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Wlodarczyk I.,Chorzow Astronomical Observatory MPC 553 | Cernis K.,Vilnius University | Boyle R.P.,Vatican Observatory Research Group | Laugalys V.,Vilnius University
Monthly Notices of the Royal Astronomical Society | Year: 2014

The near-Earth asteroid belt is continuously replenished with material originally moving in Amor-class orbits. Here, the orbit of the dynamically interesting Amor-class asteroid 2012 XH16 is analysed. This asteroid was discovered with the Vatican Advanced Technology Telescope (VATT) at the Mt Graham International Observatory as part of an ongoing asteroid survey focused on astrometry and photometry. The orbit of the asteroid was computed using 66 observations (57 obtained with VATT and 9 from the Lunar and Planetary Laboratory-Spacewatch II project) to give a = 1.63 au, e = 0.36, i = 3°. 76. The absolute magnitude of the asteroid is 22.3 which translates into a diameter in the range 104-231 m, assuming the average albedos of S-type and C-type asteroids, respectively. We have used the current orbit to study the future dynamical evolution of the asteroid under the perturbations of the planets and the Moon, relativistic effects, and the Yarkovsky force. Asteroid 2012 XH16 is locked close to the strong 1:2 mean motion resonance with the Earth. The object shows stable evolution and could survive in near-resonance for a relatively long period of time despite experiencing frequent close encounters with Mars. Moreover, results of our computations show that the asteroid 2012 XH16 can survive in the Amor region at most for about 200-400 Myr. The evolution is highly chaotic with a characteristic Lyapunov time of 245 yr. Jupiter is the main perturber but the effects of Saturn, Mars and the Earth-Moon system are also important. In particular, secular resonances with Saturn are significant. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Source


Wlodarczyk I.,Chorzow Astronomical Observatory MPC 553
Monthly Notices of the Royal Astronomical Society | Year: 2013

We computed impact solutions of the potentially dangerous asteroid (99942) Apophis based on 4022 optical observations and seven radar observations from 2013 March 15.10789 UTC through March 28.089569 UTC. Using the freely available ORBFIT software package, we can follow its orbit forward in the future searching for close approaches with the Earth, which can lead to possible impacts up to 2110. With the example of Apophis we show that it is possible to compute additional solutions using the weighting method of Bielicki. The possible impact path of risk for 2068 is presented. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Source


Wlodarczyk I.,Chorzow Astronomical Observatory MPC 553
Monthly Notices of the Royal Astronomical Society | Year: 2012

We present computing methods that allow us to study the behaviour of the dynamically interesting potentially dangerous asteroid 2012 DA14. Using the freely available OrbFit software, we can follow the orbit of the asteroid backward and forward in the future, searching for close approaches to the Earth that might lead to possible impacts. The possible impact orbit for 2026 is computed. We show that it should be possible to recover asteroid 2012 DA14, mainly in 2013 February. It is highly unlikely that asteroid 2012 DA14 will hit any geosynchronous satellites during its close approach on 2013 February 15. © 2012 The Author Monthly Notices of the Royal Astronomical Society © 2012 RAS. Source


Wlodarczyk I.,Chorzow Astronomical Observatory MPC 553 | Cernis K.,Vilnius University | Eglitis I.,University of Latvia
Monthly Notices of the Royal Astronomical Society | Year: 2011

We present the time evolution of orbital elements of the Centaur asteroid 2009 HW77, discovered by KC and IE, forwards and backwards in time over a 10-Myr period. The dynamical behaviour is analysed using three software packages: the OrbFit, the swift and the Mercury integrators. Changes in the orbital elements of 2009 HW77 clones are calculated using the classification of Horner et al. It is shown that close approaches to the giant planets significantly change the asteroid orbit. Our computations made with the swift software and with the Mercury software give similar results. The half-life is about 5 Myr in both the forward and backward integrations. Moreover, our computations suggest that the Centaur asteroid will be temporarily locked as a periodic asteroid connected with Jupiter with a Tisserand parameter smaller than 3. Hence it is dynamically similar to the Jupiter Family Comets. The mean duration in this state is about 82 kyr, but the behaviour and lifetime depend on whether capture occurs after a few hundred thousand years or a few hundred million years. Several clones of this dynamically interesting Centaur asteroid are temporarily locked up to four times as periodic asteroids connected with Jupiter, after which they are ejected from the Solar system. According to Bailey and Malhotra, asteroid 2009 HW77 may belong to the diffusing class of Centaurs, which can evolve into Jupiter Family Comets. © 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS. Source

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