Matter Models Matt Gonderinger UW Madison NPAC Pheno, 2010.05.11 - - PowerPoint PPT Presentation

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Matter Models Matt Gonderinger UW Madison NPAC Pheno, 2010.05.11 - - PowerPoint PPT Presentation

Sep 22, 2023 166 likes •329 views

Vacuum Stability of Singlet Dark Matter Models Matt Gonderinger UW Madison NPAC Pheno, 2010.05.11 MG, Y. Li, H. Patel and M. J. Ramsey-Musolf, JHEP 1001 (2010) 053 [0910.3167] Outline Motivation for scalar singlets The real scalar

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Vacuum Stability of Singlet Dark Matter Models

Matt Gonderinger UW Madison – NPAC Pheno, 2010.05.11

MG, Y. Li, H. Patel and M. J. Ramsey-Musolf, JHEP 1001 (2010) 053 [0910.3167]

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 Motivation for scalar singlets  The real scalar singlet potential & parameters  Explanation of vacuum stability analysis  Constraining scalar singlet dark matter

Outline

Vacuum stability analysis restricts mass, self-interaction, and new physics scale in a real scalar singlet model of dark matter

  • M. Gonderinger, Pheno 2010
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 Dark matter candidate if stable  Mixing with the Higgs  Play a role in electroweak phase transition  Arise in MSSM extensions  They are simple!

Why study scalar singlets?

  • M. Gonderinger, Pheno 2010
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 ℤ2 symmetry  Minimum at ℎ = 𝑤 = 246 𝐻𝑓𝑊, 𝑇 = 0  ⇒ the singlet is a stable dark matter candidate

Real Scalar Singlet

𝑊 = 𝑛2𝐼†𝐼 + 𝜇 6 𝐼†𝐼

2

+𝑏2𝑇2𝐼†𝐼 + 𝑐2 2 𝑇2 + 𝑐4 4 𝑇4

  • M. Gonderinger, Pheno 2010
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 𝑛ℎ

2 = 𝜇𝑤2/3 (no mixing between the Higgs and

singlet)  𝑛𝑇

2 = 𝑐2 + 𝑏2𝑤2 (small 𝑛𝑇 and moderate 𝑏2 ⇒ 𝑐2 < 0)

 𝑏2 determines both direct detection cross section and relic density

Parameters

𝜏𝑒𝑒 ∼ 𝑏2

2

Ω𝑇 ∼ 1 𝜏𝑏𝑜𝑜 ∼ 1 𝑏2

2

  • M. Gonderinger, Pheno 2010
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Diagrams

∼ 𝑏2𝑤

  • M. Gonderinger, Pheno 2010
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 RG-improved one-loop effective potential is a function of the two fields, ℎ and 𝑇  Require that ℎ = 𝑤, 𝑇 = 0 be the global minimum below new physics scale Λ  Choose parameters to avoid:

 Second minimum along ℎ axis due to running of 𝜇  Deeper minimum along 𝑇 axis when 𝑐2 < 0  Runaway direction caused by negative 𝑏2

Vacuum Stability

  • M. Gonderinger, Pheno 2010
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SLIDE 8

Cartoons

𝑊 ≤ 𝑊

𝐹𝑋

ℎ 𝑇 𝑏2 > 0 𝛾𝜇 ∼ 4𝜇2 − 36𝑧𝑢

4

+12𝑏2

2 + ⋯

𝑐2 < 0 𝑇 𝑊 𝑊 ℎ

  • M. Gonderinger, Pheno 2010
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Dark Matter

CDMS excluded region

(not most recent results)

Super-CDMS sensitivity region WMAP Vacuum stability excluded Λ = 1 𝑈𝑓𝑊

  • M. Gonderinger, Pheno 2010
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More Dark Matter

Λ = 1 𝑈𝑓𝑊 Λ = 109 𝐻𝑓𝑊

  • M. Gonderinger, Pheno 2010
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Even More Dark Matter

Λ = 1 𝑈𝑓𝑊 Λ = 109 𝐻𝑓𝑊

  • M. Gonderinger, Pheno 2010
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OMG Dark Matter

XENON100?

  • M. Gonderinger, Pheno 2010

He et al., [1004.3464]

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 Can the real scalar singlet be a very light (𝑛𝑇 < 10 𝐻𝑓𝑊) dark matter particle?  Possibly, but vacuum stability requires…

 a low new physics scale Λ (𝑏2 is small)  a large self-interaction 𝑐4 (𝑐2 is negative)

 A more thorough analysis is necessary for this small 𝑛𝑇 region (including most recent experimental limits)

Hope

  • M. Gonderinger, Pheno 2010
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Summary

Direct detection + relic density

Vacuum stability analysis

Constrain mass, self- interaction, new physics scale

  • M. Gonderinger, Pheno 2010
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 Vacuum stability is a generally interesting analysis

 Complex scalar singlet?  Finite temperature electroweak phase transition?  Metastable vacuum and tunneling?  Non-zero singlet vev?  Higgs phenomenology?

For the Future

  • M. Gonderinger, Pheno 2010