000			02294nab a2200337 c 4500
001			vtls000540016
003			RU-ToGU
005			20210922130930.0
007			cr |
008			181202|2015 ru s a eng d
024	7		_a10.1134/S0030400X15010178 _2doi
035			_ato000540016
040			_aRU-ToGU _brus _cRU-ToGU
100	1		_aLavrentieva, Nina N. _995839
245	1	0	_aH216O line list for the study of atmospheres of Venus and Mars _cN. N. Lavrentieva, B. A. Voronin, A. A. Fedorova
504			_aБиблиогр.: 31 назв.
520	3		_aIR spectroscopy is an important method of remote measurement of H216O content in planetary atmospheres with initial spectroscopic information from the HITRAN, GEISA, etc., databases adapted for studies in the Earth’s atmosphere. Unlike the Earth, the atmospheres of Mars and Venus mainly consist of carbon dioxide with a CO2 content of about 95%. In this paper, the line list of H216O is obtained on the basis of the BT2 line list (R.J. Barber, J. Tennyson, G.J. Harris, et al., Mon. Not. R. Astron. Soc. 368, 1087 (2006)). The BT2 line list containing information on the centers, intensities, and quantum identification of lines is supplemented with the line contour parameters: the self-broadening and carbon dioxide broadening coefficients and the temperature dependence coefficient at 296 K in the range of 0.001–30000 cm−1. Transitions with intensity values 10−30, 10−32, and 10−35 cm/molecule, the total number of which is 323310, 753529, and 2011072, respectively, were chosen from the BT2 line list.
653			_aМарс, планета
653			_aВенера, планета
653			_aатмосфера
653			_aспектроскопия
653			_aводяной пар
655		4	_aстатьи в журналах _9745982
700	1		_aVoronin, Boris A. _cфизик _995840
700	1		_aFedorova, Anna A. _9409558
773	0		_tOptics and spectroscopy _d2015 _gVol. 118, № 1. P. 11-18 _x0030-400X
852	4		_aRU-ToGU
856	7		_uhttp://vital.lib.tsu.ru/vital/access/manager/Repository/vtls:000540016
908			_aстатья
999			_c526153