1982
DOI: 10.1016/0019-1035(82)90027-6
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Comparison of the thermal and nonthermal radiation characteristics of Jupiter at 6, 11, and 21 cm with model calculations

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Cited by 16 publications
(7 citation statements)
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“…Later, higher resolution interferometric maps displayed the regions of intense emission along the equator and at higher latitudes (de Pater et al 1982;de Pater & Dickel 1986;Leblanc et al 1997;Santos-Costa 2001;de Pater & Dunn 2003). The features of such a brightness distribution have been recently interpreted by Santos-Costa & Bolton (2008).…”
Section: Introductionmentioning
confidence: 96%
“…Later, higher resolution interferometric maps displayed the regions of intense emission along the equator and at higher latitudes (de Pater et al 1982;de Pater & Dickel 1986;Leblanc et al 1997;Santos-Costa 2001;de Pater & Dunn 2003). The features of such a brightness distribution have been recently interpreted by Santos-Costa & Bolton (2008).…”
Section: Introductionmentioning
confidence: 96%
“…The jovian NH 3 distribution can now be described as follows: (1) at pressures higher than 4 bars, the N/H ratio is enriched relatively to the solar value, with an enrichment of about 2 at 12 bars (De Pater et aL, 1982;Marten et aI., 1980); (2)there is a significant depletion at about 3.5 bars, probably related to the presence of a cloud involving nitrogen compounds (NH4SH, NH4OH...); (3)between 3.5 and 0.5 bar, below the NH3 cloud, the N/H ratio ranges between the solar value and 0.3 times the solar value (Marten et al, 1980;Combes and Encrenaz, 1979); (4) in the NH3 cloud level, the N/H ratio is depleted relatively to the saturation law, by a factor 0.2 to 0.5 Marten et al, 1980); the reason for this depletion is probably the beginning of NH 3 photodissociation by the solar UV radiation; (5) above the NH 3 cloud level, a very strong photodissociation occurs; NH 3 profiles have been inferred by Combes et aI. (1980) and Fricke et al (1982).…”
Section: B the Non-uniformely Mixed Constituentsmentioning
confidence: 99%
“…Indeed, the phenomenons which make the comet observable, as it approaches the Sun, are 'secondary' phenomenons, products of the sublimation of ices due to solar heating, the ejection of dust, and then the dissociation or ionization of the 'parent' molecules into radicals and ions identified in the cometary spectra ( Figure 16). Cometary emissions were first observed in visible spectra, as the strong CN lines (Dossin et al, 1961). The extension to the UV range, especially with the IUE satellite (Rahe, 1980;Festou et al, 1982), has provided us with the identifications of a new series of radicals and ions, especially the OH (O, O) at 3090 A, resolved for the first time with IUE on Comet Sargeant (Jackson et al, 1979).…”
Section: ) the Composition Of Cometary Nucleimentioning
confidence: 99%
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“…Higher resolution interferometric maps displayed with accuracy the regions of intense emission along the equator and at higher latitudes [ de Pater et al , 1982; de Pater and Jaffe , 1984; de Pater and Dickel , 1986; de Pater , 1981; Leblanc et al , 1997a], the brightness' dependence on the wavelength [ de Pater et al , 1982; de Pater and Dickel , 1986; de Pater , 1981; Leblanc et al , 1997a; de Pater and Dunn , 2003], longitude (east‐west asymmetry) [ de Pater , 1980; de Pater et al , 1982; de Pater and Jaffe , 1984; de Pater , 1981; Leblanc et al , 1997a], and D E (Earth's declination as seen from Jupiter) [ Dulk et al , 1999b]; and allowed a three‐dimenional reconstruction of Jupiter's synchrotron radiation [ Sault et al , 1997a; Leblanc et al , 1997a]. Observations at high resolution have proven to be valuable in constraining models for the magnetic field [ Dulk et al , 1997a, 1999a, 1999b] and the electron pitch angle and radial distributions [ de Pater , 1981; de Pater and Goertz , 1990; Levin et al , 2001; Garrett et al , 2005].…”
Section: Introductionmentioning
confidence: 99%