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1
Carruba, Valerio, Maria Helena Moreira Morais, Daniela C. Mourão, et al. "New Transient Co-orbital Asteroids of Venus." Research Notes of the AAS 8, no. 8 (2024): 213. http://dx.doi.org/10.3847/2515-5172/ad7261.
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Abstract Venus has no known natural satellites but has 5 known co-orbitals. These are objects trapped in a 1:1 mean-motion resonance with Venus. Co-orbital configurations include retrograde satellite orbits (RS), tadpole orbits (T) around the Lagrangian equilibrium points L4 or L5, and horseshoe orbits around both L4 and L5 (H). At high eccentricity or inclination, co-orbital configurations may also involve compounds of T and RS (T-RS, T-RS-T), H and RS (H-RS) orbits, or transitions between different co-orbital modes. Here we identify asteroids in 2 RS, 1 L4-tadpole, 2 H-RS, and 2 T-RS orbits, as well as 8 additional asteroids in possible temporary co-orbital status. Although the majority of these objects do not yet have well-characterized orbits, 2020 CL1, and 2020 SB do and are very likely to be new co-orbital asteroids. With the new candidates, Venus would have a population of 20 co-orbital asteroids, comparable to those of Mars and Earth.
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Zhou, Lei, Yang-Bo Xu, Li-Yong Zhou, Rudolf Dvorak, and Jian Li. "Orbital stability of Earth Trojans." Astronomy & Astrophysics 622 (February 2019): A97. http://dx.doi.org/10.1051/0004-6361/201834026.
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The only discovery of Earth Trojan 2010 TK7 and the subsequent launch of OSIRIS-REx have motived us to investigate the stability around the triangular Lagrange points of the Earth, L4 and L5. In this paper we present detailed dynamical maps on the (a0, i0) plane with the spectral number (SN) indicating the stability. Two main stability regions, separated by a chaotic region arising from the ν3 and ν4 secular resonances, are found at low (i0 ≤ 15°) and moderate (24 ° ≤i0 ≤ 37°) inclinations, respectively. The most stable orbits reside below i0 = 10° and they can survive the age of the solar system. The nodal secular resonance ν13 could vary the inclinations from 0° to ∼10° according to their initial values, while ν14 could pump up the inclinations to ∼20° and upwards. The fine structures in the dynamical maps are related to higher degree secular resonances, of which different types dominate different areas. The dynamical behaviour of the tadpole and horseshoe orbits, reflected in their secular precession, show great differences in the frequency space. The secular resonances involving the tadpole orbits are more sensitive to the frequency drift of the inner planets, thus the instabilities could sweep across the phase space, leading to the clearance of tadpole orbits. We are more likely to find terrestrial companions on horseshoe orbits. The Yarkovsky effect could destabilize Earth Trojans in varying degrees. We numerically obtain the formula describing the stabilities affected by the Yarkovsky effect and find the asymmetry between the prograde and retrograde rotating Earth Trojans. The existence of small primordial Earth Trojans that avoid being detected but survive the Yarkovsky effect for 4.5 Gyr is substantially ruled out.
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Johnson, Ancy, and Ram Krishan Sharma. "Locations of Lagrangian points and periodic orbits around triangular points in the photo gravitational elliptic restricted three-body problem with oblateness." International Journal of Advanced Astronomy 7, no. 2 (2019): 25. http://dx.doi.org/10.14419/ijaa.v7i2.29377.
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Locations of the Lagrangian points are computed and periodic orbits are studied around the triangular points in the photogravitational elliptic restricted three-body problem (ER3BP) by considering the more massive primary as the source of radiation and smaller primary as an oblate spheroid. A new mean motion taken from Sharma et al. [13] is used to study the effect of radiation pressure and oblateness of the primaries. The critical mass parameter that bifurcates periodic orbits from non-periodic orbits tends to reduce with radiation pressure and oblateness. The transition curves defining stable region of orbits are drawn for different values of radiation pressure and oblateness using the analytical method of Bennet [14]. Tadpole orbits with long- and short- periodic oscillations are obtained for Sun-Jupiter and Sun-Saturn systems.
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Hysa, Azem. "A study of the nonlinear dynamics inside the exoplanetary system Kepler-22 using MATLAB® software." EUREKA: Physics and Engineering, no. 2 (March 29, 2024): 3–12. http://dx.doi.org/10.21303/2461-4262.2024.003257.
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Kepler is a discovery-class mission designed to determine the frequency of Earth-radius planets in and near the habitable zone of solar-type stars. A habitable zone of a star is defined as a range of orbits within which a rocky planet can support liquid water on its surface. The most intriguing question driving the search for habitable planets is whether they host life.
 The aim of this paper is to study the motion of a “test particle” inside the exoplanetary system Kepler-22. This system consists of a sun-like star, Kepler-22, and a terrestrial exoplanet, Kepler-22b. This exoplanet is situated in the habitable zone of its star. Kepler-22b is located about 180 pc from Earth in the constellation of Cygnus. It was discovered by NASA’s Kepler Space Telescope in December 2011 and the planet is about 2.4 times the radius of Earth. Scientists don't yet know if Kepler-22b has a rocky, gaseous or liquid composition.
 In this study, let’s derive Lagrange points and perform several numerical tests to discover different possible orbits around the star Kepler-22. From many numerical tests performed, it is also possible to found two tadpole orbits around the Lagrange points L4 and L5 and a tadpole orbit around the exoplanet Kepler-22b, which encircles the two Lagrange points L1, and L2. Some of these orbits are found in the habitable zone and others outside. We have also examined the possibility of the existence of an exomoon around the terrestrial exoplanet Kepler-22b. In this case we have considered the mass of this exomoon.
 The Circular Restricted Three-Body Problem is used in this study. If it is further assumed that the third body (for example a planet, satellite, an asteroid or just a “test particle”) travels in the same plane as the two larger bodies, then there is the Planar Circular Restricted Three-Body Problem
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Kaplan, Murat, and Sergen Cengiz. "Horseshoe co-orbitals of Earth: current population and new candidates." Monthly Notices of the Royal Astronomical Society 496, no. 4 (2020): 4420–32. http://dx.doi.org/10.1093/mnras/staa1873.
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ABSTRACT Most co-orbital objects in the Solar system are thought to follow tadpole-type orbits, behaving as Trojans. However, most of Earth’s identified co-orbitals are moving along horseshoe-type orbits. The current tally of minor bodies considered to be Earth co-orbitals amounts to 18; of them, 12 are horseshoes, 5 are quasi-satellites, and 1 is a Trojan. The semimajor axis values of all these bodies librate between 0.983 and 1.017 au. In this work, we have studied the dynamical behaviour of objects following orbits with semimajor axis within this range that may be in a 1:1 mean-motion resonance with Earth. Our results show that asteroids 2016 CO246, 2017 SL16, and 2017 XQ60 are moving along asymmetrical horseshoe-type orbits; the asteroid 2018 PN22 follows a nearly symmetric or regular horseshoe-type orbit. Asteroids 2016 CO246, 2017 SL16, and 2017 XQ60 can remain in the horseshoe co-orbital state for about 900, 3300, and 2700 yr, respectively. Asteroid 2018 PN22 has a more chaotic dynamical behaviour; it may not stay in a horseshoe co-orbital state for more than 200 yr. The horseshoe libration periods of 2016 CO246, 2017 SL16, 2017 XQ60, and 2018 PN22 are 280, 255, 411, and 125 yr, respectively.
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Tabachnik, S. A., and N. W. Evans. "Existence of Asteroids in the Inner Solar System." Symposium - International Astronomical Union 202 (2004): 238–40. http://dx.doi.org/10.1017/s007418090021797x.
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Ensembles of in-plane and inclined orbits in the vicinity of the Lagrange points of the terrestrial planets are integrated for up to 100 million years. Mercurian Trojans probably do not exist, although there is evidence for long-lived, corotating horseshoe orbits with small inclinations. Both Venus and the Earth are much more promising, as they possess rich families of stable tadpole and horseshoe orbits. Our survey of in-plane test particles near the Martian Lagrange points shows no survivors after 60 million years. Low inclination test particles do not persist, as their inclinations are quickly increased until the effects of a secular resonance with Jupiter cause de-stabilisation. Numerical integrations of inclined test particles for timespans of 25 million years show stable zones for inclinations between 14° and 40°. Both Martian Trojans 5261 Eureka and 1998 VF31 lie deep within the stable zones, which suggests they may be of primordial origin.
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Leleu, A., J. Lillo-Box, M. Sestovic, et al. "Co-orbital exoplanets from close-period candidates: the TOI-178 case." Astronomy & Astrophysics 624 (April 2019): A46. http://dx.doi.org/10.1051/0004-6361/201834901.
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Despite the existence of co-orbital bodies in the solar system, and the prediction of the formation of co-orbital planets by planetary system formation models, no co-orbital exoplanets (also called trojans) have been detected thus far. Here we study the signature of co-orbital exoplanets in transit surveys when two planet candidates in the system orbit the star with similar periods. Such a pair of candidates could be discarded as false positives because they are not Hill-stable. However, horseshoe or long-libration-period tadpole co-orbital configurations can explain such period similarity. This degeneracy can be solved by considering the transit timing variations (TTVs) of each planet. We subsequently focus on the three-planet-candidate system TOI-178: the two outer candidates of that system have similar orbital periods and were found to have an angular separation close to π∕3 during the TESS observation of sector 2. Based on the announced orbits, the long-term stability of the system requires the two close-period planets to be co-orbital. Our independent detrending and transit search recover and slightly favour the three orbits close to a 3:2:2 resonant chain found by the TESS pipeline, although we cannot exclude an alias that would put the system close to a 4:3:2 configuration. We then analyse the co-orbital scenario in more detail, and show that despite the influence of an inner planet just outside the 2:3 MMR, this potential co-orbital system could be stable on a gigayear time-scale for a variety of planetary masses, either on a trojan or a horseshoe orbit. We predict that large TTVs should arise in such a configuration with a period of several hundred days. We then show how the mass of each planet can be retrieved from these TTVs.
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LANDESTOY T., MIGUEL A., DANIEL B. TURNER, ANGELA B. MARION, and S. BLAIR HEDGES. "A new species of Caribbean toad (Bufonidae, Peltophryne) from southern Hispaniola." Zootaxa 4403, no. 3 (2018): 523. http://dx.doi.org/10.11646/zootaxa.4403.3.6.
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Peltophryne armata sp. nov. is described from the South paleoisland of Hispaniola, West Indies. This is the only native toad species known to inhabit the Barahona Peninsula, Dominican Republic, in the southernmost part of Hispaniola, and it is allopatric with the widely distributed Hispaniolan toad species, P. guentheri Cochran. However, in a molecular phylogeny, the closest relative of P. armata sp. nov. is the Puerto Rican species P. lemur Cope, with which it shares a protrusive snout, large orbits, a depressed head, indistinct or absent infraorbital crests, and a long and complex advertisement call, but differs from it greatly by the very long cephalic crests, and in the massive and spinose parotoid glands that converge medially on the dorsum. The new species is similar in ecology and larval morphology to the Cuban P. florentinoi Moreno & Rivalta, but differs from it in adult morphology. The tadpole of the new species is described. Peltophryne fracta is placed in the synonymy of P. guentheri.
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Zhou, Lei, Li-Yong Zhou, Rudolf Dvorak, and Jian Li. "Systematic survey of the dynamics of Uranus Trojans." Astronomy & Astrophysics 633 (January 2020): A153. http://dx.doi.org/10.1051/0004-6361/201936332.
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Context. The discovered Uranus Trojan (UT) 2011 QF99 and several candidate UTs have been reported to be in unstable orbits. This implies that the stability region around the triangular Lagrange points L4 and L5 of Uranus should be very limited. Aims. In this paper, we aim to locate the stability region for UTs and find out the dynamical mechanisms responsible for the structures in the phase space. The null detection of primordial UTs also needs to be explained. Methods. Using the spectral number as the stability indicator, we constructed the dynamical maps on the (a0, i0) plane. The proper frequencies of UTs were determined precisely with a frequency analysis method that allows us to depict the resonance web via a semi-analytical method. We simulated radial migration by introducing an artificial force acting on planets to mimic the capture of UTs. Results. We find two main stability regions: a low-inclination (0° −14°) and a high-inclination regime (32° −59°). There is also an instability strip in each of these regions at 9° and 51°, respectively. These strips are supposed to be related with g − 2g5 + g7 = 0 and ν8 secular resonances. All stability regions are in the tadpole regime and no stable horseshoe orbits exist for UTs. The lack of moderate-inclined UTs is caused by the ν5 and ν7 secular resonances, which could excite the eccentricity of orbits. The fine structures in the dynamical maps are shaped by high-degree secular resonances and secondary resonances. Surprisingly, the libration centre of UTs changes with the initial inclination, and we prove it is related to the quasi 1:2 mean motion resonance (MMR) between Uranus and Neptune. However, this quasi-resonance has an ignorable influence on the long-term stability of UTs in the current planetary configuration. About 36.3% and 0.4% of the pre-formed orbits survive fast and slow migrations with migrating timescales of 1 and 10 Myr, respectively, most of which are in high inclination. Since low-inclined UTs are more likely to survive the age of the solar system, they make up 77% of all such long-life orbits by the end of the migration, making a total fraction up to 4.06 × 10−3 and 9.07 × 10−5 of the original population for fast and slow migrations, respectively. The chaotic capture, just like depletion, results from secondary resonances when Uranus and Neptune cross their mutual MMRs. However, the captured orbits are too hot to survive until today. Conclusions. About 3.81% UTs are able to survive the age of the solar system, among which 95.5% are on low-inclined orbits with i0 < 7.5°. However, the depletion of planetary migration seems to prevent a large fraction of such orbits, especially for the slow migration model. Based on the widely adopted migration models, a swarm of UTs at the beginning of the smooth outward migration is expected and a fast migration is favoured if any primordial UTs are detected.
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A, Arantza Jency, Krishan Sharma Ram, and Singh Gagandeep. "Stationary solutions, critical mass, Tadpole orbits in the circular restricted three-body problem with the more massive primary as an oblate spheroid." Indian Journal of Science and Technology 13, no. 39 (2020): 4168–88. https://doi.org/10.17485/IJST/v13i39.1396.
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Abstract <strong>Background:</strong> The location and stability of the equilibrium points are studied for the Planar Circular Restricted Three-Body Problem where the more massive primary is an oblate spheroid.<strong> Methods:</strong> The mean motion of the equations of motion is formulated from the secular perturbations as derived by(1) and used in(2–4). The singularities of the equations of motion are found for locating the equilibrium points. Their stability is analysed using the linearized variational equations of motion at the equilibrium points.<strong> Findings:</strong> As the effect of oblateness in the mean motion expression increases, the location and stability of the equilibrium points are affected by the oblateness of the more massive primary. It is interesting to note that all the three collinear points move towards the more massive primary with oblateness. It is a new result. Among the shifts in the locations of the five equilibrium points, the y–location of the triangular equilibrium points relocate the most. It is very interesting to note that the eccentricities (e) of the orbits around L1 and L3 increase, while it decreases around L2 with the addition of oblateness with the new mean motion. The decrease in e is significant in Saturn-Mimas system from 0.95036 to 0.87558. Similarly, the value of the critical mass ratio mc, which sets the limit for the linear stability of the triangular points, further reduces significantly from 0:285: : :A1 to 0:365: : :A1 with the new mean motion. The mean motion sz in the z-direction increases significantly with the new mean motion from 9A1/4 to 9A1/2. <strong>Keywords:</strong> Circular Restricted Three-Body Problem (CRTBP); oblateness; mean motion; equilibrium points; critical mass ratio; tadpole orbits
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Jency, A. Arantza. "Stationary solutions, critical mass, Tadpole orbits in the circular restricted three-body problem with the more massive primary as an oblate spheroid." Indian Journal of Science and Technology 13, no. 39 (2020): 4168–88. http://dx.doi.org/10.17485/ijst/v13i39.1396.
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Background: The location and stability of the equilibrium points are studied for the Planar Circular Restricted Three-Body Problem where the more massive primary is an oblate spheroid. Methods: The mean motion of the equations of motion is formulated from the secular perturbations as derived by(1) and used in(2–4). The singularities of the equations of motion are found for locating the equilibrium points. Their stability is analysed using the linearized variational equations of motion at the equilibrium points. Findings: As the effect of oblateness in the mean motion expression increases, the location and stability of the equilibrium points are affected by the oblateness of the more massive primary. It is interesting to note that all the three collinear points move towards the more massive primary with oblateness. It is a new result. Among the shifts in the locations of the five equilibrium points, the y–location of the triangular equilibrium points relocate the most. It is very interesting to note that the eccentricities (e) of the orbits around L1 and L3 increase, while it decreases around L2 with the addition of oblateness with the new mean motion. The decrease in e is significant in Saturn-Mimas system from 0.95036 to 0.87558. Similarly, the value of the critical mass ratio mc, which sets the limit for the linear stability of the triangular points, further reduces significantly from 0:285: : :A1 to 0:365: : :A1 with the new mean motion. The mean motion sz in the z-direction increases significantly with the new mean motion from 9A1/4 to 9A1/2.
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Anugrah, Diko, and Ludy Dhyani Rahmartani. "SDPS-06 A 4 YEAR-OLD GIRL WITH EMBRYONAL RHABDOMYOSARCOMA IN RETROAURICULAR AND MIDDLE EAR : A RARE CASE REPORT FROM INDONESIA." Neuro-Oncology Advances 5, Supplement_3 (2023): iii18. http://dx.doi.org/10.1093/noajnl/vdad070.067.
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Abstract Rhabdomyosarcoma is the most common sarcoma of childhood, and this tumor is the third most common neoplasm after neuroblastoma and nephroblastoma. Rhabdomyosarcomas may originate in any anatomical site, occurring predominantly in head and neck regions, orbits, skull base, nasal cavity, and nasopharynx, where there is little or no musculoskeletal tissue. The involvement of the ear and mastoid bone in rhabdomyosarcoma is uncommon. The embryonal rhabdomyosarcoma includes about 60– 70% of rhabdomyosarcoma cases. A four years-old girl presented with pain in neck and difficult to moving, there was a mass in the left auricular that was getting bigger. 4 days prior to admission, there was a drooping mouth to the left, the voice sounds hoarse, but there was no weakness in the side and no loss of consciousness. On physical examination, there was a N.VII palsy, without hyperreflexia, paraplegia, and nystagmus. High resolution Mastoid CT-Scan showed a characteristic malignant solid mass involving the external acoustic canal and the left tympanic and mastoid cavities, destroying the auditory and temporal bones, involving the left internal acoustic canal, and reaching the left nasopharynx, extending into the intracranial region of the left cerebellopontine angle and left temporal duramater. In Pathology examination showed Tumor cells are spherical, spindle-shaped with pleomorphic nuclei, hyperchromatic, coarse chromatin, vesicular, some with real nuclear daughters, eosinophilic cytoplasm. Mitosis is discovered. eccentricallynucleated cells with eosinophilic cytoplasm, suggesting rhabdomyoblast differentiation, some with a "tadpole" appearance, and conclusion according to embryonal rhabdomyosarcoma. The patient is treated with chemotherapy using Vincristine, Actinomycin-D, and Ifosfamide.
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Poon, Sanson T. S., Richard P. Nelson, Seth A. Jacobson, and Alessandro Morbidelli. "Formation of compact systems of super-Earths via dynamical instabilities and giant impacts." Monthly Notices of the Royal Astronomical Society 491, no. 4 (2019): 5595–620. http://dx.doi.org/10.1093/mnras/stz3296.
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ABSTRACT The NASA’s Kepler mission discovered ∼700 planets in multiplanet systems containing three or more transiting bodies, many of which are super-Earths and mini-Neptunes in compact configurations. Using N-body simulations, we examine the in situ, final stage assembly of multiplanet systems via the collisional accretion of protoplanets. Our initial conditions are constructed using a subset of the Kepler five-planet systems as templates. Two different prescriptions for treating planetary collisions are adopted. The simulations address numerous questions: Do the results depend on the accretion prescription?; do the resulting systems resemble the Kepler systems, and do they reproduce the observed distribution of planetary multiplicities when synthetically observed?; do collisions lead to significant modification of protoplanet compositions, or to stripping of gaseous envelopes?; do the eccentricity distributions agree with those inferred for the Kepler planets? We find that the accretion prescription is unimportant in determining the outcomes. The final planetary systems look broadly similar to the Kepler templates adopted, but the observed distributions of planetary multiplicities or eccentricities are not reproduced, because scattering does not excite the systems sufficiently. In addition, we find that ∼1 per cent of our final systems contain a co-orbital planet pair in horseshoe or tadpole orbits. Post-processing the collision outcomes suggests that they would not significantly change the ice fractions of initially ice-rich protoplanets, but significant stripping of gaseous envelopes appears likely. Hence, it may be difficult to reconcile the observation that many low-mass Kepler planets have H/He envelopes with an in situ formation scenario that involves giant impacts after dispersal of the gas disc.
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Kaneko, Miyuki, Tomoharu Oka, Hiroki Yokozuka, et al. "Discovery of the Tadpole Molecular Cloud near the Galactic Nucleus." Astrophysical Journal 942, no. 1 (2023): 46. http://dx.doi.org/10.3847/1538-4357/aca66a.
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Abstract In this paper, we report the discovery of an isolated, peculiar compact cloud with a steep velocity gradient at 2.′6 northwest of Sgr A*. This “Tadpole” molecular cloud is unique owing to its characteristic head-tail structure in the position–velocity space. By tracing the CO J = 3–2 intensity peak in each velocity channel, we noticed that the kinematics of the Tadpole can be well reproduced by a Keplerian motion around a point-like object with a mass of 1 × 105 M ⊙. Changes in line intensity ratios along the orbit are consistent with the Keplerian orbit model. The spatial compactness of the Tadpole and absence of bright counterparts in other wavelengths indicate that the object could be an intermediate-mass black hole.
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Dobrovolskis, Anthony R., José Luis Alvarellos, Kevin J. Zahnle, and Jack J. Lissauer. "Exchange of ejecta between Telesto and Calypso: Tadpoles, horseshoes, and passing orbits." Icarus 210, no. 1 (2010): 436–45. http://dx.doi.org/10.1016/j.icarus.2010.06.023.
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Yousuf, Saleem, Ram Kishor, and Manoj Kumar. "Motion about equilibrium points in the Jupiter-Europa system with oblateness." Applied Mathematics and Nonlinear Sciences, April 15, 2022. http://dx.doi.org/10.2478/amns.2021.2.00124.
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Abstract The study of motion of a test mass in the vicinity of an equilibrium point under the frame of restricted three body problem (RTBP) plays an important role in the trajectory design for different space missions. In this paper, motion of an infinitesimal mass has been described under the frame of Jupiter-Europa system with oblateness. At first, we have determined equilibrium points and then performed linear stability tests under the influence of oblateness of both the primaries. We found that due to oblateness, a considerable deviation in the existing results has occurred. Next, we have computed tadpole and horseshoe orbits in the neighbourhood of triangular equilibrium points and then the oblateness effect is recorded on these orbits. Finally, the evolution of orbits of infinitesimal mass about triangular equilibrium points have been estimated by using Poincaré surface of section technique and it is noticed that in presence of oblateness, quasi-periodic orbit dominates over the chaotic zones. These results will help in further study of more generalised models with perturbations.
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Shen, Xinhe, Tao Liu, and Xinhao Liao. "Analytical study of the co-orbital motion in the circular restricted three-body problem." Research in Astronomy and Astrophysics, March 8, 2023. http://dx.doi.org/10.1088/1674-4527/acc29c.
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Abstract In the restricted three-body problem (RTBP), if a small body and a planet stably orbit around a central star with almost exactly the same semimajor axis, and thus almost the same mean motion, this phenomenon is called the co-orbital motion, or equivalently, the 1:1 mean motion resonance. The classical expansion of the disturbing function is divergent when the semimajor axis ratio of the small body to the planet is close to unity. Thus, most of the previous studies on the co-orbital dynamics were carried out through numerical integrations or semi-analytical approaches. In this work, we construct an analytical averaged model for the co-orbital motion in the framework of the circular RTBP. This model is valid in the entire coorbital region except in the vicinity of the collision singularity. The results of the analytical averaged model are in good agreement with the numerical averaged model even for moderate eccentricities and inclinations. The analytical model can reproduce the tadpole, horseshoe and quasi-satellite orbits common in the planar problem. Furthermore, the asymmetry of 1:1 resonance and the compound orbits (F. Namouni. 1999, Icarus 137:293–314) in the general spatial problem can also be obtained from the analytical model.
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de la Fuente Marcos, R., J. de Leon, C. de la Fuente Marcos, et al. "Dynamics of 2023 FW14, the second L4 Mars trojan, and a physical characterization using the 10.4 m Gran Telescopio Canarias." Astronomy & Astrophysics, March 8, 2024. http://dx.doi.org/10.1051/0004-6361/202449688.
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Known Mars trojans could be primordial small bodies that have remained in their present-day orbits for the age of the Solar System. Their orbital distribution is strongly asymmetric; there are over a dozen objects at the L$_ $ point and just one at L$_ $, (121514) 1999 UJ$_ $. Most L$_ $ trojans appear to form a collision-induced asteroid cluster, known as the Eureka family. Asteroid 2023 FW$_ $ was recently discovered and it has a robust orbit determination that may be consistent with a Mars trojan status. Our aim is determine the nature and dynamical properties of 2023 FW$_ We carried out an observational study of 2023 FW$_ $ to derive its spectral class using the OSIRIS camera spectrograph at the 10.4 m Gran Telescopio Canarias. We investigated its possible trojan resonance with Mars using direct $N$-body simulations. The reflectance spectrum of 2023 FW$_ $ is not compatible with the olivine-rich composition of the Eureka family; it also does not resemble the composition of the Moon, although (101429) 1998 VF$_ $ does. The Eureka family and 101429 are at the L$_ $ point. The spectrum of 2023 FW$_ $ is also different from two out of the three spectra in the literature of the other known L$_ $ trojan, 121514, which are of C-type. The visible spectrum of 2023 FW$_ $ is consistent with that of an X-type asteroid, as is the third spectrum of 121514. Our calculations confirm that 2023 FW$_ $ is the second known L$_ $ Mars trojan although it is unlikely to be primordial; it may remain in its present-day ``tadpole'' path for several million years before transferring to a Mars-crossing orbit. It might be a fragment of 121514, but a capture scenario seems more likely. The discovery of 2023 FW$_ $ suggests that regular Mars-crossing asteroids can be captured as temporary Mars trojans.
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Christou, A., N. Georgakarakos, A. Marshall-Lee, A. Humpage, M. Ćuk, and A. Dell'Oro. "New asteroid clusters and evidence of collisional fragmentation in the L5 Trojan cloud of Mars." Astronomy & Astrophysics, April 21, 2025. https://doi.org/10.1051/0004-6361/202553804.
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Trojan asteroids of Mars date from an early phase of Solar System evolution. The Mars Trojan (MT) distribution has been previously shown to be highly asymmetric and inhomogeneous. Remarkably, a single asteroid family associated with (5261) Eureka (H∼16) at mbox L contains all stable Trojans fainter than H=18. A possible culprit is the action of thermal radiation forces on the orbits and rotation states of these small asteroids. Using a larger MT sample than previously available, we took a fresh look at this population to re-evaluate these earlier conclusions. We also searched for additional features diagnostic of MT evolutionary history and of the Eureka family in particular. We performed harmonic analysis on numerical time series of the osculating elements to compile a new proper element catalogue comprising 16 mbox L and 1 mbox L MT asteroids. We then combined sample variance analysis with statistical hypothesis testing to identify clusters in the distribution of orbits and assess their significance. We identify two small clusterings significant at 95% confidence of three H=20-21 asteroids each and investigate their likely origin. One of the clusters is probably the result of rotational breakup of a Eureka family asteroid ∼10^8 yr ago. The significantly higher tadpole libration width of asteroids in the other cluster is more consistent with an origin as impact ejecta from Eureka itself on a timescale comparable to the ∼1 gigayear age of its family. We further confirm the previously reported correlations in Eureka family orbital distribution attributed to the long-term action of radiation-driven forces and torques on the asteroids.
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Luo, Yan, Xiao-Jun Wu, Shu-Rui Zhang, Jian-Min Wang, Luis C. Ho, and Ye-Fei Yuan. "White dwarf–white dwarf collisions in AGN disks via close encounters." Monthly Notices of the Royal Astronomical Society, July 22, 2023. http://dx.doi.org/10.1093/mnras/stad2188.
Full textAbstract:
Abstract White dwarfs (WDs) in active galactic nucleus (AGNs) disks might migrate to the inner radii of the disks and form restricted three-body systems with two WDs moving around the central supermassive black hole (SMBH) in close orbits. These systems could be dynamical unstable, which can lead to very close encounters or direct collisions. In this work, we use N-body simulations to study the evolution of such systems with the different initial orbital separation p, relative orbital inclination Δi and SMBH mass M. It is found that the close encounters of WDs mainly occur at $1.1R_{\rm H} \lesssim p \lesssim 2\sqrt{3}R_{\rm H}$, where RH is the mutual Hill radius. For p &lt; 1.1RH, the majority of the WDs move in horseshoe or tadpole orbits, and only few of them with small initial orbital phase difference undergo close encounters. For p = 3.0RH, the WD-WD collisions occur in most of the samples within the time of 105P1, and there are a considerable collisions occur within the time of t &lt; 62P1 for small orbital radii, where P1 is the orbital period. The peak of the closest separation distribution increase and the WD-WD collision fraction decrease as the increase of the relative inclination. The closest separation distribution is similar in the cases with the different SMBH mass, but the WD-WD collision fraction decrease as the increase of the mass of SMBHs. According to our estimation, the event rate of the cosmic WD-WD collision in AGN disks is about 300Gpc−3yr−1, roughly 1 % of the one of the observed type Ia supernova. The corresponding electromagnetic emission signals can be observed by large surveys of AGNs.
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Raymond, Sean N., Dimitri Veras, Matthew S. Clement, Andre Izidoro, David Kipping, and Victoria Meadows. "Constellations of co-orbital planets: horseshoe dynamics, long-term stability, transit timing variations, and potential as SETI beacons." Monthly Notices of the Royal Astronomical Society, March 2, 2023. http://dx.doi.org/10.1093/mnras/stad643.
Full textAbstract:
Abstract Co-orbital systems contain two or more bodies sharing the same orbit around a planet or star. The best-known flavors of co-orbital systems are tadpoles (in which two bodies’ angular separations oscillate about the L4/L5 Lagrange points 60○ apart) and horseshoes (with two bodies periodically exchanging orbital energy to trace out a horseshoe shape in a co-rotating frame). Here, we use N-body simulations to explore the parameter space of many-planet horseshoe systems. We show that up to 24 equal-mass, Earth-mass planets can share the same orbit at 1 au, following a complex pattern in which neighboring planets undergo horseshoe oscillations. We explore the dynamics of horseshoe constellations, and show that they can remain stable for billions of years and even persist through their stars’ post-main sequence evolution. With sufficient observations, they can be identified through their large-amplitude, correlated transit timing variations. Given their longevity and exotic orbital architectures, horseshoe constellations may represent potential SETI beacons.