Quintessence field equation of state

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SUMMARY

The discussion centers on the equation of state parameter w for quintessence fields, specifically those with the potential m²Phi². It concludes that w is not constrained between 0 and 1/3 due to the treatment of scalar fields as classical rather than quantum entities. This distinction arises because scalar fields, particularly in the context of inflation, are understood as pure classical fields, which diverges from the treatment of matter and radiation fields. The conversation also touches on the implications of low mass and large wavelength in the context of fuzzy dark matter, although this reasoning is not directly applied to inflation fields.

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  • Understanding of quintessence fields in cosmology
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fhenryco
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TL;DR
Quintessence field equation of state
Why the equation of state parameter w for a quintessence field with potential m²Phi² is not in between 0 and 1/3 depending on the energy of its particles relative to the mass of the field instead of the w resulting from formula 9 of https://arxiv.org/pdf/1504.04037.pdf which seems to be assuming that the field is classical ? !

In other words why is the scalar field treated differently than usual matter and radiation field when we want to compute it's w ?
 
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Because it is a classical scalar field, not a collection of particles.
 
It's also what i suspected but i wanted confirmation because i did not realize before that the scalar fields used for instance in inflation are understood as pure classical fields: i believed that in modern physics everything was always quantum and that nobody would accept a field which is not a quantum field !
 
fhenryco said:
It's also what i suspected but i wanted confirmation because i did not realize before that the scalar fields used for instance in inflation are understood as pure classical fields: i believed that in modern physics everything was always quantum and that nobody would accept a field which is not a quantum field !
Another possibility i was thinking about is that they treat it like a classical field because of it's extremely low mass (extremely large wavelength) ... this is what they do for fuzzy dark matter ... but i found nowhere the same argument for inflation fields
 

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