## Presentation

The LPT is based at the University of Toulouse. It has been founded in 1991 and its administrative structure was established in 2003. Before 2003, researchers where rassembled in the Group of Theoretical Physics. This group was hosted by the Laboratoire de Physique Quantique (now LCPQ).

The LPT is member of IRSAMC (The Institute of Research on Complex Atomic and Molecular Systems).

=> There publications before 2003: HAL-LPQ_GPT

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### Last submission

[hal-02309051] Gravitational phase transitions and instabilities of self-gravitating fermions in general relativity  (11/10/2019)
We discuss the occurrence of gravitational phase transitions and instabilities in a gas of self-gravitating fermions within the framework of general relativity. In the classical (nondegenerate) limit, the system undergoes a gravitational collapse at low energies $E<E_c$ and low temperatures $T<T_c$. This is called "gravothermal catastrophe" in the microcanonical ensemble and "isothermal collapse" in the canonical ensemble. When quantum mechanics is taken into account and when the particle number is below the Oppenheimer-Volkoff limit ($N<N_{\rm OV}$), complete gravitational collapse is prevented by the Pauli exclusion principle. In that case, the Fermi gas undergoes a gravitational phase transition from a gaseous phase to a condensed phase. The condensed phase represents a compact object like a white dwarf, a neutron star, or a dark matter fermion ball. When $N>N_{\rm OV}$, there can be a subsequent gravitational collapse below a lower critical energy $E<E''_c$ or a lower critical temperature $T<T'_c$ leading presumably to the formation of a black hole. The evolution of the system is different in the microcanonical and canonical ensembles. In the microcanonical ensemble, the system takes a "core-halo" structure. The core consists in a compact quantum object or a black hole while the hot halo is expelled at large distances. This is reminiscent of the red giant structure of low-mass stars or the implosion-explosion of massive stars (supernova). In the canonical ensemble, the system collapses as a whole towards a compact object or a black hole. This is reminiscent of the implosion of supermassive stars (hypernova).

[hal-02309050] Caloric curves of classical self-gravitating systems in general relativity  (11/10/2019)
[hal-02308390] Many-Body Effective Energy Theory: Photoemission at Strong Correlation  (11/10/2019)
[hal-02303069] Quench, thermalization and residual entropy across a non-Fermi liquid to Fermi liquid transition  (11/10/2019)
[hal-02303030] Statistical mechanics of self-gravitating systems in general relativity: I. The quantum Fermi gas  (11/10/2019)