Linelist of HD16O for study of atmosphere of terrestrial planets (Earth, Venus and Mars)
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B. A. Voronin | Anna Fedorova | A. D. Bykov | Olga V. Naumenko | N. N. Lavrentieva | A. Fedorova | O. Naumenko | N. Lavrentieva | A. Bykov | B. Voronin
[1] J. Tennyson,et al. Intracavity laser absorption spectroscopy of HDO between 12145 and 13160 cm 1 , 2007 .
[2] P. Bernath,et al. IUPAC Critical Evaluation of the Rotational-Vibrational Spectra of Water Vapor. Part II. Energy Levels and Transition Wavenumbers for HD16O, HD17O, and HD18O , 2010 .
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[13] J. Lamouroux,et al. Half-widths, their temperature dependence, and line shifts for the HDO–CO2 collision system for applications to CO2-rich planetary atmospheres , 2011 .
[14] Robert R. Gamache,et al. CO2-broadening of water-vapor lines , 1995 .
[15] R. Wilson,et al. Investigation of the nature and stability of the Martian seasonal water cycle with a general circulation model , 2002 .
[16] R. Tolchenov,et al. A high accuracy computed line list for the HDO molecule , 2010 .
[17] I. L. Barnes,et al. Isotopic abundances and atomic weights of the elements , 1984 .
[18] J. Tennyson,et al. Line lists for H218O and H217O based on empirical line positions and ab initio intensities , 2012 .
[19] N. Lavrentieva. Rotational dependence of the broadening of lines of the ν2 band of H2O induced by nitrogen pressure , 2004 .
[20] Ronald K. Hanson,et al. Temperature-Dependent Collision-Broadening Parameters of H2O Lines in the 1.4-μm Region Using Diode Laser Absorption Spectroscopy , 1994 .
[21] P. Bernath,et al. IUPAC critical evaluation of the rotational–vibrational spectra of water vapor. Part I—Energy levels and transition wavenumbers for H217O and H218O , 2009 .
[22] Anna Fedorova,et al. The 1.10- and 1.18-μm nightside windows of Venus observed by SPICAV-IR aboard Venus Express , 2011 .
[23] Robert R. Gamache,et al. CO2-broadened water in the pure rotation and ν2 fundamental regions , 2007 .
[24] R. Tolchenov,et al. Potential energy surface of HDO up to 25,000 cm-1. , 2008, The Journal of chemical physics.
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[26] P. Anderson. Pressure Broadening in the Microwave and Infra-Red Regions , 1949 .
[27] F. Forget,et al. Modeling the annual cycle of HDO in the Martian atmosphere , 2005 .
[28] Laurence S. Rothman,et al. Einstein A-coefficients and statistical weights for molecular absorption transitions in the HITRAN database , 2006 .
[29] A. D. Jong,et al. Wide-band simultaneous observations of pulsars: disentangling dispersion measure and profile variations , 2012, Astronomy & Astrophysics.
[30] Jonathan Tennyson,et al. DVR3D: a program suite for the calculation of rotation-vibration spectra of triatomic molecules , 2004, Comput. Phys. Commun..
[31] Harry Partridge,et al. The determination of an accurate isotope dependent potential energy surface for water from extensive ab initio calculations and experimental data , 1997 .
[32] R. Tolchenov,et al. Shift of the centers of H2O absorption lines in the region of 1.06 μm , 2008 .
[33] J. Hartmann,et al. Calculated tabulations of H(2)O line broadening by H(2)O, N(2), O(2), and CO(2) at high temperature. , 1989, Applied optics.
[34] Deuterated water: partition functions and equilibrium constants , 2005 .
[35] O. Naumenko,et al. CW-Cavity Ring Down Spectroscopy of deuterated water in the 1.58 μm atmospheric transparency window , 2014 .
[36] V. Krasnopolsky. Spatially-resolved high-resolution spectroscopy of Venus 2. Variations of HDO, OCS, and SO2 at the cloud tops , 2010 .
[37] N. Lavrentieva,et al. Nitrogen and oxygen broadening of ozone infrared lines in the 5µm region: theoretical predictions by semiclassical and semiempirical methods , 2009 .
[38] Eric Villard,et al. HDO and H2O vertical distributions and isotopic ratio in the Venus mesosphere by Solar Occultation at Infrared spectrometer on board Venus Express , 2008 .
[39] Yu. N. Ponomarev,et al. Pressure broadening and shift coefficients of H2O due to perturbation by N2, O2, H2 and He in the 1.39 μm region: experiment and calculations , 2004 .
[40] A. Watson,et al. Venus Was Wet: A Measurement of the Ratio of Deuterium to Hydrogen , 1982, Science.
[41] V. Krasnopolsky,et al. Oxygen and carbon isotope ratios in the martian atmosphere , 2007 .
[42] J. Tennyson,et al. A high-accuracy computed water line list , 2006, astro-ph/0601236.
[43] Adrian A. Borsa,et al. Modeling the topography of the salar de Uyuni, Bolivia, as an equipotential surface of Earth's gravity field , 2008 .
[44] V. I. Starikov,et al. Self- and air-broadening coefficients of HD16O spectral lines , 2012 .
[45] Laurence S. Rothman,et al. Observations of D/H ratios in H2O, HCl, and HF on Venus and new DCl and DF line strengths☆ , 2013 .
[46] Thomas Widemann,et al. HDO and SO2 thermal mapping on Venus: evidence for strong SO2 variability , 2012 .
[47] V. Krasnopolsky,et al. A photochemical model for the Venus atmosphere at 47–112 km , 2011 .
[48] G. Villanueva,et al. Measurement of the Isotopic Signatures of Water on Mars: Implications for Studying Methane , 2011 .
[49] A. Titov,et al. Near infrared diode laser spectroscopy of C2H2, H2O, CO2 and their isotopologues and the application to TDLAS, a tunable diode laser spectrometer for the martian PHOBOS-GRUNT space mission , 2010 .
[50] A. D. Bykov,et al. Semi-empiric approach to the calculation of H2O and CO2 line broadening and shifting , 2004 .
[51] Gordon L. Bjoraker,et al. High‐resolution spectroscopy of Mars at 3.7 and 8 μm: A sensitive search for H2O2, H2CO, HCl, and CH4, and detection of HDO , 1997 .
[52] Gang Li,et al. The HITRAN 2008 molecular spectroscopic database , 2005 .
[53] Pascal Rannou,et al. Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model , 2004 .
[54] P. Bernath,et al. IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part I—Energy levels and transition wavenumbers , 2013 .
[55] T. Y. Chesnokova,et al. Estimate of the J′J″ dependence of water vapor line broadening parameters , 2010 .