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Design and Simulation of Stellar Occultation Infrared Band Constellation. REMOTE SENSING 2022. [DOI: 10.3390/rs14143327] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
This study provides an in-depth analysis of the characteristics of stellar occultation events. Using 10 target star sources, the influence of orbital elements on the number, duration, and distribution of stellar occultation events was simulated and analyzed, and the constellation configuration was designed. The results showed the following points: (1) the orbital inclination had the greatest influence on the number of occultation events, with obvious upward and downward trends in the range of 10–40° and 150–180°, and the amount of occultation data remained at about 303 times under the other angle conditions. The orbital height had an effect on the number of occultations, but the amplitude was small. (2) The use of four orbits had an impact on the occultation duration. The duration decreased with an increase in the orbit height and inclination, the distribution was symmetrical with the perigee angular distance, and it increased with an increase in the ascending intersection right ascension. (3) The higher the orbital height, the less comprehensive the longitudinal and latitudinal distribution of occultation events. With an orbital inclination of less than 150°, the greatest occultation event was covered to encompass the entire world. The other two orbital elements had negligible effects on the longitudinal and latitudinal distribution of occultation events. (4) The elevation of the occultation event increased with an increase in the orbital altitude, but the azimuth showed no obvious change trends. A considerable number of normal occultations can be obtained with an orbital inclination of less than 120°. The other two orbital elements had a negligible effect on the distribution of altitude and azimuth of occultation events. A stellar occultation constellation configuration was designed based on the simulation results, and the results showed that the following parameters of satellites can be used to realize the global distribution of occultation events: orbital height of 500 km, orbital inclination of 97.3771°, perigee angular distance of 40°, and ascending node right ascension steps of 40°. This configuration will ensure that an adequate number of normal occultations are obtained, which will ensure the quality of data inversion under the condition of 152 infrared target star sources.
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Moore L, Melin H, O'Donoghue J, Stallard TS, Moses JI, Galand M, Miller S, Schmidt CA. Modelling H 3+ in planetary atmospheres: effects of vertical gradients on observed quantities. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2019; 377:20190067. [PMID: 31378180 PMCID: PMC6710898 DOI: 10.1098/rsta.2019.0067] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 04/07/2019] [Indexed: 05/20/2023]
Abstract
Since its detection in the aurorae of Jupiter approximately 30 years ago, the H3+ ion has served as an invaluable probe of giant planet upper atmospheres. However, the vast majority of monitoring of planetary H3+ radiation has followed from observations that rely on deriving parameters from column-integrated paths through the emitting layer. Here, we investigate the effects of density and temperature gradients along such paths on the measured H3+ spectrum and its resulting interpretation. In a non-isothermal atmosphere, H3+ column densities retrieved from such observations are found to represent a lower limit, reduced by 20% or more from the true atmospheric value. Global simulations of Uranus' ionosphere reveal that measured H3+ temperature variations are often attributable to well-understood solar zenith angle effects rather than indications of real atmospheric variability. Finally, based on these insights, a preliminary method of deriving vertical temperature structure is demonstrated at Jupiter using model reproductions of electron density and H3+ measurements. The sheer diversity and uncertainty of conditions in planetary atmospheres prohibits this work from providing blanket quantitative correction factors; nonetheless, we illustrate a few simple ways in which the already formidable utility of H3+ observations in understanding planetary atmospheres can be enhanced. This article is part of a discussion meeting issue 'Advances in hydrogen molecular ions: H3+, H5+ and beyond'.
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Affiliation(s)
- L. Moore
- Boston University, Boston, MA, USA
| | - H. Melin
- University of Leicester, Leicester, UK
| | - J. O'Donoghue
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | | | - M. Galand
- Department of Physics, Imperial College London, London, UK
| | - S. Miller
- University College London, London, UK
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Yelle RV, McConnell JC, Sandel BR, Broadfoot AL. The dependence of electroglow on the solar flux. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja092ia13p15110] [Citation(s) in RCA: 31] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Broadfoot AL, Sandel BR, Shemansky DE, McConnell JC, Smith GR, Holberg JB, Atreya SK, Donahue TM, Strobel DF, Bertaux JL. Overview of the Voyager ultraviolet spectrometry results through Jupiter encounter. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia10p08259] [Citation(s) in RCA: 215] [Impact Index Per Article: 17.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Smith GR, Shemansky DE, Holberg JB, Broadfoot AL, Sandel BR, McConnell JC. Saturn's upper atmosphere from the Voyager 2 Euv solar and stellar occultations. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja088ia11p08667] [Citation(s) in RCA: 95] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Herbert F, Sandel BR, Yelle RV, Holberg JB, Broadfoot AL, Shemansky DE, Atreya SK, Romani PN. The upper atmosphere of Uranus: EUV occultations observed by Voyager 2. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja092ia13p15093] [Citation(s) in RCA: 81] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Moses JI, Fouchet T, Bézard B, Gladstone GR, Lellouch E, Feuchtgruber H. Photochemistry and diffusion in Jupiter's stratosphere: Constraints from ISO observations and comparisons with other giant planets. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002411] [Citation(s) in RCA: 141] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- J. I. Moses
- Lunar and Planetary Institute; Houston Texas USA
| | - T. Fouchet
- LESIA; Observatoire de Paris; Meudon France
- Université Paris 6; Paris France
| | - B. Bézard
- LESIA; Observatoire de Paris; Meudon France
| | - G. R. Gladstone
- Space Sciences Department; Southwest Research Institute; San Antonio Texas USA
| | | | - H. Feuchtgruber
- Max-Planck-Institut für Extraterrestrische Physik; Garching Germany
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Bougher SW. Jupiter Thermospheric General Circulation Model (JTGCM): Global structure and dynamics driven by auroral and Joule heating. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2003je002230] [Citation(s) in RCA: 56] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Majeed T, Waite JH, Bougher SW, Gladstone GR. Processes of equatorial thermal structure at Jupiter: An analysis of the Galileo temperature profile with a three-dimensional model. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002351] [Citation(s) in RCA: 15] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Atreya SK, Wong MH, Owen TC, Mahaffy PR, Niemann HB, de Pater I, Drossart P, Encrenaz TH. A comparison of the atmospheres of Jupiter and Saturn: deep atmospheric composition, cloud structure, vertical mixing, and origin. PLANETARY AND SPACE SCIENCE 1999; 47:1243-1262. [PMID: 11543193 DOI: 10.1016/s0032-0633(99)00047-1] [Citation(s) in RCA: 19] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
We present our current understanding of the composition, vertical mixing, cloud structure and the origin of the atmospheres of Jupiter and Saturn. Available observations point to a much more vigorous vertical mixing in Saturn's middle-upper atmosphere than in Jupiter's. The nearly cloud-free nature of the Galileo probe entry site, a 5-micron hotspot, is consistent with the depletion of condensable volatiles to great depths, which is attributed to local meteorology. Somewhat similar depletion of water may be present in the 5-micron bright regions of Saturn also. The supersolar abundances of heavy elements, particularly C and S in Jupiter's atmosphere and C in Saturn's, as well as the progressive increase of C from Jupiter to Saturn and beyond, tend to support the icy planetesimal model of the formation of the giant planets and their atmospheres. However, much work remains to be done, especially in the area of laboratory studies, including identification of possible new microwave absorbers, and modelling, in order to resolve the controversy surrounding the large discrepancy between Jupiter's global ammonia abundance, hence the nitrogen elemental ratio, derived from the earth-based microwave observations and that inferred from the analysis of the Galileo probe-orbiter radio attenuation data for the hotspot. We look forward to the observations from Cassini-Huygens spacecraft which are expected to result not only in a rich harvest of information for Saturn, but a better understanding of the formation of the giant planets and their atmospheres when these data are combined with those that exist for Jupiter.
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Affiliation(s)
- S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, The University of Michigan, Ann Arbor 48109-2143, USA.
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Perry JJ, Kim YH, Fox JL, Porter HS. Chemistry of the Jovian auroral ionosphere. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999je900022] [Citation(s) in RCA: 51] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Sada PV, Bjoraker GL, Jennings DE, McCabe GH, Romani PN. Observations of CH4, C2H6, and C2H2 in the stratosphere of Jupiter. ICARUS 1998; 136:192-201. [PMID: 11878354 DOI: 10.1006/icar.1998.6021] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
We have performed high-resolution spectral observations at mid-infrared wavelengths of CH4 (8.14 micrometers), C2H6 (12.16 micrometers), and C2H2 (13.45 micrometers) on Jupiter. These emission features probe the stratosphere of the planet and provide information on the carbon-based photochemical processes taking place in that region of the atmosphere. The observations were performed using our cryogenic echelle spectrometer CELESTE, in conjunction with the McMath-Pierce 1.5-m solar telescope between November 1994 and February 1995. We used the methane observations to derive the temperature profile of the jovian atmosphere in the 1-10 mbar region of the stratosphere. This profile was then used in conjunction with height-dependent mixing ratios of each hydrocarbon to determine global abundances for ethane and acetylene. The resulting mixing ratios are 3.9(+1.9)(-1.3) x 10(-6) for C2H6 (5 mbar pressure level), and 2.3 +/- 0.5 x 10(-8) for C2H2 (8 mbar pressure level), where the quoted uncertainties are derived from model variations in the temperature profile which match the methane observation uncertainties.
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Affiliation(s)
- P V Sada
- Planetary Systems Branch, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA.
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Seiff A, Kirk DB, Knight TCD, Young RE, Mihalov JD, Young LA, Milos FS, Schubert G, Blanchard RC, Atkinson D. Thermal structure of Jupiter's atmosphere near the edge of a 5-μm hot spot in the north equatorial belt. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je01766] [Citation(s) in RCA: 250] [Impact Index Per Article: 9.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Seiff A, Kirk DB, Knight TCD, Young LA, Milos FS, Venkatapathy E, Mihalov JD, Blanchard RC, Young RE, Schubert G. Thermal Structure of Jupiter's Upper Atmosphere Derived from the Galileo Probe. Science 1997; 276:102-4. [PMID: 9082977 DOI: 10.1126/science.276.5309.102] [Citation(s) in RCA: 73] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
Temperatures in Jupiter's atmosphere derived from Galileo Probe deceleration data increase from 109 kelvin at the 175-millibar level to 900 ± 40 kelvin at 1 nanobar, consistent with Voyager remote sensing data. Wavelike oscillations are present at all levels. Vertical wavelengths are 10 to 25 kilometers in the deep isothermal layer, which extends from 12 to 0.003 millibars. Above the 0.003-millibar level, only 90- to 270- kilometer vertical wavelengths survive, suggesting dissipation of wave energy as the probable source of upper atmosphere heating.
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Affiliation(s)
- A Seiff
- A. Seiff, Department of Meteorology, San Jose State University Foundation and MS 245-1, Ames Research Center, Moffett Field, CA 94035, USA. D. B. Kirk, University of Oregon, 37465 Riverside Drive, Pleasant Hill, Oregon 97455, USA. T. C. D. Knight, 2370 S. Brentwood St., Lakewood, CO 80227, USA. L. A. Young, Center for Space Physics, Boston University, 725 Commonwealth Ave., Boston, Massachusetts 02215, USA. F. S. Milos, M.S. 234-1, Ames Research Center, NASA, Moffett Field, CA 94035, USA. E. Venkatapathy, Eloret Institute, MS 230-2, Ames Research Center, Moffett Field, CA 94035, USA. J. D. Mihalov and R. E. Young, MS 245-3, Ames Research Center, Moffett Field, CA 94035, USA. R. C. Blanchard, MS 408A, Langley Research Center, NASA, Hampton, VA 23681, USA. G. Schubert, Department of Earth and Space Sciences, University of California, Los Angeles, CA 90024, USA
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Yelle RV, Young LA, Vervack RJ, Young R, Pfister L, Sandel BR. Structure of Jupiter's upper atmosphere: Predictions for Galileo. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/95je03384] [Citation(s) in RCA: 62] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Orton G, A'Hearn M, Baines K, Deming D, Dowling T, Goguen J, Griffith C, Hammel H, Hoffmann W, Hunten D. Collision of comet Shoemaker-Levy 9 with Jupiter observed by the NASA infrared telescope facility. Science 1995; 267:1277-82. [PMID: 7871423 DOI: 10.1126/science.7871423] [Citation(s) in RCA: 52] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
The National Aeronautics and Space Administration (NASA) Infrared Telescope Facility was used to investigate the collision of comet Shoemaker-Levy 9 with Jupiter from 12 July to 7 August 1994. Strong thermal infrared emission lasting several minutes was observed after the impacts of fragments C, G, and R. All impacts warmed the stratosphere and some the troposphere up to several degrees. The abundance of stratospheric ammonia increased by more than 50 times. Impact-related particles extended up to a level where the atmospheric pressure measured several millibars. The north polar near-infrared aurora brightened by nearly a factor of 5 a week after the impacts.
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Affiliation(s)
- G Orton
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena 91109
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Rego D, Prangé R, Gérard JC. Auroral Lyman α and H2bands from the giant planets: 1. Excitation by proton precipitation in the Jovian atmosphere. ACTA ACUST UNITED AC 1994. [DOI: 10.1029/93je03432] [Citation(s) in RCA: 41] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Fox JL. Dissociative Recombination in Planetary Ionospheres. ACTA ACUST UNITED AC 1993. [DOI: 10.1007/978-1-4615-2976-7_21] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/19/2023]
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20
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Orton GS, Friedson AJ, Baines KH, Martin TZ, West RA, Caldwell J, Hammel HB, Bergstralh JT, Malcom ME, Golisch WF, Griep DM, Kaminski CD, Tokunaga AT, Baron R, Shure M. Thermal Maps of Jupiter: Spatial Organization and Time Dependence of Stratospheric Temperatures, 1980 to 1990. Science 1991; 252:537-42. [PMID: 17838486 DOI: 10.1126/science.252.5005.537] [Citation(s) in RCA: 74] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The spatial organization and time dependence of Jupiter's stratospheric temperatures have been measured by observing thermal emission from the 7.8-micrometer CH(4) band. These temperatures, observed through the greater part of a Jovian year, exhibit the influence of seasonal radiative forcing. Distinct bands of high temperature are located at the poles and mid-latitudes, while the equator alternates between warm and cold with a period of approximately 4 years. Substantial longitudinal variability is often observed within the warm mid-latitude bands, and occasionally elsewhere on the planet. This variability includes small, localized structures, as well as large-scale waves with wavelengths longer than approximately 30,000 kilometers. The amplitudes of the waves vary on a time scale of approximately 1 month; structures on a smaller scale may have lifetimes of only days. Waves observed in 1985, 1987, and 1988 propagated with group velocities less than +/-30 meters per second.
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Waite JH. Comment on “Bremsstrahlung X rays from Jovian auroral electrons” by D. D. Barbosa. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91ja02143] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Horanyi M, Cravens TE, Waite JH. The precipitation of energetic heavy ions into the upper atmosphere of Jupiter. ACTA ACUST UNITED AC 1988. [DOI: 10.1029/ja093ia07p07251] [Citation(s) in RCA: 74] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Clarke JT, Hudson MK, Yung YL. The excitation of the far ultraviolet electroglow emissions on Uranus, Saturn, and Jupiter. JOURNAL OF GEOPHYSICAL RESEARCH 1987; 92:15139-47. [PMID: 11542130 DOI: 10.1029/ja092ia13p15139] [Citation(s) in RCA: 30] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Abstract
We propose that the diffuse FUV emissions of H and H2 in excess of photoelectron excitation observed from the sunlit atmospheres of Uranus, Saturn, and Jupiter are produced by electric field acceleration of photoelectrons and ions locally in the upper atmospheres. This in situ acceleration is required to satisfy the many observational constraints on the altitude distribution, exciting particle energy, and total input energy requirements of the electroglow mechanism. We further suggest that a primary mechanism leading to this acceleration is an ionospheric dynamo, which is created in the same manner as the Earth's dynamo. The calculated altitude of charge separation by the neutral wind drag on ions across magnetic field lines is consistent with the observed peaks in electroglow emissions from the Voyager ultraviolet spectrometer limb scan data on both Saturn (near the homopause) and Uranus (just above the homopause). This dynamo action therefore appears to initiate the acceleration process, which must have the form of field-aligned potentials to accelerate the magnetized electrons. We propose that these field-aligned potentials are due to anomalous resistivity, which results from sufficiently high field-aligned currents in the ionosphere to generate plasma instabilities and therefore runaway electrons and ions above some critical lower initial energy. There are multiple candidate processes for inducing these currents, including polarization in the equivalent F regions and inner magnetospheric convection, and each of these processes should exhibit latitudinal structure. The acceleration of low-energy electrons in an H2 atmosphere preferentially results in FUV radiation and further ionization, whereas electron acceleration in a nitrogen/oxygen atmosphere such as the Earth's is dominated by elastic scattering and thus results in electric currents. Individual electron and proton collisions with H2 molecules will result in excitation, ionization, and heating, so that considerable enhancement of the ionospheric density and heating of the upper atmosphere will accompany the FUV emission.
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Affiliation(s)
- J T Clarke
- Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
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Herbert F, Sandel BR, Broadfoot AL. Observations of the Jovian UV aurora by Voyager. ACTA ACUST UNITED AC 1987. [DOI: 10.1029/ja092ia04p03141] [Citation(s) in RCA: 52] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cravens TE. Vibrationally excited molecular hydrogen in the upper atmosphere of Jupiter. ACTA ACUST UNITED AC 1987. [DOI: 10.1029/ja092ia10p11083] [Citation(s) in RCA: 81] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Waite JH, Cravens TE, Kozyra J, Nagy AF, Atreya SK, Chen RH. Electron precipitation and related aeronomy of the Jovian thermosphere and ionosphere. ACTA ACUST UNITED AC 1983. [DOI: 10.1029/ja088ia08p06143] [Citation(s) in RCA: 198] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Shemansky DE, Ajello JM. The Saturn spectrum in the EUV-electron excited hydrogen. ACTA ACUST UNITED AC 1983. [DOI: 10.1029/ja088ia01p00459] [Citation(s) in RCA: 66] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Gérard JC, Singh V. A model of energy deposition of energetic electrons and EUV emission in the Jovian and Saturnian atmospheres and implications. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/ja087ia06p04525] [Citation(s) in RCA: 69] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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