Nanodust dynamics during a coronal mass ejection

Czechowski, A.; Kleimann, J.

doi:10.5194/angeo-35-1033-2017

Cited by 12 publications

(17 citation statements)

References 37 publications

(58 reference statements)

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“…However, in a recent study (Czechowski & Kleimann 2017) based on a numerical MHD model of the solar corona during a coronal mass ejection (CME), it was found that some predictions of our model remain valid. In particular, the trapped nanodust population predicted by Czechowski & Mann (2010 was found to appear and survive in the simulated CME.…”

Section: Discussionmentioning

confidence: 78%

“…The drag force due to ion impacts on the grain (Minato et al 2004) was found in Czechowski & Kleimann (2017) to have a significant effect on nanodust (particularly, the trapped component) in the solar corona. We therefore included, in part of our simulations, the proton drag force described by the same approximate expression as in Czechowski & Kleimann (2017), with the plasma parameters taken from our models (1 to 3).…”

Section: Discussionmentioning

confidence: 99%

“…We therefore included, in part of our simulations, the proton drag force described by the same approximate expression as in Czechowski & Kleimann (2017), with the plasma parameters taken from our models (1 to 3). For particles bypassing the Sun by more than ∼0.015 AU, we found drag to be unimportant.…”

Section: Discussionmentioning

confidence: 99%

“…18). For the case of trapped nanodust studied in Czechowski & Kleimann (2017) the particles return repeatedly to the vicinity of the Sun and the effect of drag is cumulative, leading to contraction of the orbit and ultimate destruction of the particle. According to present simulations, the nanodust particles emitted from high-eccentricity orbits do not approach close to the Sun more than once.…”

Section: Effect Of the Proton Drag Forcementioning

confidence: 99%

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Dynamics of nanodust particles emitted from elongated initial orbits

Czechowski

Mann

2018

A&A

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Context. Because of high charge-to-mass ratio, the nanodust dynamics near the Sun is determined by interplay between the gravity and the electromagnetic forces. Depending on the point where it was created, a nanodust particle can either be trapped in a non-Keplerian orbit, or escape away from the Sun, reaching large velocity. The main source of nanodust is collisional fragmentation of larger dust grains, moving in approximately circular orbits inside the circumsolar dust cloud. Nanodust can also be released from cometary bodies, with highly elongated orbits. Aims. We use numerical simulations and theoretical models to study the dynamics of nanodust particles released from the parent bodies moving in elongated orbits around the Sun. We attempt to find out whether these particles can contribute to the trapped nanodust population. Methods. We use two methods: the motion of nanodust is described either by numerical solutions of full equations of motion, or by a two-dimensional (heliocentric distance vs. radial velocity) model based on the guiding-center approximation. Three models of the solar wind are employed, with different velocity profiles. Poynting-Robertson and the ion drag are included. Results. We find that the nanodust emitted from highly eccentric orbits with large aphelium distance, like those of sungrazing comets, is unlikely to be trapped. Some nanodust particles emitted from the inbound branch of such orbits can approach the Sun to within much shorter distances than the perihelium of the parent body. Unless destroyed by sublimation or other processes, these particles ultimately escape away from the Sun. Nanodust from highly eccentric orbits can be trapped if the orbits are contained within the boundary of the trapping region (for orbits close to ecliptic plane, within ∼0.16 AU from the Sun). Particles that avoid trapping escape to large distances, gaining velocities comparable to that of the solar wind.

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Section: Discussionmentioning

confidence: 78%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Effect Of the Proton Drag Forcementioning

confidence: 99%

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Dynamics of nanodust particles emitted from elongated initial orbits

Czechowski

Mann

2018

A&A

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“…We further assume that the magnetic field does not vary in time. A force caused by momentum transfer between the streaming stellar wind particles and the dust particles was considered by Czechowski & Kleimann (2017), but is not considered here. The full equation of motion for the dust particles can then be written as…”

Section: Acting Forces and Equation Of Motionmentioning

confidence: 99%

Dust trajectory simulations around the Sun, Vega, and Fomalhaut

Stamm

Czechowski

Mann

et al. 2019

A&A

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Context. Vega and Fomalhaut display a thermal emission brightness that could possibly arise from hot dust near the stars, an inner extension of their planetary debris disks. An idea has been suggested that nanometer-sized dust particles are kept in the vicinity of the stars by electromagnetic forces. This resembles the trapping that model calculations show in the corotating magnetic field in the inner heliosphere within approximately 0.2 AU from the Sun. Aims. The aim of this work is to study whether the trapping of dust due to electromagnetic forces acting on charged dust near the Sun can occur around Vega and Fomalhaut and what are the conditions for trapping. Methods. We studied the dust trajectories with numerical calculations of the full equation of motion, as well as by using the guiding center approximation. We assumed a constant dust charge and a Parker-type magnetic field, which we estimated for the two stars.Results. We find no bound trajectories of charged particles around Vega or Fomalhaut as long as the radiation pressure force exceeds the gravitational force, that is, for particles smaller than 1 µm. A trapping zone could exist inside of 0.02 AU for Vega and 0.025 AU for Fomalhaut, but only for those particles with radiation pressure force smaller than gravitational force. In comparison to the Sun, the trapping conditions would occur closer to the stars because their faster rotation leads to a more closely wound-up magnetic field spiral. We also show that plasma corotation can be consistent with trapping. Our model calculations show that the charged particles are accelerated to stellar wind velocity very quickly, pass 1 AU after approximately three days, and are further ejected outward where they pass the debris disks at high velocity. We find this for particles with a surface charge-to-mass ratio larger than 10 −6 elementary charges per proton mass for both negatively and positively charged dust and independent of the strength of the radiation pressure force. Based on charging assumptions, this would correspond to dust of sizes 100 nm and smaller.

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