Thermodynamics of Plasmas workshop

5 Oct 2026, 09:00 → 7 Oct 2026, 20:30 Europe/Zurich

Bernoulli center (EPFL)

The first workshop on "The Thermodynamics of Collisionless Plasmas” will be held October 5th–7th 2026. Hosted and sponsored by the Bernoulli center at EPFL, Switzerland, with a view of Lac Léman (Lake Geneva), the workshop brings together researchers from plasma physics, statistical mechanics, and astrophysics. The aim is to connect researchers, establish a shared framework, and discuss emerging challenges. The workshop will host talks of 16 speakers.

Monday 5 October

09:00 → 09:50 Arrival, croissants, and coffee

09:50 → 10:00 Block Introduction

10:00 → 12:30 Energy bounds

Convener: Dr Robert Ewart (Stanford University)

10:00 Upper bounds on gyrokinetic instabilities

For several decades, an enormous effort has been devoted to the gyrokinetic theory of instabilities and turbulence in stellarators and tokamaks. Thousands of papers have been published on this subject, and millions of lines of code have been written for the purpose of numerically solving gyrokinetic equations.

As a result of this effort, a great deal of knowledge about various microinstabilities has accumulated. Ion- and electron-temperature-gradient-driven modes, trapped-electron modes, kinetic ballooning modes and microtearing modes have, for instance, been found to be unstable and cause turbulence in tokamaks and stellarators. However, these instabilities tend to be sensitive to assumptions made about plasma parameters and the magnetic-field geometry. As a result, little is known in general about gyrokinetic microinstaiblities, despite the great effort devoted to their study.

Proceeding from thermodynamic considerations, we derive universal upper bounds on the growth rates of local gyrokinetic instabilities in any magnetised plasma, regardless of the geometry of the magnetic field, the number of particle species, beta, and collisions. A large number of results that have earlier been derived in special cases or observed in numerical simulations are thus brought into a unifying framework. Moreover, these upper bounds hold not only for linear instabilities but also for the nonlinear growth of free energy in a turbulent plasma.

The same theoretical framework can also be used to derive upper bounds on turbulent transport fluxes. Without additional assumptions about the nature of the turbulence, these bounds are unrealistically high, but can be lowered if such assumptions are made. The formalism may thus offer a useful technique for making concepts like critical balance quantitatively precise.

Speaker: Per Helander

10:40 Unified theory of classical and quantum ergotropy

Quantifying the ergotropy (also known as available energy), namely the maximal amount of energy that can be extracted from a thermally isolated system, is a central problem in quantum thermodynamics. Notably, the same problem has been long studied for classical systems as well, e.g., in plasma physics and astrophysics, where the basic principles for its solution are known for the case of collisionless fluids. Here we provide the general analytical expression of ergotropy of classical systems valid regardless of their size and the type of interparticle interactions, and show that it emerges as the classical limit of the quantum expression of ergotropy, for quantum systems that are classically ergodic. We thus establish a unified theory of classical and quantum ergotropy, whose applicability ranges from atomic to galactic scale. Such unified theory is indispensable for studying the genuine quantum signatures of ergotropy: We show that the celebrated decomposition of quantum ergotropy into coherent ant inchoherent parts survives in the classical regime, indicating that coherences do not necessarily reveal quantumness. The unified theory also allows to port tools and methods across the classical-quantum boundary to unlock the solution of standing problems. We apply this to swiftly solve the open problem of ergotropy extraction in the classical regime.

Speaker: Michele Campisi (Istituto Nanoscienze CNR, Pisa, Italy)

11:20 Coffee break

11:50 Ground states: constraints from the field equations and unresolved issues

Given a collisionless plasma, how much of its energy can turbulence actually extract? A natural answer is to rearrange the distribution function into its lowest-energy configuration, subject to the constraints of the underlying dynamics; an idea that has been used across time and disciplines, from Lorenz's available potential energy in meteorology to Gardner's restacking argument [1] and the ergotropy of quantum systems. In a Vlasov plasma the constraints are the Casimir invariants, and the energy difference between the initial and resulting ground state is the available energy. We point out that this construction, in its usual form, is inconsistent with the field equations: the Gardner ground state is homogeneous and therefore supports no electric field, even though energy conservation requires the liberated energy to reside in precisely that field. We show how to repair this by additionally constraining the ground-state density, and we illustrate the consequences with deliberately simple examples: a two-stream waterbag model, in which energy conservation, Debye screening and positivity of the density conspire to produce phase-transition-like behaviour; and drift-kinetic ions with adiabatic electrons, for which the available energy falls by 83% relative to the naïve bound. Several issues remain unresolved, notably the excessive freedom given by a kinetic electron species.

References:
[1] CS Gardner, Phys. Fluids 6, 839 (1963)

Speaker: Ralf Johannes Josephus Mackenbach (EPFL-SPC)

12:30 → 14:00 Lunch break

14:00 → 17:10 Instabilities and confinement

Convener: Per Helander

14:00 Available Energy and Ground States of Convective Hydrodynamic and Hydromagnetic Instabilities

We propose a method for predicting the nonlinear saturation level of convective instabilities in neutral and magnetized fluids. The method combines Gardner's restacking algorithm, which computes the available energy and ground states of collisionless plasmas in phase space, and Lagrangian relaxation, where fluid elements find lower-energy equilibria while preserving local invariants. For the incompressible Rayleigh-Taylor instability, the problem is formally equivalent to Gardner's and the restacking algorithm directly applies in configuration space. To treat compressibility, we follow restacking with Lagrangian relaxation to obtain the ground state, and the results show excellent agreement with direct numerical simulations. Successful extension to the interchange instability in a Z-pinch demonstrates the method's potential as a general framework for estimating the nonlinear extent of convective instabilities, which can facilitate the design and operation of fusion reactors.

Speaker: Kaixuan Fan (Shanghai Jiao Tong University)

14:40 Thermodynamic bounds on linear gyrokinetic microinstabilities

The microinstabilities that cause the confinement-limiting turbulence in modern fusion devices are driven by the radial gradients of density and temperature in the plasma. In multi‑scale gyrokinetic theory [1], these gradients act as a source of background free energy that feeds instabilities on the fluctuating micro scales, giving rise to turbulence, and ultimately, energy transport down the plasma gradients. Linear instability analyses, in which the unstable linear eigenmodes of the gyrokinetic system are studied, are central to our understanding of this process. However, in realistic magnetic geometry, these analyses often involve expensive gyrokinetic simulations.
Recent work has revealed that there is a thermodynamic upper bound on the rate at which free energy can be extracted by instabilities [2]. This bound is computed by constructing optimal modes, distribution functions that maximise the energetic growth on the micro scales. Due to the low-dimensionality of the optimal mode equations, these bounds can be computed very efficiently.
However, because the bound is valid in any confining magnetic field, the optimal modes are independent of the details of the magnetic geometry, which are often central to determining the growth rate of linear instabilities [3].
With the aim of capturing more of this geometric dependence in the upper bound, we develop a theory of constrained optimal modes: distribution functions that maximise free energy growth subject to a set of constraints that are also obeyed by the linear instabilities. We consider the linear gyrofluid equations as constraints, which restrict the moments of the distribution function in the variational principle, retaining some of the geometric dependence of the linear instabilities. The result is a system of gyrofluid equations to be solved for the upper bound on the linear growth rate, where the dimensionality of the system depends on the number of constraints considered; a tight bound is given in the limit of infinite constraints. We demonstrate, by comparison with gyrokinetic simulations and dispersion relations in simple limits, that the upper bounds capture some of the key geometry dependencies of the linear growth rate, even with a relatively small number of constraints. We then leverage this geometry dependence to perform a proof-of-principle optimisation of a quasi-isodynamic stellarator with reduced linear instability growth.

[1] I G Abel, G G Plunk, E Wang, M Barnes, S C Cowley, W Dorland, and A A Schekochihin. Rep. Prog. Phys., 76(11):
116201, November 2013. ISSN 0034-4885, 1361-6633. doi: 10.1088/0034-4885/76/11/116201.
[2] P. Helander and G. G. Plunk. Journal of
Plasma Physics, 88(2):905880207, April 2022. ISSN 0022-3778, 1469-7807. doi: 10.1017/S0022377822000277.
[3] L. Podavini, P. Helander, G. G. Plunk, and A. Zocco. Journal of Plasma Physics, 91(3):E79,
June 2025. ISSN 0022-3778, 1469-7807. doi: 10.1017/S0022377825000479.

Speaker: Paul Costello (Max Planck Institute for Plasma Physics)

15:20 Coffee break

15:50 Constrained Nonequilibrium Dynamics and the Formation of Transport Barriers in Magnetized Plasmas

Transport barriers in magnetically confined plasmas pose an intriguing thermodynamic problem: large gradients, and hence substantial free energy, can coexist with strongly reduced turbulent transport. We examine this phenomenon from the perspective of constrained nonequilibrium dynamics. A macroscopic thermodynamic model treats the plasma boundary layer as a heat engine in which incoming power drives ordered flows and currents, producing a bifurcation to a stable high-gradient state above critical thresholds [1]. This picture is complemented by gyrokinetic considerations. Low-frequency fluctuations are subject to a constraint requiring the fluctuation-driven charge-weighted radial particle flux to vanish. In sufficiently strong-gradient regimes, this constraint can become incompatible with growing fluctuations, preventing access to available free energy even when conventional energetic considerations suggest instability. Gyrokinetic simulations demonstrate this constrained stabilization and associated changes in mode structure [2]. Recent DIII-D pedestal studies provide an experimentally relevant example of related threshold behavior, including microtearing stability boundaries and second-stable kinetic ballooning modes [3]. Together, these results suggest that transport barriers may arise not simply through reduced thermodynamic drive, but through restrictions on the dynamical pathways by which free energy can be relaxed.

[1] S. M. Mahajan, D. R. Hatch, Z. Yoshida, and M. Kotschenreuther, “A unified theory of transport barriers (TBs) in magnetically confined systems,” arXiv preprint arXiv:2603.26919, 2026.
[2] M. Kotschenreuther, X. Liu, S. M. Mahajan, D. R. Hatch, and G. Merlo, “Transport barriers in magnetized plasmas—general theory with dynamical constraints,” Nucl. Fusion, vol. 64, no. 7, Art. no. 076033, 2024, doi: 10.1088/1741-4326/ad4c75.
[3] D. R. Hatch, L. A. Leppin, M. T. Kotschenreuther, S. Houshmandyar, S. M. Mahajan, J. Schmidt, and P.-Y. Li, “Microtearing thresholds and second-stable ballooning in the DIII-D pedestal: Reduced modeling and core-edge implications,” Phys. Plasmas, vol. 33, Art. no. 072512, 2026, doi: 10.1063/5.0337081.

Speaker: DR Hatch

16:30 Impact of Magnetic Configuration on Energy Confinement and Available Energy in Fusion Device

Plasma turbulence is a dominant factor limiting energy confinement time in toroidal fusion plasmas, making computationally cheap confinement proxies highly desirable for quickly identifying experimentally attractive scenarios. In this presentation, we investigate whether "Available Energy (AE)” - an upper limit on the thermal energy available to drive Trapped Electron Mode (TEM) turbulence in collisionless plasmas - can serve as such a proxy in the Heliotron J device [1], offering the first direct comparison between AE and experiment. Observations from Heliotron J show that energy confinement is significantly influenced by the toroidal mirror ripple (bumpiness), and the rotational transform [2,3]. We have verified if AE, calculated across the entire plasma, exhibits similar dependencies. We have demonstrated that AE varies significantly when altering the bumpiness and rotational transform, and, importantly, exhibits a clear negative correlation with the normalized stored energy ($W_p/V_p$) found in experiment. These findings suggest that AE can serve as an effective proxy of confinement by capturing the characteristics of the TEM-driven turbulence. Next, this AE-based proxy of confinement is applied to different configurations of the Varying Symmetry Torus (VAST), a next-generation advanced helical device at NIFS. We show that the quasi-axisymmetric (QA), quasi-isodynamic (QI), and symmetry-broken (SB1) magnetic fields of VAST can suppress TEM turbulence more effectively than Heliotron J, confirming the benefits of magnetic configuration optimization. Furthermore, to perform a comprehensive comparison between tokamak and helical systems, we will apply the AE simulation to tokamak geometries, aiming to further clarify the relationship between magnetic geometry and turbulence.

[1] R. Mackenbach, J. Proll, et al., Phys. Rev. Lett. 17 (2022) 175001
[2] T. Mizuuchi, et al., Fus. Sci. Technol. 50 (2006) 352
[3] K. Nagasaki, et al., 28th IAEA Fus. Energy Conf., EX/P6-34

Speaker: Daishi Toriyama (GSES, Kyoto Univ.)

17:10 → 19:30 Apéro (welcome drinks) and dinner

Tuesday 6 October

09:00 → 10:00 Croissants and coffee

10:00 → 12:30 Universal equilibria

Convener: Ralf Johannes Josephus Mackenbach (EPFL-SPC)

10:00 Relaxation to universal non-Maxwellian equilibria

We review the Lynden-Bell formalism of deriving maximum entropy states subject to the short-time conservation of certain (fragile) collisionless invariants. The conservation of these collisionless invariants endows the system with a partial “memory” of its prior conditions but is fragile precisely due to the development of a turbulent cascade to small scales, which breaks the precise conservation of phase volume, making this memory imprecise. The equilibria are still determined by the short-time collisionless invariants, but the invariants themselves are driven to a simple (and possibly universal form). This is numerically confirmed for the case of beam instabilities in one-dimensional electrostatic plasmas, where sufficiently strong turbulence appears to cause the distribution function of particle energies to develop a universal power-law tail, with exponent −2.

Speaker: Dr Robert Ewart (Stanford University)

10:40 Non-thermal particle acceleration in multi-species kinetic plasmas: universal power-law distribution functions and temperature inversion in the solar corona

Non-thermal power-law distribution functions are ubiquitous in astrophysical, space, and laboratory kinetic plasmas, but their origin remains unclear. A related puzzle is the temperature inversion of the solar corona. We show that these phenomena are deeply connected by developing a self-consistent quasilinear theory for electromagnetically driven, unmagnetized kinetic plasmas. The theory yields a multi-species Fokker--Planck equation containing drive-induced diffusion, due to direct acceleration by broad-band turbulent or narrow-band wave-like fields and indirect acceleration by the waves excited, together with Balescu--Lenard diffusion and drag from self-generated Debye-scale fluctuations and Coulomb collisions. For a super-Debye turbulent electric-field spectrum, $|{\bf E}_{\bf k}|^2\propto k^{-\alpha}$, both electron and ion distributions relax toward a universal $f(v)\propto v^{-5}$, or $N(E)\propto E^{-2}$, attractor, equivalent to the high-energy fall-off of a $\kappa=1.5$ distribution, provided $\alpha\ge5$. This universality follows from Debye screening: large-scale fields accelerate unscreened fast particles but not screened slow ones. For shallower spectra, $\alpha<5$, the tail scales as $v^{-\alpha}$; incomplete relaxation and anisotropy can further break universality. Anisotropic wave drives produce branch- and spectrum-dependent exponents. Collisions do not efficiently decelerate suprathermal particles, so high-velocity tails resist Maxwellianization. In the solar atmosphere, such tails may be generated by chromospheric convection or nanoflares despite collisional and radiative losses. Direct wave heating preferentially energizes electrons through Landau-resonant interactions with whistler and electron-cyclotron waves, while ions may be accelerated by turbulent ambipolar fields. The resulting $\kappa\simeq1.5$--$3$ distributions naturally produce an abrupt upper-chromosphere/lower-corona temperature transition and velocity-filtration-driven inverted profiles, yielding coronal temperatures $\sim10^6\,{\rm K}$.

Speaker: Uddipan Banik (Institute for Advanced Study)

11:20 Coffee break

11:50 Dynamical Accessibility of Phase-Space Holes and Gravity Cusps in One-Dimensional Vlasov-Poisson Dynamics

The dynamical accessibility of a quasistationary state from the infinitely many formal equilibria of the Vlasov-Poisson system is addressed. We give a first-principles asymptotic selection theory for Bernstein-Greene-Kruskal (BGK) holes produced by two-stream relaxation and cold gravitational clumps produced by collisionless collapse. The analytic construction rests on two central ideas. First, repeated shell crossing winds phase space into caustic whorls, leading to particle bunching and phase-space granulation. Nonlinear phase mixing erases the angle information but preserves the action dependence of the distribution function (DF). Following Berry and O'Dell's work on ergodic momentum density generated by caustic whorls, and Jarzynski's least-biased information-theoretic interpretation of Berry's random-wave ensemble, we show that the resulting coarse-grained DF is a circus-tent (CT) DF, now made self-consistent for Vlasov-Poisson dynamics. Second, the selected potential is constrained by the Painleve property (PP) of Poisson's equation written in Sagdeev form. PP implies that the once-integrated Poisson equation must belong to an algebraic class reducible to Riccati or Weierstrass form up to suitable variable transformations, which must be determined by the underlying physical processes. In the plasma problem this leads to the Weierstrass form, with coefficients satisfying virial identities. In the gravity problem, the regular bulk stays elliptic, while the strict cold cusp is the root-collision degeneration of the regular elliptic curve. Extensive numerical diagnostics test analytical predictions rather than fit arbitrary profiles. In the plasma case, we validate the theoretical BGK hole depth and shape, and how closely the measured Sagdeev coefficients satisfy the virial identities. In the gravity case, the Colombi-Touma cusp branch, its coefficient scale, and its regularized core follow from the measured action distribution and Poisson closure. The cold center is resolved as a physical core, the thermal de-singularization of the cold cusp rather than numerical grid rounding, while the CT controls the bulk outside it. The adiabatic theory excludes the regions where action-angle variables fail: the O-point caustic sheet in gravity and the X-point separatrix sheet in BGK. These layers mark the boundary between regular coherent self-organization and the phase-space-turbulence problem, which we leave for subsequent work.

Speaker: Dr W Sengupta

12:30 → 14:00 Lunch break

14:00 → 16:30 Violent relaxation

Convener: W Sengupta

14:00 "Collisionless relaxation" of a stratified fluid plasma

Motivated by explosive releases of energy in fusion, space and astrophysical plasmas, we consider the nonlinear stability of stratified magnetohydrodynamic (MHD) equilibria against two-dimensional interchanges of straight magnetic-flux tubes. We demonstrate that, even within this restricted class of dynamics, the linear stability of an equilibrium does not guarantee its nonlinear stability: equilibria can be metastable. We show that the minimum-energy state accessible to a metastable equilibrium under non-diffusive 2D dynamics can be found by solving a combinatorial optimisation problem analogous to Gardner restacking. These minimum-energy states are, to good approximation, the final states reached by our simulations of destabilised metastable equilibria for which turbulent mixing is suppressed by viscosity. To predict the result of fully turbulent relaxation, we construct a statistical mechanical theory based on the maximisation of Boltzmann's mixing entropy. This theory is analogous to the Lynden-Bell statistical mechanics of collisionless stellar systems and plasma, and to the Robert-Sommeria-Miller (RSM) theory of 2D vortex turbulence.

Speaker: David Hosking (University of Cambridge)

14:40 Violent relaxation redux

Nearly collisionless self-gravitating systems far from equilibrium, such as merging galaxies, rapidly relax toward virialized equilibria through violent relaxation. I will present a framework for predicting the equilibria of violent relaxing systems that combines Lynden-Bell statistical mechanics and the time evolution of the system’s Casimir invariants [1]. The Casimirs evolve because finite-$N$ effects break the conservation of phase-space volume on a timescale given by the dynamical time multiplied by a logarithmic factor in $N$, the number of particles. This (relatively) fast dissipation arises due to gravitational turbulence, in which large-scale fluctuations in the gravitational field drive chaotic mixing of the distribution function in six-dimensional phase space. This turbulence obeys universal scaling laws below the Jeans scale for the fluctuation spectra of the gravitational field and the distribution function, which can be derived from a phenomenological scaling theory. The scale separation (in $\log N$) between the dynamical and dissipation timescales enables systems to relax "adiabatically" through a sequence of Lynden-Bell equilibria, each with nearly fixed Casimirs. In the long-time limit, the system tends toward its "ground state": a Lynden-Bell equilibrium that is both the maximum-entropy and minimum-energy state corresponding to the system’s late-time Casimirs. This framework is corroborated by 1D N-body simulations of violent relaxation and may be able to explain the universal equilibria of galaxies and dark matter halos. I will also discuss connections with turbulent relaxation in nearly collisionless plasmas [2, 3].

[1] Nastac, M. L., Ginat, Y. B., Ewart, R. J., Barnes, M. & Schekochihin, A. A. 2026 Violent relaxation redux, in preparation.
[2] Ewart, R. J., Nastac, M. L., Bilbao, P. J., Silva, T., Silva, L. O. & Schekochihin, A. A. 2025 Relaxation to universal non-Maxwellian equilibria in a collisionless plasma, PNAS 122, e2417813122.
[3] Nastac, M. L., Ewart, R. J., Juno, J., Barnes, M. & Schekochihin, A. A. 2025 Universal fluctuation spectrum of Vlasov-Poisson turbulence, e-print arXiv:2503.17278.

Speaker: Michael Nastac (University of Oxford)

15:20 Coffee break

15:50 Relaxation of Cold Dark Matter Systems to Lynden-Bell Equilibria

Gravitational collapse in large-scale structure formation is a highly non-linear process, governed by the Vlasov-Poisson system. In this talk, I will describe how this process leads to a flow of structure to small phase-space scales, in a manner which gives rise to a universal power-law scaling of the phase-space power-spectrum at small scales. Then, I will describe how this process leads to a relaxation of the mean field, towards a generalised Lynden-Bell distribution (in 1D). This distribution has a specific power-law tail in energy, which can be derived using statistical mechanical techniques. I will also comment on 3D implications for violent relaxation.

Speaker: Barry Ginat (University of Oxford)

16:30 → 22:00 Dinner and social event

Wednesday 7 October

09:00 → 10:00 Croissants and coffee

10:00 → 12:30 Self-gravitating systems

Convener: Barry Ginat (University of Oxford)

10:00 The Gaia Snail as a Collisionless Relaxation Problem: Power Spectra, Caustic Counts, and Self-Gravity

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 results and Gkeyll simulation verification for this gravitational cousin of classic plasma kinetic problems. The self-gravity operator around the classic Spitzer equilibrium, which is a reflectionless soliton potential, produces an exactly zero first-order shift. The quasi-linear second-order shift is shown to be negative. Self-gravity decelerates phase mixing. The winding power spectrum is exactly Gaussian in action space, computed by a technique due to Lundgren from a vortex spiral model of fluid turbulence. The nonlinear endpoint is a BGK quasi-stationary state, approached through a free-energy cascade in action space. The relevant statistical mechanics is not Lynden-Bell violent relaxation but phase-mixing entropy production: fine-grained Casimir invariants are conserved while coarse-grained power cascades irreversibly to sub-resolution scales.

Speaker: Amitava Bhattacharjee (Princeton University)

10:40 Gravitational turbulence in stellar dynamics

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 and the resulting power spectra, drawing connections with recent work on universal fluctuation spectra in collisionless plasmas. By varying the sharpness of the interaction kernel, I will explore how the turbulent state changes as the scaling of the long-range coupling (gravity) is modified, and discuss the emergence of critical behavior. More broadly, these results indicate that some aspects of turbulent cascades may be universal across a wider class of long-range interacting systems, from stars orbiting a massive black hole to liquid crystals and classical spins.

Speaker: Sofia Flores

11:20 Coffee break

11:50 Phase transition in a self-gravitating system: spontaneous orbital alignment of stars around a supermassive black hole

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 stars to spontaneously self-align within a narrow disc. We present a maximum entropy method to systematically determine this non-trivial long-term thermodynamical distribution. We explore the dependence of this phase transition as a function of the clusters' parameters. Presentation based on https://arxiv.org/abs/2111.09011

Speaker: Jean-Baptiste FOUVRY (Institut d'Astrophysique de Paris)

12:30 → 14:00 Lunch

14:00 → 16:00 Town hall discussion

19:00 → 20:30 Dinner (provisional)