The radiative transition probabilities in hydrogen have been calculated for all Stark transitions through $n=25$ . In general, the total transition probability and lifetime of a particular state are a function of the parabolic quantum numbers ${n}_{1}$ , ${n}_{2}$ , and $m$ . For $m>0$ and to within an error of the order of one percent the radiative lifetimes are functions only of $n$ , $m$ . The radiative lifetimes are presented graphically for all states from $n=2$ through $n=25$ .The radiative transition probabilities in hydrogen have been calculated for all Stark transitions through $n=25$. In general, the total transition probability and lifetime of a particular state are a function of the parabolic quantum numbers ${n}_{1}$, ${n}_{2}$, and $m$. For $m>0$ and to within an error of the order of one percent the radiative lifetimes are functions only of $n$, $m$. The radiative lifetimes are presented graphically for all states from $n=2$ through $n=25$.

Physical ReviewJan 20, 196449 citations

Radiative Transitions

James H Scofield

Elsevier eBooksJan 1, 197534 citations

Radiative Transitions

Richard C. Powell

Springer eBooksJan 1, 19980 citations

The radiative transition probabilities in hydrogen have been calculated for all Stark transitions through

n=25

. In general, the total transition probability and lifetime of a particular state are a function of the parabolic quantum numbers

{n}_{1}

{n}_{2}

, and

m

. For

m>0

and to within an error of the order of one percent the radiative lifetimes are functions only of

n

m

. The radiative lifetimes are presented graphically for all states from

n=2

through

n=25