arXiv subjects

Paweł Wajer

Publications and source records attributed to Paweł Wajer.

3 recordsLinked to original sources

arXiv2026

Numerical analysis of Lyapunov Times for Trans-Neptunian Objects and Main-Belt Asteroids: stability, accuracy, and methodological comparisons

We computed Lyapunov times ($T_L$) for a sample of trans-Neptunian objects (TNOs) and outer main-belt asteroids (MBAs) using three numerical approaches: the variational method and two implementations of the renormalization technique. For each object, $T_L$ was derived both from the nominal orbit and from ensembles of 1001 orbital clones, enabling direct comparison between single-orbit and ensemble-based estimates. Across the sample, the methods generally produced consistent results, though larger discrepancies were observed for some MBAs. TNOs, in contrast, displayed greater consistency across methods, likely due to fewer overlapping resonances. Importantly, clone ensembles provided more robust and reliable stability indicators than nominal-orbit computations. Median values from clone populations reduced method-dependent biases and revealed dynamical behaviors that would remain hidden in single-orbit analyses, especially for objects with poorly constrained orbits or evolving in resonant regions. While our study focused on a limited but diverse set of objects, the methodology can be directly extended to larger populations, offering a systematic framework for exploring the long-term stability and dynamical evolution of main-belt asteroids, trans-Neptunian objects or other classes of objects in the Solar System.

astro-ph.EP↗

arXiv2014

Comet C/2013 A1 Siding Spring. How treatment of data and NG effects can change our predictions about close encounters with Mars ?

We show that the estimates of close encounter of this comet with Mars depend on data treatment. Using the data taken in the two-year period, we derived that the comet will miss Mars on 2014 October 19 at the distance of about $140\,150\pm 55$ km or $140\,300\pm 45$ km from its center, depending on the method of data processing in the purely gravitational model of motion (based on non-weighted data or weighted data, respectively). Unfortunately, the non-gravitational model of motion is still very uncertain, thus we can only speculate about estimates of expected distances for non-gravitational orbital solutions. However, we did not obtain a significant differences in close encounter prediction between the non-gravitational solutions and the gravitational ones.

physics.space-ph↗

arXiv2012

Behavior of Jupiter Non-Trojan Co-Orbitals

Searching for the non-Trojan Jupiter co-orbitals we have numerically integrated orbits of 3\,160 asteroids and 24 comets discovered by October 2010 and situated within and close to the planet co-orbital region. Using this sample we have been able to select eight asteroids and three comets and have analyzed their orbital behavior in a great detail. Among them we have identified five new Jupiter co-orbitals: \cu, \sa, \ql, \gh, and \Larsen, as well as we have analyzed six previously identified co-orbitals: \hr, \ug, \qq, \aee, \wc\ and \ar. \cu\ is currently on a quasi-satellite orbit with repeatable transitions into the tadpole state. Similar behavior shows \gh\ which additionally librates in a compound tadpole-quasi-satellite orbit. \ql\ and \Larsen\ are the co-orbitals of Jupiter which are temporarily moving in a horseshoe orbit occasionally interrupted by a quasi-satellite behavior. \sa\ is moving in a pure horseshoe orbit. Orbits of the latter three objects are unstable and according to our calculations, these objects will leave the horseshoe state in a few hundred years. Two asteroids, \qq\ and \aee, are long-lived quasi-satellites of Jupiter. They will remain in this state for a few thousand years at least. The comets \ar\ and \wc\ are also quasi-satellites of Jupiter. However, the non-gravitational effects may be significant in the motion of these comets. We have shown that \wcs\ is moving in a quasi-satellite orbit and will stay in this regime to at least 2500 year. Asteroid \hr\ will be temporarily captured in a quasi-satellite orbit near 2050 and we have identified another one object which shows similar behavior - the asteroid \ug, although, its guiding center encloses the origin, it is not a quasi-satellite. The orbits of these two objects can be accurately calculated for a few hundred years forward and backward.

astro-ph.EP↗