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M K Dougherty - One of the best experts on this subject based on the ideXlab platform.
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survey of saturn s magnetopause and bow shock positions over the entire Cassini Mission boundary statistical properties and exploration of associated upstream conditions
Journal of Geophysical Research, 2019Co-Authors: C M Jackman, M F Thomsen, M K DoughertyAbstract:The Cassini spacecraft orbited the planet Saturn from July 2004 to September 2017, and its varied orbital trajectory took it across the magnetopause and bow shock boundaries multiple times, at varying radial distances, local times, latitudes, and phases of the solar cycle. Here we present a comprehensive list of these boundary crossings, derived primarily using data from the Cassini magnetometer instrument, with cross‐validation against the electron spectrometer data where available. There are a multitude of scientific avenues for exploitation of this list. In this work, we examine the variability in boundary location and use the crossing times in concert with models of the bow shock and magnetopause to infer the upstream solar wind dynamic pressure at the times of crossings. This analysis allows us to understand the limitations of the Cassini trajectory for studying boundary physics under a range of solar wind driving conditions. In addition, rapid traversals of the magnetosheath are used to estimate the range of speeds of boundary motion.
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currents associated with saturn s intra d ring azimuthal field perturbations
Journal of Geophysical Research, 2019Co-Authors: G J Hunt, S W H Cowley, G Provan, M K Dougherty, E J Bunce, Hao Cao, D J SouthwoodAbstract:During the final 22 full revolutions of the Cassini Mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low‐latitude current system via the associated azimuthal perturbation field peaking typically at ~10‐30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field‐aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field‐aligned current densities above the ionosphere are typically ~5‐10 nA m^(‐2), more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field‐aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north‐south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller‐scale structures, possibly due to rapid temporal or local time variations.
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variability of intra d ring azimuthal magnetic field profiles observed on Cassini s proximal periapsis passes
Journal of Geophysical Research, 2019Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Work at the University of Leicester was supported by STFC grant ST/N000749/1. Work at Imperial College was supported by STFC grant ST/N000692/1. EJB was supported by a Royal Society Wolfson Research Merit Award. MKD was supported by Royal Society Research Professorship RP140004. TJB was supported by STFC Quota Studentship ST/N504117/1. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data. We also thank the reviewers for useful comments. Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
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field aligned currents in saturn s nightside magnetosphere subcorotation and planetary period oscillation components during northern spring
Journal of Geophysical Research, 2018Co-Authors: T J Bradley, S W H Cowley, G Provan, G J Hunt, E J Bunce, S J Wharton, I I Alexeev, E S Belenkaya, V V Kalegaev, M K DoughertyAbstract:Calibrated data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/)
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planetary period oscillations in saturn s magnetosphere Cassini magnetic field observations over the northern summer solstice interval
Journal of Geophysical Research, 2018Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
G Provan - One of the best experts on this subject based on the ideXlab platform.
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the structure of planetary period oscillations in saturn s equatorial magnetosphere results from the Cassini Mission
arXiv: Space Physics, 2019Co-Authors: D J Andrews, S W H Cowley, G Provan, G J Hunt, Lina Hadid, Michiko Morooka, Janerik WahlundAbstract:Saturn's magnetospheric magnetic field, planetary radio eMissions, plasma populations and magnetospheric structure are all known to be modulated at periods close to the assumed rotation period of the planetary interior. These oscillations are readily apparent despite the high degree of axi-symmetry in the internally produced magnetic field of the planet, and have different rotation periods in the northern and southern hemispheres. In this paper we study the spatial structure of (near-) planetary period magnetic field oscillations in Saturn's equatorial magnetosphere. Extending previous analyses of these phenomena, we include all suitable data from the entire Cassini Mission during its orbital tour of the planet, so as to be able to quantify both the amplitude and phase of these field oscillations throughout Saturn's equatorial plane, to distances of 30 planetary radii. We study the structure of these field oscillations in view of both independently rotating northern and southern systems, finding spatial variations in both magnetic fields and inferred currents flowing north-south that are common to both systems. With the greatly expanded coverage of the equatorial plane achieved during the latter years of the Mission, we are able to present a complete survey of dawn-dusk and day-night asymmetries in the structure of the oscillating fields and currents. We show that the general structure of the rotating currents is simpler than previously reported, and that the relatively enhanced nightside equatorial fields and currents are due in part to related periodic vertical motion of Saturn's magnetotail current sheet.
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currents associated with saturn s intra d ring azimuthal field perturbations
Journal of Geophysical Research, 2019Co-Authors: G J Hunt, S W H Cowley, G Provan, M K Dougherty, E J Bunce, Hao Cao, D J SouthwoodAbstract:During the final 22 full revolutions of the Cassini Mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low‐latitude current system via the associated azimuthal perturbation field peaking typically at ~10‐30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field‐aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field‐aligned current densities above the ionosphere are typically ~5‐10 nA m^(‐2), more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field‐aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north‐south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller‐scale structures, possibly due to rapid temporal or local time variations.
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variability of intra d ring azimuthal magnetic field profiles observed on Cassini s proximal periapsis passes
Journal of Geophysical Research, 2019Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Work at the University of Leicester was supported by STFC grant ST/N000749/1. Work at Imperial College was supported by STFC grant ST/N000692/1. EJB was supported by a Royal Society Wolfson Research Merit Award. MKD was supported by Royal Society Research Professorship RP140004. TJB was supported by STFC Quota Studentship ST/N504117/1. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data. We also thank the reviewers for useful comments. Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
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Planetary Period Oscillations in Saturn's Magnetosphere: Comparison of Magnetic and SKR Modulation Periods and Phases During Northern Summer to the End of the Cassini Mission
2019Co-Authors: G Provan, S W H Cowley, L Lamy, E J BunceAbstract:We compare periods and phases of Saturn planetary period oscillations determined from Cassini magnetic field and Saturn kilometric radiation (SKR) data from the beginning of 2016 to the end of Mission in mid-September 2017, encompassing northern summer solstice in May 2017. Both data sets show that the periods are almost unchanging, varying by only ~ ±0.01 hr about 10.79 hr for the northern system and 10.68 hr for the southern system, close to values attained by mid-2015 after period coalescence between mid-2013 and mid-2014. The mean absolute differences between the magnetic and SKR periods are ~0.0036 hr (~13 s), consistent with estimated magnetic measurement uncertainties, while the overall mean difference is less than 0.001 hr (~2–3 s), at the limit of resolution. The relative phasing between magnetic and SKR modulations is correspondingly near constant and such that the equatorial planetary period oscillation fields of the northern/southern systems point radially outward near-oppositely at ~14.3/2.5 hr local time at corresponding SKR maxima, with upward planetary period oscillation currents located ~2 hr postdawn for both systems, consistent with previous intervals having dawnside spacecraft apoapsides. Southern SKR eMissions are found to be significantly dual modulated at both southern and northern periods in data limited to lie well within the southern shadow zone of the northern sources. These northern period modulations are shown to be approximately in phase with those in the northern eMissions, consistent with a recent suggestion that bidirectional auroral electron acceleration may generate in phase SKR eMissions in both hemispheres
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field aligned currents in saturn s nightside magnetosphere subcorotation and planetary period oscillation components during northern spring
Journal of Geophysical Research, 2018Co-Authors: T J Bradley, S W H Cowley, G Provan, G J Hunt, E J Bunce, S J Wharton, I I Alexeev, E S Belenkaya, V V Kalegaev, M K DoughertyAbstract:Calibrated data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/)
S W H Cowley - One of the best experts on this subject based on the ideXlab platform.
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the structure of planetary period oscillations in saturn s equatorial magnetosphere results from the Cassini Mission
arXiv: Space Physics, 2019Co-Authors: D J Andrews, S W H Cowley, G Provan, G J Hunt, Lina Hadid, Michiko Morooka, Janerik WahlundAbstract:Saturn's magnetospheric magnetic field, planetary radio eMissions, plasma populations and magnetospheric structure are all known to be modulated at periods close to the assumed rotation period of the planetary interior. These oscillations are readily apparent despite the high degree of axi-symmetry in the internally produced magnetic field of the planet, and have different rotation periods in the northern and southern hemispheres. In this paper we study the spatial structure of (near-) planetary period magnetic field oscillations in Saturn's equatorial magnetosphere. Extending previous analyses of these phenomena, we include all suitable data from the entire Cassini Mission during its orbital tour of the planet, so as to be able to quantify both the amplitude and phase of these field oscillations throughout Saturn's equatorial plane, to distances of 30 planetary radii. We study the structure of these field oscillations in view of both independently rotating northern and southern systems, finding spatial variations in both magnetic fields and inferred currents flowing north-south that are common to both systems. With the greatly expanded coverage of the equatorial plane achieved during the latter years of the Mission, we are able to present a complete survey of dawn-dusk and day-night asymmetries in the structure of the oscillating fields and currents. We show that the general structure of the rotating currents is simpler than previously reported, and that the relatively enhanced nightside equatorial fields and currents are due in part to related periodic vertical motion of Saturn's magnetotail current sheet.
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currents associated with saturn s intra d ring azimuthal field perturbations
Journal of Geophysical Research, 2019Co-Authors: G J Hunt, S W H Cowley, G Provan, M K Dougherty, E J Bunce, Hao Cao, D J SouthwoodAbstract:During the final 22 full revolutions of the Cassini Mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low‐latitude current system via the associated azimuthal perturbation field peaking typically at ~10‐30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field‐aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field‐aligned current densities above the ionosphere are typically ~5‐10 nA m^(‐2), more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field‐aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north‐south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller‐scale structures, possibly due to rapid temporal or local time variations.
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variability of intra d ring azimuthal magnetic field profiles observed on Cassini s proximal periapsis passes
Journal of Geophysical Research, 2019Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Work at the University of Leicester was supported by STFC grant ST/N000749/1. Work at Imperial College was supported by STFC grant ST/N000692/1. EJB was supported by a Royal Society Wolfson Research Merit Award. MKD was supported by Royal Society Research Professorship RP140004. TJB was supported by STFC Quota Studentship ST/N504117/1. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data. We also thank the reviewers for useful comments. Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
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Planetary Period Oscillations in Saturn's Magnetosphere: Comparison of Magnetic and SKR Modulation Periods and Phases During Northern Summer to the End of the Cassini Mission
2019Co-Authors: G Provan, S W H Cowley, L Lamy, E J BunceAbstract:We compare periods and phases of Saturn planetary period oscillations determined from Cassini magnetic field and Saturn kilometric radiation (SKR) data from the beginning of 2016 to the end of Mission in mid-September 2017, encompassing northern summer solstice in May 2017. Both data sets show that the periods are almost unchanging, varying by only ~ ±0.01 hr about 10.79 hr for the northern system and 10.68 hr for the southern system, close to values attained by mid-2015 after period coalescence between mid-2013 and mid-2014. The mean absolute differences between the magnetic and SKR periods are ~0.0036 hr (~13 s), consistent with estimated magnetic measurement uncertainties, while the overall mean difference is less than 0.001 hr (~2–3 s), at the limit of resolution. The relative phasing between magnetic and SKR modulations is correspondingly near constant and such that the equatorial planetary period oscillation fields of the northern/southern systems point radially outward near-oppositely at ~14.3/2.5 hr local time at corresponding SKR maxima, with upward planetary period oscillation currents located ~2 hr postdawn for both systems, consistent with previous intervals having dawnside spacecraft apoapsides. Southern SKR eMissions are found to be significantly dual modulated at both southern and northern periods in data limited to lie well within the southern shadow zone of the northern sources. These northern period modulations are shown to be approximately in phase with those in the northern eMissions, consistent with a recent suggestion that bidirectional auroral electron acceleration may generate in phase SKR eMissions in both hemispheres
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field aligned currents in saturn s nightside magnetosphere subcorotation and planetary period oscillation components during northern spring
Journal of Geophysical Research, 2018Co-Authors: T J Bradley, S W H Cowley, G Provan, G J Hunt, E J Bunce, S J Wharton, I I Alexeev, E S Belenkaya, V V Kalegaev, M K DoughertyAbstract:Calibrated data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/)
E J Bunce - One of the best experts on this subject based on the ideXlab platform.
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currents associated with saturn s intra d ring azimuthal field perturbations
Journal of Geophysical Research, 2019Co-Authors: G J Hunt, S W H Cowley, G Provan, M K Dougherty, E J Bunce, Hao Cao, D J SouthwoodAbstract:During the final 22 full revolutions of the Cassini Mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low‐latitude current system via the associated azimuthal perturbation field peaking typically at ~10‐30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field‐aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field‐aligned current densities above the ionosphere are typically ~5‐10 nA m^(‐2), more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field‐aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north‐south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller‐scale structures, possibly due to rapid temporal or local time variations.
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variability of intra d ring azimuthal magnetic field profiles observed on Cassini s proximal periapsis passes
Journal of Geophysical Research, 2019Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Work at the University of Leicester was supported by STFC grant ST/N000749/1. Work at Imperial College was supported by STFC grant ST/N000692/1. EJB was supported by a Royal Society Wolfson Research Merit Award. MKD was supported by Royal Society Research Professorship RP140004. TJB was supported by STFC Quota Studentship ST/N504117/1. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data. We also thank the reviewers for useful comments. Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
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Planetary Period Oscillations in Saturn's Magnetosphere: Comparison of Magnetic and SKR Modulation Periods and Phases During Northern Summer to the End of the Cassini Mission
2019Co-Authors: G Provan, S W H Cowley, L Lamy, E J BunceAbstract:We compare periods and phases of Saturn planetary period oscillations determined from Cassini magnetic field and Saturn kilometric radiation (SKR) data from the beginning of 2016 to the end of Mission in mid-September 2017, encompassing northern summer solstice in May 2017. Both data sets show that the periods are almost unchanging, varying by only ~ ±0.01 hr about 10.79 hr for the northern system and 10.68 hr for the southern system, close to values attained by mid-2015 after period coalescence between mid-2013 and mid-2014. The mean absolute differences between the magnetic and SKR periods are ~0.0036 hr (~13 s), consistent with estimated magnetic measurement uncertainties, while the overall mean difference is less than 0.001 hr (~2–3 s), at the limit of resolution. The relative phasing between magnetic and SKR modulations is correspondingly near constant and such that the equatorial planetary period oscillation fields of the northern/southern systems point radially outward near-oppositely at ~14.3/2.5 hr local time at corresponding SKR maxima, with upward planetary period oscillation currents located ~2 hr postdawn for both systems, consistent with previous intervals having dawnside spacecraft apoapsides. Southern SKR eMissions are found to be significantly dual modulated at both southern and northern periods in data limited to lie well within the southern shadow zone of the northern sources. These northern period modulations are shown to be approximately in phase with those in the northern eMissions, consistent with a recent suggestion that bidirectional auroral electron acceleration may generate in phase SKR eMissions in both hemispheres
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field aligned currents in saturn s nightside magnetosphere subcorotation and planetary period oscillation components during northern spring
Journal of Geophysical Research, 2018Co-Authors: T J Bradley, S W H Cowley, G Provan, G J Hunt, E J Bunce, S J Wharton, I I Alexeev, E S Belenkaya, V V Kalegaev, M K DoughertyAbstract:Calibrated data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/)
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planetary period oscillations in saturn s magnetosphere Cassini magnetic field observations over the northern summer solstice interval
Journal of Geophysical Research, 2018Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
G J Hunt - One of the best experts on this subject based on the ideXlab platform.
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the structure of planetary period oscillations in saturn s equatorial magnetosphere results from the Cassini Mission
arXiv: Space Physics, 2019Co-Authors: D J Andrews, S W H Cowley, G Provan, G J Hunt, Lina Hadid, Michiko Morooka, Janerik WahlundAbstract:Saturn's magnetospheric magnetic field, planetary radio eMissions, plasma populations and magnetospheric structure are all known to be modulated at periods close to the assumed rotation period of the planetary interior. These oscillations are readily apparent despite the high degree of axi-symmetry in the internally produced magnetic field of the planet, and have different rotation periods in the northern and southern hemispheres. In this paper we study the spatial structure of (near-) planetary period magnetic field oscillations in Saturn's equatorial magnetosphere. Extending previous analyses of these phenomena, we include all suitable data from the entire Cassini Mission during its orbital tour of the planet, so as to be able to quantify both the amplitude and phase of these field oscillations throughout Saturn's equatorial plane, to distances of 30 planetary radii. We study the structure of these field oscillations in view of both independently rotating northern and southern systems, finding spatial variations in both magnetic fields and inferred currents flowing north-south that are common to both systems. With the greatly expanded coverage of the equatorial plane achieved during the latter years of the Mission, we are able to present a complete survey of dawn-dusk and day-night asymmetries in the structure of the oscillating fields and currents. We show that the general structure of the rotating currents is simpler than previously reported, and that the relatively enhanced nightside equatorial fields and currents are due in part to related periodic vertical motion of Saturn's magnetotail current sheet.
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currents associated with saturn s intra d ring azimuthal field perturbations
Journal of Geophysical Research, 2019Co-Authors: G J Hunt, S W H Cowley, G Provan, M K Dougherty, E J Bunce, Hao Cao, D J SouthwoodAbstract:During the final 22 full revolutions of the Cassini Mission in 2017, the spacecraft passed at periapsis near the noon meridian through the gap between the inner edge of Saturn's D ring and the denser layers of the planet's atmosphere, revealing the presence of an unanticipated low‐latitude current system via the associated azimuthal perturbation field peaking typically at ~10‐30 nT. Assuming approximate axisymmetry, here we use the field data to calculate the associated horizontal meridional currents flowing in the ionosphere at the feet of the field lines traversed, together with the exterior field‐aligned currents required by current continuity. We show that the ionospheric currents are typically~0.5–1.5 MA per radian of azimuth, similar to auroral region currents, while the field‐aligned current densities above the ionosphere are typically ~5‐10 nA m^(‐2), more than an order less than auroral values. The principal factor involved in this difference is the ionospheric areas into which the currents map. While around a third of passes exhibit unidirectional currents flowing northward in the ionosphere closing southward along exterior field lines, many passes also display layers of reversed northward field‐aligned current of comparable or larger magnitude in the region interior to the D ring, which may reverse sign again on the innermost field lines traversed. Overall, however, the currents generally show a high degree of north‐south conjugacy indicative of an interhemispheric system, certainly on the larger overall spatial scales involved, if less so for the smaller‐scale structures, possibly due to rapid temporal or local time variations.
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variability of intra d ring azimuthal magnetic field profiles observed on Cassini s proximal periapsis passes
Journal of Geophysical Research, 2019Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Work at the University of Leicester was supported by STFC grant ST/N000749/1. Work at Imperial College was supported by STFC grant ST/N000692/1. EJB was supported by a Royal Society Wolfson Research Merit Award. MKD was supported by Royal Society Research Professorship RP140004. TJB was supported by STFC Quota Studentship ST/N504117/1. We thank Steve Kellock and the Cassini magnetometer team at Imperial College for access to processed magnetic field data. We also thank the reviewers for useful comments. Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).
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field aligned currents in saturn s nightside magnetosphere subcorotation and planetary period oscillation components during northern spring
Journal of Geophysical Research, 2018Co-Authors: T J Bradley, S W H Cowley, G Provan, G J Hunt, E J Bunce, S J Wharton, I I Alexeev, E S Belenkaya, V V Kalegaev, M K DoughertyAbstract:Calibrated data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/)
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planetary period oscillations in saturn s magnetosphere Cassini magnetic field observations over the northern summer solstice interval
Journal of Geophysical Research, 2018Co-Authors: G Provan, S W H Cowley, G J Hunt, E J Bunce, T J Bradley, M K DoughertyAbstract:Calibrated magnetic field data from the Cassini Mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds.jpl.nasa.gov/).