MAVEN observations of magnetic flux ropes with a strong field amplitude in the Martian magnetosheath during the ICME passage on 8 March 2015

Hara, Takuya; Luhmann, J. G.; Halekas, J. S.; Espley, J. R.; Seki, K.; Brain, David; Hasegawa, Hiroshi; McFadden, J. P.; Mitchell, David; Mazelle, C.; Harada, Yuki; Livi, R.; DiBraccio, G. A.; Connerney, J. E. P.; Andersson, L.; Jakosky, B. M.

doi:10.1002/2016gl068960

Cited by 15 publications

(12 citation statements)

References 52 publications

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“…For example, their observed duration is about several tens of seconds with a peak field ranging between ∼10 and 25 nT. Multiple ion species including H + , O + , and O + 2 are simultaneously recorded during their encounters that is consistent with the previous MAVEN observations [Hara et al, , 2016[Hara et al, , 2017. However, it should be noted that the flux ropes with ≥ 60 ∘ tend to be observed in a series of multiple flux rope signatures across a single magnetotail current sheet as shown in Figure 3.…”

Section: Statistical Resultssupporting

confidence: 83%

On the origins of magnetic flux ropes in near‐Mars magnetotail current sheets

Hara

Harada

Mitchell

et al. 2017

Geophysical Research Letters

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We analyze Mars Atmosphere and Volatile EvolutioN (MAVEN) observations of magnetic flux ropes embedded in Martian magnetotail current sheets, in order to evaluate the role of magnetotail reconnection in their generations. We conduct a minimum variance analysis to infer the generation processes of magnetotail flux ropes from the geometrical configuration of the individual flux rope axial orientation with respect to the overall current sheet. Of 23 flux ropes detected in current sheets in the near‐Mars (∼1–3 Martian radii downstream) magnetotail, only 3 (possibly 4) can be explained by the magnetotail reconnection scenario, while the vast majority of the events (19 events) are more consistent with flux ropes that are originally generated in the dayside ionosphere and subsequently transported into the nightside magnetotail. The mixed origins of the detected flux ropes imply complex nature of generation and transport of Martian magnetotail flux ropes.

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Section: Statistical Resultssupporting

confidence: 83%

On the origins of magnetic flux ropes in near‐Mars magnetotail current sheets

Hara

Harada

Mitchell

et al. 2017

Geophysical Research Letters

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“…The plasma β ; the ratio of the plasma pressure relative to the magnetic pressure, can be computed to be approximately 0.3 across the structure. This feature is consistent with previous flux rope events detected by MAVEN [ Hara et al , , ].…”

Section: Maven Observations Of a Giant Ionospheric Flux Ropesupporting

confidence: 93%

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

et al. 2017

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We present Mars Atmosphere and Volatile EvolutioN (MAVEN) observations of a giant magnetic flux rope in the Martian dayside ionosphere. The flux rope was observed at an altitude of <300 km, downstream from strong subsolar crustal magnetic fields. The peak field amplitude was ∼200 nT, resulting in the largest difference between the observed magnetic field strength and a model for crustal magnetic fields of the entire MAVEN primary science phase. MAVEN detected planetary ions, including H+, O+, and O2+, across the structure. The axial orientation estimated for the flux rope indicates that it likely formed as a result of interactions between the local crustal and overlaid draped interplanetary magnetic fields. Pitch angle distributions of ionospheric photoelectrons imply that this structure is connected to the Martian upper atmosphere. However, the flux rope is not present in observations at the next commensurable orbit crossing (approximately two Martian days later), implying that it eventually detaches from the atmosphere and is carried downstream. The flux rope observations occurred during an interplanetary coronal mass ejection event at Mars, suggesting that the disturbed upstream state played a role in allowing the interplanetary magnetic field to penetrate deeper into the Martian ionosphere than is typical, allowing the formation of the flux rope.

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“…[] analyzed MAVEN magnetic field and electron data to assess the complex field topology in the tail, suggesting that the Martian magnetotail configuration appears to be a hybrid between induced and intrinsic magnetospheres. MAVEN has also made great progress in terms of the tail plasma dynamics: tailward escape of planetary ions has been observed in the form of plasma clouds [ Halekas et al ., ], detached magnetic flux ropes [ DiBraccio et al ., ; Hara et al ., , ], bulk acceleration due to magnetic reconnection [ Harada et al ., ], and the tailward transport of suprathermal (>25 eV) planetary ions [ Brain et al ., ; Dong et al ., ; Harada et al ., ].…”

Section: Introductionmentioning

confidence: 99%

“…TAIL CURRENT SHEET FLAPPING AT MARS 4308 of the tail plasma dynamics: tailward escape of planetary ions has been observed in the form of plasma clouds [Halekas et al, 2016], detached magnetic flux ropes [DiBraccio et al, 2015;Hara et al, , 2016, bulk acceleration due to magnetic reconnection [Harada et al, 2015a], and the tailward transport of suprathermal (>25 eV) planetary ions Dong et al, 2015;Harada et al, 2015b].…”

Section: Introductionmentioning

confidence: 99%

MAVEN observations of tail current sheet flapping at Mars

et al. 2017

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The Martian magnetotail is a complex regime through which atmospheric particles are lost to space. Our current understanding of Mars' tail continues to develop with the comprehensive particle and field data collected by Mars Atmosphere and Volatile EvolutioN (MAVEN). In this work, we identify periods when MAVEN encounters multiple current sheet crossings through a single tail traversal in order to understand tail dynamics. We apply an analysis technique that has been developed and validated by using multipoint measurements in order to separate the spatial and temporal properties associated with current sheet flapping. Events are classified into periods of steady flapping, due to a global motion of the current sheet, and kink‐like flapping, resulting from localized wave propagation along the tail current sheet. Out of 106 periods during which multiple current sheet crossings were observed, 20 were due to steady flapping and 10 from kink‐like flapping. A majority of the kink‐like events resulted from waves propagating in the opposite direction of the solar wind convection electric field, regardless of their location in the tail, unlike at Earth and Venus. This finding suggests that possible magnetosphere energy sources, whereby plasma is accelerated and removed from the Martian environment, are not located in the central magnetotail; rather, these waves may be driven by a source located at the tail flank based on the direction of the solar wind electric field. Therefore, by identifying potential sources of impulsive energy release in the tail, we may better understand mechanisms that drive atmospheric loss at Mars.

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MAVEN observations of magnetic flux ropes with a strong field amplitude in the Martian magnetosheath during the ICME passage on 8 March 2015

Cited by 15 publications

References 52 publications

On the origins of magnetic flux ropes in near‐Mars magnetotail current sheets

On the origins of magnetic flux ropes in near‐Mars magnetotail current sheets

MAVEN observations of a giant ionospheric flux rope near Mars resulting from interaction between the crustal and interplanetary draped magnetic fields

MAVEN observations of tail current sheet flapping at Mars

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