Diamagnetic depression observations at Saturn's magnetospheric cusp by the Cassini spacecraft

Jasinski, Jamie M.; Arridge, C. S.; Coates, A. J.; Jones, G. H.; Sergis, N.; Thomsen, M. F.; Krupp, N.

doi:10.1002/2016ja023738

Cited by 11 publications

(10 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The dense cusp plasma in the magnetosphere causes diamagnetic effects where a depression in the magnetic field is observed. Similar depressions in the outer magnetospheric cusp at Saturn have also been observed (Jasinski et al 2017a).…”

Section: The Cuspsupporting

confidence: 80%

Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2

et al. 2022

Self Cite

View full text Add to dashboard Cite

The “pole-on” configuration occurs when the polar magnetosphere of a planet is directed into the solar wind velocity vector. Such magnetospheric configurations are unique to the ice giant planets. This means that magnetic reconnection, a process that couples a magnetosphere to the solar wind, will be different at the ice giants when they are pole-on compared to other planets. The only available in situ measurements of a pole-on magnetosphere are from the Neptune flyby by Voyager 2, which we analyze in this paper. We show that dayside magnetopause conditions were conducive to magnetic reconnection. A plasma depletion layer in the magnetosheath adjacent to the magnetopause was observed. Plasma measurements inside the magnetospheric cusp show evidence of multiple reconnection taking place at the magnetopause before the spacecraft crossed the open–closed field line boundary. A possible traveling compression region from a nearby passing flux rope was also observed, providing further supporting evidence that multiple X-line reconnection occurred during the flyby. During a perfectly pole-on configuration, reconnection will not depend on the orientation of the interplanetary magnetic field, as is the case at other planetary magnetospheres. The rate of reconnection will not vary because the area of the dayside magnetopause where antiparallel shears occur will be approximately equal for all interplanetary magnetic field orientations. Therefore, we suggest that rotating into and out of the pole-on configuration will likely drive the “on–off”/“switch-like” dynamics observed in simulations. Consequently, the pole-on configuration is most likely an important rotational phase for driving ice giant magnetospheric dynamics.

show abstract

Section: The Cuspsupporting

confidence: 80%

Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…Using the magnetic and plasma pressures we can then estimate the plasma‐β (i.e. the plasma to magnetic pressure ratio) by taking averages of 1, 5, 10, and 15 min for MAG, ELS, MIMI, and IMS data, respectively (method previously used by Masters et al., 2012 and Jasinski, 2015). The plasma‐β for this magnetopause crossing is shown to be ∼4 in the magnetosheath and ∼1 in the magnetosphere.…”

Section: Observations and Analysismentioning

confidence: 99%

Flux Transfer Events at a Reconnection‐Suppressed Magnetopause: Cassini Observations at Saturn

et al. 2021

Self Cite

View full text Add to dashboard Cite

show abstract

“…This current could represent the dayside cusp. Saturn's cusp has been observed at approximately the same location in individual passes using magnetic field and plasma instruments (Jasinski et al, 2014(Jasinski et al, , 2016(Jasinski et al, , 2017.…”

Section: 1029/2018ja026284mentioning

confidence: 99%

Three‐Dimensional Currents in Saturn's Magnetosphere

Carbary

2019

JGR Space Physics

View full text Add to dashboard Cite

Observations of Saturn's magnetic field from July 2004 to December 2016 have been combined to allow a numerical calculation of ∇ × B throughout the magnetosphere, thus permitting the first global mapping of Saturn's currents in three dimensions. The azimuthal ring current Jϕ dominates the magnetospheric currents, peaking near the orbit of the moon Rhea and having a total magnitude of over 10 mega‐Amperes integrated within the L‐shell of Titan. In meridional cross section, the ring current has a teardrop shape rather than a block shape. Jϕ also has a noticeable local time asymmetry, being the largest in the midnight and dawn sectors. The meridional currents Jρ and Jz are smaller than the ring current by an order of magnitude; they flow radially outward near the equator and return at higher latitudes in a looping pattern reminiscent of Hadley cell atmospheric convection. There are two such loops: one in the northern hemisphere and one in the south, flowing in opposing directions. In the noon sector, a strong Jz current may indicate the dayside cusp.

show abstract

Diamagnetic depression observations at Saturn's magnetospheric cusp by the Cassini spacecraft

Cited by 11 publications

References 61 publications

Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2

Neptune’s Pole-on Magnetosphere: Dayside Reconnection Observations by Voyager 2

Flux Transfer Events at a Reconnection‐Suppressed Magnetopause: Cassini Observations at Saturn

Three‐Dimensional Currents in Saturn's Magnetosphere

Contact Info

Product

Resources

About