The Effects of Solar Wind Structure on Nanodust Dynamics in the Inner Heliosphere

Poppe, A. R.; Lee, Christina O.

doi:10.1029/2020ja028463

Cited by 7 publications

(14 citation statements)

References 116 publications

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“…We make this comparison with the full understanding that the response mechanism of the STEREO/WAVES instruments to high‐velocity nanodust grains is poorly understood and apparently different between STEREO A and B, likely due to their opposite attitude with respect to the nanodust grain fluxes (e.g., see Meyer‐Vernet, Lecacheux, et al., 2009). We also reiterate that per our previous study (Poppe & Lee, 2020), we found that the episodic nature of the observed single‐hits on STEREO A suggested a strong degree of variability in the initial production of nanodust grains themselves in the inner heliosphere, something we do not model here. Thus, this comparison primarily pertains to whether or not nanodust grain fluxes can access 1 au at a given point in time, not whether STEREO/WAVES will definitively experience nanodust grain impacts at such times.…”

Section: Model Resultssupporting

confidence: 83%

“…In addition to the magnitude of the HCS tilt, the sign of Denoted in colors (green, red, blue) are specific CRs for which we have modeled nanodust dynamics for our current study. For reference, our previous study (Poppe & Lee, 2020) (1936, 1956, 1976, 1996, 2016, 2036, 2056, and 2076) that straddle the defocusing-to-focusing transition that occurred near CR 1950. A similar defocusing-to-focusing transition is expected in the upcoming solar cycle 25, and thus, we use these eight CRs to model and predict the behavior of nanodust grains during solar cycle 25 in Section 3.3.…”

Section: Model Descriptionmentioning

confidence: 99%

“…(1976, 1981), based on rocket and Helios 1/2 zodiacal light photometry measurements, given by,

n(r)={r}^{-1.3}\mathrm{exp}\left(-2.6\vert \mathrm{sin}\,{\beta }_{\odot }\vert \right),

where r is the heliocentric distance and β ⊙ is the ecliptic latitude. The collisional production distribution of nanodust grains, Γ( r ), is then given by the product of the density squared and the relative impact velocity (assumed to scale as, v imp ( r ) ∝ r −0.5 ) as,

{\Gamma}(r)={n}^{2}(r)\cdot {r}^{-0.5}={r}^{-3.1}{\mathrm{exp}}^{2}\left(-2.6\vert \mathrm{sin}\,{\beta }_{\odot }\vert \right).

Both the interplanetary dust density and collisional production rate distributions are depicted in Figure 1 of Poppe and Lee (2020). Once each nanodust grain was initialized, the model integrated a coupled set of equations describing the grain position, velocity, and charge.…”

Section: Model Descriptionmentioning

confidence: 99%

“…Here, we continue to explore the dynamics of inner‐heliospheric nanodust grains using the modeling framework developed in Poppe and Lee (2020), focusing in particular on the variability in nanodust dynamics as a function of both solar cycle and focusing or defocusing interplanetary magnetic fields. In contrast to our previous study, however, we do not make an attempt to calculate “absolutely calibrated” nanodust fluxes to the STEREO spacecraft (or any other object).…”

Section: Introductionmentioning

confidence: 99%

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The Effects of Solar Cycle Variability on Nanodust Dynamics in the Inner Heliosphere: Predictions for Future STEREO A/WAVES Measurements

Poppe

Lee

2022

JGR Space Physics

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The collisional grinding of interplanetary meteoroids should continually produce grains over a wide range of sizes, including down to the nanometer‐size regime. Once generated, nanodust grains are subject to interplanetary electromagnetic forces from the solar wind due to their relatively large charge‐to‐mass ratios, resulting in complex and highly time‐dependent dynamics. Here, we use the coupled Wang‐Sheeley‐Arge solar corona and Enlil solar wind models together with a nanodust charging and dynamics model to explore the behavior and variability of nanodust dynamics in the inner heliosphere (<1 au) both within and across multiple solar cycles. In particular, we quantify the relative accessibility of these grains to 1 au across solar cycles 23 and 24, including focusing and defocusing heliospheric conditions. Finally, we qualitatively compare our model results with STEREO A (STA)/WAVES observations and identify correlations between the STA/WAVES single‐hit rate and the relative flux of >10 nm grains. Using solar cycle 23 as a proxy for the behavior of solar cycle 25, since both solar cycles share the same defocusing‐to‐focusing transition, we predict the relative flux of nanodust grains in the future and identify times at which nanodust impacts may reappear in the STA/WAVES data set. Continued analysis of future STA/WAVES observations will provide an important test of this prediction, either bolstering or weakening the interpretation of electromagnetically accelerated nanodust grains as the source of single‐hit events in the STA/WAVES Time Domain Sampler data set.

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Section: Model Resultssupporting

confidence: 83%

Section: Model Descriptionmentioning

confidence: 99%

“…(1976, 1981), based on rocket and Helios 1/2 zodiacal light photometry measurements, given by,

n(r)={r}^{-1.3}\mathrm{exp}\left(-2.6\vert \mathrm{sin}\,{\beta }_{\odot }\vert \right),

{\Gamma}(r)={n}^{2}(r)\cdot {r}^{-0.5}={r}^{-3.1}{\mathrm{exp}}^{2}\left(-2.6\vert \mathrm{sin}\,{\beta }_{\odot }\vert \right).

Section: Model Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Effects of Solar Cycle Variability on Nanodust Dynamics in the Inner Heliosphere: Predictions for Future STEREO A/WAVES Measurements

Poppe

Lee

2022

JGR Space Physics

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“…A sharp drop in temperature value (almost two times, in HCS region during periods of solar minimum) may be associated with the properties of plasma sources near the HCS, as well as, possibly, with the interaction of plasma flows with a rarefied dust component or with other possible factors not taken into account that require further investigation and interpretation (e.g., [65][66][67][68][69]).…”

Section: Comparison Of Numerical Results With the Observational Datamentioning

confidence: 99%

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

et al. 2022

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A model capable of reproducing a set of solar wind parameters along the virtual spacecraft orbit out of an ecliptic plane has been developed. In the framework of a quasi-stationary axisymmetric self-consistent MHD model the spatial distributions of magnetic field and plasma characteristics at distances from 20 to 1200 Solar radii at almost all solar latitudes could be obtained and analyzed. This model takes into account the Sun’s magnetic field evolution during the solar cycle, when the dominant dipole magnetic field is replaced by the quadrupole one. Self-consistent solutions for solar wind characteristics were obtained, depending on the phase of the solar cycle. To verify the model, its results are compared with the observed characteristics of solar wind along the Ulysses trajectory during its flyby around the Sun from 1990 to 2009. It is shown that the results of numerical simulation are generally consistent with the observational data obtained by the Ulysses spacecraft. A comparison of the model and experimental data confirms that the model can adequately describe the solar wind parameters and can be used for heliospheric studies at different phases of the solar activity cycle, as well as in a wide range of latitudinal angles and distances to the Sun.

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The distribution of the near-solar bound dust grains detected with Parker Solar Probe

Kočiščák,

Theodorsen,

Mann

2024

A&A

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Context. Parker Solar Probe (PSP) counts dust impacts in the near-solar region, but modeling effort is needed to understand the dust population’s properties. Aims. We aim to constrain the dust cloud’s properties based on the flux observed by PSP. Methods. We developed a forward model for the bound dust detection rates using the formalism of 6D phase space distribution of the dust. We applied the model to the location table of different PSP solar encounter groups. We explain some of the near-perihelion features observed in the data as well as the broader characteristic of the dust flux between 0.15 AU and 0.5 AU. We compare the measurements of PSP to the measurements of Solar Orbiter near 1 AU to expose the differences between the two spacecraft. Results. We found that the dust flux observed by PSP between 0.15 AU and 0.5 AU in post-perihelia can be explained by dust on bound orbits and is consistent with a broad range of orbital parameters, including dust on circular orbits. However, the dust number density as a function of the heliocentric distance and the scaling of detection efficiency with relative speed are important to explain the observed flux variation. The data suggest that the slope of differential mass distribution, δ, is between 0.14 and 0.49. The near-perihelion observations, however, show the flux maxima, which are inconsistent with the circular dust model, and additional effects may play a role. We found an indication that the sunward side of PSP is less sensitive to the dust impacts than PSP’s other surfaces. Conclusions. We show that the dust flux on PSP can be explained by noncircular bound dust and the detection capabilities of PSP. The scaling of flux with impact speed is especially important, and shallower than previously assumed.

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The Effects of Solar Wind Structure on Nanodust Dynamics in the Inner Heliosphere

Cited by 7 publications

References 116 publications

The Effects of Solar Cycle Variability on Nanodust Dynamics in the Inner Heliosphere: Predictions for Future STEREO A/WAVES Measurements

The Effects of Solar Cycle Variability on Nanodust Dynamics in the Inner Heliosphere: Predictions for Future STEREO A/WAVES Measurements

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

The distribution of the near-solar bound dust grains detected with Parker Solar Probe

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