Orbital and physical characteristics of micrometeoroids in the inner solar system as observed by Helios 1

Grün, E.; Pailer, N.; Fechtig, H.; Kissel, J.

doi:10.1016/0032-0633(80)90022-7

Cited by 95 publications

(46 citation statements)

References 18 publications

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“…These two components may have different optical properties and, due to their different initial orbits, they may also have different distributions of orbital elements. The existence of two different dust populations in the ecliptic plane with different bulk densities and different relative velocities to the spacecraft has been revealed from the Helios in situ measurements and explained with a component of cometary dust and a component of asteroidal dust particles (Grün et al 1980, Fechtig 1989.…”

Section: Introductionmentioning

confidence: 99%

Dust Cloud near the Sun

Mann

Krivov

Kimura

2000

Icarus

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Section: Introductionmentioning

confidence: 99%

Dust Cloud near the Sun

Mann

Krivov

Kimura

2000

Icarus

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“…While the impactor distribution of the ecliptic sensor can almost be completely explained by impactors on circular or low eccentric orbits, highly eccentric orbits are needed to account for the impactors distribution of the south sensor. This fact was already discussed by Grün et al (1980). According to the interpretation of this author, the ecliptic sensor was not sensitive to particles of low material density on high eccentric orbits because of the foil protecting the instrument against thermal radiation (see Sect.…”

Section: Data Descriptionmentioning

confidence: 88%

“…The impactors detected with the south sensor and those obtained with the ecliptic sensor are shown in a (η, θ)-diagram in Fig. 6, (Grün et al 1980). The contour-lines represent the sensitive area of the instrument to populations on circular prograde orbits.…”

Section: Data Descriptionmentioning

confidence: 99%

A new look into the Helios dust experiment data: presence of interstellar dust inside the Earth's orbit

Altobelli¹,

Grün²,

Landgraf³

2006

A&A

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An analysis of the Helios in situ dust data for interstellar dust (ISD) is presented in this work. Recent in situ dust measurements with impact ionization detectors on-board various spacecraft (Ulysses, Galileo, and Cassini) showed the deep penetration of an ISD stream into the Solar System. The Helios dust data provide a unique opportunity to monitor and study the ISD stream alteration at very close heliocentric distances. This work completes therefore the comprehensive picture of the ISD stream properties within the heliosphere. In particular, we show that gravitation focusing facilitates the detection of big ISD grains (micrometer-size), while radiation pressure prevents smaller grains from penetrating into the innermost regions of the Solar System. A flux value of about 2.6±0.3×10−6 m −2 s −1 is derived for micrometer-size grains. A mean radiation pressure-to-gravitation ratio (so-called β ratio) value of 0.4 is derived for the grains, assuming spheres of astronomical silicates to modelize the grains surface optical properties. From the ISD flux measured on the Helios trajectory, we infer a lower limit of 3 ± 3 × 10 −25 kg m −3to the spatial mass density of micron-sized grains in the Local Interstellar Cloud (LIC). In addition, compositional clues for ISD grains are obtained from the data provided by the time-of-flight mass spectrometer subsystem of the Helios instrument. No clustering of single minerals is observed but rather a varying mixture of various minerals and carbonaceous compounds.

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“…In-situ data from such instruments have been obtained over several decades; e.g. detectors on Pioneers 8 and 9 [4,60], HEOS-2 [30], Helios [23], Hiten [31]. The Galileo [24] and Ulysses [25] detectors have returned unprecedented data, and now, the Cassini CDA [54] offers a similar ionization detector, but with the capability to resolve time of flight mass spectra of impacting dust (e.g.…”

Section: Dust Camera 3 (Dc3)mentioning

confidence: 99%

DuneXpress

et al. 2008

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The DuneXpress observatory will characterize interstellar and interplanetary dust in-situ, in order to provide crucial information not achievable with remote sensing astronomical methods. Galactic interstellar dust constitutes the solid phase of matter from which stars and planetary systems form. Interplanetary dust, from comets and asteroids, represents remnant material from bodies at different stages of early solar system evolution. Thus, studies of interstellar and interplanetary dust with DuneXpress in Earth orbit will provide a comparison between the composition of the interstellar medium and primitive planetary objects. Hence DuneXpress will provide insights into the physical conditions during planetary system formation. This comparison of interstellar and interplanetary dust addresses directly themes of highest priority in astrophysics and solar system science, which are described in ESA's Cosmic Vision. The discoveries of interstellar dust in the outer and inner solar system during the last decade suggest an innovative approach to the characteriza-

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Orbital and physical characteristics of micrometeoroids in the inner solar system as observed by Helios 1

Cited by 95 publications

References 18 publications

Dust Cloud near the Sun

Dust Cloud near the Sun

A new look into the Helios dust experiment data: presence of interstellar dust inside the Earth's orbit

DuneXpress

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