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MWR: Microwave Radiometer for the Juno Mission to Jupiter

Janssen, M. A. and Ingersoll, A. P. (2017) MWR: Microwave Radiometer for the Juno Mission to Jupiter. Space Science Reviews . ISSN 0038-6308. (In Press) http://resolver.caltech.edu/CaltechAUTHORS:20170606-152130209

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Abstract

The Juno Microwave Radiometer (MWR) is a six-frequency scientific instrument designed and built to investigate the deep atmosphere of Jupiter. It is one of a suite of instruments on NASA’s New Frontiers Mission Juno launched to Jupiter on August 5, 2011. The focus of this paper is the description of the scientific objectives of the MWR investigation along with the experimental design, observational approach, and calibration that will achieve these objectives, based on the Juno mission plan up to Jupiter orbit insertion on July 4, 2016. With frequencies distributed approximately by octave from 600 MHz to 22 GHz, the MWR will sample the atmospheric thermal radiation from depths extending from the ammonia cloud region at around 1 bar to pressure levels as deep as 1000 bars. The primary scientific objectives of the MWR investigation are to determine the presently unknown dynamical properties of Jupiter’s subcloud atmosphere and to determine the global abundance of oxygen and nitrogen, present in the atmosphere as water and ammonia deep below their respective cloud decks. The MWR experiment is designed to measure both the thermal radiation from Jupiter and its emission-angle dependence at each frequency relative to the atmospheric local normal with high accuracy. The antennas at the four highest frequencies (21.9, 10.0, 5.2, and 2.6 GHz) have ∼12° beamwidths and will achieve a spatial resolution approaching 600 km near perijove. The antennas at the lowest frequencies (0.6 and 1.25 GHz) are constrained by physical size limitations and have 20° beamwidths, enabling a spatial resolution of as high as 1000 km to be obtained. The MWR will obtain Jupiter’s brightness temperature and its emission-angle dependence at each point along the subspacecraft track, over angles up to 60° from the normal over most latitudes, during at least six perijove passes after orbit insertion. The emission-angle dependence will be obtained for all frequencies to an accuracy of better than one part in 10^3, sufficient to detect small variations in atmospheric temperature and absorber concentration profiles that distinguish dynamical and compositional properties of the deep Jovian atmosphere.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1007/s11214-017-0349-5DOIArticle
https://link.springer.com/article/10.1007%2Fs11214-017-0349-5PublisherArticle
http://rdcu.be/tsLfPublisherFree ReadCube access
ORCID:
AuthorORCID
Janssen, M. A.0000-0001-5476-731X
Ingersoll, A. P.0000-0002-2035-9198
Additional Information:© 2017 Springer Science+Business Media Dordrecht. Received: 02 November 2016; Accepted: 11 March 2017; First Online: 27 March 2017. The work described in this paper was conducted at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). The author wishes to thank the numerous contributors from the Juno Project and the Lockheed-Martin spacecraft team, without whom this ambitious project would not have been possible.
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:Jupiter; Microwave radiometry; Synchrotron emission; Atmosphere; Atmospheric composition; Atmospheric dynamics
Record Number:CaltechAUTHORS:20170606-152130209
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170606-152130209
Official Citation:Janssen, M.A., Oswald, J.E., Brown, S.T. et al. Space Sci Rev (2017). doi:10.1007/s11214-017-0349-5
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77977
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:14 Jun 2017 16:22
Last Modified:14 Jun 2017 16:22

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