Magnetotail boundary crossings at lunar distances: ARTEMIS observations

Iklim Gencturk Akay*, Zerefşan Kaymaz, David G. Sibeck

*Bu çalışma için yazışmadan sorumlu yazar

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5 Atıf (Scopus)

Özet

We compare results from a preliminary analysis of two years of ARTEMIS magnetopause boundary crossings at lunar distances with available empirical models. We remove the effects of variable solar wind flow directions and aberration angles to study the magnetotail cross-section as a function of solar wind conditions. The average magnetopause distance from the central axis is 26 RE, but this distance ranges from 10 RE for high solar wind dynamic pressures and strong northward IMF orientations to 39 RE for low solar wind dynamic pressures and weak southward IMF orientations compared to the nominal solar wind conditions. The time-independent Howe and Binsack (1972) model describes the average location of the crossings very well. For high solar wind dynamic pressures, the Lu et al., (2011) model performs best, while for low pressures the Petrinec and Russell (1996) model gives the closest prediction. As predicted by theory and seen in past studies, the magnetotail cross-section is suggestive of prolate during intervals of strong IMF By, but oblate during intervals of strong IMF Bz. Any asymmetric variation of the tail boundary with respect to the sign of IMF By was not observed. The decreasing size of boundary with the increasing dynamic pressure was found when dynamic pressures are smaller than 2 nPa. Although the scatter is larger, the tail size for pressures larger than 2 nPa suggests a constant radius. The tail boundary size decreases as the strength of IMF Bz increases regardless of its polarity. However, it was also observed that an even stronger southward IMF Bz can cause larger magnetopause size in the presence of large dynamic pressures.

Orijinal dilİngilizce
Sayfa (başlangıç-bitiş)45-60
Sayfa sayısı16
DergiJournal of Atmospheric and Solar-Terrestrial Physics
Hacim182
DOI'lar
Yayın durumuYayınlandı - Oca 2019

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Publisher Copyright:
© 2018 Elsevier Ltd

Finansman

This work was supported by Turkish Scientific and Technological Research Council (TÜBİTAK) Project 113Y213 and also partially by the Istanbul Technical University Research Fund ( ITU-BAP2013 Project 37239 ). Work at GSFC was supported by the THEMIS project. We would like to acknowledge the PIs of the magnetic field (MFI) and plasma (SWE) instruments on board of ARTEMIS , ACE and WIND spacecraft. We especially would like to thank Dr. Adam Szabo at NASA/GSFC, Dr. R. Skoug at Los Alamos, and Dr. D. McComas at Princeton University for their help in clarifying the SWE data from WIND and ACE. In addition, we thank the supporters of CDAWeb for maintaining the web site. We also would like to thank both referees for their valuable comments that improved our manuscript.

FinansörlerFinansör numarası
Turkish Scientific and Technological Research Council
TÜBİTAK113Y213
Istanbul Teknik Üniversitesi37239, ITU-BAP2013

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