Interstellar dust in the solar system: model versus in situ spacecraft data

Krüger, Harald; Strub, Peter; Altobelli, Nicolás; Sterken, Veerle; Srama, R.; Grün, E.

doi:10.1051/0004-6361/201834316

Cited by 22 publications

(19 citation statements)

References 55 publications

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“…However, in addition to gravity and radiation pressure, dust particles in this size range also respond to electromagnetic forces, as they carry a positive charge and react on interplanetary magnetic fields, resulting in temporal variability of the ISD flux with solar cycle, alternating between periods of focusing toward and away from the ecliptic plane (Landgraf 2000;Sterken et al 2012Sterken et al , 2015Strub et al 2019). While the basic interactions of ISD within the heliosphere appear to be well understood, our current models (calibrated using Ulysses data) can only reproduce the measurements of all spacecraft data of the variability of their flux measured to date within a factor of 2−3 (Krüger et al 2019). Hence, the question arises whether or not SDC detected ISD during its 15 yr cruise across the solar system.…”

Section: Isd Contributionmentioning

confidence: 96%

“…Hence, according to Equation (2), the much smaller and faster ISD will be assigned a larger IDP mass. With an expected size of 0.3 μm, speed of ;26 km s −1 , and ecliptic longitude of λ ISD ; 259°shown in Figure 3, we can predict what size SDC would mistake these ISD impacts as (Frisch et al 2009;Landgraf et al 2003;McComas et al 2012;Krüger et al 2015Krüger et al , 2019. The top panel of Figure 7 shows the anticipated impact speed of a 0.3 μm ISD compared to the assumed speed used in the IDP conversion from charge to mass in Figure 4.…”

Section: Isd Contributionmentioning

confidence: 96%

“…Several in situ dust detectors on various spacecraft have covered a broad range of the solar system. HEOS 2 and HELIOS observed the IDP environment near 1 au (Dietzel et al 1973), while both Galileo and Ulysses measured from Earth to Jupiter, including measurements above/below the ecliptic plane (Krüger et al 2019). Cassini observed IDPs between Jupiter and Saturn (Altobelli et al 2007), while Pioneer 10 and 11 covered up to 9 and 18 au, respectively (Humes 1980).…”

Section: Introductionmentioning

confidence: 99%

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Student Dust Counter Status Report: The First 50 au

et al. 2022

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The Venetia Burney Student Dust Counter (SDC) is an in situ dust detector on board the New Horizons spacecraft measuring the interplanetary dust particle (IDP) distribution for grains with mass m > 10−12 g. SDC provides a near-continuous measure of the interplanetary dust environment, with recent results spanning beyond 50 au. This coverage includes the Edgeworth–Kuiper Belt (EKB), suggested by numerical models to be the dominant source of IDP in the outer solar system. Here we present the updated dust density distribution to 50 au and compare estimated flux values to existing theoretical models. SDC observes peak dust flux and densities near 42 au, and we expect a decay with increasing heliocentric distance. Based on SDC measurements, we also discuss the effects of IDP generation, transport, and loss on the evolution of the surfaces of EKB objects, the continual intermixing of their surface material, and the general tendency to homogenize their spectral properties. Continued SDC measurements remain critical for revealing the large-scale structure of the EKB and to guide the interpretation of dust disks around other stars. Additionally, we consider the potential of an interstellar dust (ISD) and “outer” Kuiper Belt contribution to SDC measurements and its effect on anticipated SDC flux values beyond 50 au, and we show that the inclusion of either source to the predicted model results in a noticeable deviation in anticipated SDC measurements beyond 50 au. Current and future SDC measurements also serve to constrain the relative contribution of ISD to SDC’s flux and density estimates.

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Section: Isd Contributionmentioning

confidence: 96%

Section: Isd Contributionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

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Student Dust Counter Status Report: The First 50 au

et al. 2022

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“…The large depletion of iron from the gas phase of LISM clouds requires that most of the iron is resident in dust grains that are likely olivene silicates (Redfield & Linsky 2008;. In situ measurements of interstellar dust by experiments on Ulysses and other spacecraft sample dust grains with sizes larger than about 0.3 µm, because solar radiation pressure and heliospheric magnetic fields filter out most of the smaller grains (Mann 2010;Krüger et al 2019). Larger grains are expected to reach the inner solar system without significant changes in direction or speed.…”

Section: Sightlines To Nearby Starsmentioning

confidence: 99%

The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and ⁶⁰Fe Accretion*

Linsky

Redfield

Tilipman

2019

ApJ

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We describe the interface between the outer heliosphere and the local interstellar medium (LISM) surrounding the Sun. The components of the inner LISM are the four partially ionized clouds [the Local Interstellar Cloud (LIC), G cloud, Blue cloud, andAql cloud] that are in contact with the outer heliosphere, and ionized gas produced by EUV radiation primarily from ǫ CMa. We construct the three-dimensional shape of the LIC based on interstellar line absorption along 62 sightlines and show that in the direction of ǫ CMa, β CMa, and Sirius B the neutral hydrogen column density from the center of the LIC is a minimum. We call this region the "hydrogen hole". In this direction, the presence of Blue cloud absorption and the absence of LIC absorption can be simply explained by the Blue cloud lying just outside of the heliosphere. We propose that the outer edge of the Blue cloud is a Strömgren shell driven toward the heliosphere Corresponding author: Jeffrey L. Linsky jlinsky@jila.colorado.edu * Based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS AR-09525.01A. These observations are associated with programs #12475, 12596.Linsky, Redfield, and Tilipman by high pressures in the H II region. We find that the vectors of neutral and ionized helium flowing through the heliosphere are inconsistent with the LIC flow vector, and that the nearby intercloud gas is consistent with ionization by ǫ CMa and other stellar sources without requiring additional sources of ionization or million degree plasma. In the upwind direction, the heliosphere is passing through an environment of several LISM clouds, which may explain the recent influx of interstellar grains containing 60 Fe from supernova ejecta measured in Antarctica snow.

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“…The spacecraft were equipped with two in situ dust sensors each, which measured the distribution of interplanetary dust in the inner Solar System for the first time (Grün et al 1980;Grün 1981). Altobelli et al (2006) re-analysed the Helios dust data searching for interstellar impactors (Grün et al 1994;Krüger et al 2019b). The authors recognised a cluster of seven impacts in a very narrow range of the spacecraft's true anomaly angle.…”

Section: Introductionmentioning

confidence: 99%

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

Krüger

Strub

Sommer

et al. 2020

A&A

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Context. Cometary meteoroid trails exist in the vicinity of comets, forming a fine structure of the interplanetary dust cloud. The trails consist predominantly of the largest cometary particles (with sizes of approximately 0.1 mm-1 cm), which are ejected at low speeds and remain very close to the comet orbit for several revolutions around the Sun. In the 1970s, two Helios spacecraft were launched towards the inner Solar System. The spacecraft were equipped with in situ dust sensors which measured the distribution of interplanetary dust in the inner Solar System for the first time. Recently, when re-analysing the Helios data, a clustering of seven impacts was found, detected by Helios in a very narrow region of space at a true anomaly angle of 135 ± 1 • , which the authors considered as potential cometary trail particles. However, at the time, this hypothesis could not be studied further. Aims. We re-analyse these candidate cometary trail particles in the Helios dust data to investigate the possibility that some or all of them indeed originate from cometary trails and we constrain their source comets. Methods. The Interplanetary Meteoroid Environment for eXploration (IMEX) dust streams in space model is a new and recently published universal model for cometary meteoroid streams in the inner Solar System. We use IMEX to study the traverses of cometary trails made by Helios. Results. During ten revolutions around the Sun, the Helios spacecraft intersected 13 cometary trails. For the majority of these traverses the predicted dust fluxes are very low. In the narrow region of space where Helios detected the candidate dust particles, the spacecraft repeatedly traversed the trails of comets 45P/Honda-Mrkos-Pajdušáková and 72P/Denning-Fujikawa with relatively high predicted dust fluxes. The analysis of the detection times and particle impact directions shows that four detected particles are compatible with an origin from these two comets. By combining measurements and simulations we find a dust spatial density in these trails of approximately 10 −8-10 −7 m −3. Conclusions. The identification of potential cometary trail particles in the Helios data greatly benefited from the clustering of trail traverses in a rather narrow region of space. The in situ detection and analysis of meteoroid trail particles which can be traced back to their source bodies by spacecraft-based dust analysers provides a new opportunity for remote compositional analysis of comets and asteroids without the necessity to fly a spacecraft to or even land on those celestial bodies. This provides new science opportunities for future missions like DESTINY + (Demonstration and Experiment of Space Technology for INterplanetary voYage with Phaethon fLyby and dUst Science), Europa Clipper, and the Interstellar Mapping and Acceleration Probe.

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Interstellar dust in the solar system: model versus in situ spacecraft data

Cited by 22 publications

References 55 publications

Student Dust Counter Status Report: The First 50 au

Student Dust Counter Status Report: The First 50 au

The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and ⁶⁰Fe Accretion*

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

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Interstellar dust in the solar system: model versus in situ spacecraft data

Cited by 22 publications

References 55 publications

Student Dust Counter Status Report: The First 50 au

Student Dust Counter Status Report: The First 50 au

The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and 60Fe Accretion*

Helios spacecraft data revisited: detection of cometary meteoroid trails by following in situ dust impacts

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The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and ⁶⁰Fe Accretion*