Dear user, changes will soon be made to Orfeo. We will undertake the migration to a new version, another environment (and therefore a new URL: https://orfeo.belnet.be/) and another provider. Belnet will take over the management of Orfeo in the future. For you, this means that no changes, modifications or uploads can be made to the database Orfeo from the 1st of December 2021 to the 10th of December 2021. The database remains available for consultation. From the 10th of December 2021 onwards, you can reach Orfeo via the new url https://orfeo.belenet.be/. Our apologies for the inconvenience.

Show simple item record

dc.contributor.authorRichard, C.
dc.contributor.authorGordon, I.E.
dc.contributor.authorRothman, L.S.
dc.contributor.authorAbel, M.
dc.contributor.authorFrommhold, L.
dc.contributor.authorGustafsson, M.
dc.contributor.authorHartmann, J.-M.
dc.contributor.authorHermans, C.
dc.contributor.authorLafferty, W.J.
dc.contributor.authorOrton, G.S.
dc.contributor.authorSmith, K.M.
dc.contributor.authorTran, H.
dc.date2012
dc.date.accessioned2016-03-29T10:07:38Z
dc.date.available2016-03-29T10:07:38Z
dc.identifier.urihttps://orfeo.kbr.be/handle/internal/3036
dc.descriptionThis 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, CO 2, and CH 4 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.
dc.languageeng
dc.titleNew section of the HITRAN database: Collision-induced absorption (CIA)
dc.typeArticle
dc.subject.frascatiEarth and related Environmental sciences
dc.audienceScientific
dc.subject.freeAtmospheric absorption
dc.subject.freeBrown dwarfs
dc.subject.freeCollision-induced absorption
dc.subject.freeCool whites
dc.subject.freeExtended range
dc.subject.freeExtra solar planets
dc.subject.freeHITRAN
dc.subject.freeHITRAN database
dc.subject.freeMain sequence stars
dc.subject.freeMolecular pairs
dc.subject.freeOvertone bands
dc.subject.freePlanetary atmosphere
dc.subject.freeSpectral data
dc.subject.freeStellar atmospheres
dc.subject.freeCarbon dioxide
dc.subject.freeMolecules
dc.subject.freeStars
dc.subject.freeabsorption
dc.subject.freeastrophysics
dc.subject.freedatabase
dc.subject.freeplanetary atmosphere
dc.subject.freetemperature
dc.source.titleJournal of Quantitative Spectroscopy and Radiative Transfer
dc.source.volume113
dc.source.issue11
dc.source.page1276-1285
Orfeo.peerreviewedYes
dc.identifier.doi10.1016/j.jqsrt.2011.11.004
dc.identifier.scopus2-s2.0-84860917852


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record