Coordinated Study on Solar Wind Turbulence During the Venus-Express, ACE and Ulysses Alignment of August 2007

Bruno, R.; Carbone, V.; Vörös, Z.; D’Amicis, R.; Bavassano, B.; Cattaneo, M. B. Bavassano; Mura, A.; Milillo, A.; Orsini, S.; Veltri, P.; Sorriso‐Valvo, L.; Zhang, T.; Biernat, H. K.; Rücker, H. O.; Baumjohann, W.; Jankovičovà, D.; Kovács, Péter

doi:10.1007/s11038-008-9272-9

Cited by 26 publications

(28 citation statements)

References 2 publications

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“…λ increases with heliocentric distance both in the inner and outer heliosphere, as has been shown in previous observational works (e.g., Matthaeus, Smith, and Bieber, 1999;Bruno et al, 2005;Bruno et al, 2009;D'Amicis et al, 2010) and model calculations (e.g., Smith et al, 2001). A least-squares fit to the data (dashed line), illustrates this behavior, yielding a power law λ(D) = 0.89(D/1 AU ) 0.43 × 10 6 km.…”

Section: Evolution Of λ With Heliocentric Distance and Nominal Agingsupporting

confidence: 82%

Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units

et al. 2014

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The solar wind is a structured and complex system, in which the fields vary strongly over a wide range of spatial and temporal scales. As an example, the turbulent activity in the wind affects the evolution in the heliosphere of the integral turbulent scale or correlation length [λ], usually associated with the breakpoint in the turbulent-energy spectrum that separates the inertial range from the injection range. This large variability of the fields demands a statistical description of the solar wind. In this work, we study the probability distribution function (PDF) of the magnetic autocorrelation lengths observed in the solar wind at different distances from the Sun. We use observations from Helios, ACE, and Ulysses spacecraft. We distinguish between the usual solar wind and one of its transient components (Interplanetary Coronal Mass Ejections, ICMEs), and study also solar wind samples with low and high proton beta [β p ]. We find that in the last 3 regimes the PDF of λ is a log-normal function, consistent with the multiplicative and non-linear processes that take place in the solar wind, the initial λ (before the Alfvénic point) being larger in ICMEs.

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Section: Evolution Of λ With Heliocentric Distance and Nominal Agingsupporting

confidence: 82%

Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units

et al. 2014

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“…In this framework, energy injected into the interplanetary plasma at large scales is transferred by non-linear interactions to microscales where it is finally dissipated, thus heating the plasma. The low-frequency part of the magnetic field and plasma-velocity power spectra often exhibits a clear f −1 scaling, from DC up to frequencies of about 10 −4 Hz in the fast Alfvénic wind (Bruno et al 2009), where the turbulent energy cascade becomes active. It is worth noting that, contrary to the fast solar wind, in the low-speed streams the injection range may cover a smaller range of frequencies and sometimes not to be present at all (Bruno et al 2019).…”

Section: Fluctuations In the Sub-millihertz: Interplanetary Magnetic mentioning

confidence: 99%

Spacecraft and interplanetary contributions to the magnetic environment on-board LISA Pathfinder

Armano

Audley

Baird

et al. 2020

Monthly Notices of the Royal Astronomical Society

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LISA Pathfinder (LPF) has been a space-based mission designed to test new technologies that will be required for a gravitational wave observatory in space. Magnetically driven forces play a key role in the instrument sensitivity in the low-frequency regime (mHz and below), the measurement band of interest for a space-based observatory. The magnetic field can couple to the magnetic susceptibility and remanent magnetic moment from the test masses and disturb them from their geodesic movement. LISA Pathfinder carried on-board a dedicated magnetic measurement subsystem with noise levels of 10 nT Hz −1/2 from 1 Hz down to 1 mHz. In this paper we report on the magnetic measurements throughout LISA Pathfinder operations. We characterise the magnetic environment within the spacecraft, study the time evolution of the magnetic field and its stability down to 20 µHz, where we measure values around 200 nT Hz −1/2 and identify two different frequency regimes, one related to the interplanetary magnetic field and the other to the magnetic field originating inside the spacecraft. Finally, we characterise the non-stationary component of the fluctuations of the magnetic field below the mHz and relate them to the dynamics of the solar wind.

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“…The set of scaling exponents (τ q ) describes the inhomogeneity of the singularity strength, and thus the multifractal properties of the field [21]. In particu- [10]. For the parameter c, two power-law fits are also superposed.…”

Section: Statistical Properties Of the Local Energy Transfer Ratementioning

confidence: 99%

On the Statistical Properties of Turbulent Energy Transfer Rate in the Inner Heliosphere

Sorriso‐Valvo

Carbone²,

Perri

et al. 2018

Sol Phys

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The transfer of energy from large to small scales in solar wind turbulence is an important ingredient of the longstanding question about the mechanism of the interplanetary plasma heating. Previous studies have shown that magnetohydrodynamic (MHD) turbulence is statistically compatible with the observed solar wind heating as it expands in the heliosphere. However, in order to understand which processes contribute to the plasma heating, it is necessary to have a local description of the energy flux across scales. To this aim, it is customary to use indicators such as the magnetic field partial variance of increments (PVI), which is associated with the local, relative, scale-dependent magnetic energy. A more complete evaluation of the energy transfer should also include other terms, related to velocity and cross-helicity. This is achieved here by introducing a proxy for the local, scale dependent turbulent energy transfer rate ǫ∆t(t), based on the third-order moment scaling law for MHD turbulence. Data from Helios 2 are used to determine the statistical properties of such a proxy in comparison with the magnetic and velocity fields PVI, and the correlation with local solar wind heating is computed. PVI and ǫ∆t(t) are generally well correlated, however ǫ∆t(t) is a very sensitive proxy that can exhibit large amplitude values, both positive and negative, even for low amplitude peaks in the PVI. Furthermore, ǫ∆t(t) is very well correlated with local increases of temperature when large amplitude bursts of energy transfer are localized, thus suggesting an important role played by this proxy in the study of plasma energy dissipation.

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Coordinated Study on Solar Wind Turbulence During the Venus-Express, ACE and Ulysses Alignment of August 2007

Cited by 26 publications

References 2 publications

Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units

Characterization of the Turbulent Magnetic Integral Length in the Solar Wind: From 0.3 to 5 Astronomical Units

Spacecraft and interplanetary contributions to the magnetic environment on-board LISA Pathfinder

On the Statistical Properties of Turbulent Energy Transfer Rate in the Inner Heliosphere

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