Scattering in the Attractive Yukawa Potential in the Limit of Strong Interaction

Khrapak, S. A.; Ivlev, A. V.; Morfill, G. E.; Zhdanov, S. K.

doi:10.1103/physrevlett.90.225002

Cited by 195 publications

(200 citation statements)

References 13 publications

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“…Within the non-perturbative regime, analytic formulae for σ T have been obtained only within the classical limit (m X v/m φ 1) [21,82,83], given for an attractive potential by…”

Section: Dark Forces and Dark Matter Scatteringmentioning

confidence: 99%

Beyond collisionless dark matter: Particle physics dynamics for dark matter halo structure

2013

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Dark matter (DM) self-interactions have important implications for the formation and evolution of structure, from dwarf galaxies to clusters of galaxies. We study the dynamics of self-interacting DM via a light mediator, focusing on the quantum resonant regime where the scattering cross section has a non-trivial velocity dependence. While there are long-standing indications that observations of small scale structure in the Universe are not in accord with the predictions of collisionless DM, theoretical study and simulations of DM self-interactions have focused on parameter regimes with simple analytic solutions for the scattering cross section, with constant or classical velocity (and no angular) dependence. We devise a method that allows us to explore the velocity and angular dependence of self-scattering more broadly, in the strongly-coupled resonant and classical regimes where many partial modes are necessary for the achieving the result. We map out the entire parameter space of DM self-interactions -and implications for structure observations -as a function of the coupling and the DM and mediator masses. We derive a new analytic formula for describing resonant s-wave scattering. Finally, we show that DM self-interactions can be correlated with observations of Sommerfeld enhancements in DM annihilation through indirect detection experiments.

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“…Within the non-perturbative regime, analytic formulae for σ T have been obtained only within the classical limit (m X v/m φ 1) [21,82,83], given for an attractive potential by…”

Section: Dark Forces and Dark Matter Scatteringmentioning

confidence: 99%

Beyond collisionless dark matter: Particle physics dynamics for dark matter halo structure

2013

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“…The elastic scattering problem is then analogous to the screened Coulomb scattering in a plasma [29], which is well fit by a cross-section [24,30],…”

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confidence: 99%

Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential

2011

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We show that cold dark matter particles interacting through a Yukawa potential could naturally explain the recently observed cores in dwarf galaxies without affecting the dynamics of objects with a much larger velocity dispersion, such as clusters of galaxies. The velocity dependence of the associated cross-section as well as the possible exothermic nature of the interaction alleviates earlier concerns about strongly interacting dark matter. Dark matter evaporation in low-mass objects might explain the observed deficit of satellite galaxies in the Milky Way halo and have important implications for the first galaxies and reionization. PACS numbers: 95.35+d, Introduction. The collisionless cold dark matter (CDM) model has been highly successful in accounting for the gravitational growth of density perturbations from their small observed amplitude at early cosmic times (as imprinted on the cosmic microwave background anisotropies [1]) to the present-day structure of the Universe on large scales. However, it is far from clear that the predictions of this model are valid on small scales.New data on low mass galaxies indicate that their dark matter distribution has a core [2], in contrast to the cusped profile expected from collisionless CDM simulations [3]. The mean value of the inner logarithmic slope of the mass density profile in seven dwarf galaxies within the THINGS survey is observed to be −0.29±0.07[4], much shallower than the expected slope of ∼ −1 from pure CDM simulations. Moreover, the dynamics of dwarf spheroidal galaxies, such as Fornax [5], Ursa-Minor [6], and Sculptor [7], whose luminosities and dynamical masses are smaller by 2-3 orders of magnitude than the THINGS galaxies, indicates a characteristic core density of ∼ 0.1 ± 0.05M pc −3 = (7 ± 4) × 10 −24 g cm −3 . Since these dwarf spheroidals are dominated by dark matter throughout, it is challenging to explain their inferred cores by the gravitational interaction of the dark matter with the baryons [8]. Although it is conceivable that powerful gas outflows from an early baryon-dominated nucleus would reduce the central dark matter density in luminous galaxies [9,10], the formation of a massive baryonic nucleus would initially compress the CDM [11] and exacerbate the discrepancy that needs to be resolved [8], and also potentially violate the observed low luminosities from dwarf galaxies at higher redshifts [12,13]. High-redshift observations of dwarf galaxies must find evidence for the required strong feedback phase, or else an alternative process is at play. Some recent simulations that include feedback do not observe the appearance of cores within the lowest luminosity galaxies [14].To alleviate early signs of the above discrepancy, Spergel & Steinhardt [15] adopted the Strongly-

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“…In their preceding Comment, Khrapak et al have raised two objections against the analysis of our experiments: First, the use of the electron Debye length in our comparison with the standard approach of Barnes et al 9 is considered as inadequate and, second, the ion drag model of the same authors 10,11 is favored over the standard approach of Barnes et al In this Response, we will address these two points.…”

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confidence: 94%

“…In our analysis 7,8 we have used the electron Debye length, whereas Khrapak et al 10,11 argue that the linearized Debye length would be more appropriate.…”

Section: ϫ2mentioning

confidence: 99%

“…In the standard approach of Barnes et al 9 the question of the appropriate Debye length is not explicated. Also Khrapak et al 10 have left the proper choice of the shielding length open, only in their very recent paper 11 the authors propose to use the linearized Debye length under typical discharge conditions. In contrast, Kilgore et al 12 have shown in early simulations and calculations, which are very similar to those of Khrapak et al, 10,11 that the simulated ion drag force is in very good agreement with the model of Barnes et al 9 when the electron Debye length is used.…”

Section: ϫ2mentioning

confidence: 99%

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Response to “Comment on ‘Measurement of the ion drag force on falling dust particles and its relation to the void formation in complex (dusty) plasmas’ ” [Phys. Plasmas 10, 4579 (2003)]

2003

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Scattering in the Attractive Yukawa Potential in the Limit of Strong Interaction

Cited by 195 publications

References 13 publications

Beyond collisionless dark matter: Particle physics dynamics for dark matter halo structure

Beyond collisionless dark matter: Particle physics dynamics for dark matter halo structure

Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential

Response to “Comment on ‘Measurement of the ion drag force on falling dust particles and its relation to the void formation in complex (dusty) plasmas’ ” [Phys. Plasmas 10, 4579 (2003)]

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