Dust trajectory simulations around the Sun, Vega, and Fomalhaut

Stamm, Johann; Czechowski, A.; Mann, Ingrid; Baumann, Carsten; Myrvang, Margaretha

doi:10.1051/0004-6361/201834727

Cited by 7 publications

(6 citation statements)

References 28 publications

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“…In this section we specifically focus on dust particles which are not trapped near the Sun by the electromagnetic forces. These include all dust particles with a high enough radiation pressure to gravity ratio (β ∼ 0.5) and those particles with small β which are created outside the limit of the trapping region, which, near the solar equator, occurs at the heliocentric distance of ∼0.16 AU (Czechowski & Mann 2010, see also Stamm et al 2019). Assuming that these particles are created by collisional fragmentation from the larger dust, their subsequent motion will be ultimately directed outwards due to the radiation pressure or the electromagnetic forces.…”

Section: Estimations Of the Dust Flux: Escaping Particlesmentioning

confidence: 99%

Dust observations from Parker Solar Probe: dust ejection from the inner Solar System

Mann

Czechowski

2021

A&A

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Context. The FIELDS instrument onboard Parker Solar Probe (PSP) observes dust impacts on the spacecraft. The derived dust flux rates suggest that the particles originate from the vicinities of the Sun and are ejected by radiation pressure. Radiation pressure typically ejects particles of several 100 nm and smaller, which are also affected by the electromagnetic force. Aims. We aim to understand the influence of the electromagnetic force on the dust trajectories and to predict the dust fluxes along the orbit of PSP, within 1 AU and near Earth. Methods. We study the trajectories of dust particles influenced by gravity, radiation pressure, and the electromagnetic force assuming that pitch-angle scattering can be neglected (scatter-free approximation). We estimate the dust fluxes along the second orbit of PSP and in the vicinity of the Earth based on average dust velocities derived from the trajectory calculations and dust production rates derived from a fragmentation model. Results. The calculated cumulative flux of dust particles larger than 100 nm is of the same order (within a factor of ~2) as implied by PSP observations. In this size interval, the dynamics of most particles is dominated by the radiation pressure force. The Lorentz force becomes more important for smaller particles and fluxes can vary with magnetic field conditions. The calculated flux of the 30 to 75 nm particles at the PSP is negligible for most of the second orbit, except for an isolated peak at the perihelion. The 30–75 nm particles that were created inwards from 0.16 AU from the Sun are in trapped orbits if the radiation pressure force is weaker than gravity, which is the case for dust from asteroids and for cometary dust that was altered in space. Conclusions. The inner Solar System is the most likely source of dust smaller than 100 nm that enters Earth’s atmosphere and our results suggest the flux is time-variable.

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Section: Estimations Of the Dust Flux: Escaping Particlesmentioning

confidence: 99%

Dust observations from Parker Solar Probe: dust ejection from the inner Solar System

Mann

Czechowski

2021

A&A

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“…Su et al 2013Su et al , 2020Rieke et al 2015;Kimura et al 2020). Calculations of the nanodust trajectories were also made for nanodust around Vega and Fomalhaut (Stamm et al 2019), two stars with a planetary debris disk.…”

Section: Introductionmentioning

confidence: 99%

“…We show that trapping of the nanodust particles in the vicinity of the Sun or other stars is not adversely affected by plasma corotation. Some of our preliminary results were included in Stamm et al (2019). The argument relies on the model of nanodust motion (Czechowski & Mann 2010, 2011, 2018 based on the guiding centre approximation.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of nanodust in the vicinity of a stellar corona: Effect of plasma corotation

Czechowski

Mann

2021

A&A

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Context. In the vicinity of the Sun or other stars, the motion of the coronal and stellar wind plasma must include some amount of corotation, which could affect the dynamics of charged dust particles. In the case of the Sun, this region is now investigated in situ by the Parker Solar Probe. Charged dust particles coming from the vicinity of the Sun can also reach, and possibly be detected by, the Solar Orbiter. Aims. We use numerical simulations and theoretical models to study the effect of plasma corotation on the motion of charged nanodust particles released from the parent bodies moving in Keplerian orbits, with particular attention to the case of trapped particles. Methods. We used two methods: the motion of nanodust is described either by numerical solutions of full equations of motion, or by a two-dimensional (distance vs. radial velocity) model based on the guiding centre approximation. The models of the plasma and magnetic field in the vicinity of the star are based on analytical solutions that satisfy the freezing-in equations. Results. Including plasma corotation does not prevent trapping of nanodust in the vicinity of the Sun or other stars. This result can be understood with the help of the model based on the guiding centre approximation. For the amount of corotation expected near the Sun, the outer limit of the trapped region is almost unaffected. If the corotation persists outside the trapping region, the speed of particles ejected from the Sun is moderately increased. A strong effect of plasma corotation on charged particle dynamics occurs for the star with a high rotation rate and/or a low value of the stellar wind speed.

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“…The expected signals due to dust impacts in the vicinity of the Sun were recently Published by Copernicus Publications on behalf of the European Geosciences Union. 920 C. Baumann et al: Dust sputtering within the inner heliosphere considered based on the results of previous space observations and laboratory studies (Mann et al, 2019). Analysis of FIELDS observations during the three first perihelion passages suggests that the dust density within about 50 solar radii varies by about 50 % between the different encounters (David Malaspina, personal communication, 2020).…”

Section: Introductionmentioning

confidence: 99%

“…Theoretical considerations suggest that the nanodust is trapped under certain conditions in orbits around the Sun (Czechowski and Mann, 2010;Stamm et al, 2019). While the trajectories of dust particles are influenced by the bombardment of solar energetic ions (Ragot and Kahler, 2003), our work concentrates on the survival of nanodust during passages of coronal mass ejections (CMEs) and the solar wind.…”

Section: Introductionmentioning

confidence: 99%

Dust sputtering within the inner heliosphere: a modelling study

2020

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Abstract. The aim of this study is to investigate through modelling how sputtering by impacting solar wind ions influences the lifetime of dust particles in the inner heliosphere near the Sun. We consider three typical dust materials, silicate, Fe0.4Mg0.6O, and carbon, and describe their sputtering yields based on atomic yields given by the Stopping and Range of Ions in Matter (SRIM) package. The influence of the solar wind is characterized by plasma density, solar wind speed, and solar wind composition, and we assume for these parameter values that are typical for fast solar wind, slow solar wind, and coronal mass ejection (CME) conditions to calculate the sputtering lifetimes of dust. To compare the sputtering lifetimes to typical sublimation lifetimes, we use temperature estimates based on Mie calculations and material vapour pressure derived with the MAGMA chemical equilibrium code. We also compare the sputtering lifetimes to the Poynting–Robertson lifetime and to the collision lifetime. We present a set of sputtering rates and lifetimes that can be used for estimating dust destruction in the fast and slow solar wind and during CME conditions. Our results can be applied to solid particles of a few nanometres and larger. The sputtering lifetimes increase linearly with the size of particles. We show that sputtering rates increase during CME conditions, primarily because of the high number densities of heavy ions in the CME plasma. The shortest sputtering lifetimes we find are for silicate, followed by Fe0.4Mg0.6O and carbon. In a comparison between sputtering and sublimation lifetimes we concentrate on the nanodust population. The comparison shows that sublimation is the faster destruction process within 0.1 AU for Fe0.4Mg0.6O, within 0.05 AU for carbon dust, and within 0.07 AU for silicate dust. The destruction by sputtering can play a role in the vicinity of the Sun. We discuss our findings in the context of recent F-corona intensity measurements onboard Parker Solar Probe.

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Dust trajectory simulations around the Sun, Vega, and Fomalhaut

Cited by 7 publications

References 28 publications

Dust observations from Parker Solar Probe: dust ejection from the inner Solar System

Dust observations from Parker Solar Probe: dust ejection from the inner Solar System

Dynamics of nanodust in the vicinity of a stellar corona: Effect of plasma corotation

Dust sputtering within the inner heliosphere: a modelling study

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