A Monitoring Campaign (2013–2020) of ESA’s Mars Express to Study Interplanetary Plasma Scintillation

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aut.relation.articlenumbere013
aut.relation.journalPublications of the Astronomical Society of Australia
aut.relation.startpagee013
aut.relation.volume40
dc.contributor.authorKummamuru, P
dc.contributor.authorMolera Calvés, G
dc.contributor.authorCimò, G
dc.contributor.authorPogrebenko, SV
dc.contributor.authorBocanegra-Bahamón, TM
dc.contributor.authorDuev, DA
dc.contributor.authorMd Said, MD
dc.contributor.authorEdwards, J
dc.contributor.authorMa, M
dc.contributor.authorQuick, J
dc.contributor.authorNeidhardt, A
dc.contributor.authorDe Vicente, P
dc.contributor.authorHaas, R
dc.contributor.authorKallunki, J
dc.contributor.authorMacCaferri, G
dc.contributor.authorColucci, G
dc.contributor.authorYang, WJ
dc.contributor.authorHao, LF
dc.contributor.authorWeston, S
dc.contributor.authorKharinov, MA
dc.contributor.authorMikhailov, AG
dc.contributor.authorJung, T
dc.date.accessioned2023-05-15T23:53:36Z
dc.date.available2023-05-15T23:53:36Z
dc.date.issued2023-04-12
dc.description.abstractThe radio signal transmitted by the Mars Express (MEX) spacecraft was observed regularly between the years 2013-2020 at X-band (8.42 GHz) using the European Very Long Baseline Interferometry (EVN) network and University of Tasmania's telescopes. We present a method to describe the solar wind parameters by quantifying the effects of plasma on our radio signal. In doing so, we identify all the uncompensated effects on the radio signal and see which coronal processes drive them. From a technical standpoint, quantifying the effect of the plasma on the radio signal helps phase referencing for precision spacecraft tracking. The phase fluctuation of the signal was determined for Mars' orbit for solar elongation angles from 0 to 180 deg. The calculated phase residuals allow determination of the phase power spectrum. The total electron content of the solar plasma along the line of sight is calculated by removing effects from mechanical and ionospheric noises. The spectral index was determined as which is in agreement with Kolmogorov's turbulence. The theoretical models are consistent with observations at lower solar elongations however at higher solar elongation ($ ]]>160 deg) we see the observed values to be higher. This can be caused when the uplink and downlink signals are positively correlated as a result of passing through identical plasma sheets.
dc.identifier.citationPublications of the Astronomical Society of Australia, ISSN: 1323-3580 (Print); 1448-6083 (Online), Cambridge University Press (CUP), 40, e013-. doi: 10.1017/pasa.2023.12
dc.identifier.doi10.1017/pasa.2023.12
dc.identifier.issn1323-3580
dc.identifier.issn1448-6083
dc.identifier.urihttps://hdl.handle.net/10292/16154
dc.languageen
dc.publisherCambridge University Press (CUP)
dc.relation.urihttps://www.cambridge.org/core/journals/publications-of-the-astronomical-society-of-australia/article/monitoring-campaign-20132020-of-esas-mars-express-to-study-interplanetary-plasma-scintillation/D9E5DBCFDCE5CA3325FF1A4BEBC22BF1
dc.rights.accessrightsOpenAccess
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/
dc.subject5109 Space Sciences
dc.subject5101 Astronomical Sciences
dc.subject51 Physical Sciences
dc.subject0201 Astronomical and Space Sciences
dc.subject0299 Other Physical Sciences
dc.subjectAstronomy & Astrophysics
dc.subject5101 Astronomical sciences
dc.subject5107 Particle and high energy physics
dc.titleA Monitoring Campaign (2013–2020) of ESA’s Mars Express to Study Interplanetary Plasma Scintillation
dc.typeJournal Article
pubs.elements-id504997
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