2019-DissipativeeffectsonMSSMinflation在MSSM通貨膨脹耗散效應(yīng)-文檔資料

1、Dissipative effectson MSSM inflation26th Aug. 98 COSMO08Kohei Kamada(RESCEUzThe University of Tokyo,Japan)Collaboration with Junlchi YokoyamaIn troduction>Inflation(Guth/ SatoC81)Solution of many cosmological problemsWMAP results strongly support inflation.>MSSM(Minimal SupersymmetricStandard

2、Model)*f dirCCl'IOKlPossible candidate for inflaton(MSSM inflation;Allahverdi et. al. (”06)輕i no need for extra fields beyond MSSMSevere fine-tuning of potential and initial conditionCan irrterac十ions with other fields help these difficulties?MSSM inflation>Flat direction/ Vacuum degenerate i

3、n the scalar potential(SUSY and renormalizable limit)/ Slightly lifted by SUSY-breaking effect and non- renormalizable operator一 Flat potentialInflaton candidate!>MSSM inflationPotential including SUSY breaking effect and non-renormalizable operatorAA06 入 2010'1 I 1124Afg32 墟0 :parameterizati

4、on of udd flat directionm、ITeV 入、0(1) Mg : reduced Planck massIf A2 = 20m2, saddle point at 如=(普尹)'-io145GeV/Hubble parameter：Hinf =2mQcO-IGeV、10-0* Low energy inflation Last inflation !?>Fine-tuningRequirement for inflation,A2 20m2/一、_川、Potential parameter： 喬品1K)(to generate correct density

5、perturbation)Initial condition 血： O(10-9)(Slow-roll region :衛(wèi)o(io_1()0cOCan we relax these conditions using the dissipative effect?Dissipative effect on the MSSMinflation>Equation of motion in the dissipativeregime (88 Yokoyama & Maeda) dVt + (3H += 0r : dissipative coefficientIf r » 3H,

6、 slow-roll condition will change.>Slow-roll conditionWhen dissipative coefficient is larger than Hubble parameter, slow-roll conditions change from usual form as follows :Slow-roll parameters :耳三A殆：0三兒広幵Slow-roll conditions :a > 0 and $2U (0)3切一0|異3V （捫d（/）3H+ Consistency checkf Decay product

7、must be the sub dominant component of the Universe.AMochfication to the MSSM inflationSlow-roll condition for r < 1053忖0|異* 21I。一叫20cOcf.) no dissipation 妙一0co|lO_lo(/)coEZ> Slow-roll region is enhanced!Fine-tuning of the potential parameter and the initial condition is relaxed!(condition for

8、slow-roll region to emerge)Derivation of dissipativeeffect>Interactions of inflatonMnt =圧(|殲|%1|2 + W2X22 + |%1F|%22) + 仇認(rèn)2(摳歿* +H.C.) BmkTFlyil2 + I%1F 協(xié) 22 + |yi|2|y2|2+ hi 麗xPL蚊 + 護(hù)石xPRx) + h2 (X©yPL»y + 燈yPRy),X acquires mass from the inflatonmv = h(b,、A：udd : (s)quarksX : Q、Hu, Hd

9、:(S)quarks & Higgs(ino)sy : L,e ： (s)leptons>Derivation of dissipative terms In-in(closed time path) formalism Generating functionalexp卜匚町陽七恥）-branch三 eJioo w+bra nch> +ook timeEffective actionr = w dxJ(f)Effective equation of motionar=0>Effective actionWith dressed propagator of X (inc

10、lude the dissipative process)>Equation of motion in the slow-roll limit0c (t)8（險(xiǎn)九仏-匸血0d）=0,</>A=02048嚴(yán)處r 104 for h?O(10_i)Concl usion/MSSM inflation is a candidate for lowenergy inflation. Dissipative effect can relax the problems of the MSSM inflation./Using in-in formalism, we have derived the dissipative term in the equation of motionDissipation coefficient can be larger than Hubble para mete r.(It depends on the Yukawa couplin