Sample return of interstellar matter (SARIM)

Srama, R.; Stephan, T.; Grün, E.; Pailer, N.; Kearsley, A. T.; Graps, A. L.; Laufer, René; Ehrenfreund, P.; Altobelli, Nicolás; Altwegg, Kathrin; Auer, S.; Baggaley, J.; Burchell, M. J.; Colangeli, L.; Esposito, F.; Green, Simon; Henkel, H.; Horányi, M.; Jäckel, A.; Kempf, S.; McBride, Neil; Moragas-Klostermeyer, G.; Krüger, Harald; Palumbo, P.; Srowig, A.; Trieloff, M.; Tsou, P.; Sternovsky, Z.; Zeile, Oliver; Röser, Hans‐Peter

doi:10.1007/s10686-008-9088-7

Cited by 14 publications

(11 citation statements)

References 60 publications

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“…Measurements of the ISD flux along the orbits of asteroids, Mars or Jupiter are very well suited to characterizing the ISD dynamics, size distribution, and grain composition with time. Suited space missions were proposed to ESA, such as DUNEeXpress (Srama et al 2006), SARIM (Srama et al 2009), or SARIM PLUS (Srama et al 2012). Cassini will use the opportunity to continue ISD measurements at Saturn in the remaining years of the tour.…”

Section: Discussionmentioning

confidence: 99%

The filtering of interstellar dust in the solar system

Sterken

Altobelli

Kempf

et al. 2013

A&A

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Context. Theoretical predictions demonstrate that small (<0.1 µm) interstellar grains are mostly excluded from reaching the planetary system by electromagnetic interactions in the heliopause region and in the inner heliosphere. Bigger interstellar grains have been recorded in the planetary system by dust measurements on board Ulysses and other spacecraft. It was found that the interstellar dust flux is modulated by the interplanetary magnetic field. Aims. The objective of this study is to analyze the heliospheric filtering of the interstellar dust flow through the solar system and throughout the solar cycle. In the heliosphere the dynamics of interstellar dust is governed by the gravitational pull of the Sun, by the repulsion of solar radiation, and by the deflection caused by the interaction of the charged interstellar dust (ISD) grains with the interplanetary magnetic field. These interactions are described by the parameters of the radiation pressure constant β and the charge-to-mass ratio Q/m, which depend on the particle's size, physical properties, and composition. A previous paper studied the flow characteristics of ISD moving through the solar system were studied. In this follow-up paper, we focus on how the ISD size distribution varies during its passage through the solar system. Methods. In a parametric study of 70 different β and Q/m values, we calculated interstellar dust trajectories starting at the boundary of the heliosphere with starting times spread over a complete solar cycle of 22 years. Results. As a result we obtained the interstellar dust flux and dust speed for these times and positions and demonstrate the effects of the filtering on the dust size distributions. The size distribution of ISD observed at any time and at any position in the planetary system is strongly modified from when it entered the heliosphere. Peaks in relative flux of 10 times the original flux possibly depend on the grain size and place and time in the solar system. We did a detailed study of three cases of the flux and size distribution of interstellar grains reaching the planets Saturn, Jupiter, and the main-belt asteroid Ceres. These cases are used to get a first idea of what a dust detector or collector on a mission to these bodies might see of ISD.

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Section: Discussionmentioning

confidence: 99%

The filtering of interstellar dust in the solar system

Sterken

Altobelli

Kempf

et al. 2013

A&A

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“…comm. ), and for future dust astronomy space missions aiming at the in-situ analysis and sample return of interstellar dust (CosmicDUNE, SARIM; Grün et al 2005;Srama et al 2008).…”

Section: Discussionmentioning

confidence: 99%

Interstellar Dust Inside and Outside the Heliosphere

Krüger

Grün

2008

Space Sci Rev

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In the early 1990s, after its Jupiter flyby, the Ulysses spacecraft identified interstellar dust in the solar system. Since then the in-situ dust detector on board Ulysses continuously monitored interstellar grains with masses up to 10 −13 kg, penetrating deep into the solar system. While Ulysses measured the interstellar dust stream at high ecliptic latitudes between 3 and 5 AU, interstellar impactors were also measured with the in-situ dust detectors on board Cassini, Galileo and Helios, covering a heliocentric distance range between 0.3 and 3 AU in the ecliptic plane. The interstellar dust stream in the inner solar system is altered by the solar radiation pressure force, gravitational focussing and interaction of charged grains with the time varying interplanetary magnetic field. The grains act as tracers of the physical conditions in the local interstellar cloud (LIC). Our in-situ measurements imply the existence of a population of 'big' interstellar grains (up to 10 −13 kg) and a gas-to-dust-mass ratio in the LIC which is a factor of 1.5-2 larger than the one derived from astronomical observations, indicating a concentration of interstellar dust in the very local interstellar medium. Until 2004, the interstellar dust flow direction measured by Ulysses was close to the mean apex of the Sun's motion through the LIC, while in 2005, the data showed a 30°shift, the reason of which is presently unknown. We review the results from spacecraft-based in-situ interstellar dust measurements in the solar system and their implications for the physical and chemical state of the LIC.

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“…The results and methods presented here provide quantitative constraints on the thermal heating experienced by captured dust grains in the Stardust cometary dust collectors and can potentially be applied to modeling the interstellar dust collection side as well. Given the success of the Stardust Mission and the proposed use of aerogel in future sample return missions Srama et al 2008), understanding the capture and track formation processes is of critical importance in maximizing the scientific output of these missions.…”

Section: Discussionmentioning

confidence: 99%

Time evolution and temperatures of hypervelocity impact‐generated tracks in aerogel

Domínguez

2009

Meteorit & Planetary Scien

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available online at http://meteoritics.org Time evolution and temperatures of hypervelocity impact-generated tracks in aerogelGerardo DOMINGUEZ Here, a general model of track formation that allows for the existence of partially and completely vaporized aerogel material in tracks is developed. It is shown that under certain conditions, this general track model reduces to the kinetic "snowplow" model that has previously been proposed. It is also shown, based on energetic considerations, that track formation is dominated by an expansion that is snowplow-like in the later stages of track formation. The equation of motion for this snowplow-like stage can be solved analytically, thus placing constraints on the amount of heating experienced by cometary dust fragments embedded in track walls. It is found that the heating of these fragments, for a given impact velocity, is expected to be greater for those embedded in larger tracks. Given the expected future use of aerogels for sample return missions, the results presented here imply that the choice of aerogel compositions can have a significant effect on the modification of samples captured and retrieved by these collectors.

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Sample return of interstellar matter (SARIM)

Cited by 14 publications

References 60 publications

The filtering of interstellar dust in the solar system

The filtering of interstellar dust in the solar system

Interstellar Dust Inside and Outside the Heliosphere

Time evolution and temperatures of hypervelocity impact‐generated tracks in aerogel

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