Solar cycle variation of ion escape from Mars

Nilsson, Hans; Zhang, Qi; Wieser, Gabriella Stenberg; Holmström, Mats; Barabash, S.; Futaana, Yoshifumi; Fedorov, A.; Persson, Moa; Wieser, Martin

doi:10.1016/j.icarus.2021.114610

Cited by 19 publications

(33 citation statements)

References 66 publications

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“…Our results are also consistent with previous studies that positively correlate net escape and solar activity level at Mars (e.g., Y. Dong et al, 2017;Dubinin et al, 2017;Nilsson et al, 2021;Ramstad et al, 2015).…”

Section: Influence Of Solar Activity Levelsupporting

confidence: 93%

“…For this event, the net sunward flux of O + and O 2 + is about 6.4 × 10 5 and 4.8 × 10 5 cm −2 s −1 respectively, which is about one order of magnitude lower than the average observed escape flux in the magnetotail (on the order of 10 6 cm −2 s −1 ) (e.g., Brain et al., 2015; Inui et al., 2019; Nilsson et al., 2011, 2021).…”

Section: Case Studymentioning

confidence: 79%

“…In this study, we have removed all known types these noise contaminations by following the same method as in Nilsson et al. (2010, 2011, 2012, 2021).…”

Section: Methodsmentioning

confidence: 99%

“…In addition, solar ultraviolet (UV), and the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) which was onboard the Mars Express also affect ion measurements (Voshchepynets et al, 2018). In this study, we have removed all known types these noise contaminations by following the same method as in Nilsson et al (2010Nilsson et al ( , 2011Nilsson et al ( , 2012Nilsson et al ( , 2021.…”

Section: Moment Calculationmentioning

confidence: 99%

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Mars‐Ward Ion Flows in the Martian Magnetotail: Mars Express Observations

Zhang

Futaana

Nilsson

et al. 2022

Geophysical Research Letters

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Section: Influence Of Solar Activity Levelsupporting

confidence: 93%

Section: Case Studymentioning

confidence: 79%

“…In this study, we have removed all known types these noise contaminations by following the same method as in Nilsson et al. (2010, 2011, 2012, 2021).…”

Section: Methodsmentioning

confidence: 99%

Section: Moment Calculationmentioning

confidence: 99%

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Mars‐Ward Ion Flows in the Martian Magnetotail: Mars Express Observations

Zhang

Futaana

Nilsson

et al. 2022

Geophysical Research Letters

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“…The draped IMF is stretched by the solar wind and slips into the wake to form an elongated induced magnetotail (e.g., Acuña et al., 1998; Luhmann et al., 2004; Ma et al., 2002; McComas et al., 1986). Researchers realize that most of the planetary ions escape to interplanetary space via the electromagnetic force, for example, the solar wind electric fields ( E ), the hall electric fields, and the ambipolar electric fields (e.g., Barabash et al., 2007; C. Zhang et al., 2021; Dubinin & Fraenz, 2015; Dubinin et al., 2011; Futaana et al., 2017; Lundin, 2011; Nilsson et al., 2021); therefore, knowledge of the magnetic field structure around the Mars is vital for understanding associated magnetospheric processes (e.g., the escape of planetary ions).…”

Section: Introductionmentioning

confidence: 99%

Three‐Dimensional Configuration of Induced Magnetic Fields Around Mars

et al. 2022

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Using over 6 years of magnetic field data (October 2014–December 2020) collected by the Mars Atmosphere and Volatile EvolutioN, we conduct a statistical study on the three‐dimensional average magnetic field structure around Mars. We find that this magnetic field structure conforms to the pattern typical of an induced magnetosphere, that is, the interplanetary magnetic field (IMF) which is carried by the solar wind and which drapes, piles up, slips around the planet, and eventually forms a tail in the wake. The draped field lines from both hemispheres along the direction of the solar wind electric field (E) are directed toward the nightside magnetic equatorial plane, indicating that they are “sinking” toward the wake. These “sinking” field lines from the +E‐hemisphere (E pointing away from the plane) are more flared and dominant in the tail, while the field lines from the –E‐hemisphere (E pointing toward) are more stretched and “pinched” toward the plasma sheet. Such highly “pinched” field lines even form a loop over the pole of the –E‐hemisphere. The tail current sheet also shows an E‐asymmetry: the sheet is thicker with a stronger tailward trueJ→×trueB→ $\overrightarrow{J}\times \overrightarrow{B}$ force at +E‐flank, but much thinner and with a weaker trueJ→×trueB→ $\overrightarrow{J}\times \overrightarrow{B}$ (even turns sunward) at –E‐flank. Additionally, we find that IMF Bx can induce a kink‐like field structure at the boundary layer; the field strength is globally enhanced and the field lines flare less during high dynamic pressure.

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Sunward Ion Flows in the Martian Magnetotail: Mars Express Observations

Zhang

Futaana

Nilsson

et al. 2022

Preprint

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We investigate sunward planetary ions in the Martian magnetotail that potentially reduce the amount of escaping ions. The global properties of sunward flows in the Martian magnetotail are characterized, based on over 13-years of ion data (May 2007-December 2020) collected by the ASPERA-3 instrument on Mars Express. We find that sunward flows mainly occur in the vicinity of the crustal fields, implying that crustal fields may play a key role in producing such flows. The occurrence rate and sunward flux are higher during solar maximum rather than solar minimum. However, we identify a relatively low occurrence rate of sunward flows and low sunward flux, suggesting that sunward flows have negligible influence on total ion escape at Mars. This is different from those at Venus, where sunward flows can significantly decrease the total escape rates of ions.

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Solar cycle variation of ion escape from Mars

Cited by 19 publications

References 66 publications

Mars‐Ward Ion Flows in the Martian Magnetotail: Mars Express Observations

Mars‐Ward Ion Flows in the Martian Magnetotail: Mars Express Observations

Three‐Dimensional Configuration of Induced Magnetic Fields Around Mars

Sunward Ion Flows in the Martian Magnetotail: Mars Express Observations

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