HYBRID INFLATION

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HYBRID INFLATION

• Serena Nobili
• Course in Inflation, Structure formation and CMB

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http//cas.bellarmine.edu/tietjen/EcEv_Distance_l
earning/cosmology.htm
H Y B R I D
POWER LAW INFLATION
OLD INFLATION
CHAOTIC
NEW INFLATION
SLOW ROLLING
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1 FIELD THEORY

• Initial conditions thermal equilibrium at high
  temperature
• Regime during inflation
• slow roll
• exponential growth
• End of inflation
• never ending
• First order phase transition
• Second order phase transition

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ZOOLOGY of INFLATION

• 1st initial conditions
• Thermal equilibrium
• at high temperature
• (Old and New inflation)
• All possible initial
• conditions
• (Chaotic inflation)

• 2nd regime during inflation
• Exponential inflation
• Power law inflation

• 3rd end of inflation
• Slow rollover
• First order phase transition
• Second order phase transition

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HYBRID INFLATION

• 2 scalar fields s and f
• f drives the inflation while s drives f
• No problems with initial conditions

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The effective mass squared of the field s

• For fgtfc the only minimum of the effective
  potential is at s0
• For ffc waterfall!
• For fgtfc phase transition with symmetry breaking

Condition for inflation
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WHY HYBRID INFLATION?

• It solves the main problems with a 1 field model
  specific initial conditions
• Agreement with supersymmetric theories
• and supergravity
• Amplitude of adiabatic perturbations

If ??g?1, M1015 GeV m5 ?1010 GeV galaxy scale
l ? lc ?e50 ? ??/??5 ? 10-5
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References

• http//physics.stanford.edu/linde/
• http//wlap.physics.lsa.umich.edu/umich/mctp/conf/
  2001/sto2001/linde/real/thumb.htm
• http//nedwww.ipac.caltech.edu/level5/Liddle/Liddl
  e_contents.html
• astro-ph/9307002 (Andrei Linde)
• astro-ph/0009491 (A.R.Liddle)
• astro-ph/9401011 (Copeland, Liddle, Lyth)