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Evolution of the Schr\"odinger--Newton system for a self--gravitating scalar field

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arxiv gr-qc/0404014 v2 pith:MQV3VP75 submitted 2004-04-02 gr-qc astro-ph

F. Siddhartha Guzman , L. Arturo Urena-Lopez This is my paper · ORCID
classification gr-qcastro-ph
keywords systemconfigurationconfigurationsequilibriumevolutionfieldnewtoniannumerical
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Using numerical techniques, we study the collapse of a scalar field configuration in the Newtonian limit of the spherically symmetric Einstein--Klein--Gordon (EKG) system, which results in the so called Schr\"odinger--Newton (SN) set of equations. We present the numerical code developed to evolve the SN system and topics related, like equilibrium configurations and boundary conditions. Also, we analyze the evolution of different initial configurations and the physical quantities associated to them. In particular, we readdress the issue of the gravitational cooling mechanism for Newtonian systems and find that all systems settle down onto a 0--node equilibrium configuration.

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Cited by 3 Pith papers

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  1. Spin-1 Ultralight Dark Matter under Cosmological Scrutiny: Mass Constraints from CMB and Distance Probes

    astro-ph.CO 2026-07 conditional novelty 6.0 of 10

    Cosmological data place a lower bound near 10⁻²⁴ eV on spin-1 ultralight dark matter and predict a CMB anisotropy signature that may be detectable when the vector field is a minor dark-matter component.

  2. Self-gravitating quantum stars with a globally relevant Bohm potential

    hep-th 2026-05 conditional novelty 6.0 of 10

    The equilibrium radius of self-gravitating dark fermion stars is determined by the fermion mass once the total mass is given, with the Bohm potential supplying outward pressure for heavier species and inward tension f...

  3. Updated bounds on ultra-light dark matter from the tiniest galaxies

    astro-ph.CO 2025-09 conditional novelty 6.0 of 10

    If Ursa Major III/UNIONS 1 is a galaxy, ultra-light dark matter particles must be heavier than 8 x 10^-18 eV, the strongest such bound.

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