The FIELDS Instrument Suite for Solar Probe Plus

Bale, S. D.; Goetz, K.; Harvey, P.; Turin, P.; Bonnell, J. W.; Wit, T. Dudok de; Ergun, R. E.; MacDowall, R. J.; Pulupa, M.; André, Mats; Bolton, M.; Bougeret, Jean‐Louis; Bowen, T. A.; Burgess, David; Cattell, C. A.; Chandran, Benjamin D. G.; Chaston, C. C.; Chen, C. H. K.; Choi, Michael K.; Connerney, J. E. P.; Cranmer, Steven R.; Diaz-Aguado, Millan; Donakowski, William; Drake, J. F.; Farrell, W. M.; Fergeau, P.; Fermin, J.; Fischer, James M.; Fox, N. J.; Glaser, Donald A.; Goldstein, M. L.; Gordon, D.; Hanson, E.; Harris, S.; Hayes, L. M.; Hinze, Juergen; Hollweg, Joseph V.; Horbury, T. S.; Howard, R. A.; Hoxie, V. C.; Jannet, G.; Karlsson, Magnus; Kasper, J. C.; Kellogg, P. J.; Kien, M.; Klimchuk, J. A.; Krasnoselskikh, V.; Krucker, S.; Lynch, J.J.; Maksimović, M.; Malaspina, D.; Marker, S.; Martin, Philippe; Oliveros, J. Martinez; McCauley, Jeremy; McComas, D. J.; McDonald, T.; Meyer‐Vernet, N.; Moncuquet, M.; Monson, S. J.; Mozer, F. S.; Murphy, Scott D.; Odom, J.; Oliverson, Ronald J.; Olson, Joseph; Parker, E. N.; Pankow, D.; Phan, T. D.; Quataert, Eliot; Quinn, Thomas; Ruplin, S. W.; Salem, C. S.; Seitz, D. N.; Sheppard, D.; Siy, A.; Stevens, Ken; Summers, D.; Szabó, Á.; Timofeeva, Maria; Vaivads, A.; Velli, M.; Yehle, A.; Werthimer, Dan; Wygant, J. R.

doi:10.1007/s11214-016-0244-5

Cited by 592 publications

(376 citation statements)

References 38 publications

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“…We predict that, depending on the parameters of the model, the magnetic energy spectrum in the reconnection-mediated interval can vary from E(k)∝k −8/3 to E(k)∝k −3 , both in low-beta plasmas (e.g., as the solar corona, interplanetary coronal mass ejections, planetary magnetospheres, etc. ; e.g., Chaston et al 2008;Chen et al 2014;Bale et al 2016) and plasmas with β∼1. These spectral predictions are valid for wavenumbers such that l…”

Section: Discussionmentioning

confidence: 99%

Collisionless Reconnection in Magnetohydrodynamic and Kinetic Turbulence

Loureiro

Boldyrev

2017

ApJ

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It has recently been proposed that the inertial interval in magnetohydrodynamic (MHD) turbulence is terminated at small scales not by a Kolmogorov-like dissipation region, but rather by a new sub-inertial interval mediated by tearing instability. However, many astrophysical plasmas are nearly collisionless so the MHD approximation is not applicable to turbulence at small scales. In this paper, we propose an extension of the theory of reconnectionmediated turbulence to plasmas which are so weakly collisional that the reconnection occurring in the turbulent eddies is caused by electron inertia rather than by resistivity. We find that the transition scale to reconnectionmediated turbulence depends on the plasma beta and on the assumptions of the plasma turbulence model. However, in all of the cases analyzed, the energy spectra in the reconnection-mediated interval range from μ^-(

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Section: Discussionmentioning

confidence: 99%

Collisionless Reconnection in Magnetohydrodynamic and Kinetic Turbulence

Loureiro

Boldyrev

2017

ApJ

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“…The electric field was measured by Bale et al (2005) to follow the magnetic field, having a spectral index of −5/3 at MHD scales 8 . Since the perpendicular plasma velocity in this range should be the E × B drift, the velocity was expected to display a similar spectrum, however, it has been shown to be shallower, with a value nearer −3/2 (e.g.…”

Section: Spectral Indices and Residual Energymentioning

confidence: 99%

“…Typical spectra of the density and magnetic fluctuations are shown in figure 9. Electric field spectra have also been reported to flatten at ion scales (Bale et al 2005;Sahraoui et al 2009;Salem et al 2012) and ion velocity and temperature spectra to steepen (Šafránková et al 2013, 2016).…”

Section: Phenomenological Models Of Kinetic Range Turbulencementioning

confidence: 99%

“…While being an intriguing and complex aspect of our universe of intrinsic interest, it can also have an important impact on the large-scale properties of these systems. For example, it can enable angular momentum transport in accretion disks (Balbus & Hawley 1998), galactic magnetic field amplification (Kulsrud & Zweibel 2008), limit thermal conduction in galaxy clusters , determine the dispersal and mixing of elements in the interstellar medium (Scalo & Elmegreen 2004) and play a key role in star formation (McKee & Ostriker 2007). In addition, the dissipation of turbulent energy may explain the large temperatures observed in many astrophysical systems, such as the solar corona (Cranmer et al 2015) and galaxy clusters (Zhuravleva et al 2014).…”

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confidence: 99%

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Recent progress in astrophysical plasma turbulence from solar wind observations

2016

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This paper summarises some of the recent progress that has been made in understanding astrophysical plasma turbulence in the solar wind, from in situ spacecraft observations. At large scales, where the turbulence is predominantly Alfvénic, measurements of critical balance, residual energy and three-dimensional structure are discussed, along with comparison to recent models of strong Alfvénic turbulence. At these scales, a few per cent of the energy is also in compressive fluctuations, and their nature, anisotropy and relation to the Alfvénic component is described. In the small-scale kinetic range, below the ion gyroscale, the turbulence becomes predominantly kinetic Alfvén in nature, and measurements of the spectra, anisotropy and intermittency of this turbulence are discussed with respect to recent cascade models. One of the major remaining questions is how the turbulent energy is dissipated, and some recent work on this question, in addition to future space missions which will help to answer it, are briefly discussed.

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“…We then generalize our calculations of the pulses' risetime to microdust detection on other spacecraft, thereby explaining previous observations left uninterpreted. Finally, we derive some consequences of our results for future wave instruments, in particular Plasma Wave Investigation (PWI) on Bepi‐Colombo, RPW on Solar Orbiter, and FIELDS on Solar Probe Plus [ Bale et al , ], since the pulses' risetime determines the optimal frequency range for dust detection. Unless otherwise stated, units are SI.…”

Section: Introductionmentioning

confidence: 99%

Frequency range of dust detection in space with radio and plasma wave receivers: Theory and application to interplanetary nanodust impacts on Cassini

et al. 2017

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Wave instruments can detect dust in space via the charges released by impact ionization of fast dust grains. Each hypervelocity dust impact produces an electrostatic pulse whose short risetime is a major property determining the frequency range of detection. We propose a simplified analytical model to calculate this risetime and its variation with grains' mass and photoelectron or ambient plasma density, for pulses in spacecraft potential due to fast interplanetary nanodust impacts. We test these calculations by analyzing the high‐frequency receiver data of the radio and plasma wave instrument during the cruise phase of the Cassini mission between Earth and Jupiter. These data confirm the dependence of the risetime on grains' mass and speed and heliocentric distance predicted by our calculations. Furthermore, the data show that the nanodust properties follow closely the fluctuations of the solar wind velocity component perpendicular to the magnetic field, as predicted by dynamics. The calculations can be generalized to microdust detection on other spacecraft and might explain previous observations left uninterpreted. These calculations are also relevant for the design of wave receivers, by determining the optimal frequency range for dust detection on future missions.

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The FIELDS Instrument Suite for Solar Probe Plus

Cited by 592 publications

References 38 publications

Collisionless Reconnection in Magnetohydrodynamic and Kinetic Turbulence

Collisionless Reconnection in Magnetohydrodynamic and Kinetic Turbulence

Recent progress in astrophysical plasma turbulence from solar wind observations

Frequency range of dust detection in space with radio and plasma wave receivers: Theory and application to interplanetary nanodust impacts on Cassini

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