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Equation of state (cosmology)

In cosmology, the equation of state of a perfect fluid is characterized by a dimensionless number , equal to the ratio of its pressure to its energy density  :

.

It is closely related to the thermodynamic equation of state and ideal gas law.

Contents

The equationEdit

The perfect gas equation of state may be written as

 

where   is the mass density,   is the particular gas constant,   is the temperature and   is a characteristic thermal speed of the molecules. Thus

 

where   and   for a "cold" gas,   = speed of light.

FLRW equations and the equation of stateEdit

The equation of state may be used in Friedmann–Lemaître–Robertson–Walker equations to describe the evolution of an isotropic universe filled with a perfect fluid. If   is the scale factor then

 

If the fluid is the dominant form of matter in a flat universe, then

 

where   is the proper time.

In general the Friedmann acceleration equation is

 

where   is the cosmological constant and   is Newton's constant, and   is the second proper time derivative of the scale factor.

If we define (what might be called "effective") energy density and pressure as

 
 

and

 

the acceleration equation may be written as

 

Non-relativistic matterEdit

The equation of state of ordinary non-relativistic matter (e.g. cold dust) is  , which means that it is diluted as  , where   is the volume. This means that the energy density red-shifts as the volume, which is natural for ordinary non-relativistic matter.

Ultra-relativistic matterEdit

The equation of state of ultra-relativistic matter (e.g. radiation, but also matter in the very early universe) is   which means that it is diluted as  . In an expanding universe, the energy density decreases more quickly than the volume expansion, because radiation has momentum and, by the de Broglie hypothesis a wavelength, which is red-shifted.

Acceleration of cosmic inflationEdit

Cosmic inflation and the accelerated expansion of the universe can be characterized by the equation of state of dark energy. In the simplest case, the equation of state of the cosmological constant is  . In this case, the above expression for the scale factor is not valid and  , where the constant H is the Hubble parameter. More generally, the expansion of the universe is accelerating for any equation of state  . The accelerated expansion of the Universe was indeed observed.[1] According to observations, the value of equation of state of cosmological constant is near -1.

Hypothetical phantom energy would have an equation of state  , and would cause a Big Rip. Using the existing data, it is still impossible to distinguish between phantom   and non-phantom  .

FluidsEdit

In an expanding universe, fluids with larger equations of state disappear more quickly than those with smaller equations of state. This is the origin of the flatness and monopole problems of the big bang: curvature has   and monopoles have  , so if they were around at the time of the early big bang, they should still be visible today. These problems are solved by cosmic inflation which has  . Measuring the equation of state of dark energy is one of the largest efforts of observational cosmology. By accurately measuring  , it is hoped that the cosmological constant could be distinguished from quintessence which has  .

Scalar modelingEdit

A scalar field   can be viewed as a sort of perfect fluid with equation of state

 

where   is the time-derivative of   and   is the potential energy. A free   scalar field has  , and one with vanishing kinetic energy is equivalent to a cosmological constant:  . Any equation of state in between, but not crossing the   barrier known as the Phantom Divide Line (PDL),[2] is achievable, which makes scalar fields useful models for many phenomena in cosmology.

NotesEdit

  1. ^ Hogan, Jenny. "Welcome to the Dark Side." Nature 448.7151 (2007): 240-245. http://www.nature.com/nature/journal/v448/n7151/full/448240a.html
  2. ^ Vikman, Alexander (2005). "Can dark energy evolve to the Phantom?". Phys. Rev. D. 71: 023515. arXiv:astro-ph/0407107 . Bibcode:2005PhRvD..71b3515V. doi:10.1103/PhysRevD.71.023515.