This HTML5 document contains 35 embedded RDF statements represented using HTML+Microdata notation.

The embedded RDF content will be recognized by any processor of HTML5 Microdata.

Namespace Prefixes

PrefixIRI
dctermshttp://purl.org/dc/terms/
dbohttp://dbpedia.org/ontology/
foafhttp://xmlns.com/foaf/0.1/
n12https://global.dbpedia.org/id/
dbthttp://dbpedia.org/resource/Template:
rdfshttp://www.w3.org/2000/01/rdf-schema#
freebasehttp://rdf.freebase.com/ns/
rdfhttp://www.w3.org/1999/02/22-rdf-syntax-ns#
owlhttp://www.w3.org/2002/07/owl#
wikipedia-enhttp://en.wikipedia.org/wiki/
dbchttp://dbpedia.org/resource/Category:
dbphttp://dbpedia.org/property/
provhttp://www.w3.org/ns/prov#
xsdhhttp://www.w3.org/2001/XMLSchema#
wikidatahttp://www.wikidata.org/entity/
dbrhttp://dbpedia.org/resource/

Statements

Subject Item
dbr:FUTBOLIN
rdfs:label
FUTBOLIN
rdfs:comment
FUTBOLIN (FUll Transfer By Optimized LINe-by-line methods) is a multi-level multiple scattering radiative transfer model for the calculation of line-by-line atmospheric emission/transmission spectra in planetary atmospheres. It has been developed by Javier Martín-Torres (AS&M. Inc, NASA/Langley Research Center, Hampton, VA, USA; Jet Propulsion Laboratory, Pasadena, CA; Now at IACT (CSIC-URG), Granada, SPAIN). It allows generating high-resolution synthetic spectra in the 0.3-1000 micrometre spectral range.
dcterms:subject
dbc:Planetary_atmospheres dbc:Scattering
dbo:wikiPageID
3172467
dbo:wikiPageRevisionID
1098872704
dbo:wikiPageWikiLink
dbr:Nitrogen dbr:Celestial_body_atmosphere dbc:Scattering dbr:Oxygen dbr:Transmittance dbr:Venus dbr:Water_(molecule) dbr:Absorption_spectrum dbr:Micrometre dbr:Radiative_transfer dbr:Reflectivity dbr:Mars dbr:Titan_(moon) dbr:Spectral_lines dbr:Scattering dbr:Javier_Martín-Torres dbc:Planetary_atmospheres dbr:Earth dbr:Carbon_dioxide
owl:sameAs
freebase:m.08w_33 wikidata:Q17015066 n12:fux1
dbp:wikiPageUsesTemplate
dbt:Planetary-science-stub dbt:Scattering-stub dbt:For
dbo:abstract
FUTBOLIN (FUll Transfer By Optimized LINe-by-line methods) is a multi-level multiple scattering radiative transfer model for the calculation of line-by-line atmospheric emission/transmission spectra in planetary atmospheres. It has been developed by Javier Martín-Torres (AS&M. Inc, NASA/Langley Research Center, Hampton, VA, USA; Jet Propulsion Laboratory, Pasadena, CA; Now at IACT (CSIC-URG), Granada, SPAIN). It allows generating high-resolution synthetic spectra in the 0.3-1000 micrometre spectral range. The code can handle spherical or plane-parallel atmospheres. It reads spectral lines in HITRAN or GEISA format and can handle CO2 line mixing and continuum absorption from H2O, O2, N2 and CO2. It also takes into account the Non Local Thermodynamic Equilibrium (NLTE) effects on the rotational, electronic and vibrational populations of the atmospheric species and allows to specify any combinations of clouds, coverage and spectral albedo. It has been used to model the Earth's atmosphere, and the atmospheres of Mars, Venus, and Titan. The code can calculate reflection, transmission, absorption, infrared cooling rate, and flux spectra.
prov:wasDerivedFrom
wikipedia-en:FUTBOLIN?oldid=1098872704&ns=0
dbo:wikiPageLength
2147
foaf:isPrimaryTopicOf
wikipedia-en:FUTBOLIN