Abstract
A Sturmian theory of three-body recombination is presented which provides a unified treatment of bound states, quasibound states, and continuum states. The Sturmian representation provides a numerical quadrature of the two-body continuum which may be used to generate a complete set of states within any desired three-body recombination pathway. Consequently, the dynamical calculation may be conveniently formulated using the simplest energy transfer mechanism, even for reactive systems which allow substantial rearrangement. The Sturmian theory generalizes the quantum kinetic theory of Snider and Lowry to include metastable states which are formed as independent species. Steady-state rate constants are expressed in terms of a pathway-independent part plus a nonequilibrium correction which depends on tunneling lifetimes and pressure. Numerical results are presented for H2 recombination due to collisions with H and He using quantum-mechanical coupled states and infinite-order sudden approximations. These results may be used to remove some of the uncertainties that have limited astrophysical simulations of primordial star formation.
| Original language | English (US) |
|---|---|
| Article number | 052709 |
| Journal | Physical Review A - Atomic, Molecular, and Optical Physics |
| Volume | 88 |
| Issue number | 5 |
| DOIs | |
| State | Published - Nov 25 2013 |
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All Science Journal Classification (ASJC) codes
- Atomic and Molecular Physics, and Optics
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Sturmian theory of three-body recombination : Application to the formation of H2 in primordial gas. / Forrey, Robert C.
In: Physical Review A - Atomic, Molecular, and Optical Physics, Vol. 88, No. 5, 052709, 25.11.2013.Research output: Contribution to journal › Article
TY - JOUR
T1 - Sturmian theory of three-body recombination
T2 - Application to the formation of H2 in primordial gas
AU - Forrey, Robert C.
PY - 2013/11/25
Y1 - 2013/11/25
N2 - A Sturmian theory of three-body recombination is presented which provides a unified treatment of bound states, quasibound states, and continuum states. The Sturmian representation provides a numerical quadrature of the two-body continuum which may be used to generate a complete set of states within any desired three-body recombination pathway. Consequently, the dynamical calculation may be conveniently formulated using the simplest energy transfer mechanism, even for reactive systems which allow substantial rearrangement. The Sturmian theory generalizes the quantum kinetic theory of Snider and Lowry to include metastable states which are formed as independent species. Steady-state rate constants are expressed in terms of a pathway-independent part plus a nonequilibrium correction which depends on tunneling lifetimes and pressure. Numerical results are presented for H2 recombination due to collisions with H and He using quantum-mechanical coupled states and infinite-order sudden approximations. These results may be used to remove some of the uncertainties that have limited astrophysical simulations of primordial star formation.
AB - A Sturmian theory of three-body recombination is presented which provides a unified treatment of bound states, quasibound states, and continuum states. The Sturmian representation provides a numerical quadrature of the two-body continuum which may be used to generate a complete set of states within any desired three-body recombination pathway. Consequently, the dynamical calculation may be conveniently formulated using the simplest energy transfer mechanism, even for reactive systems which allow substantial rearrangement. The Sturmian theory generalizes the quantum kinetic theory of Snider and Lowry to include metastable states which are formed as independent species. Steady-state rate constants are expressed in terms of a pathway-independent part plus a nonequilibrium correction which depends on tunneling lifetimes and pressure. Numerical results are presented for H2 recombination due to collisions with H and He using quantum-mechanical coupled states and infinite-order sudden approximations. These results may be used to remove some of the uncertainties that have limited astrophysical simulations of primordial star formation.
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U2 - 10.1103/PhysRevA.88.052709
DO - 10.1103/PhysRevA.88.052709
M3 - Article
AN - SCOPUS:84890380480
VL - 88
JO - Physical Review A
JF - Physical Review A
SN - 2469-9926
IS - 5
M1 - 052709
ER -