Consequences of DM/antiDM Oscillations for Asymmetric WIMP Dark Matter

Cirelli, Marco; Panci, Paolo; Zaharijas, Gabrijela; Servant, Geraldine

doi:10.1088/1475-7516/2012/03/015

Article
Report number	arXiv:1110.3809 ; CERN-PH-TH-2011-045 ; SACLAY-T11-022 ; CP3-ORIGINS-2011-031 ; DIAS-2011-23 ; CERN-PH-TH-2011-045 ; SACLAY-T11-022 ; CP3-ORIGINS-2011-031 ; DIAS-2011-23
Title	Consequences of DM/antiDM Oscillations for Asymmetric WIMP Dark Matter
Author(s)	Cirelli, Marco (CERN ; Saclay, SPhT) ; Panci, Paolo (CERN ; L'Aquila U. ; Gran Sasso ; Paris U., VI-VII) ; Servant, Geraldine (CERN ; Saclay, SPhT) ; Zaharijas, Gabrijela (Saclay, SPhT ; Paris, Inst. Astrophys.)
Publication	2012
Imprint	19 Oct 2011
Number of pages	26
Note	Comments: 25 pages, 5+1 figures 27 pages, 6+1 figures; v2: version submitted to JCAP for publication, one new figure and one new table added, summary plots slightly revised, a few clarifications added, main point emphasized, results unchanged
In:	JCAP 03 (2012) 015
DOI	10.1088/1475-7516/2012/03/015
Subject category	Particle Physics - Phenomenology
Abstract	Assuming the existence of a primordial asymmetry in the dark sector, a scenario usually dubbed Asymmetric Dark Matter (aDM), we study the effect of oscillations between dark matter and its antiparticle on the re-equilibration of the initial asymmetry before freeze-out, which enable efficient annihilations to recouple. We calculate the evolution of the DM relic abundance and show how oscillations re-open the parameter space of aDM models, in particular in the direction of allowing large (WIMP-scale) DM masses. A typical wimp with a mass at the EW scale (\sim 100 GeV - 1 TeV) presenting a primordial asymmetry of the same order as the baryon asymmetry naturally gets the correct relic abundance if the DM-number-violating Delta(DM) = 2 mass term is in the \sim meV range. The re-establishment of annihilations implies that constraints from the accumulation of aDM in astrophysical bodies are evaded. On the other hand, the ordinary bounds from BBN, CMB and indirect detection signals on annihilating DM have to be considered.
Copyright/License	Preprint: © 2011-2025 CERN (License: CC-BY-3.0)

$\em \small Illustrative plots of the solutions of the evolution equations in the case of annihilations only (top left panel, discussed in Sec.~\ref{sec:annonly}), annihilations with oscillations (top right panel, Sec.~\ref{sec:ann+osc}) and in the case which includes elastic scatterings (bottom left panel, Sec.~\ref{sec:wscatterings}). The blue (magenta) line represents the comoving population of $n^+$ ($n^-$), the black line their sum. The arrow points to the value of the primordial asymmetry, the green band is the correct relic abundance ($\pm\, 1 \sigma$).$ $\em \small Illustrative plots of the solutions of the evolution equations in the case of annihilations only (top left panel, discussed in Sec.~\ref{sec:annonly}), annihilations with oscillations (top right panel, Sec.~\ref{sec:ann+osc}) and in the case which includes elastic scatterings (bottom left panel, Sec.~\ref{sec:wscatterings}). The blue (magenta) line represents the comoving population of $n^+$ ($n^-$), the black line their sum. The arrow points to the value of the primordial asymmetry, the green band is the correct relic abundance ($\pm\, 1 \sigma$).$ $\em \small Illustrative plots of the solutions of the evolution equations in the case of annihilations only (top left panel, discussed in Sec.~\ref{sec:annonly}), annihilations with oscillations (top right panel, Sec.~\ref{sec:ann+osc}) and in the case which includes elastic scatterings (bottom left panel, Sec.~\ref{sec:wscatterings}). The blue (magenta) line represents the comoving population of $n^+$ ($n^-$), the black line their sum. The arrow points to the value of the primordial asymmetry, the green band is the correct relic abundance ($\pm\, 1 \sigma$).$ Show more plots

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