The Mars express MARSIS sounder instrument

Jordan, R.; Picardi, G.; Plaut, J. J.; Wheeler, K.; Kirchner, D. L.; Safaeinili, A.; Johnson, W. L.; Seu, R.; Calabrese, D.; Zampolini, E.; Cicchetti, A.; Huff, R. L.; Gurnett, D. A.; Ivanov, A. B.; Kofman, W.; Orosei, R.; Thompson, T. W.; Edenhofer, P.; Bombaci, O.

doi:10.1016/j.pss.2009.09.016

Cited by 150 publications

(114 citation statements)

References 5 publications

Supporting

Mentioning

114

Contrasting

Order By: Relevance

“…Frames contain a variable number of pulses, as a function of altitude and frequency. Dualfrequency modes (see previous section) transmit two closely spaced pulses at different frequencies receiving their echoes separately (Jordan et al, 2009 (Jordan et al, 2009). Further processing is required on ground, as the transmitted waveform is much longer than the required range resolution of 150 m in free space, corresponding to 1 μs in pulse width.…”

Section: Data Characteristicsmentioning

confidence: 99%

See 1 more Smart Citation

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Orosei

Jordan

Morgan

et al. 2015

Planetary and Space Science

Self Cite

View full text Add to dashboard Cite

Section: Data Characteristicsmentioning

confidence: 99%

“…In SS mode, MARSIS transmits a modulated waveform to achieve a range resolution equal to the inverse of the transmitted bandwidth, after processing on ground (Jordan et al, 2009). Such processing is called range compression, and consists in the correlation between the received echo and the transmitted waveform.…”

Section: Ground Data Processingmentioning

confidence: 99%

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Orosei

Jordan

Morgan

et al. 2015

Planetary and Space Science

Self Cite

View full text Add to dashboard Cite

“…The MARSIS instrument and techniques are introduced by several authors (e.g., Picardi et al, 2004;Gurnett et al, 2005;Jordan et al, 2009;Morgan et al, 2013). Nevertheless, we shall briefly describe the radar parameters and data records of the MARSIS radar in the AIS mode for ease of reference.…”

Section: Marsis Radar Parameters and Observationsmentioning

confidence: 99%

Topside of the martian ionosphere near the terminator: Variations with season and solar zenith angle and implications for the origin of the transient layers

Zhang

Orosei

Huang

et al. 2015

Icarus

View full text Add to dashboard Cite

a b s t r a c tIn this paper, the morphological variations of the M2 layer of the martian ionosphere with the martian seasons and solar zenith angle (SZA) at the terminator are investigated. The data used are the MARSIS (Mars Advanced Radar for Subsurface and Ionosphere Sounding) measurements (approximately 5000 ionograms) that were acquired from 2005 to 2012, which have a SZA P 85°and detect the topside transient layers. A simple, effective data inversion method is developed for the situation in which the upper portion of the height profile is non-monotonic and the observed data are insufficient for adequate reduction. The inverted parameters are subsequently explored using a statistical approach. The results reveal that the main body of the M2 layer (approximately 10 km below the first topside layer) can be well-characterized as a Chapman layer near the terminator (SZA = 85-98°), notwithstanding the high SZA and the presence of the topside layers. The height of the first topside layer tends to be concentrated approximately 60 km (with a standard deviation of $20 km) above the main density peak. The peak density and height of the first topside layer are positively correlated to the density and height of the main peak, respectively. The density and height of the first topside layer appear to be independent of the SZA, but possess seasonal variations that are similar to those of the main layer. The height of the topside layer is greater (by $10 km on average) in the southern spring and summer than in the southern autumn and winter, coinciding with the observation that, in the southern spring and summer, the underlying atmosphere is warmer due to dust heating (e.g., Smith, M.D. [2004]. Icarus 167,[148][149][150][151][152][153][154][155][156][157][158][159][160][161][162][163][164][165]. The statistical regularities of the parameters suggest a possibility that the formation of the topside layers are closely related to the processes of photoionization and diffusion that occur on the topside of the M2 layer. We propose that development of beam-plasma instabilities in the transitional region (between the lower Chapman region and the upper transport-dominating region) is possibly a mechanism that is responsible for the occurrences of the topside layers.

show abstract

“…In order to suppress the hyperbolic-pattern echoes caused by the off-nadir point reflectors, the multiple Doppler filters were implemented in MARSIS onboard the Mars Express (MEX) Jordan et al 2009). The frequency differences between the echo signals and the reference chirp signal depend on the ranges between spacecraft and targets, and the velocity of the spacecraft.…”

Section: Initial Results Of Radar Sounder Observationsmentioning

confidence: 99%

The Lunar Radar Sounder (LRS) Onboard the KAGUYA (SELENE) Spacecraft

et al. 2010

View full text Add to dashboard Cite

The Lunar Radar Sounder (LRS) onboard the KAGUYA (SELENE) spacecraft has successfully performed radar sounder observations of the lunar subsurface structures and passive observations of natural radio and plasma waves from the lunar orbit. After the transfer of the spacecraft into the final lunar orbit and antenna deployment, the operation of LRS started on hours worth of radar sounder data and 8961 hours worth of natural radio and plasma wave data have been obtained. It was revealed through radar sounder observations that there are distinct reflectors at a depth of several hundred meters in the nearside maria, which are inferred to be buried regolith layers covered by a basalt layer with a thickness of several hundred meters. Radar sounder data were obtained not only in the nearside maria but also in other regions such as the farside highland region and polar region. LRS also performed passive observations of natural plasma waves associated with interaction processes between the solar wind plasma and the moon, and the natural waves from the Earth, the sun, and Jupiter. Natural 146 T. Ono et al. radio waves such as auroral kilometric radiation (AKR) with interference patterns caused by the lunar surface reflections, and Jovian hectometric (HOM) emissions were detected. Intense electrostatic plasma waves around 20 kHz were almost always observed at local electron plasma frequency in the solar wind, and the electron density profile, including the lunar wake boundary, was derived along the spacecraft trajectory. Broadband noises below several kHz were frequently observed in the dayside and wake boundary of the moon and it was found that a portion of them consist of bipolar pulses. The datasets obtained by LRS will make contributions for studies on the lunar geology and physical processes of natural radio and plasma wave generation and propagation.

show abstract

The Mars express MARSIS sounder instrument

Cited by 150 publications

References 5 publications

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Topside of the martian ionosphere near the terminator: Variations with season and solar zenith angle and implications for the origin of the transient layers

The Lunar Radar Sounder (LRS) Onboard the KAGUYA (SELENE) Spacecraft

Contact Info

Product

Resources

About