====== QFT at Finite Temperature ======

<tabbox Why is it interesting?> 
While nowadays we can use as a good approximation that the temperature is zero, in the early universe it was significantly higher. Thus, if we want to understand the fundamental interactions in the early universe, i.e. shortly after the Big Bang, we need to take into account that the temperature is non-zero. 



See also: [[advanced_notions:symmetry_breaking:higgs_mechanism:effective_potential|Effective Potential]]

<tabbox Layman> 

<note tip>
Explanations in this section should contain no formulas, but instead colloquial things like you would hear them during a coffee break or at a cocktail party.
</note>
  
<tabbox Student> 

Good introductions are

  * {{ :advanced_notions:quantum_field_theory:quantum_field_theory_for_children.pdf |}} and 
  * [[https://arxiv.org/pdf/hep-ph/0609226.pdf|Thermodynamics of electroweak matter]] by A. Gynther 
 

Standard References:

  * [[https://arxiv.org/abs/hep-ph/9901312|Finite Temperature Field Theory and Phase Transitions]] by  Mariano Quiros
  * Finite-Temperature Field Theory by Joseph I. Kapusta




<tabbox Researcher> 

<note tip>
The motto in this section is: //the higher the level of abstraction, the better//.
</note>

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<tabbox Examples> 

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<tabbox History> 

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