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PoS(DIS2014)137 http://pos.sissa.it/ ∗ [email protected] Speaker. is a good candidatemotivated models for of dark dark . matter. Indark However this matter, talk there especially I about are give , more a , short interesting and review right-handed and on scalar some well- of dark the matter. non-neutralino ∗ Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

XXII. International Workshop on Deep-Inelastic Scattering28 and April Related - Subjects 2 May 2014 Warsaw, Poland Ki-Young CHOI Korea Astronomy and Space Science Institute E-mail: Non-neutralino PoS(DIS2014)137 in 30 . However 2 Z M / Ki-Young CHOI to 1 2 P M / and cross section from 1 P 2 M eV to mass : DM is non-relativistic to seed the properly. µ : The amount of relic DM at present should be around 25% of the energy : DM do not have and only the upper bound is given to the mag- : DM have existed from early Universe as well as in the present Universe around Stability contents of the present Universe. Coldness (or warm) galaxies and clusters. Neutrality nitudes of self interactions. Relic density Dark matter should have existed from the early Universe at least before the relevant scales for Weakly interacting massive (WIMP) is one of the most popular candidate for DM. Dark matter (DM) is a solution to the missing mass problem to explain the discrepancies be- At least dark matter as a particle can explain all the observational anomalies in different scales, • • • • the large scale structure formation enterthesis the horizon, (BBN) which epoch. might be just Thereforestrong after constraints DM big are bang production applied nucleosyn- must for the have models been where completed the production before of BBN.They DM occurs So were after in the this the period. thermalples equilibrium from with them thermal after plasms it incompared became to the the non-relativistc. early background Universe radiation Therefore and and the iterasing then number depends all decou- only the density on information is the during the annihilation quite thermal crosssuppressed suppressed equilibrium. section compared of Even to DMs though the the radiation, number density thesity is energy quite of density becomes DM enough due to to explainWIMPs the the include relic large neutralino, den- mass scalar of neutrino,on. DM, RH which neutrino, minimal is DM, typically Klauza-Klein around DM 100GeV. and so The candidates of the production of DM is modelin dependent and the there Literature are several different ways suggested up to now 2. Production of dark matter tween the visible matter andwhich the can gravitational absorb matter. or The emit telescopesnamics light can of only. directly the observe celestial However body the orsince method the the using gravitational gravitational lensing is effects can universal. such detectscale as all The to dy- forms large difference scale of in of matter both the and measurements Universe. energy, exist in all scalessuch from as small galaxy rotational curve,background bullet radiation cluster, (CMB) large and scale etc, with structureof additional formation, dark single matter cosmic component as microwave of a particle. particle The should properties satisfy Non-neutralino Dark Matter 1. Introduction the magnitude: mass from There are many well-motivated candidatessterile of neutrino dark etc. matter The such mass as and WIMP, interactions axion, of axino, the gravitino, DM candidates spans over more than 10 PoS(DIS2014)137 Ki-Young CHOI , and the correct reh T GeV for the DM mass 10 3 ]. Or the large injection of energy can also change the spectrum 5 , 4 , 3 ]. 2 , 1 If the DM is charged particle, then there could be an asymmetry between DM particle and DM The extremely weakly interacting massive particle (E-WIMP) may not be in the thermal equi- For scalars, the classical value can be displaced from the vacuum in the early Universe. In this In supersymmetric theory, the lightest supersymmetric particle (LSP) is stable if the R-parity is Since the interaction is very weak, the could not be in the thermal equilibrium in However due to the small interaction, it has serious constraints from the big bang nucleosyn- GeV [ 8 of cosmic background radiation andTherefore make BBN and it CMB deviate put fromitino strong Planckian dark constraints distribution on matter. by the observation. Due nextalmost LSP to ruled-out, and the while the BBN stau production constraints,10 NLSP of for the is grav- GeV viable Gravitino when DM, the the reheating neutralino temperature NLSP is is less than around . This asymmetry may affectchanges the depending thermal on decoupling the of asymmetry. DMDM The asymmetry and to asymmetric thus that dark the of matter relic .around has density Because 10 been with GeV tried the mass similar to number gives connectin of correct the the asymmetry, relic the direct density light detection for DM together. of DM, they were used to explainlibrium the in anomalies the early Universe ifcase, the even reheating though temperature the after interaction inflation is iscan not not produce enough high enough to enough. make of In them DM, that is equilibrium, while negligible the the since opposite thermal the process plasma number (E-WIMPs still density into ofcan thermal them be particles) is enough quite to suppressed. explain Thisthese small the amount examples relic of such density E-WIMPs as of gravitino DM and if axino more their in mass the is next around section. case, 100GeV. when the We will mass get isposition to comparable and to then the oscillate Hubble around expansion,matter the it and vacuum. begins becomes The to a oscillating run good scalar frombelow candidate behaves the the for like misaligned QCD DM. non-relativistic phase The transition famous and example has is coherent axion, oscillations. which has potential 3. Gravitino dark matter conserved. The lightest neutralino is onefor example E-WIMP of DM WIMP if DM it and is gravitino LSP. Thewhen is gravitino another the is candidate the SUSY of is broken.breaking and the mechanism. mass The is generated mass The can interactionscale. be is from set eV from to the TeV theory depending itself, on and thethe is early suppressed Universe. by Planck However smallscatterings. amount This could thermal be production produced depends from on the the thermal reheating backgrounds temperature, by thesis and cosmic microwave background radiation.ticle Because can the decay next to lightest Gravitino supersymmetric at par- lateof times high usually energetic after big particles bang into nucleosynthesischange the epoch, plasma the their injection can abundance destroy [ the standard production of light nuclei and Non-neutralino Dark Matter amount of DM can bearound produced 100GeV. if Therefore the if reheating thepreserved, temperature it gravitino can is around be the 10 a lightest good supersymmetric candidate particle for and DM. R-parity is PoS(DIS2014)137 ]. For 10 ]. 13 , Ki-Young CHOI 12 , 11 ]. 8 , ] and DFSZ model [ 7 9 , 6 ]. The large production of entropy ]. 18 22 , ]. However the large Yukawa coupling ]. 17 21 GeV from the energy loss in the stars and 16 , , 12 20 15 , 4 14 GeV and 10 9 In a supersymmetric neutrinophilic Higgs model, the right-handed sneutrino can be in the If axino is heavy, then it can decay to produce DM [ Dark matter is one of the fundamental problems in the cosmology, and particle When R-parity is broken, there is no more problem with BBN, since the NLSP decay much The axino is the fermionic superpartner of the axion, which is introduced to explain the strong There are two representative models of axion, KSVZ model [ There is also non-thermal production of axinos from the decay of NLSP after out-of-equilibrium. thermal equilibrium in the earlypectation Universe value with in the the large neutrinophilic Yukawa coupling Higgs and model small [ vacuum ex- from the decay of axinos cancase, dilute a the large gravitinos annihilation and cross thus section relaxespreferred. of the neutralino problem is of needed, gravitino. and In thus this -like neutralino is 5. Right-handed scalar neutrino dark matter generates a lot of problems together suchand as LEP, flavour decay violation, collider experiments constraints andregion from dark LHC where matter the relic deviation density.model of However from there the the could predicted observation be can muon a be small anomalous explained in magnetic this moment model [ in the standard physics. The existence is evidentmoment. from many For observations WIMP, and the only interaction the of identification DM is might left at be the the weak scale and fortunately detected in 6. Discussion earlier than BBN epoch.lifetime much Through longer the than R-parity therays breaking age that of interactions, can the be Gravitino Universe. detectable can in The decay the decay future with of Gamma-ray Graviitnos observation can [ produce gamma- CP problem. The interaction ofwhich axino to is ordinary constrained matter to is be determined between by the 10 Peccei-Quinn scale, For heavy axinos with mass largerinant than source around 100MeV, for axino the production. non-thermalsource production for For can the be light production dom- axinos, of then axino dark the matter thermal [ production can be the main Non-neutralino Dark Matter 4. Axino dark matter overabundance of axion production. The massbe of between axino keV is and also Gravitino model mass. dependent and considered to KSVZ model, the axion interactionfrom is the mediated scatterings by or the decays heavyproportional of to and the the the thermal reheating axinos particles. temperature, areas , produced while The squark those axino or abundance from from theis is scatterings decays independent large is on of enough the thermal reheating to particles temperaturedominated produce such by once the the the Higgsino temperature heavy coupling, thermal which is particles. also temperature independent For [ DFSZ model, axino production is PoS(DIS2014)137 (2006) 0606 Ki-Young CHOI (2010) 028 1003 (2013) 1685 (2008) 065011 (2010) 033 [arXiv:1007.1728 (2008) 123501 [arXiv: 63 78 (2009) 103 [arXiv:0903.3974 77 1010 (2012) 106 [arXiv:1108.2282 (2001) 033 [hep-ph/0101009]. 0905 (2012) 083529 [arXiv:1208.2496 (1999) 4180 [hep-ph/9905212]. 1204 (1981) 199; A. P. Zhitnitskii, Sov. J. 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D Ki-Young Choi, D. Restrepo, C. E. Yaguna and O. Zapata, JCAP [9] J. E. Kim, Phys. Rev. Lett. Non-neutralino Dark Matter the direct, indirect detection oreven in though the the collider. interaction For isdetection E-WIMP might very such be weak, as more the axion, difficultaxion axino, correct and experiment and abundance depends or gravitino, of on in the DM the model.probe can cavity in experiment. be the can obtained. direct However detection. be the gravitino detected However Their in it or in the might axino astrophysical the give signatures. is solar signatures quite in the difficult collider to as missing energy or References [11] E. J. Chun, Phys. Rev. [18] Kiwoon Choi, K. -Y. Choi and C. S. Shin, Phys. Rev. D [19] Ki-Young Choi, Jihn E. Kim and L. Roszkowski, J. Korean Phys. Soc. [10] M. Dine, W. Fischler and M. Srednicki, Phys. Lett. B [12] K. J. Bae, K. Choi and[13] S. H.K. Im, J. JHEP Bae, E. J. Chun[14] and S.L. H. Covi, Im, J. JCAP E. Kim and L. Roszkowski, Phys. Rev. Lett. [17] Ki-Young Choi, Jihn E. Kim, H. M. Lee, and O. Seto, Phys. Rev. D [15] L. Covi, H. B. Kim, J.[16] E. KimK. and -Y. L. Choi, Roszkowski, L. JHEP Covi, J. E. Kim and L. Roszkowski, JHEP PoS(DIS2014)137 Ki-Young CHOI 089904 (2012)]. 86 6 043515 (2012) [Erratum-ibid. D (2013) 035005 [arXiv:1305.4322 [hep-ph]]. 86 88 [arXiv:1205.3276 [hep-ph]]. [21] K. -Y. Choi and O. Seto, Phys. Rev. D Non-neutralino Dark Matter [20] K. -Y. Choi and O. Seto, Phys. Rev. D [22] K. -Y. Choi, O. Seto and C. S. Shin, arXiv:1406.0228 [hep-ph].