The distribution of inelastic dark matter in the Sun

Blennow, Mattias; Clementz, Stefan; Herrero-García, Juan

doi:10.1140/epjc/s10052-018-5863-4

Cited by 18 publications

(32 citation statements)

References 66 publications

(96 reference statements)

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“…In [12] it is argued that equilibrium between capture and annihilation of DM particles in this scenario is eventually reached also for the case of pure inelastic scattering (but see also [14]). As for the previous case of elastic scattering, we thus assume equilibrium, i.e.…”

Section: B Inelastic Dark Mattermentioning

confidence: 96%

“…In the framework of these models, gamma rays and electrons produced from DM captured by the Sun are also detectable at Earth. In a further class of models, DM scatters inelastically off Sun nuclei, instead of elastically (see for instance [8][9][10][11][12][13][14]). This leads to a significant accumulation of DM particles just outside the surface of the Sun.…”

Section: Introductionmentioning

confidence: 99%

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Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

et al. 2020

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We use 7 years of electron and positron Fermi-LAT data to search for a possible excess in the direction of the Sun in the energy range from 42 GeV to 2 TeV. In the absence of a positive signal we derive flux upper limits which we use to constrain two different dark matter (DM) models producing e + e − fluxes from the Sun. In the first case we consider DM model being captured by the Sun due to elastic scattering and annihilation into e + e − pairs via a long-lived light mediator that can escape the Sun. In the second case we consider instead a model where DM density is enhanced around the Sun through inelastic scattering and the DM annihilates directly into e + e − pairs. In both cases we perform an optimal analysis, searching specifically for the energy spectrum expected in each case, i.e., a box-like shaped and line-like shaped spectrum respectively. No significant signal is found and we can place limits on the spin-independent cross-section in the range from 10 −46 cm 2 to 10 −44 cm 2 and on the spin-dependent cross-section in the range from 10 −43 cm 2 to 10 −41 cm 2 . In the case of inelastic scattering the limits on the cross-section are in the range from 10 −43 cm 2 to 10 −41 cm 2 . The limits depend on the life time of the mediator (elastic case) and on the mass splitting value (inelastic case), as well as on the assumptions made for the size of the deflections of electrons and positrons in the interplanetary magnetic field. PACS numbers: 95.35.+d, 95.85.Ry

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Section: B Inelastic Dark Mattermentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

et al. 2020

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“…This talk is devoted to a new halo-independent (HI) framework to compare DD signals with upper limits from neutrino telescopes [1,2].…”

Section: Motivation: a New Halo-independent Frameworkmentioning

confidence: 99%

“…Right) The shaded area represents the horizontal integration needed for the capture rate in the case of inelastic scattering, see ref. [2] for details.…”

Section: Motivation: a New Halo-independent Frameworkmentioning

confidence: 99%

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Predicting the capture rate in the Sun from a direct detection signal independently of the astrophysics

Herrero-García¹

2016

J. Phys.: Conf. Ser.

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Abstract. The goal of the works on which this talk is based is to relate a direct detection signal with neutrino limits from the Sun independently of the astrophysics. In order to achieve this we derive a halo-independent lower bound on the dark matter capture rate in the Sun from a direct detection signal, with which one can set upper limits on the branching ratios into different channels from the absence of a high-energy neutrino flux in neutrino observatories. We also extend this bound to the case of inelastic scattering, both endothermic and exothermic.From two inelastic signals we show how the dark matter mass, the mass difference of the states and the couplings to neutrons and protons can be obtained. Furthermore, one can also pin down the exothermic/endothermic nature of the scattering, and therefore a precise lower bound on the solar capture rate is predicted. We also discuss isospin violation and uncertainties due to form factors. Motivation: a new halo-independent frameworkIt is well-known that dark matter (DM) direct detection (DD) signals are very sensitive to the astrophysical uncertainties of the halo, which makes their compatibility with other results astrophysics-dependent. This talk is devoted to a new halo-independent (HI) framework to compare DD signals with upper limits from neutrino telescopes [1,2].Let us first review the basic expressions for DM DD and the well-known HI framework used for comparing among DD signals. For SI interactions, the DM event rate in underground detectors can be written as [3]where f det (v) is the (unknown) velocity distribution in the detector rest-frame, F A (E R ) is a nuclear form factor, A 2 eff = (Z + κ (A − Z)) 2 with κ = f n /f p andThe mass-splitting parameter δ appears in inelastic interactions [4], given by δ ≡ m χ * − m χ , and thus it is positive (negative) for endothermic (exothermic [5]) interactions. For δ = 0 elastic interactions are recovered. σ SI is the total DM-proton scattering cross section at zero momentum transfer, µ χp is the DM-proton reduced mass and ρ χ is the local DM mass density.

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Testing theories of gravity with planetary ephemerides

Fienga,

Minazzoli

2024

Living Rev Relativ

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We describe here how planetary ephemerides are built in the framework of General Relativity and how they can be used to test alternative theories. We focus on the definition of the reference frame (space and time) in which the planetary ephemeris is described, the equations of motion that govern the orbits of solar system bodies and electromagnetic waves. After a review on the existing planetary and lunar ephemerides, we summarize the results obtained considering full modifications of the ephemeris framework with direct comparisons with the observations of planetary systems, with a specific attention for the PPN formalism. We then discuss other formalisms such as Einstein-dilaton theories, the massless graviton and MOND. The paper finally concludes on some comments and recommendations regarding misinterpreted measurements of the advance of perihelia.

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The distribution of inelastic dark matter in the Sun

Cited by 18 publications

References 66 publications

Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

Predicting the capture rate in the Sun from a direct detection signal independently of the astrophysics

Testing theories of gravity with planetary ephemerides

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