Modeling the motion and distribution of interstellar dust inside the heliosphere

Landgraf, Markus

doi:10.1029/1999ja900243

Cited by 116 publications

(125 citation statements)

References 24 publications

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“…The dust dynamics follow the description of Sect. 2, which are largely the same assumptions (except for the β and Q/m parameters) as in Landgraf (1998Landgraf ( , 2000. The Lorentz forces depend on the IMF.…”

Section: Simulation Toolmentioning

confidence: 98%

“…4. Figure 12 gives an overview of the relative importance of the Lorentz force, solar gravitation, and solar radiation pressure force, from Landgraf (1998). Solar gravitation and solar radiation pressure force are combined into one "effective gravitation" term (see Eq.…”

Section: Lorentz Forcesmentioning

confidence: 99%

“…The model on which the simulation tool is based is similar to the one in Landgraf (2000) and Gustafson & Misconi (1979) models, but some extra options are included to optimize the tool for various applications (e.g. for missions at Earth's distance from the Sun).…”

Section: Introductionmentioning

confidence: 99%

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The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

A&A

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Context. Interstellar dust (ISD) is a major component in the formation and evolution of stars, stellar systems, and planets. Astronomical observations of interstellar extinction and polarization, and of the infrared emission of the dust, are the most commonly used technique for characterizing interstellar dust. Besides this, the interstellar dust from the local interstellar cloud enters the solar system owing to the relative motion of the Sun with respect to this cloud. Once in the solar system, in-situ observations can be made by spacecraft using impact ionization detectors and time-of-flight spectrometers like the ones flown on the Cassini, Ulysses, and Galileo, spacecrafts. Also a sample return can be done, as in the Stardust mission. Once in the solar system, the trajectories of these dust grains are shaped by gravitational, solar radiation pressure, and Lorentz forces. The Lorentz forces result from the interaction of the charged dust particles with the interplanetary magnetic field. The ISD densities in the solar system thus depend both on the location in the solar system and on time, correlated to the solar cycle. Aims. This paper aims at giving the reader insight into the flow patterns of ISD when it moves through the solar system. This is useful for designing future in-situ or sample return missions or for knowing whether for specific missions, simplified assumptions can be used for the dust flux and direction, or whether full simulations are needed. Methods. We characterize the flow of ISD through the solar system using simulations of the dust trajectories. We start from the simple case without Lorentz forces and expand to the full simulation. We pay attention to the different ways of modeling the interplanetary magnetic field and discuss the influence of the dust parameters on the resulting flow patterns. Dust densities, fluxes, and directionalities are derived from the trajectory simulations. Different graphics representations are used to gain insight into the flow patterns. As an illustration of how the model can be used, we predict the fluxes and directionalities of the ISD for the Cassini mission. Results. The characteristics of the flow of ISD through the solar system have been investigated to gain insight in the patterns of the flow. The modeling can also be used for predicting dust fluxes for different space missions or planets, and for understanding spacecraft measurements, such as those from Ulysses, Cassini, and Stardust.

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Section: Simulation Toolmentioning

confidence: 98%

Section: Lorentz Forcesmentioning

confidence: 99%

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The flow of interstellar dust into the solar system

Sterken

Altobelli

Kempf

et al. 2012

A&A

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“…Since the simplified models ignore the sector structure of the magnetic field, the reduction of the effective magnetic field leading to the increased probability of particle penetration into the inner solar system (Landgraf 2000;Czechowski & Mann 2003) is missing from these models; (2) bending of the HCS. In calculations with low tilt heliospheric current sheet, the current sheet was found to avoid the stagnation point by bending into the northern or the southern parts of the heliosheath, with the shape of the heliopause becoming asymmetric in result (Pogorelov et al 2004).…”

Section: Relation To the Numerical Models Of The Heliospheric Currentmentioning

confidence: 99%

“…Another is the effect of mixed polarity field on the transport of charged particles. As shown by Jokipii & Levy (1977), drift along the HCS is important for modulation of galactic cosmic rays; the effects of a wavy HCS were also considered (Miyake et al 2005;Usoskin et al 2008) Penetration of small charged grains into the heliosphere is facilitated by effective reduction of the magnetic field in the mixed polarity regions (Landgraf 2000;Czechowski & Mann 2003). Also, the distribution of energetic (>28 keV) particles in the heliosheath, which can now be studied in detail thanks to Voyager observations (Decker et al 2005(Decker et al , 2008Stone et al 2005Stone et al , 2008, is likely to be affected by the drift along the folded current sheet extending to high latitudes.…”

Section: Introductionmentioning

confidence: 99%

Structure of the heliospheric current sheet from plasma convection in time-dependent heliospheric models

Czechowski¹,

Strumik²,

Grygorczuk³

et al. 2010

A&A

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Context. The heliospheric current sheet is a plasma layer dividing the heliosphere into the regions of different magnetic field polarity. Since it is very thin compared to the size of the system, it is difficult to incorporate into the numerical models of the heliosphere. Because of the solar magnetic field reversals and the diverging and slowing down plasma flow in the outer heliosphere, the heliospheric current sheet is expected to have a complicated structure, with important consequences for transport processes in the heliosheath. Aims. We determine the shape and time evolution of the current sheet in selected time-dependent 3-D models of the heliosphere, assuming that the heliospheric current sheet is a tangential discontinuity convected by the plasma flow. Methods. We have derived the shape of the heliospheric current sheet at a given time by following the plasma flow lines originating at the neutral line on the source surface surrounding the Sun. The plasma flow was obtained from numerical MHD or gas-dynamical solutions.Results. The large-scale structure of the magnetic field polarity regions and the heliospheric current sheet in time-dependent asymmetric models of the heliosphere differs from the results obtained in simpler models. In particular, in the forward heliosheath it is characterized by secondary folds in the heliospheric current sheet that are caused by the solar wind latitudinal variation over the solar cycle. We present examples illustrating some cases of interest: a "bent" current sheet, and the HCS structure during the magnetic field reversal at the solar maximum. We also discuss the evolution of the magnetic polarity structure in the region close to the heliopause.

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Introduction: Paleoheliosphere versus PaleoLISM

Frisch

Solar Journey: The Significance of Our Galactic Environment for the Heliosphere and Earth

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Speculations that encounters with interstellar clouds modify the terrestrial climate have appeared in the scientific literature for over 85 years. The articles in this volume seek to give substance to these speculations by examining the exact mechanisms that link the pressure and composition of the interstellar medium surrounding the Sun to the physical properties of the inner heliosphere at the Earth.

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Modeling the motion and distribution of interstellar dust inside the heliosphere

Cited by 116 publications

References 24 publications

The flow of interstellar dust into the solar system

The flow of interstellar dust into the solar system

Structure of the heliospheric current sheet from plasma convection in time-dependent heliospheric models

Introduction: Paleoheliosphere versus PaleoLISM

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