In the DARKexp framework for collisionless isotropic relaxation of self-gravitating matter, the central object is the differential energy distribution n(E), which takes a maximum-entropy form proportional to exp[-β(E - Φ(0))] - 1, Φ(0) being the depth of the potential well and β the standard Lagrange multiplier. Then the first and quite non-trivial problem consists in the determination of an ergodic phase-space distribution which reproduces this n(E). In this work we present a very extensive and accurate numerical solution of such DARKexp problem for systems with cored mass density and finite size. This solution holds throughout the energy interval Φ(0)≤ E≤ 0 and is double-valued for a certain interval of β. The size of the system represents a unique identifier for each member of this solution family and diverges as β approaches a specific value. In this limit, the tail of the mass density ρ(r) dies off as r-4, while at small radii it always starts off linearly in r, that is ρ(r)-ρ(0) r.

Destri, C. (2018). Cored DARKexp systems with finite size: Numerical results. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2018(8), 026-026 [10.1088/1475-7516/2018/08/026].

Cored DARKexp systems with finite size: Numerical results

Destri, C
2018

Abstract

In the DARKexp framework for collisionless isotropic relaxation of self-gravitating matter, the central object is the differential energy distribution n(E), which takes a maximum-entropy form proportional to exp[-β(E - Φ(0))] - 1, Φ(0) being the depth of the potential well and β the standard Lagrange multiplier. Then the first and quite non-trivial problem consists in the determination of an ergodic phase-space distribution which reproduces this n(E). In this work we present a very extensive and accurate numerical solution of such DARKexp problem for systems with cored mass density and finite size. This solution holds throughout the energy interval Φ(0)≤ E≤ 0 and is double-valued for a certain interval of β. The size of the system represents a unique identifier for each member of this solution family and diverges as β approaches a specific value. In this limit, the tail of the mass density ρ(r) dies off as r-4, while at small radii it always starts off linearly in r, that is ρ(r)-ρ(0) r.
Articolo in rivista - Articolo scientifico
dark matter theory; gravity;
English
026
026
1
Destri, C. (2018). Cored DARKexp systems with finite size: Numerical results. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2018(8), 026-026 [10.1088/1475-7516/2018/08/026].
Destri, C
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/206628
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