In physics, quintessence is a hypothetical form of dark energy, more precisely a scalar field, postulated as an explanation of the observation of an accelerating rate of expansion of the universe. The first example of this scenario was proposed by Ratra and Peebles (1988)^[1] and Wetterich (1988).^[2][3] The concept was expanded to more general types of time-varying dark energy, and the term "quintessence" was first introduced in a 1998 paper by Robert R. Caldwell, Rahul Dave and Paul Steinhardt.^[4] It has been proposed by some physicists to be a fifth fundamental force.^[5][6][7][8] Quintessence differs from the cosmological constant explanation of dark energy in that it is dynamic; that is, it changes over time, unlike the cosmological constant which, by definition, does not change. Quintessence can be either attractive or repulsive depending on the ratio of its kinetic and potential energy. Those working with this postulate believe that quintessence became repulsive about ten billion years ago, about 3.5 billion years after the Big Bang.^[9]

A group of researchers argued in 2021 that observations of the Hubble tension may imply that only quintessence models with a nonzero coupling constant are viable.^[10]

Terminology

The name comes from quinta essentia (fifth element). So called in Latin starting from the Middle Ages, this was the (first) element added by Aristotle to the other four ancient classical elements because he thought it was the essence of the celestial world. Aristotle posited it to be a pure, fine, and primigenial element. Later scholars identified this element with aether. Similarly, modern quintessence would be the fifth known "dynamical, time-dependent, and spatially inhomogeneous" contribution to the overall mass–energy content of the universe.

Of course, the other four components are not the ancient Greek classical elements, but rather "baryons, neutrinos, dark matter, [and] radiation." Although neutrinos are sometimes considered radiation, the term "radiation" in this context is only used to refer to massless photons. Spatial curvature of the cosmos (which has not been detected) is excluded because it is non-dynamical and homogeneous; the cosmological constant would not be considered a fifth component in this sense, because it is non-dynamical, homogeneous, and time-independent.^[4]

Scalar field

Quintessence (Q) is a scalar field with an equation of state where w_q, the ratio of pressure p_q and density ${\displaystyle \rho }$_q, is given by the potential energy ${\displaystyle V(Q)}$ and a kinetic term:

${\displaystyle w_{q}={\frac {p_{q}}{\rho _{q}}}={\frac {{\frac {1}{2}}{\dot {Q}}^{2}-V(Q)}{{\frac {1}{2}}{\dot {Q}}^{2}+V(Q)}}}$

Hence, quintessence is dynamic, and generally has a density and w_q parameter that varies with time. By contrast, a cosmological constant is static, with a fixed energy density and w_q = −1.

Tracker behavior

Many models of quintessence have a tracker behavior, which according to Ratra and Peebles (1988) and Paul Steinhardt et al. (1999) partly solves the cosmological constant problem.^[11] In these models, the quintessence field has a density which closely tracks (but is less than) the radiation density until matter-radiation equality, which triggers quintessence to start having characteristics similar to dark energy, eventually dominating the universe. This naturally sets the low scale of the dark energy.^[12] When comparing the predicted expansion rate of the universe as given by the tracker solutions with cosmological data, a main feature of tracker solutions is that one needs four parameters to properly describe the behavior of their equation of state,^[13][14] whereas it has been shown that at most a two-parameter model can optimally be constrained by mid-term future data (horizon 2015–2020).^[15]

Specific models

Some special cases of quintessence are phantom energy, in which w_q < −1,^[16] and k-essence (short for kinetic quintessence), which has a non-standard form of kinetic energy. If this type of energy were to exist, it would cause a big rip^[17] in the universe due to the growing energy density of dark energy, which would cause the expansion of the universe to increase at a faster-than-exponential rate.

Quintom scenario

In 2004, when scientists fitted the evolution of dark energy with the cosmological data, they found that the equation of state had possibly crossed the cosmological constant boundary (w = –1) from above to below. A proven no-go theorem indicates this situation, called the Quintom scenario, requires at least two degrees of freedom for dark energy models involving ideal gases or scalar fields.^[21]

See also

• Aether (classical element)

References

Further reading

• Christof, Wetterich (1987-09-24). "Cosmology and the fate of dilatation symmetry". Nuclear Physics B. 302 (4): 668–696. arXiv:1711.03844. Bibcode:1988NuPhB.302..668W. doi:10.1016/0550-3213(88)90193-9. S2CID 118970077.
• Ostriker, J. P.; Steinhardt, P. (January 2001). "The Quintessential Universe". Scientific American. 284 (1): 46–53. Bibcode:2001SciAm.284a..46O. doi:10.1038/scientificamerican0101-46. PMID 11132422.
• Krauss, Lawrence M. (2000). Quintessence: The Search for Missing Mass in the Universe. Basic Books. ISBN 978-0465037414.