Dayside induced magnetic field in the ionosphere of Mars

Akalin, F.; Morgan, D. D.; Gurnett, D. A.; Kirchner, D. L.; Brain, David; Modolo, Ronan; Acuña, M. H.; Espley, J. R.

doi:10.1016/j.icarus.2009.03.021

Cited by 50 publications

(59 citation statements)

References 14 publications

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“…The time difference between these horizontal lines is used to calculate the magnitude of the local magnetic field [Gurnett et al, 2008;Akalin et al, 2010].…”

Section: Mhzmentioning

confidence: 99%

“…When an ionospheric profile is visible, the peak ionospheric density can be identified. MARSIS is also able to obtain the local density and the magnitude of the local magnetic field through local electron plasma frequency harmonics and electron cyclotron echoes observed on the ionograms, which are plots of echo intensity as a function of time delay and frequency [Gurnett et al, 2005;Duru et al, 2008;Akalin et al, 2010]. In remote sounding, a short radio pulse with frequency f is emitted and the time delay of the returning echo is measured.…”

Section: Introductionmentioning

confidence: 99%

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Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

Duru

Gurnett

Morgan

et al. 2017

Planetary and Space Science

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Key points:Solar activity in a two week period starting from 25 February 2015 altered the conditions in the Martian ionosphere.The solar wind conditions and nightside ionosphere of Mars are studied simultaneously, with MAVEN, MEX and Mars Odyssey.High ion escape rates and enhanced densities are observed during SEP enhancements and ICME. Atmosphere and Volatile Evolution Mission (MAVEN), and Mars Odyssey (MO). The ICME disturbances were characterized by an increase in ion speed, plasma temperature, magnetic field magnitude, and energetic electron flux. Furthermore, increased solar wind density and speeds, unusually high local electron densities and high flow velocities were detected on the nightside at high altitudes during the March 8 th event. These effects are thought to be due to the transport of ionospheric plasma away from Mars. The peak electron density at periapsis shows a substantial increase, reaching number densities about 2.7 x 10 4 cm -3 during the second ICME in the deep nightside, which corresponds to an increase in the MOHigh-Energy Neutron Detector flux, suggesting an increase in the ionization of the neutral atmosphere due to the high intensity of charged particles. SEPs show a substantial enhancement before the shock of fourth ICME causing impact ionization and absorption of the surface echo intensity which drops to the noise levels. Moreover, the peak ionospheric density exhibits a discrete enhancement over a period of about 30 hrs around the same location, which maybe due to impact ionization. Ion escape rates at this time are calculated to be in the order of 10 25 -10 26 s -1 , consistent with MAVEN results, but somewhat higher.

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“…The time difference between these horizontal lines is used to calculate the magnitude of the local magnetic field [Gurnett et al, 2008;Akalin et al, 2010].…”

Section: Mhzmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

Duru

Gurnett

Morgan

et al. 2017

Planetary and Space Science

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“…The electron echoes and the resulting magnetic field strengths were first used en masse by Akalin et al (2010) to map the field strength as a function of altitude and solar zenith angle. The data are taken manually using an adjustable scale on a computer monitor with the visual ionogram displayed, exactly the same as with the plasma frequency harmonics.…”

Section: Ground Data Processingmentioning

confidence: 99%

“…3 were first explained by Gurnett et al (2005) and Gurnett et al (2008). Statistical results from these data were given by Akalin et al (2010). An example is shown in Fig.…”

Section: Local Magnetic Field Strength From the Electron Cyclotron Ecmentioning

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

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“…The induced magnetic field has been measured at Mars by the Mars Global Surveyor orbiter [Brain et al, 2003] and the Mars Express orbiter [Akalin et al, 2010]. These authors show that the induced magnetic field is mainly horizontal; its strength decreases with increasing altitude and with increasing solar zenith angle.…”

Section: Numerical Modelmentioning

confidence: 99%

He²⁺ transport in the Martian upper atmosphere with an induced magnetic field

et al. 2013

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[1] Solar wind helium may be a significant source of neutral helium in the Martian atmosphere. The precipitating particles also transfer mass, energy, and momentum. , and the energy flux is equal to 9-10 Â 10 -3 erg cm -2 s -1. The calculations of the upward flux have been made for the Martian atmosphere during solar minimum. It was found, that if the induced magnetic field is not introduced in the simulations the precipitating He 2+ ions are not backscattered at all by the Martian upper atmosphere. If we include a 20 nT horizontal magnetic field, a typical field measured by Mars Global Surveyor in the altitude range of 85-500 km, we find that up to 30%-40% of the energy flux of the precipitating He 2+ ions is backscattered depending on the velocity distribution of the precipitating particles. We thus conclude that the induced magnetic field plays a crucial role in the transport of charged particles in the upper atmosphere of Mars and, therefore, that it determines the energy deposition of the solar wind.

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Dayside induced magnetic field in the ionosphere of Mars

Cited by 50 publications

References 14 publications

Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

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

He²⁺ transport in the Martian upper atmosphere with an induced magnetic field

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Dayside induced magnetic field in the ionosphere of Mars

Cited by 50 publications

References 14 publications

Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

Response of the Martian ionosphere to solar activity including SEPs and ICMEs in a two-week period starting on 25 February 2015

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

He2+ transport in the Martian upper atmosphere with an induced magnetic field

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He²⁺ transport in the Martian upper atmosphere with an induced magnetic field