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Picosecond pulse amplification in isotopic CO2 active medium

Mikhail N. Polyanskiy, Igor V. Pogorelsky, and Vitaly Yakimenko

Open Access Open Access

Abstract

Using a high-pressure carbon-dioxide laser amplifier enriched with the oxygen-18 isotope, we produced a 5-ps, 10-µm pulse of the 1 TW peak power without splitting, which otherwise occurs due to spectral modulation by the rotation structure of the CO2 amplification band.

©2011 Optical Society of America

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Figures (5)
Fig. 1
Fig. 1 Simulated gain spectra at10 bar for three CO2 isotopologues with different combinations of oxygen-16 and oxygen-18 atoms: 16O-12C-16O (626), 16O-12C-18O (628) and 18O-12C-18O (828) and a combined spectrum of their mixture in the statistically equilibrium proportion 1:2:1 (MIX). The arrow shows the 10R branch used in our laser.

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Fig. 2
Fig. 2 5-ps (FWHM) pulse splitting upon 106× amplification in a 10 bar CO2 laser amplifier. a) normalized gain profile and pulse spectra; b) pulse temporal structure (power vs. time).

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Fig. 3
Fig. 3 Layout and pulse dynamics in the CO2 laser system. PS: polarizing splitter.

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Fig. 4
Fig. 4 5-ps (FWHM) pulse amplification in a natural- (top) and isotopically enriched- (bottom) CO2 laser gas mixture. Inserts in the time structure graphs show raw streak-camera images. The simulation curves are identical to those in the Fig. 2 (106× net amplification).

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Fig. 5
Fig. 5 Simulation results for a 5-ps (FWHM) pulse amplification in the final amplifier.

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Tables (1)

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Table 1 Laser amplifier’s parameters

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Equations (6)

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Δ ν ˜ p r e s s u r e = 0.1149 P C O 2 + 0.0794 P N 2 + 0.0598 P H e [8]
Ω [ s -1 ] = d [ C ⋅ m ] E [ V ⋅ m -1 ] h [ J ⋅ s ] ,
E [ V ⋅ m -1 ] = 2 I [ W ⋅ m -2 ] ε 0 [ F ⋅ m -1 ] c [ m ⋅ s -1 ] ,
Δ ν ˜ p o w e r [ cm -1 ] = Ω [ s -1 ] c [ cm ⋅ s -1 ] = 4 .609 × 10 − 4 d [ D ] I [ W ⋅ cm -2 ] .
G s e q / G r e g = 2 exp ( − h ν 3 / k T 3 ) ,
∂ E ∂ z = − 2 π i ω 0 c n ˜ ∑ j P j , ∂ P j ∂ t = − ( i ( ω 0 2 − Ω j 2 ) 2 ω 0 + 1 T 2 ) P j + i Ω j d j 2 ω 0 ℏ n j E , ∂ n ∂ t = Im ( E P j * ) ℏ − n j − ρ j N T R ,
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