The horizon problem is concerned with the near-equivalence of this property of the CMBR everywhere.
The derivative of this quantity with respect to depth scales with the energy flux in a plane-parallel material in the Rosseland approximation. Cosmologically, this property of photons exceeds this property for neutrinos by a factor of the cube root of eleven-fourths, in part due to electron-positron annihilation. A log-log plot that displays the evolution of this quantity over time exhibits a kink at the transition from a radiation-dominated universe to a matter-dominated one. This property of the CMBR is inversely proportional to the cosmological scale factor. The horizon problem is concerned with the near-equivalence of this property of the CMBR everywhere. One form of this quantity, described by the word "color," is determined by fitting non-normalized data to a Planck's law curve. For 10 points, name this property, to whose fourth power luminosity is proportional, according to the Stefan-Boltzmann law.
The derivative of this quantity with respect to depth scales with the energy flux in a plane-parallel material in the Rosseland approximation.
temperature