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|Title:||Evolution of the dust trail of comet 17P/Holmes|
Silber, E. A.
|Citation:||Evolution of the dust trail of comet 17P/Holmes / M. Gritsevich, M. Nissinen, A. Oksanen et al. // Monthly Notices of the Royal Astronomical Society. — 2022. — Vol. 513. — Iss. 2. — P. 2201-2214.|
|Abstract:||The massive outburst of the comet 17P/Holmes in 2007 October is the largest known outburst by a comet thus far. We present a new comprehensive model describing the evolution of the dust trail produced in this phenomenon. The model comprises of multiparticle Monte Carlo simulation including the solar radiation pressure effects, gravitational disturbance caused by Venus, Earth and Moon, Mars, Jupiter and Saturn, and gravitational interaction of the dust particles with the parent comet itself. Good accuracy of computations is achieved by its implementation in Orekit, which executes Dormad-Prince numerical integration methods with higher precision. We demonstrate performance of the model by simulating particle populations with sizes from 0.001 to 1 mm with corresponding spherically symmetric ejection speed distribution, and towards the Sun outburst modelling. The model is supplemented with and validated against the observations of the dust trail in common nodes for 0.5 and 1 revolutions. In all cases, the predicted trail position showed a good match to the observations. Additionally, the hourglass pattern of the trail was observed for the first time within this work. By using variations of the outburst model in our simulations, we determine that the assumption of the spherical symmetry of the ejected particles leads to the scenario compatible with the observed hourglass pattern. Using these data, we make predictions for the two-revolution dust trail behaviour near the outburst point that should be detectable by using ground-based telescopes in 2022. © 2022 The Author(s).|
METEORITES, METEORS, METEOROIDS
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITY
MONTE CARLO METHODS
METEORITES METEORS METEOROIDS
MONTE CARLO'S SIMULATION
PLANETS AND SATELLITES: DYNAMICAL EVOLUTION AND STABILITIES
SOLAR RADIATION PRESSURE
|metadata.dc.description.sponsorship:||Academy of Finland, AKA: 325806|
This work was supported, in part, by the Academy of Finland project no. 325806 (PlanetS). The authors express deep gratitude and dedication to Esko Lyytinen, in particular, for initiating this research and for putting in place ef fecti ve collaboration under the umbrella of the Ursa Astronomical Association and the Finnish Fireball Network. Intense collaborative work with Esko allowed us to provide a comprehensive representation of the ideas earlier discussed with Esko in the form of personal communications. We are grateful to Pekka Lehtikoski for his contribution to the programming of the mathematical model. We thank Jérémie Vaubaillon for insightful comments and discussion, which helped us to impro v e the earlier version of this paper. We thank Jorma Ryske for his enthusiastic observations of the trail in 2022 February and March and for confirming the observability and position of the trail as described and predicted in this study. This research made use of TOPCAT for visualization and figures (Taylor 2005 ).
|Appears in Collections:||Научные публикации, проиндексированные в SCOPUS и WoS CC|
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