Evolution of a typical ion-scale magnetic flux rope caused by thermal pressure enhancement
2017 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 122, no 2, 2040-2050 p.Article in journal (Refereed) Published
With high time-resolution field and plasma measurements by the Magnetospheric Multiscale spacecraft, interior fine structures of two ion-scale magnetic flux ropes (similar to 5 and similar to 11 ion inertial length radius) separated by similar to 14 s are resolved. These two ion-scale flux ropes (FR1 and FR2) show non-frozen-in ion behavior and consist of a strong axial magnetic field at the reversal of the negative-then-positive bipolar field component. The negative bipolar field component of the FR2 is found to be depressed, where magnetic pressure and total pressure decrease, but ion and electron thermal pressures increase, a feature akin to a crater-like flux rope. The pressure enhancement is due to the magnetosheath plasma feeding into the flux rope along the field lines. Magnetic field draping and energetic electrons are also observed in the trailing part of the FR2. The ratio of perpendicular and parallel currents indicates that the FR1 appears force-free but the FR2 seems not. Moreover, the FR2 is time-dependent as a result of a low correlation coefficient (CC = 0.75) for the derivation of the deHoffmann-Teller frame using the direct measured electric fields, while the FR1 is in quasi-steady conditions (CC = 0.94). It is concluded that the crater formation within the FR2 can be interpreted by the analytical flux rope simulation as the evolution of typical flux rope to crater-like one due to the thermal pressure enhancement, which could be induced by the depression of transverse magnetic fields of the flux rope.
Place, publisher, year, edition, pages
AMER GEOPHYSICAL UNION , 2017. Vol. 122, no 2, 2040-2050 p.
Fusion, Plasma and Space Physics
IdentifiersURN: urn:nbn:se:kth:diva-205142DOI: 10.1002/2016JA023777ISI: 000397022900042ScopusID: 2-s2.0-85014159604OAI: oai:DiVA.org:kth-205142DiVA: diva2:1088467
QC 201704122017-04-122017-04-122017-04-12Bibliographically approved