Core mass-halo mass relation of bosonic and fermionic dark matter halos harboring a supermassive black hole

Chavanis, Pierre‐Henri

doi:10.1103/physrevd.101.063532

Cited by 22 publications

(26 citation statements)

References 88 publications

(183 reference statements)

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“…One has therefore to solve the optimization problem min {F | M fixed}. (38) One can easily show that the equilibrium states in the microcanonical and in the canonical ensembles are the same: an extremum of free energy at fixed mass is also an extremum of entropy at fixed mass and energy [75]. However, their stability may be different in the two ensembles.…”

Section: B Caloric Curves and Ensembles Inequivalencementioning

confidence: 99%

“…Furthermore, as shown in a previous paper [98], the maximization of the entropy S(M c ) with respect to the core mass M c at fixed total mass M h and total energy E h determines a core masshalo mass relation M c (M h ) which agrees with the relation obtained in direct numerical simulations of noninteracting bosons [74], giving further support to our effective thermodynamical approach. This thermodynamical approach also allowed us to derive the general expression of the core mass -halo mass relation M c (M h ) for self-interacting bosons and fermions [98,99], making new predictions that still have to be confirmed numerically.…”

Section: Introductionmentioning

confidence: 99%

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Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere

Chavanis

2019

Phys. Rev. D

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121

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We develop a model of Bose-Einstein condensate dark matter halos with a solitonic core and an isothermal atmosphere based on a generalized Gross-Pitaevskii-Poisson equation [P.H. Chavanis, Eur. Phys. J. Plus 132, 248 (2017)]. This equation provides a heuristic coarse-grained parametrization of the ordinary Gross-Pitaevskii-Poisson equation accounting for violent relaxation and gravitational cooling. It involves a cubic nonlinearity taking into account the self-interaction of the bosons, a logarithmic nonlinearity associated with an effective temperature, and a source of dissipation. It leads to superfluid dark matter halos with a core-halo structure. The quantum potential or the self-interaction of the bosons generates a solitonic core that solves the cusp problem of the cold dark matter model. The logarithmic nonlinearity generates an isothermal atmosphere accounting for the flat rotation curves of the galaxies. The dissipation ensures that the system relaxes towards an equilibrium configuration. In the Thomas-Fermi approximation, the dark matter halo is equivalent to a barotropic gas with an equation of state P = 2πas 2 ρ 2 /m 3 + ρkBT /m, where as is the scattering length of the bosons and m is their individual mass. We numerically solve the equation of hydrostatic equilibrium and determine the corresponding density profiles and rotation curves. We impose that the surface density of the halos has the universal value Σ0 = ρ0r h = 141 M /pc 2 obtained from the observations. For a boson with ratio as/m 3 = 3.28 × 10 3 fm/(eV/c 2 ) 3 , we find a minimum halo mass (M h )min = 1.86 × 10 8 M and a minimum halo radius (r h )min = 788 pc. This ultracompact halo corresponds to a pure soliton which is the ground state of the Gross-Pitaevskii-Poisson equation. For (M h )min < M h < (M h ) * = 3.30 × 10 9 M the soliton is surrounded by a tenuous isothermal atmosphere without plateau. For M h > (M h ) * we find two branches of solutions corresponding to (i) pure isothermal halos without soliton and (ii) isothermal halos harboring a central soliton and presenting a plateau. The purely isothermal halos (gaseous phase) are stable. For M h > (M h )c = 6.86 × 10 10 M , they are indistinguishable from the observational Burkert profile. For (M h ) * < M h < (M h )c, the deviation from the isothermal law (most probable state) may be explained by incomplete violent relaxation, tidal effects, or stochastic forcing. The isothermal halos harboring a central soliton (core-halo phase) are canonically unstable (having a negative specific heat) but they are microcanonically stable so they are long-lived. By extremizing the free energy (or entropy) with respect to the core mass, we find that the core mass scales as Mc/(M h )min = 0.626 (M h /(M h )min) 1/2 ln(M h /(M h )min). For a halo of mass M h = 10 12 M , similar to the mass of the halo that surrounds our Galaxy, the solitonic core has a mass Mc = 6.39×10 10 M and a radius Rc = 1 kpc. The solitonic core cannot mimic by itself a supermassive black hole at the center of the Galaxy but i...

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Section: B Caloric Curves and Ensembles Inequivalencementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere

Chavanis

2019

Phys. Rev. D

Self Cite

121

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“…[48] consider non-interacting BEC DM which forms solitonic core at the galactic centre in the absence of a BH. Therefore, this relation holds only in the case where solitonic cores are formed before SMBH [47,49,56]. Further, the M sol -M halo is valid for a very small range of m DM , around 10 −22 eV [49].…”

Section: Jhep10(2021)004mentioning

confidence: 95%

“…The relations between the SMBH, halo, and soliton masses may not be valid for the range of m DM 10 −22 eV [47,49,56]. As a consequence, in this paper, we consider ρ 0 and a as the parameters describing DM profile while demonstrating the energy dependence of the flavour ratios.…”

Section: Jhep10(2021)004mentioning

confidence: 99%

Astronomy with energy dependent flavour ratios of extragalactic neutrinos

Karmakar

Pandey

Rakshit

2021

J. High Energ. Phys.

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High energy astrophysical neutrinos interacting with ultralight dark matter (DM) can undergo flavour oscillations that induce an energy dependence in the flavour ratios. Such a dependence on the neutrino energy will reflect in the track to shower ratio in neutrino telescopes like IceCube or KM3NeT. This opens up a possibility to study DM density profiles of astrophysical objects like AGN, GRB etc., which are the suspected sources of such neutrinos.

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“…Large DM halos (like the Medium Spiral) have a solitonic core surrounded by an extended envelope. The core mass -halo mass relation Mc(M h ) has been obtained in different manners in[25,102,122,125,129,[132][133][134] 67 The mass-radius relation of the soliton scales as M ∼ h 2 /Gm 2 R.Introducing a typical velocity scale through the virial relation v 2 ∼ GM/R, we obtain R ∼ h/mv = λ dB . Since v ∼ √ αc ∼ 10 −3 c (see Appendix C), the de Broglie length is larger than the Compton length λ C = /mc by about 3 orders of magnitude.…”

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confidence: 99%

A new logotropic model based on a complex scalar field with a logarithmic potential

Chavanis

2022

Preprint

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We introduce a new logotropic model based on a complex scalar field with a logarithmic potential that unifies dark matter and dark energy. The scalar field satisfies a nonlinear wave equation generalizing the Klein-Gordon equation in the relativistic regime and the Schrödinger equation in the nonrelativistic regime. This model has an intrinsically quantum nature and returns the ΛCDM model in the classical limit → 0. It involves a new fundamental constant of physics A/c 2 = 2.10 × 10 −26 g m −3 responsible for the late accelerating expansion of the Universe and superseding the Einstein cosmological constant Λ. The logotropic model is almost indistinguishable from the ΛCDM model at large (cosmological) scales but solves the CDM crisis at small (galactic) scales. It also solves the problems of the fuzzy dark matter model. Indeed, it leads to cored dark matter halos with a universal surface density Σ th 0 = 5.85 (A/4πG) 1/2 = 133 M /pc 2 . This universal surface density is predicted from the logotropic model without adjustable parameter and turns out to be close to the observed value Σ obs 0 = 141 +83 −52 M /pc 2 . We also argue that the quantities Ω dm,0 and Ω de,0 , which are usually interpreted as the present proportion of dark matter and dark energy in the ΛCDM model, are equal to Ω th dm,0 = 1 1+e (1 − Ω b,0 ) = 0.2559 and Ω th de,0 = e 1+e (1 − Ω b,0 ) = 0.6955 in very good agreement with the measured values Ω obs dm,0 = 0.2589 and Ω obs de,0 = 0.6911 (their ratio 2.669 is close to the pure number e = 2.71828...). We point out, however, important difficulties with the logotropic model, similar to those encountered by the generalized Chaplygin gas model. These problems are related to the difficulty of forming large-scale structures due to an increasing speed of sound as the Universe expands. We discuss potential solutions to these problems, stressing in particular the importance to perform a nonlinear study of structure formation.

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Core mass-halo mass relation of bosonic and fermionic dark matter halos harboring a supermassive black hole

Cited by 22 publications

References 88 publications

Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere

Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere

Astronomy with energy dependent flavour ratios of extragalactic neutrinos

A new logotropic model based on a complex scalar field with a logarithmic potential

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