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Thursday, July 30, 2020 | History

3 edition of Pioneer-Venus radio occultation (ORO) data reduction found in the catalog.

Pioneer-Venus radio occultation (ORO) data reduction

Pioneer-Venus radio occultation (ORO) data reduction

profiles of 13 CH absorptivity : final technical report (includes quarterly report #9) for grant NAG-2-515, July 1, 1988 through September 30, 1990

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  • 17 Currently reading

Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Absorptivity.,
  • Error analysis.,
  • Pioneer Venus spacecraft.,
  • Radio occultation.,
  • Sulfuric acid.

  • Edition Notes

    Other titlesPioneer Venus radio occultation (ORO) data reduction.
    StatementPaul G. Steffes, principal investigator.
    SeriesNASA contractor report -- NASA CR-186986.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL15405701M

    Global GNSS Radio Occultation Mission for Meteorology, Ionosphere & Climate By Nick L. Yen, Chen-Joe Fong, Chung-Huei Chu, Jiun-Jih Miau, Yuei-An Liou, Cited by: 1. T. M. Bocanegra-Bahamón et al.: Venus Express radio occultation observed by PRIDE Fig. 4: Example of the S/N of a signal detection during a radio occultation. This is the VEX signal detection obtained with Bd in the session of At around s the S/N starts rapidly decreasing marking the beginning of the occultation ingress,Cited by: 2.

    Airglow emissions, radio and solar occultation data from the Voyager mission over a quarter of a century ago provided the main source of information on the composition and structure of Titan's. The Pioneer Venus Orbiter was launched on , and inserted into an elliptical orbit around Venus on December 4, The Orbiter was a flat cylinder m in diameter and m high. The Pioneer Venus Multiprobe launched on August 8, , and consisted of a bus that carried one large and three small atmospheric probes.

    Atmospheric radio occultation. Atmospheric radio occultation relies on the detection of a change in a radio signal as it passes through a planet's atmosphere, i.e. as it is occulted by the atmosphere. When electromagnetic radiation passes through the atmosphere, it is refracted (or bent). The magnitude of the refraction depends on the gradient of refractivity normal to the path, which in turn. These analyses concentrate on the comparison of the properties of both the electron density peaks and the topside profiles with the behavior expected for a Chapman layer and that observed at Venus with the Pioneer Venus orbiter radio occultation by:


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Pioneer-Venus radio occultation (ORO) data reduction Download PDF EPUB FB2

Setting the cutting edge for the field, Radio Occultations Using Earth Satellites: A Wave Theory Treatment develops a purely wave-theoretic approach to occultation analysis. This approach yields more nuanced results than either ray or hybrid (ray/wave) methodologies offer, and proves suitable for the many variables at work in today's by:   Pioneer Venus radio occultation data for four seasons between December and October are used to construct meridional cross sections of temperature and zonal wind velocity for the middle atmosphere of Venus in the altitude range of ∼40–80 km and in Cited by: This book proposes a method based on neural networks to retrieve atmospheric profiles from RO refractivity.

Once trained, the neural networks provide a suited transfer function able to obtain atmospheric profiles overcoming the requirement for additional information at each GPS : Fabrizio Pelliccia, Stefania Bonafoni. The Pioneer Venus orbiter began circling the planet every 24 hours on December 4, Four seasons of occultation data have now been collected.

It is found that the assumption of cyclostrophic balance, in conjunction with radio occultation derived temperature data, yields a zonal wind field for most of the middle atmosphere of by: ABSTRACT Radio occultation measurements of the temperature structure of the Venus atmosphere have been obtained during seven occultation easons extending from December to December Approximately vertical profiles of temperature from about 40 Cited by: Between December and February the Pioneer Venus orbiter spacecraft returned some S band and X band radio occultation measurements of the Venus atmosphere.

Results from 13 measurements, covering diverse latitudes from near equatorial to polar, are presented in this paper in the form of vertical profiles of by: Radio occultation measurements of electron density profiles from Mariner 6 and 7, the Mariner 9 extended mission, and the U.S.

Viking orbiters, together with model ion and electron temperature. Eighty-seven measurements of the thermal structure in the atmosphere of Venus between the altitudes of about 40 and 85 km were derived from Pioneer Venus Orbiter radio occultation data taken.

Abstract As in the cases of Mariner 5 and 10 and Venera 9, the Pioneer Venus radio occultation measurements of Venus show an upper region of turbulence located in the vicinity of 60 km.

Estimates of the deduced intensity of turbulence are consistent with the upper bound obtained earlier from the complementary Pioneer Venus probe measurements. Radio occultation (RO) measurements have been used in planetary atmospheric studies since (Fjeldbo and Eshleman, ), and until 14 bodies of the Solar system had been explored using RO techniques, the first ones being Mars and Venus as Mariner 4 and 5 flew past these planets (see Tableadapted from Yakovlev, ).

Radio occultation measurements of the temperature structure of the Venus atmosphere have been obtained during seven occultation "seasons" extending from December to December Approximately vertical profiles of temperature from about 40 km to. On October 5 and 6,three dual-frequency ingress radio occultation experiments were conducted at Venus during consecutive orbits of the Magellan spacecraft.

The radio signals probed a region of the atmosphere near 65°N, with a solar zenith angle of °, reaching below 35 km at cm, and below 34 km at 13 cm (above a mean radius of Cited by: Radio Occultation: Some Background • Radio occultation (RO) measurements have been used by to study planetary atmospheres (Mars, Venus) since the ’s.

Its an active technique. We simply look at how the paths of radio signals are bent by refractive index gradients in the atmosphere. • The use of RO measurements in the Earth’s. Comparison of Akatsuki RS results with the previous radio occultation results from Pioneer Venus (Kliore and Patel ) and Venus Express (Pätzold et al.

; Tellmann et al. ) would reveal long-term variation of the Venusian atmosphere. The radio occultation temperatures are used in the radiative transfer calculation for the analyses of Cited by: The Pioneer Venus project was part of the Pioneer program consisting of two spacecraft, the Pioneer Venus Orbiter and the Pioneer Venus Multiprobe, launched to Venus in The program was managed by NASA's Ames Research Center.

The Pioneer Venus Orbiter entered orbit around Venus on December 4,and performed observations to characterize the atmosphere and surface of Venus. Edited by Yuei-An Liou The book is devoted to radio occultation (RO) remote sensing of the earth’s atmosphere and ionosphere as a global method of monitoring.

This technique used the radio links satellite-to-satellite when a satellite-receiver setting or rising behind the earth’s atmosphere is relative to a satellite - emitter of radio by:   Pioneer Venus orbiter dual-frequency radio occultation measurements have produced many electron density profiles of the nightside ionosphere of Venus.

Thirty-six of these profiles, measured at solar zenith angles (χ) from degrees to degrees, are discussed here. In the "deep" nightside ionosphere (χ > degrees), the structure and magnitude of the ionization peak are highly Cited by: Pioneer Venus experiment descriptions: Publication: Space Science Reviews, vol.

20, Junep. Radiometers, Interferometry, Magnetometers, Mass Spectrometers, Nephelometers, Pioneer Venus 1 Spacecraft, Polarimetry, Radio Occultation, Radiometers, Solar Flux, Tables (Data), Venus Atmosphere, Wind Velocity This paper consists.

Extended mission radio occultation profiles from Pioneer Venus Orbiter (Kliore et al., ) • Radio occultation profiles from Venera, 16 (Yakovlev et al., ) • VeGa 1 and VeGa 2 balloon data (Sagdeev et al., ) • VeGa 2 Lander data (Linkin et al.,Zasova et al., ) •Cited by: The original Venus International Reference Atmosphere (VIRA) included an empirical model of the Venusian ionosphere (Bauer et al.

) which was based primarily on in situ and radio occultation measurements made by the Pioneer Venus Orbiter (PVO) in anda time of very high solar activity. The solar cycle variations of in situ parameters could not be determined because periapsis Cited by: 3. An introduction to GPS radio occultation and its use in numerical weather prediction.

J R Eyre. Met Office Exeter, United Kingdom. 1. An introduction to radio occultation. The GPS system Radio occultation (RO) for the Earth’s atmosphere currently relies on File Size: KB.Get this from a library!

Pioneer-Venus radio occultation (ORO) data reduction: profiles of 13 CH absorptivity: final technical report (includes quarterly report #9) for grant NAG, July 1, through Septem [P G Steffes; United States. National Aeronautics and .The Pioneer Venus Orbiter, also known as Pioneer Venus 1 or Pion was a mission to Venus conducted by the United States as part of the Pioneer Venus ed in May atop an Atlas-Centaur rocket, the spacecraft was inserted into an elliptical orbit around Venus on December 4, It returned data on Venus until October Mission type: Venus orbiter.