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The creation of a photon is fundamentally governed by quantum electrodynamics (QED). A photon is emitted when a charged particle, typically an electron, undergoes a quantum transition between discrete energy eigenstates within an atom or molecule. This spontaneous emission process can be described by Fermi’s Golden Rule, where the transition probability per unit time depends on the density of final states and the matrix element of the interaction Hamiltonian.
The photon’s energy is quantized and given by the Planck-Einstein relation:
E = hν = hc/λ
where h is Planck’s constant, ν the frequency, c the speed of light, and λ the wavelength. This quantization is a direct consequence of the boundary conditions imposed by atomic structure and the electromagnetic field’s quantization.
Once created, a photon propagates at c in vacuum, and its worldline is a null geodesic in Minkowski spacetime. Due to its zero invariant mass (m0= 0), the photon’s proper time does not advance; in its own frame, emission and absorption are instantaneous events. The relativistic energy-momentum relation simplifies to:
E2 = (m0c2)2 + (pc)2 =⇒ E = pc
This property underpins the photon’s extraordinary stability: there are no lighter particles for it to decay into, and Lorentz invariance forbids any rest frame for the photon.
Photons are considered fundamentally stable within the Standard Model. The absence of electriccharge, baryon number, and lepton number precludes any decay channel. However, extensions to the Standard Model allow for a hypothetical non zero photon mass, mγ> 0, which would enable decay into lighter particles, such as neutrinos. Observational constraints from the cosmic microwave background (CMB) and laboratory experiments place stringent upper limits on mγ and the photon’s lifetime. For instance, the CMB’s near-perfect blackbody spectrum implies that if photon decay occurs, its lifetime must exceed 1018 years in our frame. This is orders of magnitude longer than the universe’s current age, confirming the practical immortality of photons.
Traditionally, photon detection is destructive—absorption by a detector con- verts the photon’s energy into a measurable signal, annihilating the photon in the process. However, quantum non-demolition (QND) measurements allow the presence of a photon to be inferred without absorption. In such experi- ments, atoms in highly excited Rydberg states traverse a cavity containing a photon. The photon’s electromagnetic field induces a measurable phase shift in the atomic states via the AC Stark effect, leaving the photon undisturbed. This technique enables repeated, non-destructive observation of a single pho- ton’s “lifetime” within a cavity, revealing quantum jumps and the stochastic nature of photon appearance and disappearance.
While photons do not spontaneously decay, they can be annihilated through interactions with matter:
These processes are dictated by conservation laws and the interaction Hamiltonian of QED.
The universe is permeated by photons, from the relic CMB to those emitted by stars and artificial sources. Despite individual photons being absorbed or transformed, the total number of photons remains vast and continually replenished through ongoing physical processes. The CMB itself is a testament to the longevity and stability of photons over cosmological timescales.
A photon’s journey, from quantum emission to potential absorption, encapsu- lates deep principles of quantum mechanics, relativity, and field theory. Its effective immortality arises from the absence of decay channels and its unique status as a massless gauge boson. While individual photons may be absorbed, the persistence of light across the cosmos is a direct consequence of the funda- mental symmetries and conservation laws that govern our universe.