Light scattering by cometary dust: Large-particle contribution

Zubko, Evgenij

doi:10.5047/eps.2012.02.003

Cited by 27 publications

(15 citation statements)

References 24 publications

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“…This shows, that the scattered light contribution of particles larger than 3.5 µm is minor, which is in agreement with Zubko (2013). In this study, the authors analysed the contribution of large particles in cometary dust by using the Discrete Dipole Approximation method (DDA).…”

Section: Generating Imagessupporting

confidence: 84%

A multiwavelength study of the debris disc around 49 Cet

Pawellek

Moór

Milli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In a multiwavelength study of thermal emission and scattered light images we analyse the dust properties and structure of the debris disc around the A1-type main-sequence star 49 Cet. As a basis for this study, we present new scattered light images of the debris disc known to possess a high amount of both dust and gas. The outer region of the disc is revealed in former coronagraphic H-band and our new Y-band images from the Very Large Telescope SPHERE instrument. We use the knowledge of the disc’s radial extent inferred from ALMA observations and the grain size distribution found by spectral energy distribution fitting to generate semidynamical dust models of the disc. We compare the models to scattered light and thermal emission data and find that a disc with a maximum surface density at 110 au and shallow edges can describe both the thermal emission and the scattered light observations. This suggests that grains close to the blow-out limit and large grains stem from the same planetesimal population and are mainly influenced by radiation pressure. The influence of inward transport processes could not be analysed in this study.

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Section: Generating Imagessupporting

confidence: 84%

A multiwavelength study of the debris disc around 49 Cet

Pawellek

Moór

Milli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…While large particles with radius in excess of 10 μm do indeed exist in a cometary coma (e.g., Bentley et al 2016), there also are present submicron-and micron-sized dust particles in much greater quantities (e.g., Mazets et al 1986;Price et al 2010), and these smaller particles are more efficient scatterers. As demonstrated by Zubko (2013), if the index in the power-law size distribution r -n ranges from n = 1.5 -3.5, the light-scattering at phase angles  ≤ 30° is predominantly governed by particles with radius r ≤ 1.5 μm. This apparently holds for comet 41P/T-G-K on March 3-4 of 2017, when its phase angle was   24.8-26°.…”

Section: Resultsmentioning

confidence: 99%

Rapid variations of dust colour in comet 41P/Tuttle–Giacobini–Kresák

Lukyanyk

Zubko

Husárik

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We monitor the inner coma of comet 41P/Tuttle-Giacobini-Kresák searching for variations of its colour. Fast changes in colour of the comet 41P/Tuttle-Giacobini-Kresák provide important clues for better understanding of the microphysical properties of its dust. Using the 61-cm and 70-cm telescopes we measured the apparent magnitude of the comet with the V and R Johnson-Cousins filters from January 29 until April 25 of 2017. The inner coma (2000 km) reveals fast and significant variations of colour. The most significant change was found between March 3 and 4 of 2017, when it changed from blue with a colour slope S  (-10.15 ± 3.43)% per 0.1 μm to red with S  (16.48 ± 4.27)% per 0.1 μm. This finding appears in good accordance with what was previously reported by Ivanova et al. (2017) for long-period comet C/2013 UQ4 (Catalina),suggesting that fast and significant variations of colour of dust could be a common feature of short-and long-period comets. We model observations of comet 41P/Tuttle-Giacobini-Kresák using the agglomerated debris particles and conclude that its inner coma consists of a mixture of at least two types of particles made of Mg-rich silicates and organics or Mg-Fe silicates.

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“…The higher cut-off limit is not that important as long as it is high enough since when the size distribution follows the power-law, the contribution of large particles is relatively weak, especially if absorbing materials are abundant (Zubko, 2013). It is interesting to note that the particle composition has a very weak effect on the polarization in this range.…”

Section: Resultsmentioning

confidence: 99%