By G. Matthewson
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Extra resources for Constructing an astronomical telescope
2) where Qˆ is the quasienergy operator, is the quasienergy, lˆz is the z-component of the orbital angular momentum, and Á = +1(−1) corresponds to the left (right) circularly polarized light. Similar to the Floquet Hamiltonian Hˆ F in the linearly polarized case, the quasienergy operator Qˆ has no discrete ˆ −1 are located near the real axis but on higher spectrum. The complex poles of the resolvent (E − Q) Riemann sheet. 4) can be solved by either L basis set expansion or generalized pseudospectral discretization technique.
15) 9t 2 where (r; t) is the quasienergy wave function in the length gauge; U (r) is the atomic potential; F and ! are, respectively, the laser ÿeld strength and frequency (linear polarization of the laser ÿeld is assumed in Eq. 15)). Following the Floquet theorem, the wave function (r; t) can be represented as (r; t) = exp(−i t) (r; t) ; being the quasienergy. 16) m In the F → 0 limit, the Fourier component m = 0 corresponds to the unperturbed wave function. A. Telnov / Physics Reports 390 (2004) 1 – 131 41 The detachment is possible only if Re En ¿ UP ; from this inequality one can extract nmin —the minimal number of photons required for detachment.
15. Comparison of the intensity-averaged photodetachment rates for the case Ilab =4 GW=cm2 : black circles, theoretical simulation, open circles, experimental data (adapted from Ref. ). 1. 15) 9t 2 where (r; t) is the quasienergy wave function in the length gauge; U (r) is the atomic potential; F and ! are, respectively, the laser ÿeld strength and frequency (linear polarization of the laser ÿeld is assumed in Eq. 15)). Following the Floquet theorem, the wave function (r; t) can be represented as (r; t) = exp(−i t) (r; t) ; being the quasienergy.
Constructing an astronomical telescope by G. Matthewson