Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

Moreno, Fernando; Guirado, D.; Muñoz, Olga; Bertini, Ivano; Tubiana, C.; Güttler, C.; Fulle, M.; Rotundi, A.; Corte, Vincenzo Della; Ivanovski, S.; Rinaldi, G.; Bockelée‐Morvan, Dominique; Захаров, Владимир; Agarwal, Jessica; Mottola, S.; Tóth, I.; Frattin, E.; Lara, L. M.; Gutiérrez, P. J.; Lin, Z. Y.; Kolokolova, L.; Sierks, H.; Naletto, G.; Lamy, Philippe; Rodrigo, R.; Koschny, D.; Davidsson, B.; Barucci, M. A.; Bertaux, J. L.; Bodewits, Dennis; Cremonese, G.; Deppo, V. Da; Debei, S.; Cecco, M. De; Deller, Jakob; Fornasier, S.; Ip, W. H.; Keller, H. U.; Lazzarin, M.; López-Moreno, J. J.; Marzari, F.; Shi, Xian

doi:10.3847/1538-3881/aae526

Cited by 24 publications

(21 citation statements)

References 47 publications

(46 reference statements)

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“…The shaded areas correspond to the measurements in the 67P coma. sistent with constraints obtained for 67P dust (Bockelée-Morvan et al 2017;Mannel et al 2017;Ott et al 2017;Schloerb et al 2017;Moreno et al 2018;Markkanen et al 2018). For f iso = 0.8 (solution obtained for Θ = 0.1) and β = 2.5 (respectively β = 3.0), a crit is in the range 0.6 to 6 cm (respectively 0.15-1.7 cm).…”

Section: Phase Variation Of the Color Temperaturesupporting

confidence: 83%

“…Then, the phase reddening observed in the 67P coma could be related to the porous structure of the particles, providing those contributing to scattered light are sufficiently large. The relative similarity in the phase curves of the dust coma and surface (especially the backscattering enhancement) is consistent with the predominance of large and fluffy dust particles in the coma, as, e.g., discussed by Moreno et al (2018), Bertini et al (2019) and Markkanen et al (2018). Other evidence for relatively large (≥ 10 µm) scatterers in the coma of 67P include dust tail modeling (Moreno et al 2017) and the unexpected low amount of submicron and micron-sized particles collected by the Rosetta's MI-DAS experiment (Mannel et al 2017).…”

Section: Phase Reddeningsupporting

confidence: 82%

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VIRTIS-H observations of the dust coma of comet 67P/Churyumov-Gerasimenko: spectral properties and color temperature variability with phase and elevation

Bockelée‐Morvan

Leyrat

Erard

et al. 2019

A&A

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We analyze 2-5 µm spectroscopic observations of the dust coma of comet 67P/Churyumov-Gerasimenko obtained with the VIRTIS-H instrument onboard Rosetta from 3 June to 29 October 2015 at heliocentric distances r h = 1.24-1.55 AU. The 2-2.5 µm color, bolometric albedo, and color temperature are measured using spectral fitting. Data obtained at α = 90 • solar phase angle show an increase of the bolometric albedo (0.05 to 0.14) with increasing altitude (0.5 to 8 km), accompanied by a possible marginal decrease of the color and color temperature. Possible explanations include the presence in the inner coma of dark particles on ballistic trajectories, and radial changes in particle composition. In the phase angle range 50-120 • , phase reddening is significant (0.031 %/100 nm/ • ), for a mean color of 2 %/100 nm at α = 90 • , that can be related to the roughness of the dust particles. Moreover, a decrease of the color temperature with decreasing phase angle is also observed at a rate of ∼ 0.3 K/ • , consistent with the presence of large porous particles, with low thermal inertia, and showing a significant day-to-night temperature contrast. Comparing data acquired at fixed phase angle (α = 90 • ), a 20% increase of the bolometric albedo is observed near perihelion. Heliocentric variations of the dust color are not significant in the analyzed time period. Measured color temperatures are varying from 260 to 320 K, and follow a r 0.6 h variation in the r h = 1.24-1.5 AU range, close to the expected r 0.5 h value.

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Section: Phase Variation Of the Color Temperaturesupporting

confidence: 83%

Section: Phase Reddeningsupporting

confidence: 82%

VIRTIS-H observations of the dust coma of comet 67P/Churyumov-Gerasimenko: spectral properties and color temperature variability with phase and elevation

Bockelée‐Morvan

Leyrat

Erard

et al. 2019

A&A

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“…The authors considered these results to be of low significance, however. To fit the SPF of comet 67P, Moreno et al (2018) used the T-matrix and geometric optics codes. The authors found that different types of oriented elongated particles with equivalent radii of 7 to 10 µm, porosity in the range of 60% -70%, and refractive index of m = 1.6 + 0.1i reproduce the coma dust SPF very well.…”

Section: Scattering Phase Functionmentioning

confidence: 99%

HD 117214 debris disk: scattered-light images and constraints on the presence of planets

Engler

Lazzoni

Gratton

et al. 2020

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Context. Young stars with debris disks are the most promising targets for an exoplanet search because debris indicate a successful formation of planetary bodies. Debris disks can be shaped by planets into ring structures that give valuable indications on the presence and location of planets in the disk. Aims. We performed observations of the Sco-Cen F star HD 117214 to search for planetary companions and to characterize the debris disk structure. Methods. HD 117214 was observed with the SPHERE subsystems IRDIS, IFS, and ZIMPOL at optical and near-IR wavelengths using angular and polarimetric differential imaging techniques. This provided the first images of scattered light from the debris disk with the highest spatial resolution of 25 mas and the inner working angle < 0.1 . With the observations with IRDIS and IFS we derived detection limits for substellar companions. The geometrical parameters of the detected disk were constrained by fitting 3D models for the scattering of an optically thin dust disk. Investigating the possible origin of the disk gap, we introduced putative planets therein and modeled the planet-disk and planet-planet dynamical interactions. The obtained planetary architectures were compared with the detection limit curves.Results. The debris disk has an axisymmetric ring structure with a radius of 0.42(±0.01) or ∼45 au and an inclination of 71(±2.5) • and exhibits a 0.4 (∼40 au) wide inner cavity. From the polarimetric data, we derive a polarized flux contrast for the disk of (F pol ) disk /F * > (3.1 ± 1.2) · 10 −4 in the RI band. Conclusions. The fractional scattered polarized flux of the disk is eight times lower than the fractional IR flux excess. This ratio is similar to the one obtained for the debris disk HIP 79977, indicating that dust radiation properties are similar for these two disks. Inside the disk cavity we achieve high-sensitivity limits on planetary companions with a mass down to ∼ 4 M J at projected radial separations between 0.2 and 0.4 . We can exclude stellar companions at a radial separation larger than 75 mas from the star.

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“…The analysis of a large ground-based image data set by Monte Carlo dust-tail modeling (Moreno et al 2017) found a minimum particle size of 10 µm. Moreno et al (2018) showed that the dust phase function determined from Optical, Spectrocopic and Infrared Remote Imaging System (OSIRIS) observations (Bertini et al 2019) can be fit assuming that the main scatterers are ≥10 µm. MIDAS imaged the smallest particles, which provided high-resolution information on their morphology, but it did not provide quantitative information on the dust flux of submicrometer-to micrometersized particles.…”

Section: Introductionmentioning

confidence: 99%

GIADA microbalance measurements on board Rosetta: submicrometer- to micrometer-sized dust particle flux in the coma of comet 67P/Churyumov-Gerasimenko

Corte

Rotundi

Захаров

et al. 2019

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Context. From August 2014 to September 2016, Rosetta escorted comet 67P/Churyumov-Gerasimenko (67P) during its journey around the Sun. One of the aims of Rosetta was to characterize cometary activity and the consequent formation of dust flux structures in cometary comae. Aims. We characterize and quantify the submicrometer-to micrometer-sized dust flux that may be shaped in privileged directions within the coma of 67P inbound to and outbound from perihelion. Methods. The in situ dust-measuring instrument GIADA, part of the Rosetta/ESA payload, consisted of three subsystems, one of which was the Micro Balance Subsystem (MBS), composed of five quartz crystal microbalances. From May 2014 to September 2016, MBS measured the submicrometer-to micrometer-sized deposited dust mass every 5 min. Results. We characterized the submicrometer-to micrometer-sized dust mass flux in the coma of 67P. The anti-sunward and the radial direction are preferred, and the flux is higher in the anti-sunward direction. The measured cumulative dust mass in the anti-sunward direction is 2.38 ± 0.04 × 10 −7 kg, and in the radial direction, it is 1.18 ± 0.02 × 10 −7 kg. We explain the anti-sunward dust flux as the effect of nonuniform gas emission between the night-and dayside of the nucleus, which acts in combination with the solar radiation pressure. We compared the cumulated dust mass of particles ≤5 µm with particles ≥100 µm. The retrieved ratio of ≈2% implies a differential size distribution index of ≈−3.0, which confirms that particles of size ≥0.1 mm dominate the dust coma cross-section of 67P during the entire orbit. Conclusions. Submicrometer-to micrometer-sized dust mass flux measurements were made for the first time from the arising of cometary activity until its extinction. They indicate that these particles do not provide a substantial optical scattering in the coma of 67P with respect to the scattering caused by millimeter-sized particles. In addition, MBS data reveal that the measured dust flux is highly anisotropic: anti-sunward plus radial.

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Models of Rosetta/OSIRIS 67P Dust Coma Phase Function

Cited by 24 publications

References 47 publications

VIRTIS-H observations of the dust coma of comet 67P/Churyumov-Gerasimenko: spectral properties and color temperature variability with phase and elevation

VIRTIS-H observations of the dust coma of comet 67P/Churyumov-Gerasimenko: spectral properties and color temperature variability with phase and elevation

HD 117214 debris disk: scattered-light images and constraints on the presence of planets

GIADA microbalance measurements on board Rosetta: submicrometer- to micrometer-sized dust particle flux in the coma of comet 67P/Churyumov-Gerasimenko

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