Solar forcing and planetary ion escape from Mars

Lundin, R.; Barabash, S. V.; Fedorov, A.; Holmström, M.; Nilsson, Hans; Sauvaud, J. A.; Yamauchi, M.

doi:10.1029/2007gl032884

Cited by 88 publications

(118 citation statements)

References 20 publications

(23 reference statements)

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“…We compare the obtained solar wind dependence of ion escape fluxes with observations. Lundin et al (2008) suggested that there is a strong correlation between the solar wind dynamic pressure and the planetary ion loss rate. They focused on the heavy ions in the energy range of 30-800 eV, and reported that the total escape flux increases from 6.0 × 10 23 to 6.0 × 10 24 s −1 as the solar wind pressure increases from 0.1 to 10 times the nominal value.…”

Section: Discussion and Summarymentioning

confidence: 99%

IMF-induced escape of molecular ions from the Martian ionosphere

et al. 2013

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Since Mars does not possess a significant global intrinsic magnetic field, the solar wind interacts directly with the Martian ionosphere and can induce ion escapes from it. Phobos-2 and recent Mars Express (MEX) observations have shown that the escaping ions are O⁺ as well as molecular O₂⁺ and CO₂⁺. While O⁺ escape can be understood by the ion pick-up of non-thermal O corona extended around the planet, regarding the heavy molecular O₂⁺ and CO₂⁺, which are buried in the lower ionosphere, a novel escape mechanism needs to considered. Here we attack this problem by global magnetohydrodynamic (MHD) simulations. First, we clarify the global structure of the streamlines that result from the interaction with the solar wind. Then, by focusing on the streamlines that dip into the low-altitude part of the dayside ionosphere, we investigate the escape path of the molecular ions. The effects of the interplanetary magnetic field (IMF) on the molecular ion escape process are investigated by comparing the results with and without IMF. IMF has little effect on O⁺ escape via ion pick-up mediated by solar wind electron impact ionization of the O corona. O₂⁺ and CO₂⁺ are shoveled from the low-altitude regions of the dayside ionosphere by magnetic tension in the presence of IMF. These ions are pulled by the U-shaped field lines to the north and south poles, and at the terminator, they are concentrated in the noon–midnight meridian plane. These ions remain confined to the noon–midnight plane as they are transported to the nightside to form the tail ray. Then they escape along the streamlines open to the interplanetary space. Under a typical solar wind and IMF condition expected at Mars, O⁺, O₂⁺ and CO₂⁺ escape fluxes are 8.0 × 10²³, 3.5 × 10²³ and 5.0 × 10²² ion s⁻¹, respectively, which are in good agreement with the MEX observations

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Section: Discussion and Summarymentioning

confidence: 99%

IMF-induced escape of molecular ions from the Martian ionosphere

et al. 2013

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“…The main mechanisms at work are (Chassefiere & Leblanc 2004;Lundin et al 2007;Lilensten et al 2013): (a) photochemical escape, or dissociative recombination in which the ions produced by UV photoionization, electron impact and charge exchange with the solar wind protons, recombine generating escaping energetic neutrals; (b) pickup ion escape where the ions produced by photoionization are picked up by the solar wind; (c) atmospheric sputtering leading to exospheric neutrals undergoing collisions with energetic ions (mainly O + , initially formed from exospheric photoionization, being picked up and swept away by the solar wind magnetic lines, and finally re-impacting the exobase, provoking secondary escape); (d) hydrodynamic escape (escaping light neutrals transferring momentum to heavier species), particularly during the Early Noachian era (Chassefiere & Leblanc 2004). Therefore, the atmospheric escape at Mars has a strong connection to the solar activity (Luhmann et al 1987;Lundin et al 2008), since the solar EUV flux creates ions that can diffuse through the atmosphere and be picked up by the solar wind. In particular, the EUV solar flux has a strong influence on the atmospheric escape through two main mechanisms: (a) it ionizes and dissociates CO 2 to form CO 2 + , CO + , O + and some minor species such as CO ++ and C + ; these daughter-ions are lighter than the neutral CO 2 and diffuse upward, where a part of them gets picked up by the solar wind; (b) being unstable and highly energetic (i.e.…”

Section: Space Weather At Mars and Venusmentioning

confidence: 99%

“…ASPERA on-board the ESA Mars Express probe (e.g. Lundin et al 1990) showed that Mars is still experiencing atmospheric escape (Dubinin et al 2008), with an escape flux ranging between 2 · 10 24 ions per sec and 3 · 10 25 ions per sec (Lundin et al 1990;Lundin et al 2008;Nilsson et al 2011).…”

Section: Space Weather At Mars and Venusmentioning

confidence: 99%

Planetary space weather: scientific aspects and future perspectives

Plainaki

Lilensten

Radioti

et al. 2016

J. Space Weather Space Clim.

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In this paper, we review the scientific aspects of planetary space weather at different regions of our Solar System, performing a comparative planetology analysis that includes a direct reference to the circum-terrestrial case. Through an interdisciplinary analysis of existing results based both on observational data and theoretical models, we review the nature of the interactions between the environment of a Solar System body other than the Earth and the impinging plasma/radiation, and we offer some considerations related to the planning of future space observations. We highlight the importance of such comparative studies for data interpretations in the context of future space missions (e.g. ESA JUICE; ESA/JAXA BEPI COLOMBO). Moreover, we discuss how the study of planetary space weather can provide feedback for better understanding the traditional circumterrestrial space weather. Finally, a strategy for future global investigations related to this thematic is proposed.

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“…Ion sputtering: exospheric neutrals undergo collisions with energetic ions, picked up and swept away by solar wind magnetic lines, and finally re-impacting the high atmosphere. Mars' atmospheric escape has a strong connection to solar activity (Luhmann et al 1987;Lundin et al 2008): the solar EUV flux creates ions that can diffuse through the atmosphere and are taken away in the solar wind. An additional phenomenon may increase escape: the ions are sensitive to the interplanetary magnetic field and will spiral about the magnetic field lines.…”

Section: A Mixed Particle/radiation Effect: Atmospheric Escape-the Camentioning

confidence: 99%

What characterizes planetary space weather?

Lilensten

Coates

Déhant

et al. 2014

Astron Astrophys Rev

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Space weather has become a mature discipline for the Earth space environment. With increasing efforts in space exploration, it is becoming more and more necessary to understand the space environments of bodies other than Earth. This is the background for an emerging aspect of the space weather discipline: planetary space weather. In this article, we explore what characterizes planetary space weather, using some examples throughout the solar system. We consider energy sources and timescales, the characteristics of solar system objects and interaction processes. We

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Solar forcing and planetary ion escape from Mars

Cited by 88 publications

References 20 publications

IMF-induced escape of molecular ions from the Martian ionosphere

IMF-induced escape of molecular ions from the Martian ionosphere

Planetary space weather: scientific aspects and future perspectives

What characterizes planetary space weather?

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