Reproduction of Ground Magnetic Variations During the SC and the Substorm From the Global Simulation and Biot‐Savart's Law

Tanaka, Toshiaki; Ebihara, Yusuke; Watanabe, Masakazu; Den, Mitsue; Fujita, Shigeru; Kikuchi, Takashi; Hashimoto, Kumiko; Kataoka, Ryuho

doi:10.1029/2019ja027172

Cited by 15 publications

(37 citation statements)

References 33 publications

(74 reference statements)

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“…From the AU/AL magnitude, the numerically reproduced substorm is a medium-scale one. Above appearances of the simulated substorm have already been reported by and Tanaka et al (2020Tanaka et al ( , 2021.…”

Section: Resultssupporting

confidence: 73%

Development of the Substorm as a Manifestation of Convection Transient

et al. 2021

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Section: Resultssupporting

confidence: 73%

Development of the Substorm as a Manifestation of Convection Transient

et al. 2021

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“…The total number of grids in MHD calculation is 46,695,160, and the number of grids on the inner boundary is 122,882. The supplements in Tanaka et al (2020) gave visualizations of the grid system. It enables the use of a dense grid system avoiding grid accumulation points.…”

Section: Methods Of Numerical Simulationmentioning

confidence: 99%

Formation and Release of the Harang Reversal Relating With the Substorm Onset Process

et al. 2021

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With the interplanetary magnetic field (IMF) that turns from northward to southward, the global simulation successively reproduces the growth phase, the onset, and the expansion phase of the substorm. The calculated ionospheric convection for the growth phase reproduces the development of the Harang reversal (HR), the upward field‐aligned current (FAC), and the upcoming onset point as observed. Magnetic field lines traced from the center of the nightside upward FAC are open, while the magnetic field line traced from the onset point is closed. These open magnetic field lines map to flow shear just outside the O/C boundary. Seen from the magnetic configuration, the growth phase proceeds as the replacement process of nulls. Two new nulls appear on the dayside under the southward IMF, while two old nulls under the northward IMF retreat tailward forming two bifurcation regions on the dawn and dusk flanks. Flow shear around the O/C boundary forms by magnetospheric convection that returns to the dayside via bifurcation regions. The expansion phase proceeds through a topological change by the near‐earth neutral line (NENL). The NENL occurs inside the thinned structure of the northward IMF remnant, on the low‐latitude side of the flow shear, and projects down to the low‐latitude edge of the upward FAC. Associated with the NENL, the convection return path changes to the center of the plasma sheet and reveals in the ionosphere as the release of the HR. By the shrinkage of projecting magnetic field line, the O/C boundary migrates poleward in the ionosphere.

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“…The supporting information in Tanaka et al. (2020) shows the visualization of this grid system. The inner boundary of the calculation region is a sphere with a radius 6 R J , and the outer boundaries are X = 180 R J on the solar wind side, and X = −900 R J on the tail side.…”

Section: Simulation Methodsmentioning

confidence: 99%

Global Simulation of the Jovian Magnetosphere: Transitional Structure From the Io Plasma Disk to the Plasma Sheet

et al. 2021

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The structure and dynamics of the Jupiter's magnetosphere are very different from those of the earth. The planet's magnetic field is 14 times stronger than that of the earth. Such strong magnetic field and the dilute solar wind (Hanlon et al., 2004) result in the formation of a huge magnetosphere. In the Jovian magnetosphere, the average position of the bow shock is around 80 R J in front of the planet (Achilleos et al., 2004;Sarkango et al., 2019). The plasma sheet forms in the similar way as the Earth, but the plasma sheet mainly consists of plasma from the moon Io. The radius of Jupiter is 11 times larger than that of the Earth. The planetary rotation period is as short as 10 h. High-speed planetary rotation is also transmitted to Io plasma. The magnetic axis tilts about 10° from the rotation axis (Smyth et al., 2011). The shape of magnetic field deviates from the dipole, with an anomaly that provides a weak magnetic field region at high latitudes in the Northern Hemisphere (Hess et al., 2011).Io's orbit is at 5.95 R J , where neutral gas is released. Diffusing gas is ionized, then about half is picked up by rotating magnetic field. The amount of plasma supplied from Io is 0.26-1.4 t/sec (Delamere & Bagenal, 2003). The plasma components from Io are O + , O ++ , S + , S ++ , S +++ , and Na + (Bodish et al., 2017;Kim et al., 2020). This Io source plasma plays a major role in constructing the inner magnetosphere, in forming the magnetosphere-ionosphere (M-I) coupling system. Io plasma forms the plasma disk in the inner magnetosphere (<15 R J ), and the plasma sheet in the middle tail (20 R J ∼ 60 R J ). Io source plasma is predominant over these regions (Cohen et al., 2001;Radioti et al., 2005). In the distant tail (>600 R J ), plasma originating from the solar wind is predominant (McComas et al., 2017).In the inner magnetosphere, Io plasma accumulates and becomes unstable when the density exceeds a certain level (Southwood & Kivelson, 1987). Through the interchange instability possibly caused by the

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Reproduction of Ground Magnetic Variations During the SC and the Substorm From the Global Simulation and Biot‐Savart's Law

Cited by 15 publications

References 33 publications

Development of the Substorm as a Manifestation of Convection Transient

Development of the Substorm as a Manifestation of Convection Transient

Formation and Release of the Harang Reversal Relating With the Substorm Onset Process

Global Simulation of the Jovian Magnetosphere: Transitional Structure From the Io Plasma Disk to the Plasma Sheet

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