Absolute hot is a concept of temperature that postulates the existence of a highest attainable temperature of matter. The concept has been popularized by the television series Nova. In this article, absolute hot is assumed to be the high end of a temperature scale starting at absolute zero, which is the temperature at which entropy is minimal and classical thermal energy is zero.
Contemporary models of physical cosmology postulate that the highest possible temperature is the Planck temperature, which has the value 785(71)×1032 Kelvin. 1.416 Above about 1032K, particle energies become so large that gravitational forces between them would become as strong as other fundamental forces according to current theories. There is no existing scientific theory for the behavior of matter at these energies. A quantum theory of gravity would be required. The models of the origin of the universe based on the Big Bang theory assume that the universe passed through this temperature about 10−42 seconds (one Planck time) after the Big Bang as a result of enormous entropy expansion.
Another theory of absolute hot is based on the Hagedorn temperature, where the thermal energies of the particles exceed the mass-energy of a hadron particle-antiparticle pair. Instead of temperature rising, at the Hagedorn temperature more and heavier particles are produced by pair production, thus preventing effective further heating, given that only hadrons are produced. However, further heating is possible (with pressure) if the matter undergoes a phase change into a quark–gluon plasma. Therefore, this temperature is more akin to a boiling point rather than an insurmountable barrier. For hadrons, the Hagedorn temperature is 2 × 1012 K, which has been reached and exceeded in LHC and RHIC experiments. However, in string theory, a separate Hagedorn temperature can be defined, where strings similarly provide the extra degrees of freedom. However, it is so high (1030 K) that no current or foreseeable experiment can reach it.
Considering only certain degrees of freedom in matter, such as nuclear spins, systems with a negative temperature can be produced. They occur because equipartitioning is too slow to allow communication between the degrees of freedom where thermal energy is stored, such as the vibrational, rotational and nuclear spin states of molecules. These systems are familiar from e.g. lasers. For these, theory predicts a mathematical singularity in temperature. When a spin system is excited with electromagnetic radiation and undergoes population inversion into an excited state, quantum physics formally assumes that its temperature function goes through a singularity. The spin temperature tends to positive infinity, before discontinuously switching to negative infinity. However, this applies only to specific degrees of freedom (the spin temperature in this case) in the system, while others would have normal temperature dependency. Thus, this singularity cannot be observed as ordinary sensible heat. If equipartitioning is possible, the system undergoes relaxation into a thermally uniform state with release of a finite quantity of heat. Before a physical infinite temperature could be reached, realistic ordinary matter would undergo phase transitions, such as evaporation, and never actually reach the infinite temperature.
- International Temperature Scale of 1990
- Negative temperature
- Orders of magnitude (temperature)
- Thermodynamic temperature
- PBS. "Absolute zero." Archived August 5, 2009, at the Wayback Machine. NOVA. Season 33. Ep. 1.
- Absolute Hot. NOVA.
- Tyson, Peter (2007). "Absolute Hot: Is there an opposite to absolute zero?". PBS.org. Archived from the original on 6 August 2009. Retrieved 2009-08-11.
- Hubert Reeves (1991). The Hour of Our Delight. W. H. Freeman Company. p. 117. ISBN 0-7167-2220-8.
The point at which our physical theories run into most serious difficulties is that where matter reaches a temperature of approximately 1032 degrees, also known as Planck's temperature. The extreme density of radiation emitted at this temperature creates a disproportionately intense field of gravity. To go even farther back, a quantum theory of gravity would be necessary, but such a theory has yet to be written.
- Atick, Joseph J.; Witten, Edward. "The Hagedorn transition and the number of degrees of freedom of string theory". Nuclear Physics B. Elsevier. Retrieved 17 February 2014.
- C. Kittel, H. Kroemer (1980). Thermal Physics (2 ed.). W. H. Freeman Company. ISBN 0-7167-1088-9.