In astroparticle physics, an Urca process is a reaction which emits a neutrino and which is assumed to take part in cooling processes in neutron stars and white dwarfs. The process was first discussed by George Gamow and Mário Schenberg while they were visiting a casino named Cassino da Urca in Rio de Janeiro. Schenberg is reported to have said to Gamow that "the energy disappears in the nucleus of the supernova as quickly as the money disappeared at that roulette table". In Gamow's South Russian dialect, urca (Russian: урка) can also mean a robber or gangster.
The direct Urca processes are the simplest neutrino-emitting processes and are thought to be central in the cooling of neutron stars. They have the general form
1 and B
2 are baryons,
is a lepton, and
l) are (anti-)neutrinos. The baryons can be nucleons (free or bound), hyperons like
, or members of the
isobar. The lepton is either an electron or a muon.
The Urca process is especially important in the cooling of white dwarfs, where a lepton (usually an electron) is absorbed by the nucleus of an ion and then convectively carried away from the core of a star. Then, a beta decay occurs. Convection then carries the element back into the interior of the star, and the cycle repeats many times. Because the neutrinos emitted during this process are unlikely to be reabsorbed, this is effectively a cooling mechanism for white dwarfs.
The process can also be essential in the cooling of neutron stars. If a neutron star contains a central core in which the direct Urca-process is operative, the cooling timescale shortens by many orders of magnitude.
- D. Darling. "Urca process". The Internet Encyclopedia of Science. Retrieved 2010-03-02.
- D. K. Nadyozhin (1995). "Gamow and the physics and evolution of stars". Space Science Reviews. 74 (3–4): 455–461. Bibcode: . doi:10.1007/BF00751432.
- M. Brueggen; A. Kercek (10 January 2000). "The convective URCA process in white dwarfs". Max Planck Institute. Retrieved 2010-02-05.
- P. Haensel (1995). "Urca processes in dense matter and neutron star cooling". Space Science Reviews. 74 (3–4): 427–436. Bibcode: . doi:10.1007/BF00751429.