Monte Carlo modeling of neutral gas and dust in the coma of Comet 1P/Halley

Rubin, Martin; Tenishev, V.; Combi, M. R.; Hansen, K. C.; Gombosi, T. I.; Altwegg, Kathrin; Balsiger, H.

doi:10.1016/j.icarus.2011.04.006

Cited by 43 publications

(35 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This distribution agrees with interpolated results extracted from Rubin et al (2011), although normalization was required. The normalized density distribution n j (r, a) for j dust and ice scatterers is determined to be…”

Section: Density Distributionssupporting

confidence: 85%

“…Data on scattering of X-rays by cometary dust and ice particles is significantly less developed and is mostly based on empirical models (Rubin et al 2011;Fink & Rubin 2012). The classical Mie model is used as an approximation in determining differential and total cross sections for nano-sized dust and ice particles (Draine 2003), although differences between the results of Mie and quantum calculations are expected for ultra-small grains.…”

Section: Cross Sections Of Cometary Scatterersmentioning

confidence: 99%

See 1 more Smart Citation

Cometary emissions induced by scattering and fluorescence of solar X-rays

Snios

Lewkow

Kharchenko

2014

A&A

View full text Add to dashboard Cite

To establish the nature of cometary X-ray emissions above 1 keV, detailed modeling of scattering and fluorescence of solar X-rays by a cometary atmosphere is carried out over the 0.3−3.0 keV photon energy range. Computations of the X-ray emissions are performed for different distributions of the cometary neutral gas, dust, and ice grains, with an emphasis placed on nano-sized particles. The calculated emission spectra of energetic photons above 1 keV are compared to cometary observations performed by the Chandra X-ray Observatory, and emission contributions solely from cometary neutral gas are found to be an insufficient X-ray production mechanism. Further comparison between the developed model and observational data also establishes an upper limit on dust and ice nanoparticle density distributions in cometary atmospheres. In addition, similarities in spectral shape above 1 keV observed between cometary emissions, Jovian disk emissions, and scattered solar X-ray spectra during solar flare events are discussed in detail.

show abstract

Section: Density Distributionssupporting

confidence: 85%

Section: Cross Sections Of Cometary Scatterersmentioning

confidence: 99%

Cometary emissions induced by scattering and fluorescence of solar X-rays

Snios

Lewkow

Kharchenko

2014

A&A

View full text Add to dashboard Cite

show abstract

“…Highly relevant for the first of these are observations of comet outgassing, which suggest that CO (and possibly CO 2 ) is relatively abundant (∼10% relative to H 2 O, Cochran et al 2015), while O 2 occurs at a surprisingly high ∼3% (Bieler et al 2015;Rubin et al 2015b) and N 2 occurs at a surprisingly low ∼0.1% (Rubin et al 2015a). This motivates us to focus on CO. We argue in Section 4.1.1 that while exposed CO on KBO surfaces would have sublimated long ago, CO should retain its primordial abundance in layers deeper than ∼1 km and could diffuse upward rapidly upon displacement of the KBOs to warmer regions of the solar system.…”

Section: Confronting Observationsmentioning

confidence: 98%

On the Mass and Origin of Chariklo’s Rings

Pan

Wu²

2016

ApJ

View full text Add to dashboard Cite

Observations in 2013 and 2014 of the Centaur 10199 Chariklo and its ring system consistently indicated that the radial width of the inner, more massive ring varies with longitude. That strongly suggests that this ring has a finite eccentricity despite the fast differential precession that Chariklo's large quadrupole moment should induce. If the inferred apse alignment is maintained by the ring's self-gravity, as it is for the Uranian rings, we estimate a ring mass of a few times 10 16 g and a typical particle size of a few meters. These values imply a collisional spreading time of ∼10 5 years, which is somewhat shorter than the typical Centaur dynamical lifetime of a few million years and much shorter than the age of the solar system. In light of this time constraint, we evaluate previously suggested ring formation pathways including collisional ejection and satellite disruption. We also investigate in detail a contrasting formation mechanism, the lofting of dust particles off Chariklo's surface into orbit via outflows of sublimating CO and/or N 2 triggered after Chariklo was scattered inward by giant planets. This alternate scenario predicts that rings should be common among 100 km class Centaurs but rare among Kuiper Belt objects and smaller Centaurs. It also predicts that Centaurs should show seasonal variations in cometary activity with activity maxima occurring shortly after equinox.

show abstract

“…A variety of numerical results of these models are available on the web site 'Inner Coma Environment Simulator' (http://ices.engin.umich.edu; Combi 1996; Combi et al 2004;Tenishev, Combi & Davidsson 2008;Tenishev, Combi & Rubin 2011b;Rubin et al 2011). We select the model Case 1.3 with dust particles of radius 10.0 μm having a terminal velocity of 33 m s −1 .…”

Section: R a D I A L P Ro F I L E Smentioning

confidence: 99%