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Kinetic Decoupling of Neutralino Dark Matter RAPID COMMUNICATIONS PHYSICAL REVIEW D, VOLUME 64, 021302͑R͒ Kinetic decoupling of neutralino dark matter Xuelei Chen* Department of Physics, The Ohio State University, 174 West 18th Avenue, Columbus, Ohio 43210 Marc Kamionkowski† California Institute of Technology, Mail Code 130-33, Pasadena, California 91225 Xinmin Zhang‡ Institute of High Energy Physics, Chinese Academy of Sciences, P.O. Box 918-4, Beijing 100039, People’s Republic of China ͑Received 27 March 2001; published 25 June 2001͒ After neutralinos cease annihilating in the early Universe, they may still scatter elastically from other particles in the primordial plasma. At some point in time, however, they will eventually stop scattering. We calculate the cross sections for neutralino elastic scattering from standard-model particles to determine the time at which this kinetic decoupling occurs. We show that kinetic decoupling occurs above a temperature T ϳMeV. Thereafter, neutralinos act as collisionless cold dark matter. DOI: 10.1103/PhysRevD.64.021302 PACS number͑s͒: 98.80.Cq, 13.15.ϩg, 12.60.Jv, 95.35.ϩd I. INTRODUCTION matter candidates, Gunn et al. ͓6͔ showed that they would fall out of kinetic equilibrium shortly after their annihilation Neutralinos provide perhaps the most promising candidate freezes out. Later, Schmid et al. ͓7͔ estimated the decoupling for the mysterious dark matter in galactic halos ͑see, e.g., temperature of neutralino-neutrino interaction. In this paper Refs. ͓1,2͔ for reviews͒. Such particles would have existed in we consider the process of kinetic decoupling of neutralinos thermal equilibrium in the early Universe when the tempera- in more detail. We calculate the cross sections for elastic ture exceeded the mass of the particle. However, as the tem- scattering of neutrinos and photons from neutralinos, and for perature drops below the mass, the rate of the production and completeness, we consider the elastic scattering of neutrali- destruction reactions that maintain the equilibrium density nos from other particles as well. We show that the estimates become smaller than the expansion rate. At this point, anni- for neutrino-neutralino and photon-neutralino scattering used hilations cease, and a relic population of neutralinos remains. by Bœhm et al. neglect important kinematic effects, and thus The calculation of this relic density is straightforward, and to hugely overestimate these cross sections. We show that neu- a first approximation, the relic density is fixed by the cross tralinos are more likely to undergo kinetic freezeout much section for neutralino annihilation to lighter standard-model earlier, at temperatures between a MeV and a GeV, rather particles. The cross section required for the critical density is than a keV. Thus, although Bœhm et al.’s mechanism for ϳ10Ϫ37 cm2, coincidentally within a few orders of magni- collisional damping may be applicable to more general dark- tude of the neutralino annihilation cross section in the mini- matter candidates, it is unlikely to be relevant to the most mal supersymmetric extension of the standard model. promising supersymmetric dark-matter candidates. After freezeout ͑i.e., after they fall out of chemical equi- In the next section we briefly review the cross sections librium͒ neutralinos may still continue scattering elastically required for the Bœhm et al. collisional damping. In Sec. III, from other particles in the primordial plasma, and thus re- we calculate the cross section for neutralino-photon scatter- main in chemical equilibrium. In an interesting recent paper ing. In Sec. IV, we move on to the neutralino-neutrino cross ͓3͔, Bœhm et al. pointed out that if these particles remain in section. We consider elastic scattering of neutralinos from kinetic equilibrium until a temperature Tϳ0.1 keV, at other species in Sec. V, and we conclude in Sec. VI. which point the mass enclosed in a Hubble volume is com- parable to that of a dwarf galaxy, then collisional damping II. REQUIRED CROSS SECTIONS due to elastic scattering of neutrinos and/or photons from neutralinos could erase structure on such scales and thus help In the standard scenario, neutrinos undergo chemical de- resolve the discrepancy between the predicted and observed coupling at a temperature of one MeV and their kinetic de- substructure in Galactic halos ͓4,5͔. They also argued briefly coupling follows shortly thereafter. Now suppose that the that supersymmetric dark-matter candidates may have the re- neutrino has a nonzero elastic-scattering cross section with quired neutralino-photon and/or neutralino-neutrino cross the dark-matter particle ␹. This elastic scattering will keep sections. the dark-matter particles in kinetic equilibrium until the rate When heavy neutrinos were first considered as cold dark at which neutrinos scatter from a given dark-matter particle becomes comparable to the expansion rate. The scattering rate is ⌫ϭn␯␴␯␹c, where n␯ is the number density of neu- *Electronic address: xuelei@pacific.mps.ohio-state.edu trinos and ␴␯␹ is the neutrino–dark-matter elastic-scattering †Electronic address: [email protected] cross section. The Hubble expansion rate is H ‡ Electronic address: [email protected] ϭ1.66g1/2T2/m , where g ϭ3.36 is the effective number * Pl * 0556-2821/2001/64͑2͒/021302͑4͒/$20.0064 021302-1 ©2001 The American Physical Society RAPID COMMUNICATIONS XUELEI CHEN, MARC KAMIONKOWSKI, AND XINMIN ZHANG PHYSICAL REVIEW D 64 021302͑R͒ tralinos are related to these by crossing symmetry, and this led Bœhm et al. to speculate that the elastic-scattering cross sections could also be as large as 10Ϫ38 cm2. This, however, neglects a dramatic suppression of the elastic-scattering cross section that arises from the spinor structure of the amplitude. The amplitude for either process can be written, 2 e ␮ ␯ ␳ ␴ FIG. 1. One of the Feynman diagrams for neutralino annihila- Aϭ ␧␮␯␳␴k k ⑀ ⑀ A¯ , ͑2͒ 4␲2 tion to two photons. There are also other Feynman diagrams for this process. where k␮ and k␯ are the four-momenta of the photons and ⑀␳ ␴ and ⑀ are their polarization four-vectors, and ␧␮␯␳␴ is the of relativistic degrees of freedom at a temperature TϳkeV, Ӎ 19 completely antisymmetric tensor. The reduced amplitude A¯ and mPl 10 GeV is the Planck mass. The temperature at depends on the particle masses and couplings in the diagram which the Hubble volume encloses a baryonic mass M b is loops. Its value for annihilation will differ from that for elas- ϭ 9 ͒Ϫ1/3 ⍀ 2 ͒1/3 ͑ ͒ T 0.15 keV͑M b/10 M ᭪ ͑ bh /0.02 , 1 tic scattering by factors of order unity, but not by many orders of magnitude. For the annihilation process, the four- ⍀ where b is the baryon density and h is the present Hubble momenta will be equal to m␹ , while for elastic scattering, Ϫ Ϫ parameter in units of 100 km sec 1 Mpc 1. Setting ⌫ϭH, they will be equal to the photon energy. Thus, neglecting the at Tϳ0.1 keV, we find that the cross section required to A¯ Ϫ small difference in , we see that the factors of k in the Շ 9 ␴ ϳ 40 2 4 erase structure on 10 M ᭪ scales is ␯␹ 10 cm , amplitude will lead to a reduction by a factor (E␥ /m␹) of which recovers the estimate of Bœhm et al. Similar argu- the elastic-scattering cross section relative to that for annihi- ments for scattering from photons lead Bœhm et al. to esti- lation. For E␥ϳ0.1 keV and a neutralino mass m␹ Ϫ38 2 mate a dark-matter–photon cross section of 10 cm for ϳ100 GeV, this suppression is 10Ϫ36. More precisely, the collisional damping via photon scattering. annihilation cross section is In fact, we believe that Bœhm et al. may have underesti- mated the required cross section by several orders of magni- 2 2 ␣ m␹ ␴ ϭ ͉A¯ ͉2 ͑ ͒ tude. The cold-dark-matter particles are non-relativistic, so ␹␹!␥␥ ␲3 , 3 even if neutrino and photon scattering keep them in kinetic 16 equilibrium, they could hardly move far enough to smooth out fluctuations in the dark-matter density. For collisional while the elastic-scattering cross section is damping to work, the motion of photons and neutrinos must ␣2 be affected. Indeed, this is how collisional damping works in 4 2 ␴␹␥!␹␥ϭ E␥͉A¯ ͉ . ͑4͒ ͑ ͒ 2 2 the case of baryons Silk damping in which density pertur- 3␲ m␹ bations are smoothed on scales which are small compared with the photon diffusion length ͓8͔. If it is in fact the neu- We have calculated this cross section for a number of super- trinos ͑or photons͒ that are responsible for collisional damp- symmetric models using a modified version of the code ing with neutralino-neutrino scattering, then the appropriate NEUTDRIVER ͓1͔. For a range of typical supersymmetric pa- reaction rate to equate to the Hubble length is the rate at rameters and a photon energy of 100 eV, we find which a given neutrino scatters from a neutralino, rather than 10Ϫ79 cm2Ͻ␴Ͻ10Ϫ73 cm2. We thus conclude that elastic vice versa. In this case, the required neutrino–dark-matter neutralino-photon scattering will play no role in maintaining cross section must be larger by the ratio of the neutrino num- kinetic equilibrium of neutralinos, nor of scattering photons ber density to the dark-matter number density, and this factor from neutralinos. 7 is 5ϫ10 (m␹ /GeV), where m␹ is the dark-matter-particle mass. IV. NEUTRALINO-NEUTRINO SCATTERING III. NEUTRALINO-PHOTON SCATTERING The neutrino-neutralino differential scattering cross sec- tion is given by The cross section for annihilation of two neutralinos to two photons has been calculated by a number of authors d␴ ͉M͉2 ͑e.g., Refs. ͓9–14͔͒. Annihilation can proceed, e.g., through a ͩ ͪ ϭ , ͑5͒ ⍀ 2 2 Feynman diagram such as that shown in Fig.
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