CIA.bib


@article{ 12RiGoRo.CIA,
Author = {Richard, C. and Gordon, I. E. and Rothman, L. S. and Abel, M. and
   Frommhold, L. and Gustafsson, M. and Hartmann, J. -M. and Hermans, C.
   and Lafferty, W. J. and Orton, G. S. and Smith, K. M. and Tran, H.},
Title = {{New section of the HITRAN database: Collision-induced absorption (CIA)}},
Journal = JQSRT,
Year = {{2012}},
Volume = {{113}},
Pages = {{1276-1285}},
Abstract = {{This paper describes the addition of Collision-Induced Absorption (CIA)
   into the HITRAN compilation. The data from different experimental and
   theoretical sources have been cast into a consistent format and
   formalism. The implementation of these new spectral data into the HITRAN
   database is invaluable for modeling and interpreting spectra of telluric
   and other planetary atmospheres as well as stellar atmospheres. In this
   implementation for HITRAN, CIAs of N-2, H-2, O-2, CO2, and CH4 due to
   various collisionally interacting atoms or molecules are presented. Some
   CIA spectra are given over an extended range of frequencies, including
   several H-2 overtone bands that are dipole-forbidden in the
   non-interacting molecules. Temperatures from tens to thousands of Kelvin
   are considered, as required, for example, in astrophysical analyses of
   objects, including cool white dwarfs, brown dwarfs. M dwarfs, cool main
   sequence stars, solar and extra-solar planets, and the formation of
   so-called first stars. }},
DOI = {{10.1016/j.jqsrt.2011.11.004}},
Journal-ISO = {{J. Quant. Spectrosc. Radiat. Transf.}},
}

@article{ 11AbFrLi.CIA,
Author = {Abel, Martin and Frommhold, Lothar and Li, Xiaoping and Hunt, Katharine
   L. C.},
Title = {{Collision-Induced Absorption by H$_2$ Pairs: From Hundreds to Thousands of
   Kelvin}},
Journal = JPCA,
Year = {{2011}},
Volume = {{115}},
Pages = {6805-6812},
Abstract = {{An interaction-induced dipole surface (IDS) and a potential energy
   surface (PES) of collisionally interacting molecular hydrogen pairs
   H-2-H-2 was recently obtained using quantum chemical methods (Li, X.; et
   al. Computational Methods in Science and Engineering, ICCMSE. AIP Conf.
   Proc. 2009,; see also Li, X.; et al. Int. J. Spectrosc. 2010, ID
   371201). The data account for substantial rotovibrational excitations of
   the H-2 molecules, as encountered at temperatures of thousands of kelvin
   (e.g., in the atmospheres of ``cool{''} stars). In this work we use
   these results to compute the binary collision-induced absorption (CIA)
   spectra of dense hydrogen gas in the infrared at temperatures up to
   several thousand kelvin. The principal interest of the work is in the
   spectra at such higher temperatures, but we also compare our
   computations with existing laboratory measurements of CIA spectra of
   dense hydrogen gas and find agreement.}},
DOI = {{10.1021/jp109441f}},
Journal-ISO = {{J. Phys. Chem. A}},
}



@article{ 01BoJoFu.CIA,
title = {High-temperature (1000-7000 K) collision-induced absorption of \{H2\} pairs computed from the first principles, with application to cool and dense stellar atmospheres },
journal = JQSRT,
volume = {68},
number = {3},
pages = {235 - 255},
year = {2001},
note = {},
issn = {0022-4073},
doi = {http://dx.doi.org/10.1016/S0022-4073(00)00023-6},
url = {http://www.sciencedirect.com/science/article/pii/S0022407300000236},
author = {Aleksandra Borysow and Uffe G. Jorgensen and Yi Fu},
keywords = {Collision-induced spectroscopy},
keywords = {Infrared absorption},
keywords = {Quantum mechanical lineshapes computations},
keywords = {Atmospheres of cool stars },
abstract = {The collision-induced absorption (CIA) spectra of H2-H2 and H2-He are known to play an important role for modelling of low-metallicity cool and dense stellar atmospheres. In this paper we present collision-induced absorption spectra of H2–H2 complexes in the rototranslational (О”v=0), the fundamental (О”v=1), the first (О”v=2) and the second (О”v=3) overtone bands in the temperature range from 1000 to 7000 K, and in the frequency region from 0 to 20 000 cmв€’1. The translational spectral density functions are computed quantum mechanically, based on: (1) the newly developed ab initio collision-induced H2–H2 dipole functions of Zheng (Computational study of collision induced dipole moments and absorption spectra of H2–H2. Ph.D. thesis, Michigan Technological University, 1997), which account for the short-range H2–H2 intermolecular distances (as small as 2.5 a.u.) and for larger \{H2\} internuclear distances (as large as 2.15 a.u.); (2) semiempirical isotropic H2–H2 potential (Ross et al, J Chem Phys 1983;79(3):1487) suitable for high temperatures. We include the collision-induced absorption coefficient of the vibrational transitions as v1,v2,v′1,v′2≤3 which we computed rigorously. We also give our estimate for the collision-induced absorption coefficients of single vibrational transitions such as vi<3, v′i>3 in the first and second overtone bands. The dependence of \{CIA\} spectra on rotational states of \{H2\} molecules is accounted for in our computations. We have previously (Borysow et al, Astronom Astrophys. 1997;324:185–95) studied the effect of \{CIA\} for stars of a wide range of fundamental stellar parameters (effective temperature, gravity, and chemical composition), and determined for which combinations of these parameters it is necessary to include \{CIA\} in the model and spectrum computation. These calculations showed that \{CIA\} from H2–H2 plays an important, and often even a dominating role for stellar atmospheres of a wide range of stars. The approximate character of the estimates of the H2–H2 absorption coefficient we used in our previous work combined with the large effect \{CIA\} had on the stellar atmospheres, were the main inspirations to initiate the more accurate computations of the absorption coefficient we present here. The absorption coefficient we compute in the present analysis is in qualitative agreement with our preliminary estimates (Borysow et al, Astronom Astrophys 1997;324:185–95), but in some spectral regions of high importance for the stellar structure, our computed absorption coefficient is up to a factor of 3 larger than our preliminary estimates. We therefore fully confirm our previous suspicion that H2–H2 \{CIA\} will have a pronounced effect on the atmosphere for a wide range of stars. In this paper we therefore quantify the effect the new data have on a typical cool dense stellar atmosphere, and compare our new results with our previous estimates. }
}