Oct 2026
EPFL
Europe/Zurich timezone

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Session

Self-gravitating systems

Self-gravitating systems
7 Oct 2026, 10:00
Bernoulli center (EPFL)

Bernoulli center

EPFL

GA 3 34 (Building GA) Station 5 CH-1015 Ecublens Switzerland Coordinates on Google Maps: https://maps.app.goo.gl/TSx44GXiANdZa9KB9

Conveners

Self-gravitating systems: Self-gravitating systems

  • Barry Ginat (University of Oxford)

Presentation materials

There are no materials yet.

  1. 13. The Gaia Snail as a Collisionless Relaxation Problem: Power Spectra, Caustic Counts, and Self-Gravity
    Amitava Bhattacharjee (Princeton University)
    07/10/2026, 10:00
    Main track
    Oral presentation

    The Gaia Snail—a spiral pattern in stellar phase space caused by a perturbation to the Milky Way disk—is a natural laboratory for one-dimensional collisionless gravitational dynamics, the sign-flipped analog of electrostatic Vlasov–Poisson physics. Linear theory reproduces the spiral but winds it too tightly and fails to reproduce salient observed features. We present nonlinear analytical...

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  2. 9. Gravitational turbulence in stellar dynamics
    Sofia Flores
    07/10/2026, 10:40
    Main track
    Oral presentation

    Vector Resonant Relaxation (VRR), the collective reorientation of stellar orbits around a black hole, provides an interesting framework for studying turbulence beyond the plasma context. In this talk, I will present numerical simulations of VRR in the strongly turbulent regime and characterize the statistical properties of its fluctuations. I will focus on the emergence of cascade phenomena...

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  3. 16. Phase transition in a self-gravitating system: spontaneous orbital alignment of stars around a supermassive black hole
    Jean-Baptiste FOUVRY (Institut d'Astrophysique de Paris)
    07/10/2026, 11:50
    Main track
    Oral presentation

    Supermassive black holes dominate the gravitational potential in galactic nuclei. In these dense environments, stars follow nearly Keplerian orbits and see their orbital planes relax through the potential fluctuations generated by the stellar cluster itself. For typical stellar distributions, the most likely long-term outcome of this rearrangement is for the orbital planes of the most massive...

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