The Cassini Magnetic Field Investigation

Dougherty, M. K.; Kellock, S.; Southwood, D. J.; Balogh, A.; Smith, E. J.; Tsurutani, B. T.; Gerlach, B.; Glaßmeier, K.‐H.; Gleim, F.; Russell, C. T.; Erdö́s, G.; Neubauer, F. M.; Cowley, S. W. H.

doi:10.1007/s11214-004-1432-2

Cited by 468 publications

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“…Figure 6a shows the electron spectrogram color coded according to the scale on the right covering the energy range 0.6 eV to 28 keV obtained by the ELS sensor of the Cassini Plasma Spectrometer [Young et al, 2004]. Figures 6b-6g show magnetic field data obtained by the Cassini fluxgate magnetometer [Dougherty et al, 2004], specifically three pairs of panels showing residual and filtered data for each of the radial (r), colatitudinal (θ), and azimuthal (φ) spherical polar field components referenced to Saturn's spin and magnetic axis. The upper panel of each pair shows 1 min residual field data with the internal field of the planet subtracted using the "Cassini SOI" model [Dougherty et al, 2005].…”

Section: /2015ja021642mentioning

confidence: 99%

Planetary period oscillations in Saturn's magnetosphere: Examining the relationship between abrupt changes in behavior and solar wind‐induced magnetospheric compressions and expansions

et al. 2015

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We examine planetary period oscillations (PPOs) observed in Saturn's magnetospheric magnetic field data from the time of Saturn's equinox in 2009. In particular, we focus on the time period commencing February 2011, when the oscillations started to display sudden and unexpected changes in behavior at ~100–200 day intervals. These were characterized by large simultaneous changes in the amplitude of the northern and southern PPO systems, together with small changes in period and jumps in phase. Nine significant abrupt changes have been observed in the postequinox interval to date, commencing as the Sun started to emerge from a long extended solar minimum. We perform a statistical study to determine whether these modulations in PPO behavior were associated with changes in the solar and/or upstream solar wind conditions. We report that the upstream solar wind conditions show elevated values of solar wind dynamic pressure and density around the time of PPO behavioral transitions, as opposed to before and after these times. We suggest that abrupt changes in PPO behavior may be related to significant changes in the size of the Saturnian magnetosphere in response to varying solar wind conditions.

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Section: /2015ja021642mentioning

confidence: 99%

Planetary period oscillations in Saturn's magnetosphere: Examining the relationship between abrupt changes in behavior and solar wind‐induced magnetospheric compressions and expansions

et al. 2015

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“…The magnetic field data derive from the Cassini fluxgate magnetometer [Dougherty et al, 2004. The magnetometer furnishes vector measurements of the magnetic field for field strengths from ∼1 nT to 40,000 nT at a time resolution faster than that of LEMMS.…”

Section: Instrumentationmentioning

confidence: 99%

Pitch angle distributions of energetic electrons at Saturn

et al. 2011

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[1] Pitch angle distributions of energetic electrons (110-365 keV) at Saturn are statistically analyzed for [2005][2006][2007][2008][2009]. Using a nondipolar model magnetic field, pitch angle distributions are mapped to the magnetospheric equator and sorted by equatorial crossing distance. The results are quantified using a standard function for the pitch angle distribution, f(a) = Asin K a (where a is the pitch angle and K is the power). Inside of ∼10 R S , the distributions are mostly peaked at 90°(K < 0), signifying a trapping distribution. Outside of this distance, the distributions are mostly field aligned (K > 0) with maxima near 0°and 180°. The 10 R S boundary maps to Saturn's ionosphere at latitudes equatorward of the aurora. Very few "flat" distributions are observed (K ≈ 0). The pitch angle distributions are not as well organized in local time as they are in radial distance, but over the 5 year survey between 10 and 20 R S field-aligned distributions appear most often near midnight, while trapping distributions are found elsewhere.

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“…Figure 3.1 shows where each of the twelve instruments are located on the spacecraft. The data presented and interpreted in these studies are principally from Cassini's Fluxgate Magnetometer (MAG) [Dougherty et al, 2004] with supporting data from the Radio and Plasma Wave Science (RPWS) [Gurnett et al, 2004] and Ion Mass Spectrometer (IMS) [Young et al, 2004]. In this chapter, we will begin with a brief overview of the mission and then describe the instruments used.…”

Section: Spacecraft and Instrumentationmentioning

confidence: 99%

“…In an energy spectrum with increasing wave number, k, these fluctuations in the data are manifested as a power law with a distinct (and mostly more than one) spectral index depending on the range of scales [Goldstein et al, 1995]. [Dougherty et al, 2004]. This is one of the spacecraft's two magnetometers; the other being the Scalar/Vector Helium Magnetometer (S/VHM).…”

Section: Cassini Fluxgate Magnetometermentioning

confidence: 99%

“…We use data obtained from Cassini's onboard fluxgate magnetometer (MAG) [Dougherty et al, 2004] from which boundary crossings and magnetosheath signatures are identified. Since we are interested in the large-scale spatially-dependent structure of the magnetosheath, we have selected 106 complete and uninterrupted magne- These are both inbound (bow shock to magnetopause) and outbound (magnetopause to bow shock) and exclude excursions due to global boundary oscillations or surface waves.…”

Section: Data Selectionmentioning

confidence: 99%

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The Near-Saturn Magnetic Field Environment

Sulaiman

2017

Springer Theses

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Shock waves exist throughout the universe and are fundamental to understanding the nature of collisionless plasmas. The complex coupling between charged particles and electromagnetic fields in plasmas give rise to a whole host of mechanisms for dissipation and heating across shock waves, particularly at high Mach numbers. While ongoing studies have investigated these process extensively both theoretically and via simulations, their observations remain few and far between. This thesis presents a study of very high Mach number shocks in a parameter space that has been poorly explored and identifies reformation using in situ magnetic field observations from the This non-axisymmetry is revealed to have an impact in the rotation of the magnetic field and is significant enough to influence the magnetic shear at the magnetopause.

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The Cassini Magnetic Field Investigation

Cited by 468 publications

References 56 publications

Planetary period oscillations in Saturn's magnetosphere: Examining the relationship between abrupt changes in behavior and solar wind‐induced magnetospheric compressions and expansions

Planetary period oscillations in Saturn's magnetosphere: Examining the relationship between abrupt changes in behavior and solar wind‐induced magnetospheric compressions and expansions

Pitch angle distributions of energetic electrons at Saturn

The Near-Saturn Magnetic Field Environment

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