2019-DissipativeeffectsonMSSMinflation在MSSM通貨膨脹耗散效應(yīng)-文檔資料_第1頁
2019-DissipativeeffectsonMSSMinflation在MSSM通貨膨脹耗散效應(yīng)-文檔資料_第2頁
2019-DissipativeeffectsonMSSMinflation在MSSM通貨膨脹耗散效應(yīng)-文檔資料_第3頁
已閱讀5頁,還剩8頁未讀, 繼續(xù)免費(fèi)閱讀

下載本文檔

版權(quán)說明:本文檔由用戶提供并上傳,收益歸屬內(nèi)容提供方,若內(nèi)容存在侵權(quán),請進(jìn)行舉報(bào)或認(rèn)領(lǐng)

文檔簡介

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

溫馨提示

  • 1. 本站所有資源如無特殊說明,都需要本地電腦安裝OFFICE2007和PDF閱讀器。圖紙軟件為CAD,CAXA,PROE,UG,SolidWorks等.壓縮文件請下載最新的WinRAR軟件解壓。
  • 2. 本站的文檔不包含任何第三方提供的附件圖紙等,如果需要附件,請聯(lián)系上傳者。文件的所有權(quán)益歸上傳用戶所有。
  • 3. 本站RAR壓縮包中若帶圖紙,網(wǎng)頁內(nèi)容里面會有圖紙預(yù)覽,若沒有圖紙預(yù)覽就沒有圖紙。
  • 4. 未經(jīng)權(quán)益所有人同意不得將文件中的內(nèi)容挪作商業(yè)或盈利用途。
  • 5. 人人文庫網(wǎng)僅提供信息存儲空間,僅對用戶上傳內(nèi)容的表現(xiàn)方式做保護(hù)處理,對用戶上傳分享的文檔內(nèi)容本身不做任何修改或編輯,并不能對任何下載內(nèi)容負(fù)責(zé)。
  • 6. 下載文件中如有侵權(quán)或不適當(dāng)內(nèi)容,請與我們聯(lián)系,我們立即糾正。
  • 7. 本站不保證下載資源的準(zhǔn)確性、安全性和完整性, 同時(shí)也不承擔(dān)用戶因使用這些下載資源對自己和他人造成任何形式的傷害或損失。

最新文檔

評論

0/150

提交評論