SIXTEEN YEARS OF<i>ULYSSES</i>INTERSTELLAR DUST MEASUREMENTS IN THE SOLAR SYSTEM. I. MASS DISTRIBUTION AND GAS-TO-DUST MASS RATIO

Krüger, Harald; Strub, Peter; Grün, E.; Sterken, Veerle

doi:10.1088/0004-637x/812/2/139

Cited by 55 publications

(62 citation statements)

References 101 publications

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“…This result is consistent with the result of Krüger et al (2015), who detected an enhanced concentration of large (more than 1 microns) grains in the interstellar dust flow entering the Solar system precisely from the northern Galactic hemisphere together with the flow of neutral hydrogen and helium based on data from the dust detector onboard the Ulysses spacecraft. Moreover, the Galactic coordinates of the entry point of this flow into the Solar system (near l = 3…”

Section: Branch Giants Closer Than 700 Pcsupporting

confidence: 92%

Extinction law at a distance up to 25 kpc toward the Galactic poles

Gontcharov

2016

Astron. Lett.

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characteristics and properties of the Milky Way Galaxy, interstellar medium. Photometry from the Tycho-2, 2MASS, and WISE catalogues for clump and branch giants at a distance up to 25 kpc toward the Galactic poles has allowed the variations of various characteristics of the infrared interstellar extinction law with distance to be analyzed. The results obtained by the extinction law extrapolation method are consistent for different classes of stars and different characteristics as well as with previous studies. The conventional extinction law with a low infrared extinction is characteristic of only a thin layer no farther than 100 pc from the Galactic plane and of two thin layers near Z = −600 and +500 pc. Far from the Galactic plane, in the Galactic halo, the infrared extinction law is different: the extinction in the Ks, W 1, W 2, W 3, and W 4 bands is, respectively, 0.17, 0.16, 0.16, 0.07, and 0.03 of the extinction in the V band. The accuracy of these coefficients is 0.03. If the extinction law reflects primarily the grain size distribution, then the fraction of large dust grains far from the Galactic plane is greater than that in the circumsolar interstellar medium.

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Section: Branch Giants Closer Than 700 Pcsupporting

confidence: 92%

Extinction law at a distance up to 25 kpc toward the Galactic poles

Gontcharov

2016

Astron. Lett.

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“…In addition, the size distributions of the polarizing grains are poorly known. In situ measurements of interstellar dust grains by Ulysses and other spacecraft show that the size range extends from ∼0.04 to 2.0 μm if the grains are compact silicates (Frisch et al 1999;Landgraf et al 2000;Krueger et al 2015;Sterken et al 2015). Since the wavelength of maximum polarization strengths depend on grain sizes, composition, and porosity (Serkowski et al 1975;Andersson & Potter 2006;Andersson 2015), the polarization strengths can not be compared because of the different spectral bands of the various data sets.…”

Section: Polarization Data Used To Determine the Magnetic Field Direcmentioning

confidence: 99%

CHARTING THE INTERSTELLAR MAGNETIC FIELD CAUSING THEINTERSTELLAR BOUNDARY EXPLORER(IBEX) RIBBON OF ENERGETIC NEUTRAL ATOMS

Frisch

Berdyugin

Piirola

et al. 2015

ApJ

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The interstellar magnetic field (ISMF) near the heliosphere is a fundamental component of the solar galactic environment that can only be studied using polarized starlight. The results of an ongoing survey of the linear polarizations of local stars are analyzed with the goal of linking the ISMF that shapes the heliosphere to the nearby field in interstellar space. We present new results on the direction of the magnetic field within 40 pc obtained from analyzing polarization data using a merit function that determines the field direction that provides the best fit to the polarization data. Multiple magnetic components are identified, including a dominant interstellar field, B POL , that is aligned with the direction ℓ, b = 36°.2, 49°.0 (±16°.0). Stars tracing B POL have the same mean distance as stars that do not trace B POL , but show weaker average polarizations consistent with a smaller column density of polarizing material. B POL is aligned with the ISMF traced by the IBEX Ribbon to within 7.6 7.6 14.9 -+ degrees. The variations in the polarization position angle directions derived from the data that best match B POL indicate a low level of magnetic turbulence, ∼9°±1°. The direction of B POL is obtained after excluding polarization data tracing a separate magnetic structure that appears to be associated with interstellar dust deflected around the heliosphere. The velocities of local interstellar clouds relative to the Local Standard of Rest (LSR) increase with the angles between the LSR velocities and B POL , indicating that the kinematics of local interstellar material is ordered by the ISMF. The Loop I superbubble that extends close to the Sun contains dust that reddens starlight and whose distance is determined by the color excess E(B − V) of starlight. Polarizations caused by grains aligned with respect to B POL are consistent with the location of the Sun in the rim of the Loop I superbubble. An angle of 76.8 27.6 23.5 -+ between B POL and the bulk LSR velocity the local interstellar material indicates a geometry that is consistent with an expanding superbubble. The efficiency of grain alignment in the local interstellar medium has been assessed using stars where both polarization data and hydrogen column density data are available. Nearby stars appear to have larger polarizations than expected based on reddened sightlines, which is consistent with previous results, but uncertainties are large. Optical polarization and color excess E(B − V) data indicate the presence of nearby interstellar dust in the BICEP2 field. Color excess E(B − V) indicates an optical extinction of A V >0.6 in the BICEP2 field, while the polarization data indicate that A V >0.09 mag. The IBEX Ribbon ISMF extends to the boundaries of the BICEP2 region.

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“…The corresponding grains mass ranges are, roughly, M > 10 −14 kg for β ≤ 0.2, 10 −16 kg < M < 10 −14 kg for 0.2 < β < 1 and 5·10 −17 kg < M < 10 −16 kg for β > 1. Finally, to provide an upper value for the kinetic energy flux of impactors described by their β value, we have done the following simplification, which we believe is sufficient for the purpose of this study: Considering the ISD mass distribution and flux values reported by (Krüger et al, ), we apply a flux of 5·10 −5 m −2 /s to the particles with β = 1.3, 10 −5 m −2 /s to the particles with β = 1 and 10 −6 m −2 /s to the particles with β = 0.2.…”

Section: Interplanetary Dust Impactors: Methods and Simulation Resultsmentioning

confidence: 99%

Space Weathering Induced Via Microparticle Impacts: 1. Modeling of Impact Velocities and Flux of Micrometeoroids From Cometary, Asteroidal, and Interstellar Origin in the Main Asteroid Belt and the Near‐Earth Environment

et al. 2019

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The processes of alteration of airless bodies exposed to the space environment are referred to be as “space weathering.” Multiple agents contribute generally to space weathering, to an extent that depends on the specific location of the surface within the solar system. Typical space weathering agents encountered in the solar system are solar radiation, solar wind and cosmic rays, magnetospheric plasma (e.g., at Jupiter or Saturn), and cosmic dust. The effect of space weathering is generally assessed by measuring the surfaces optical properties, for example, by near‐infrared spectroscopy. The alteration of the surfaces is due to a cumulative effect over time of all agents. We investigate in this paper the contribution of micrometeoroid (dust) bombardment on different asteroids, by using the Interplanetary Micrometeoroid Environment Model for the interplanetary dust populations and a simplified model of interstellar dust dynamics. We quantify, for different representative asteroids (main belt and Near Earth Objects [NEOs]), the particle cumulative flux, mass flux, impact velocity, and the kinetic impact energy deposited. This work is primarily intended to support laboratory work investigating the effect of energy deposition onto sample surfaces, as well as astronomical observations of optical properties of asteroid surfaces.

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SIXTEEN YEARS OFULYSSESINTERSTELLAR DUST MEASUREMENTS IN THE SOLAR SYSTEM. I. MASS DISTRIBUTION AND GAS-TO-DUST MASS RATIO

Cited by 55 publications

References 101 publications

Extinction law at a distance up to 25 kpc toward the Galactic poles

Extinction law at a distance up to 25 kpc toward the Galactic poles

CHARTING THE INTERSTELLAR MAGNETIC FIELD CAUSING THEINTERSTELLAR BOUNDARY EXPLORER(IBEX) RIBBON OF ENERGETIC NEUTRAL ATOMS

Space Weathering Induced Via Microparticle Impacts: 1. Modeling of Impact Velocities and Flux of Micrometeoroids From Cometary, Asteroidal, and Interstellar Origin in the Main Asteroid Belt and the Near‐Earth Environment

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