# Quantum Transitions

## Quantum Transitions

discontinuous transitions of a quantum system (an atom, a molecule, an atomic nucleus, a solid) from one state to another. The most important are quantum transitions between stationary states that correspond to different energies of the quantum system—the quantum transitions of a system from one energy level to another. During a transition from a higher energy level ε* _{k}* to a lower level the system releases the energy ε

_{k}–ε

_{i}and during the reverse transition, absorbs it (see Figure 1).

Quantum transitions may be radiative or nonradiative. In radiative transitions the system emits (the transition ε_{k} ε_{i}) or absorbs (the transition ε_{i} → ε_{k}) a quantum of electromagnetic radiation—the photon—of energy *hv* (*v* is the frequency of radiation and ℏ is the Planck constant), which satisfies the fundamental relation

(which is the law of conservation of energy for such a transition). Depending on the energy difference between the states of the system in which the quantum transitions take place, photons of radio-frequency, infrared, visible, ultraviolet, and gamma radiation and X-radiation are emitted or absorbed. The aggregate of radiative quantum transitions from lower energy levels to higher ones forms the absorption spectrum of a given quantum system, while the aggregate of the reverse transitions forms its emission spectrum.

In nonradiative quantum transitions, the system acquires or releases energy on interaction with other systems. For example, on colliding with each other and with electrons, the atoms or molecules of a gas may gain energy (be excited) or lose it.

The transition probability, which defines how often a given quantum transition occurs, is the most important characteristic of any quantum transition. It is measured by the number of transitions of a given type in the quantum system under consideration per unit time (1 sec). Therefore, it may assume any values from 0 to ∞ (in contrast to the probability of a single event, which cannot exceed 1). Transition probabilities are calculated by the methods of quantum mechanics.

Quantum transitions in atoms and molecules will be examined below.

** Radiative transitions**. Radiative quantum transitions may be spontaneous, independent of external influences on the quantum system (the spontaneous emission of a photon), or stimulated, induced by the action of external electromagnetic radiation of a resonance [satisfying relation (1)] frequency

*v*(absorption and stimulated emission of photons). Insofar as spontaneous emission is possible, a quantum system remains at an excited energy level ε

_{k}for some finite time, and then jumps to some lower level. The mean time period τ

_{k}that the system remains at the excited level ε

*is called the lifetime of the energy level. The smaller the τ*

_{k}_{k}, the greater the probability of the system’s transition to a state of lower energy. The quantity

*A*= 1/τ

_{k}^{2}, which defines the average number of photons emitted by a single particle (an atom or molecule) per second (τ

*is expressed in seconds) is called the probability of spontaneous emission from the level ε*

_{k}*. For the simplest case of spontaneous transition from the first excited level ε*

_{k}_{2}to the ground level ε

_{1}the quantity

*A*

_{2}= 1/τ

_{2}defines the probability of this transition; it may be designated

*A*

_{21}. Quantum transitions to various lower levels are possible from excited higher levels (see Figure 1). The total number

*A*

_{k}of photons emitted on the average by one particle with an energy ε

_{k}per second is equal to the total number

*A*

_{ki}of photons emitted upon the individual transitions:

that is, the total probability *A _{k}* of spontaneous emission from the level ε

*is equal to the sum of the probabilities*

_{k}*A*of the individual spontaneous transitions ε

_{ki}*→ε*

_{k}*i*, the quantity

*A*is called Einstein’s coefficient of spontaneous emission upon such a transition. For the hydrogen atom,

_{ki}*A*≈ (10

_{ki}^{7}-10

^{8}) sec

^{-1}.

For induced quantum transitions the number of transitions is proportional to the radiation density p_{v} of the frequency *v* = (ε* _{k}* — ε

_{i})/

*h*that is, to the energy of photons of frequency

*v*per 1 cm

^{3}. The probabilities of absorption and stimulated emission are characterized by Einstein’s coefficients

*B*and

_{ik}*B*, respectively, which are equal to the number of photons absorbed and stimulated to emission on the average by one particle per second at a radiation density equal to 1. The products

_{ki}*B*p

_{ik}*and*

_{v}*B*define the probabilities of stimulated absorption and emission on exposure to external electromagnetic radiation of density p

_{ki}p_{v}_{v}, and, like

*A*are expressed in sec

_{ki}^{-1}.

The coefficients *A _{ki}*,

*B*, and

_{ik}*B*are interconnected by the following relations, which were first derived by Einstein and have been rigorously substantiated in quantum electrodynamics:

_{ki}where g_{i}(g* _{k}*) is the degeneration multiplicity of the level ε

_{i}, (ε

_{k}), that is, the number of different states of the system that have the same energy ε

_{i}, (or ε

*) and*

_{k}*c*is the velocity of light. For transitions between nondegenerate levels (

*g*, =

_{i}*g*= 1),

_{k}*B*= B

_{ki}*, that is, the probabilities of induced quantum transitions—direct and reverse—are identical. If one of the Einstein coefficients is known, then the others can be determined from relations (3) and (4).*

_{ik}The probabilities of radiative transitions are different for different transitions and depend on the properties of the energy levels ε* _{i}*, and ε

*between which the transition takes place. The more strongly the electric and magnetic properties of the quantum system that are characterized by its electric and magnetic moments change upon transition, the greater the probabilities of quantum transitions. The possibility of radiative quantum transitions between the energy levels ε*

_{k}*, and ε*

_{i}*with assigned characteristics is defined by the selection rules. (For greater detail,*

_{k}*see*RADIATION, ELECTROMAGNETIC.)

** Nonradiative transitions**. Nonradiative quantum transitions are also characterized by the probabilities of the corresponding transitions C

*and*

_{ki}*C*—the average number of processes of release and acquisition of energy ε

_{ik}*— ε*

_{k}*, per 1 sec, calculated for one particle with an energy ε*

_{i}*(for the energy release process) or an energy ε, (for the energy acquisition process). If both radiative and nonradiative quantum transitions are possible, then the total transition probability is equal to the sum of the transition probabilities of both types.*

_{k}It is essential to take into account nonradiative quantum transitions when the transition probability is of the same order or greater than the corresponding quantum transition involving radiation. For example, if spontaneous radiative transition to the ground level ε_{1} from the first excited state ε_{2} is possible with a probability *A*_{21} and nonradiative transition to the same level is possible with a probability *C*_{21} then the total transition probability will be equal to *A*_{21} + *C*_{2} the energy level lifetime is equal to τ’_{2} = 1/(*A*_{21} + *C*_{21}) instead of τ_{2} = 1/*A*_{2} in the absence of a nonradiative transition. Thus, the energy level lifetime decreases because of nonradiative quantum transitions. When *C*_{21}≫*A*_{21}, the time τ_{2}’ is very small in comparison with τ_{2}, and the majority of particles will lose their excitation energy ε_{2} — ε_{1} in nonradiative processes—the quenching of spontaneous emissions will take place.

M. IA. EL’IASHEVICH