OSU Navigation Bar

The Ohio State University University Libraries Knowledge Bank

The Knowledge Bank is scheduled for regular maintenance on Sunday, April 20th, 8:00 am to 12:00 pm EDT. During this time users will not be able to register, login, or submit content.

FAR LINE WINGS STUDY OF THE $15 \mu m CO_{2}$ BAND: LABORATORY AND ATMOSPHERIC SPECTRA

Please use this identifier to cite or link to this item: http://hdl.handle.net/1811/20807

Show full item record

Files Size Format View
2003-MG-08.jpg 293.6Kb JPEG image Thumbnail of FAR LINE WINGS STUDY OF THE $15 \mu m CO_{2}$ BAND: LABORATORY AND ATMOSPHERIC SPECTRA

Title: FAR LINE WINGS STUDY OF THE $15 \mu m CO_{2}$ BAND: LABORATORY AND ATMOSPHERIC SPECTRA
Creators: Niro, C. F.; Hartmann, J.- M.; Boulet, C.; Hase, F.
Issue Date: 2003
Abstract: While a number of studies have been devoted to the analysis of the far wings of the $\nu_{3}$ band lines of $CO_{2}$ near $4 \mu m$ those of the $\nu_{2}$ band have never been investigated although precise modeling of absorption in the $10-15 \mu m$ region is essential due to its importance for atmospheric sounding. Starting from the successful results obtained in the modeling of Q branch line $mixing,^{a}$ the ECS (Energy Corrected Sudden) approach is extended in order to predict all line-mixing between P, Q, and R lines. The relaxation matrix is then constructed without use of any adjustable parameter for all $CO_{2}$ bands and with proper accounting of the coupling of angular momenta and of the symmetry of the vibrational transition. High pressure laboratory spectra have been recorded in the $600-1200 cm^{-1}$ region for temperature condition spanning the typical atmospheric range $(200-300 K)$. Comparisons with calculated values demonstrate the quality of the model which gives much better results than purely Lorentzian profiles. This result is confirmed when comparisons are made in the $4 \mu m$ region of the $\nu_{3}$ band wings. A compilation of first order coefficients derived from the relaxation matrix has then been used to compute atmospheric spectra. The comparison of calculated values with high-resolution ground based solar occultation spectra gives a further validation of our approach.
URI: http://hdl.handle.net/1811/20807
Other Identifiers: 2003-MG-08
Bookmark and Share