FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2000604452> ?p ?o ?g. }

• W2000604452 endingPage "1005" @default.
• W2000604452 startingPage "989" @default.
• W2000604452 abstract "Recently the Cassini Ultraviolet Imaging Spectrograph (UVIS) has revealed the presence of N2 Vegard–Kaplan (VK) band A3Σu+-X1Σg+ emissions in Titan’s dayglow limb observation. We present model calculations for the production of various N2 triplet states (viz., A3Σu+,B3Πg,C3Πu,E3Σu,W3Δu, and B3Σu ) in the upper atmosphere of Titan. The Analytical Yield Spectra technique is used to calculate steady state photoelectron fluxes in Titan’s atmosphere, which are in agreement with those observed by the Cassini’s CAPS instrument. Considering direct electron impact excitation, inter-state cascading, and quenching effects, the population of different levels of N2 triplet states are calculated under statistical equilibrium. Densities of all vibrational levels of each triplet state and volume production rates for various triplet states are calculated in the model. Vertically integrated overhead intensities for the same date and lighting conditions as reported by the UVIS observations for N2 Vegard–Kaplan A3Σu+-X1Σg+, First Positive B3Πg-A3Σu+, Second Positive (C3Πu − B3Πg), Wu–Benesch (W3Δu − B3Πg), and Reverse First Positive bands of N2 are found to be 132, 114, 19, 22, and 22 R, respectively. Overhead intensities are calculated for each vibrational transition of all the triplet band emissions of N2, which span a wider spectrum of wavelengths from ultraviolet to infrared. The calculated limb intensities of total and prominent transitions of VK band are presented. The model limb intensity of VK emission within the 150–190 nm wavelength region is in good agreement with the Cassini UVIS observed limb profile. An assessment of the impact of solar EUV flux on the N2 triplet band emission intensity has been made by using three different solar flux models, viz., Solar EUV Experiment (SEE), SOLAR2000 (S2K) model of Tobiska (Tobiska, W.K. [2004]. Adv. Space Res. 34, 1736–1746), and HEUVAC model of Richards et al. (Richards, P.G., Woods, T.N., Peterson, W.K. [2006]. Adv. Space Res. 37 (2), 315–322). The calculated N2 VK band intensity at the peak of limb intensity due to S2K and HEUVAC solar flux models is a factor of 1.2 and 0.9, respectively, of that obtained using SEE solar EUV flux. The effects of higher N2 density and solar zenith angle on the emission intensity are also studied. The model predicted N2 triplet band intensities during moderate (F10.7 = 150) and high (F10.7 = 240) solar activity conditions, using SEE solar EUV flux, are a factor of 2 and 2.8, respectively, higher than those during solar minimum (F10.7 = 68) condition." @default.
• W2000604452 created "2016-06-24" @default.
• W2000604452 creator A5039355092 @default.
• W2000604452 creator A5070110695 @default.
• W2000604452 date "2012-04-01" @default.
• W2000604452 modified "2023-09-27" @default.
• W2000604452 title "Production of N2 Vegard–Kaplan and other triplet band emissions in the dayglow of Titan" @default.
• W2000604452 cites W1966185507 @default.
• W2000604452 cites W1969657995 @default.
• W2000604452 cites W1974908932 @default.
• W2000604452 cites W1977435008 @default.
• W2000604452 cites W1981454865 @default.
• W2000604452 cites W1982713889 @default.
• W2000604452 cites W1987305918 @default.
• W2000604452 cites W1993347324 @default.
• W2000604452 cites W1994881758 @default.
• W2000604452 cites W1998172406 @default.
• W2000604452 cites W1998798364 @default.
• W2000604452 cites W2003392069 @default.
• W2000604452 cites W2012081513 @default.
• W2000604452 cites W2016380186 @default.
• W2000604452 cites W2023657277 @default.
• W2000604452 cites W2026740000 @default.
• W2000604452 cites W2026914628 @default.
• W2000604452 cites W2029824029 @default.
• W2000604452 cites W2030877475 @default.
• W2000604452 cites W2032062912 @default.
• W2000604452 cites W2042925900 @default.
• W2000604452 cites W2047039407 @default.
• W2000604452 cites W2048811578 @default.
• W2000604452 cites W2054154024 @default.
• W2000604452 cites W2056876979 @default.
• W2000604452 cites W2057438537 @default.
• W2000604452 cites W2061577344 @default.
• W2000604452 cites W2062158979 @default.
• W2000604452 cites W2062322776 @default.
• W2000604452 cites W2064181215 @default.
• W2000604452 cites W2070849843 @default.
• W2000604452 cites W2071060409 @default.
• W2000604452 cites W2079331684 @default.
• W2000604452 cites W2081188848 @default.
• W2000604452 cites W2082742684 @default.
• W2000604452 cites W2083571778 @default.
• W2000604452 cites W2089715385 @default.
• W2000604452 cites W2110515514 @default.
• W2000604452 cites W2111941049 @default.
• W2000604452 cites W2111968417 @default.
• W2000604452 cites W2119251049 @default.
• W2000604452 cites W2125730700 @default.
• W2000604452 cites W2149751608 @default.
• W2000604452 cites W2166761015 @default.
• W2000604452 cites W3100532889 @default.
• W2000604452 cites W3103253403 @default.
• W2000604452 cites W4238854702 @default.
• W2000604452 doi "https://doi.org/10.1016/j.icarus.2012.01.019" @default.
• W2000604452 hasPublicationYear "2012" @default.
• W2000604452 type Work @default.
• W2000604452 sameAs 2000604452 @default.
• W2000604452 citedByCount "14" @default.
• W2000604452 countsByYear W20006044522012 @default.
• W2000604452 countsByYear W20006044522013 @default.
• W2000604452 countsByYear W20006044522014 @default.
• W2000604452 countsByYear W20006044522015 @default.
• W2000604452 countsByYear W20006044522016 @default.
• W2000604452 countsByYear W20006044522017 @default.
• W2000604452 countsByYear W20006044522018 @default.
• W2000604452 countsByYear W20006044522019 @default.
• W2000604452 countsByYear W20006044522020 @default.
• W2000604452 crossrefType "journal-article" @default.
• W2000604452 hasAuthorship W2000604452A5039355092 @default.
• W2000604452 hasAuthorship W2000604452A5070110695 @default.
• W2000604452 hasBestOaLocation W20006044522 @default.
• W2000604452 hasConcept C120665830 @default.
• W2000604452 hasConcept C121332964 @default.
• W2000604452 hasConcept C1276947 @default.
• W2000604452 hasConcept C144024400 @default.
• W2000604452 hasConcept C149923435 @default.
• W2000604452 hasConcept C181500209 @default.
• W2000604452 hasConcept C184779094 @default.
• W2000604452 hasConcept C192562407 @default.
• W2000604452 hasConcept C2776798109 @default.
• W2000604452 hasConcept C2908647359 @default.
• W2000604452 hasConcept C4839761 @default.
• W2000604452 hasConcept C50805821 @default.
• W2000604452 hasConcept C6260449 @default.
• W2000604452 hasConcept C76766466 @default.
• W2000604452 hasConcept C96141758 @default.
• W2000604452 hasConceptScore W2000604452C120665830 @default.
• W2000604452 hasConceptScore W2000604452C121332964 @default.
• W2000604452 hasConceptScore W2000604452C1276947 @default.
• W2000604452 hasConceptScore W2000604452C144024400 @default.
• W2000604452 hasConceptScore W2000604452C149923435 @default.
• W2000604452 hasConceptScore W2000604452C181500209 @default.
• W2000604452 hasConceptScore W2000604452C184779094 @default.
• W2000604452 hasConceptScore W2000604452C192562407 @default.
• W2000604452 hasConceptScore W2000604452C2776798109 @default.
• W2000604452 hasConceptScore W2000604452C2908647359 @default.
• W2000604452 hasConceptScore W2000604452C4839761 @default.

• next