Mercury and orbfit packages for numerical integration of planetary systems: implementation of the yarkovsky and yorp effects

Fenucci, Marco; Novaković, Bojan

doi:10.2298/saj2204051f

Cited by 9 publications

(4 citation statements)

References 64 publications

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“…Therefore, N-body simulations that incorporate the Yarkovsky effect may lead to a greater number of fragments reaching the escape routes identified in this study. This could be achieved in future works using a new recent public implementation of the Yarkovsky and YORP effects into MERCURY (Fenucci & Novaković 2022).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Gravitational study of escape routes and residence regions of Ceres and Vesta fragments

Zain,

Di Sisto

2023

A&A

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Aims. Ceres and Vesta are the two largest bodies in the main asteroid belt (MB) and have been extensively studied, particularly since the DAWN mission. Vesta is known to have an associated asteroid family, while the existence of a Ceres family is uncertain. This study investigates the fate of multi-kilometre fragments ejected from Ceres and Vesta due to impacts over a timescale of several hundred million years. Methods. We performed purely gravitational N-body simulations to investigate the dynamical evolution of multi-kilometre-sized fragments ejected from Ceres and Vesta. We tracked the trajectories of these fragments and identified their residence regions within the MB. We analysed the escape routes and end states of the fragments that manage to leave the MB, including the delivery to the near-Earth asteroids (NEAs). We also estimated the number of collisions with Earth that could be attributed to large fragments ejected from Ceres and Vesta. Results. Our simulations show that the Ceres fragments are dispersed over a larger region in the MB compared to Vesta fragments due to their higher ejection velocities. We identified the escape routes of the fragments that leave the MB, which for the Ceres fragments are the 5:2 and 8:3 mean-motion resonances (MMR), and for the Vesta fragments are the 3:1 MMR and ν6 secular resonance, where they can be delivered to the NEA region. We also find that the Pristine region, located between the 5:2 and 7:3 MMR, is the most likely place to find any surviving member of a Ceres family. There were no collisions of large Ceres or Vesta fragments with Earth over the age of the Solar System, suggesting that, under the model considered here, the howardite–eucrite–diogenite meteorites originate from smaller NEAs from Vesta.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Gravitational study of escape routes and residence regions of Ceres and Vesta fragments

Zain,

Di Sisto

2023

A&A

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“…The initial argument of pericenter, ω, and the initial argument of the node, Ω, were both set to 0 • , while the initial mean anomaly, ℓ, was chosen randomly between 0 • and 360 • . Numerical integrations were performed by using a hybrid symplectic scheme (Chambers 1999) that is able to handle close encounters with planets, that is included in the MERCURY 2 package (see also Fenucci & Novaković 2022). The gravitational attraction of the Sun and of all the planets from Mercury to Neptune were included in the model and the initial conditions for planets at epoch 58800 MJD were taken from the JPL Horizons 3 ephemeris system.…”

Section: Comparison With Numerical Integrationsmentioning

confidence: 99%

Maps of secular resonances in the NEO region

Fenucci

Gronchi

Novaković

2023

A&A

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Context. From numerical simulations, it is known that some secular resonances may affect the motion of near-Earth objects (NEOs). However, the specific location of the secular resonance inside the NEO region is not fully known because the methods previously used to predict their location cannot be applied to highly eccentric orbits or the time when the NEOs cross the orbits of the planets. Aims. In this paper, we aim to map the secular resonances with the planets from Venus to Saturn in the NEO region, while including high eccentricity values as well. Methods. We used an averaged semi-analytical model that can deal with orbit-crossing singularities for the computation of the secular dynamics of NEOs, from which we were able to obtain suitable proper elements and proper frequencies. Then, we computed the proper frequencies over a uniform grid in the proper elements space. Secular resonances can thus be located by the level curves corresponding to the proper frequencies of the planets. Results. We determined the location of the secular resonances with the planets from Venus to Saturn, showing that they appear well within the NEO region. By using full numerical N-body simulations, we also showed that the location predicted by our method is fairly accurate. Finally, we provided some indications about possible dynamical paths inside the NEO region due to the presence of secular resonances.

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“…We used the orbital and Yarkovsky clones to investigate the dynamical stability further and possible scenarios of asteroid 248370 past orbit evolution. For this purpose, we made 500 clones, and their orbits are propagated for 200 Myr using a version of OrbFit 6 software package extended by Fenucci & Novaković (2022) by implementing nongravitational effects. The dynamical model includes the gravitational effects of the Sun and seven major planets (from Venus to Neptune) as well as non-gravitational forces.…”

Section: Long-term Dynamical Stabilitymentioning

confidence: 99%

“…Additionally, heat capacity is fixed to C = 600 J kg −1 K −1 , based on the measurements for the CI chondrite meteorites (Piqueux et al 2021). The other model parameters defining the strength of the YORP effect are set to default values as given in Fenucci & Novaković (2022). The results of the orbital evolution of the clones are shown in Fig.…”

Section: Long-term Dynamical Stabilitymentioning

confidence: 99%

Photometric and dynamic characterization of active asteroid (248370) 2005QN173

Novaković

Pavela

Hsieh

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present the physical and dynamical properties of the recently discovered active asteroid (248370) 2005QN173 (aka 433P). From our observations, we derived two possible rotation period solutions of 2.7 ± 0.1 and 4.1 ± 0.1 hours. The corresponding light curve amplitudes computed after correcting for the effect of coma are 0.28 and 0.58 mag, respectively. Both period solutions are shorter than the critical rotation limit computed for a strengthless triaxial ellipsoid, suggesting that rotation mass shedding should at least partly be responsible for the observed activity. We confirm that the activity level is fading further, but at a very modest rate of only 0.006 mag/day, still also compatible with sublimation-driven activity. We found that 248370 likely belongs to the Themis asteroid family, making it a fourth main-belt comet associated with this group. Orbital characteristics of 248370 are also consistent with its origin in the young 288P cluster of asteroids. The 288P cluster is associated with its namesake main-belt comet, providing an exciting possibility for a comparative analysis of intriguing main-belt comets 248370 and 288P.

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Mercury and orbfit packages for numerical integration of planetary systems: implementation of the yarkovsky and yorp effects

Cited by 9 publications

References 64 publications

Gravitational study of escape routes and residence regions of Ceres and Vesta fragments

Gravitational study of escape routes and residence regions of Ceres and Vesta fragments

Maps of secular resonances in the NEO region

Photometric and dynamic characterization of active asteroid (248370) 2005QN173

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