The Universe's Horizon as a Heat Engine express

Original: "Apparent horizon thermodynamics in an exponential $$f(Q)$$ gravity model"
· A. Oliveros, Ivan R. Vasquez
arXiv:2608.08302v1 · 2026-08-08 · CC BY 4.0 · 2 min
The cosmic horizon we cannot see beyond behaves like a heated object, and its heat imposes constraints on the workings of gravity.

Stare long enough into the night sky, and sooner or later your gaze hits a blackness beyond which nothing is visible. This is not just a distant fence: it is the edge of the universe accessible to us, the cosmic horizon. Light from more distant stars simply hasn't had time to reach us. Surprisingly, this invisible boundary behaves almost like a heated skillet: it has a temperature, and it obeys the laws of heat.

The authors of the new study took one of the modified theories of gravity — one where the force of attraction changes slightly over enormous distances due to an additional term in the equations, resembling an exponential (a rapidly decaying curve). In this theory, the horizon also has a temperature and a reservoir of thermal disorder — entropy. But the formula for entropy is no longer just a quarter of the horizon's area, as in textbook black holes, but includes a small addition that depends on the parameter of expansion of the universe. When this parameter is set to zero, everything returns to the good old formula discovered by Bekenstein and Hawking.

The temperature of the Hubble horizon today is about a billion billion times lower than room temperature — around 10⁻³⁰ Kelvin. To boil a kettle on it, you'd have to wait longer than the universe has existed.

The physicists went further and checked whether the generalized second law of thermodynamics is violated — the rule that the total entropy of the horizon and everything inside it should not decrease. It turns out that for the parameters that best fit observations of distant supernovae and the distribution of galaxies, the law holds across the entire range of redshifts, from the early universe to the present day. But if you artificially increase the deviation parameter from the standard model, to about 0.26, then in the future, at negative redshifts, the horizon would start losing entropy faster than matter gains it. That's like a cup of hot coffee that suddenly heats itself up in a cool room — for the horizon, such a thing is forbidden.

Redshift is the stretching of light on its way to us: the farther a galaxy, the more its light 'reddens.' A negative redshift would mean we are looking into the future when the universe contracts, but in our reality, that is not expected.

Thus, the thermal properties of the invisible boundary help weed out unsuitable variants of gravity. The horizon, like a sensitive thermometer, shows which additions to Einstein's theory are still permissible and which make the universe 'catch a cold.'

If the cosmic horizon radiated in the visible range, its light would be billions of times fainter than the dimmest nightlight, but theoretically, it emits particles like a black hole.

In Peter Watts' novel 'Blindsight', the cosmic horizon plays the role of a barrier behind which incomprehensible forms of intelligence hide, and the very idea of the horizon as a source of radiation echoes Hawking evaporation of black holes.

S = \frac{A}{4} + \text{поправки порядка } b
The entropy S of the horizon equals one quarter of its area A plus small corrections depending on the parameter b, which describes the deviation from standard cosmology.
f_Q + 2Q f_{QQ} \geq 0
Condition for the generalized second law of thermodynamics: the combination of derivatives of the function f(Q) with respect to the parameter Q must be non-negative.
Scientists
Ludwig BoltzmannRudolf ClausiusJacob BekensteinStephen HawkingChristian DopplerWilhelm Wien
Concepts
horizon area apparent horizon hawking area law Hubble's law equivalence principle general relativity hubble constant surface gravity wald entropy black hole thermodynamics cosmological homogeneity fq gravity equipartition theorem cosmological parameters entropic shadow gravitational constant Einstein field equations Friedmann equations cosmic horizon First law of black hole mechanics