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Journal articles on the topic 'Orbital Collisions'

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Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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1

Abedin, Abedin Y., J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, and Kathryn Volk. "OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt." Astronomical Journal 164, no. 6 (November 30, 2022): 261. http://dx.doi.org/10.3847/1538-3881/ac9cdb.

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Abstract We investigate different conditions, including the orbital and size–frequency distribution (SFD) of the early Kuiper Belt, that can trigger catastrophic planetesimal destruction. The goal of this study is to test if there is evidence for collisional grinding in the Kuiper Belt that has occurred since its formation. This analysis has important implications for whether the present-day SFD of the cold classical trans-Neptunian objects (TNOs) is a result of collisional equilibrium or if it reflects the primordial stage of planetesimal accretion. As an input to our modeling, we use the most up-to-date debiased OSSOS++ ensemble sample of the TNO population and orbital model based on the present-day architecture of the Kuiper Belt. We calculate the specific impact energies between impactor–target pairs from different TNO groups and compare our computed energies to catastrophic disruption results from smoothed particle hydrodynamics simulations. We explore different scenarios by considering different total primordial Kuiper Belt masses and power slopes of the SFD and allowing collisions to take place over different timescales. The collisional evolution of the Kuiper Belt is a strong function of the unknown initial mass in the trans-Neptunian region, where collisional grinding of planetesimals requires a total primordial Kuiper Belt mass of M > 5 M ⊕, collision speeds as high as 3 km s−1, and collisions over at least 0.5 Gyr. We conclude that presently, most of the collisions in the trans-Neptunian region are in the cratering rather than disruption regime. Given the low collision rates among the cold classical Kuiper Belt objects, their SFD most likely represents the primordial planetesimal accretion.
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2

Zhang, Haitao, Zhi Li, Weilin Wang, Yasheng Zhang, and Hao Wang. "Geostationary Orbital Debris Collision Hazard after a Collision." Aerospace 9, no. 5 (May 10, 2022): 258. http://dx.doi.org/10.3390/aerospace9050258.

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Many space objects are densely distributed in the geostationary (GEO) band, and the long-term impact of the collision of GEO spacecraft and space debris on the GEO environment has attracted more and more attention. After summarizing the advantages and disadvantages of the long-term evolution model based on the “Cube” collision probability calculation model, the “Grid” model, a long-term evolution model especially suitable for GEO band, was established. For four types of collision and disintegration events, the “Grid” model was used to study the space environment in the GEO band after collisions between GEO spacecraft and space debris. Future collisions were simulated, and the number of space objects in the next 100 years was counted. Once space debris and massive spacecraft were completely disintegrated after collision, the number of space objects and the collision probability increased sharply, and this caused a collision cascading syndrome. Even if there was no initial disintegration event, collision and disintegration events occurred in the long-term evolution of the GEO band, which led to an increase in the number of space objects. However, the collision probability was much lower, and the number of space objects grew much more slowly without the initial collision.
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3

Knowles, Stephen H. "Space Object Traffic Control." International Astronomical Union Colloquium 112 (1991): 165. http://dx.doi.org/10.1017/s0252921100003912.

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ABSTRACTThe task of avoiding collisions between orbiting objects requires more than a statistical description of the objects’ positions. The paper describes the general procedures used for such cataloging, together with an indication of the accuracy required for orbital collision avoidance.
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4

Nicolas, Timothée. "Impact of azimuthal forcing on the Brillouin limit in a collisional two-species Ohkawa filter." Physics of Plasmas 29, no. 4 (April 2022): 042105. http://dx.doi.org/10.1063/5.0073198.

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This paper investigates the physics of plasma separation in a two species rotating collisional Ohkawa filter, when the source of rotation is an orbital angular momentum carrying wave. The electric field is treated self-consistently with ion and electron radial motion. The injection of angular momentum causes radial currents leading to charge penetration and electric field build up. The electric field varies until an equilibrium with the friction forces is reached. Both collisions with neutrals and Coulomb collisions are considered. In the case where the electric field is driven by the resonant wave, there is no collisional breakdown of the Brillouin limit [Rax et al., Phys. Plasmas 22, 092101 (2015)]; on the contrary, the maximum achievable electric field decreases when the collision frequency is increased. When two species are present, one that undergoes the wave forcing while the second does not interact with the wave, we find the following: the first species is confined, while the second species can be expelled or confined depending on the charge to mass ratio and the collisionalities. Assuming equal charge numbers, if the second species is the heavy one, it is always expelled, which is a standard result. When the second species is the light one, it can also be expelled in the common case where neutral collisions dominate over Coulomb collisions, which constitutes a new result.
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5

TROSHIN, S. M., and N. E. TYURIN. "ELLIPTIC FLOW IN pp-COLLISIONS AT THE LHC." Modern Physics Letters A 26, no. 15 (May 20, 2011): 1095–102. http://dx.doi.org/10.1142/s0217732311035559.

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We consider collective effects in pp-collisions at the LHC energies related to presence of the large orbital angular momentum in the initial state and role of this orbital momentum in the elliptic flow behavior.
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6

Appleton, P. N. "Collisional Ring Galaxies." Symposium - International Astronomical Union 186 (1999): 97–104. http://dx.doi.org/10.1017/s007418090011232x.

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Ring galaxies are believed to represent a special case of a collision between two galaxies, in which one of the galaxies impacts and passes through the center of another disk system (e.g. Lynds & Toomre 1976). Although rare, this kind of low orbital-angular-momentum collision leads to a recognizable structure, namely a luminous blue star-forming ring (Appleton & Marston 1997), which should be easily identifiable even at moderate redshift. Indeed, Lavery et al. (1996) have used this fact, and their relative rarity at low-redshift, to conclude that rings (and therefore presumably all collisions) are over-represented in deep HST fields.
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7

Mikhailov V. S., Babenko P. Yu., Shergin A. P., and Zinoviev A. N. "Auger transition probabilities and electron emission cross sections for vacancy decay into the 2pπ-orbital in the Ne-=SUP=-+-=/SUP=--Ne quasimolecule." Technical Physics Letters 48, no. 1 (2022): 70. http://dx.doi.org/10.21883/tpl.2022.01.52475.19018.

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The paper reports the calculation of the probabilities of Auger transitions taking place in the process of filling a vacancy on the 2pπ-orbital in an Ne+-Ne quasimolecule, a short-lived system which arises when the ion and atom approach each other and decays when they fly apart. Calculations for various ionization degrees of the quasimolecule particles were performed for the first time. It was found out that the system ionization degree increases very significantly (from 2 to 6) with increasing collision energy and decreasing distance of the particles closest approach. Using of the quantum mechanical approach and taking into account the collision dynamics made it possible to quantitatively describe for the first time the experimental Auger electron spectra of a complex many-electron quasimolecule. The contribution of the transition from the initial 3dπ-3dπ state to the 2pπ orbital was shown to be predominant among the whole variety of possible Auger decay channels. Keywords: atomic collisions, quasimolecule, Auger transitions, electron emission cross sections, vacancy decay
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8

Crespi, Samuele, Ian Dobbs-Dixon, Nikolaos Georgakarakos, Nader Haghighipour, Thomas I. Maindl, Christoph M. Schäfer, and Philip Matthias Winter. "Protoplanet collisions: Statistical properties of ejecta." Monthly Notices of the Royal Astronomical Society 508, no. 4 (October 13, 2021): 6013–22. http://dx.doi.org/10.1093/mnras/stab2951.

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ABSTRACT The last phase of the formation of rocky planets is dominated by collisions among Moon- to Mars-sized planetary embryos. Simulations of this phase need to handle the difficulty of including the post-impact material without saturating the numerical integrator. A common approach is to include the collision-generated material by clustering it into few bodies with the same mass and uniformly scattering them around the collision point. However, this approach oversimplifies the properties of the collision material by neglecting features that can play important roles in the final structure and composition of the system. In this study, we present a statistical analysis of the orbital architecture, mass, and size distributions of the material generated through embryo–embryo collisions and show how they can be used to develop a model that can be directly incorporated into the numerical integrations. For instance, results of our analysis indicate that the masses of the fragments follow an exponential distribution with an exponent of −2.21 ± 0.17 over the range of 10−7 to 2 × 10−2 Earth-masses. The distribution of the post-impact velocities show that a large number of fragments are scattered towards the central star. The latter is a new finding that may be quite relevant to the delivery of material from the outer regions of the asteroid belt to the accretion zones of terrestrial planets. Finally, we present an analytical model for the 2D distribution of fragments that can be directly incorporated into numerical integrations.
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9

Dougherty, Ralph C. "Molecular orbital treatment of gas-phase ion molecule collision rates: Reactive and nonreactive collisions." Mass Spectrometry Reviews 20, no. 3 (2001): 142–52. http://dx.doi.org/10.1002/mas.10002.

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10

Choksi, Nick, Eugene Chiang, Harold C. Connolly, Zack Gainsforth, and Andrew J. Westphal. "Chondrules from high-velocity collisions: thermal histories and the agglomeration problem." Monthly Notices of the Royal Astronomical Society 503, no. 3 (February 22, 2021): 3297–308. http://dx.doi.org/10.1093/mnras/stab503.

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ABSTRACT We assess whether chondrules, once-molten mm-sized spheres filling the oldest meteorites, could have formed from super-km s−1 collisions between planetesimals in the solar nebula. High-velocity collisions release hot and dense clouds of silicate vapour which entrain and heat chondrule precursors. Thermal histories of CB chondrules are reproduced for colliding bodies ∼10–100 km in radius. The slower cooling rates of non-CB, porphyritic chondrules point to colliders with radii ≳ 500 km. How chondrules, collisionally dispersed into the nebula, agglomerated into meteorite parent bodies remains a mystery. The same orbital eccentricities and inclinations that enable energetic collisions prevent planetesimals from re-accreting chondrules efficiently and without damage; thus the sedimentary laminations of the CB/CH chondrite Isheyevo are hard to explain by direct fallback of collisional ejecta. At the same time, planetesimal surfaces may be littered with the shattered remains of chondrules. The micron-sized igneous particles recovered from comet 81P/Wild-2 may have originated from in-situ collisions and subsequent accretion in the proto-Kuiper belt, obviating the need to transport igneous solids across the nebula. Asteroid sample returns from Hayabusa2 and OSIRIS-REx may similarly contain chondrule fragments.
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11

Khan, M. A., J. P. Connerade, and M. Rafique. "Orbital contraction in Ca and its effect on collisions." Journal of Physics B: Atomic, Molecular and Optical Physics 27, no. 17 (September 14, 1994): L563—L569. http://dx.doi.org/10.1088/0953-4075/27/17/001.

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12

Fukuda, Hiroshi, and Takeshi Ishihara. "Distorted atomic-orbital expansion for slow ion-atom collisions." Physical Review A 46, no. 9 (November 1, 1992): 5531–38. http://dx.doi.org/10.1103/physreva.46.5531.

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13

Xu, Ming, Stephanie Dillon, J. Daniel Kimel, and Ralph C. Dougherty. "Molecular Orbital Model for Ion Polar-Molecule Capture Collisions." Journal of Physical Chemistry A 104, no. 32 (August 2000): 7511–17. http://dx.doi.org/10.1021/jp0005266.

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14

Михайлов, В. С., П. Ю. Бабенко, А. П. Шергин, and А. Н. Зиновьев. "Вероятности оже-переходов и сечения эмиссии электронов при распаде вакансии на 2pπ-орбитали в квазимолекуле Ne-=SUP=-+-=/SUP=--Ne." Письма в журнал технической физики 48, no. 2 (2022): 30. http://dx.doi.org/10.21883/pjtf.2022.02.51918.19018.

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The Auger transition probabilities are calculated while filling a vacancy on 2pπ orbital in a Ne+-Ne quasimolecule, a short-lived system which is formed when ion and atom approach each other and decays when they scatter. For the first time calculations were performed for various degrees of particles ionization in quasimolecule. It was found that with increase of collision energy and decrease of distance of the closest approach of particles the system ionization degree increases very significantly (from 2 to 6). Using of the quantum mechanical approach and taking into account the dynamics of collisions made it possible for the first time to describe quantitatively the experimental spectra of Auge electrons for a complex many-electron quasimolecule. From the whole variety of possible Auger decay channels the dominant contribution of the transition was established, from the initial 3dπ-3dπ state to the 2pπ orbital.
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15

Illescas, Clara, Luis Méndez, Santiago Bernedo, and Ismanuel Rabadán. "Charge Transfer and Electron Production in Proton Collisions with Uracil: A Classical and Semiclassical Study." International Journal of Molecular Sciences 24, no. 3 (January 21, 2023): 2172. http://dx.doi.org/10.3390/ijms24032172.

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Cross sections for charge transfer and ionization in proton–uracil collisions are studied, for collision energies 0.05<E<2500 keV, using two computational models. At low energies, below 20 keV, the charge transfer total cross section is calculated employing a semiclassical close-coupling expansion in terms of the electronic functions of the supermolecule (H-uracil)+. At energies above 20 keV, a classical-trajectory Monte Carlo method is employed. The cross sections for charge transfer at low energies have not been previously reported and have high values of the order of 40 Å2, and, at the highest energies of the present calculation, they show good agreement with the previous results. The classical-trajectory Monte Carlo calculation provides a charge transfer and electron production cross section in reasonable agreement with the available experiments. The individual molecular orbital contributions to the total electron production and charge transfer cross sections are analyzed in terms of their energies; this permits the extension of the results to other molecular targets, provided the values of the corresponding orbital energies are known.
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16

Thomsen, Jan W. "Alignment effects in electron transfer: Experimental studies for singly charged ion collisions with Na(3p) atoms." Canadian Journal of Physics 74, no. 11-12 (November 1, 1996): 950–54. http://dx.doi.org/10.1139/p96-812.

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This paper reports experimental results for the influence of target excitation and orbital alignment on the electron-transfer process in ion–Na(3s, 3p) collisions. Systematic experimental investigations with a range of simple ions reveal a similar behavior of the electron-transfer cross-section parameters as a function velocity. The experimental findings are compared with atomic and molecular orbital calculations.
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17

Mahdi, Mohammed Chessab. "Study the Space Debris Impact in the Early Stages of the Nano-Satellite Design." Artificial Satellites 51, no. 4 (December 1, 2016): 163–72. http://dx.doi.org/10.1515/arsa-2016-0014.

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Abstract The probability of KufaSat collisions with different sizes of orbital debris and with other satellites which operating in the same orbit during orbital lifetime was determined. Apogee/Perigee Altitude History was used to graph apogee and perigee altitudes over KufaSat lifetime. The required change in velocity for maneuvers necessary to reentry atmospheric within 25 years was calculated. The prediction of orbital lifetime of KufaSat using orbital parameters and engineering specifications as inputs to the Debris Assessment Software (DAS) was done, it has been verified that the orbital lifetime will not be more than 25 years after end of mission which is compatible with recommendation of Inter-Agency Space Debris Coordination Committee (IADC).
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18

Esteves, Leandro, André Izidoro, Sean N. Raymond, and Bertram Bitsch. "The origins of nearly coplanar, non-resonant systems of close-in super-Earths." Monthly Notices of the Royal Astronomical Society 497, no. 2 (July 20, 2020): 2493–500. http://dx.doi.org/10.1093/mnras/staa2112.

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ABSTRACT Some systems of close-in ‘super-Earths’ contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet–disc interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here, we mine a large data set of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity, and non-resonant state. This subset has dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations (≲1○) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations (i ≲ 1○), orbital inclinations are barely increased by encounters before planets collide. When planetary scattering pumps orbital inclinations to higher values (≳1○) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers’ orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system.
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19

Dermott, Stanley F., Dan Li, Apostolos A. Christou, Thomas J. J. Kehoe, Carl D. Murray, and J. Malcolm Robinson. "Dynamical evolution of the inner asteroid belt." Monthly Notices of the Royal Astronomical Society 505, no. 2 (May 17, 2021): 1917–39. http://dx.doi.org/10.1093/mnras/stab1390.

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ABSTRACT A determination of the dynamical evolution of the asteroid belt is difficult because the asteroid belt has evolved since the time of asteroid formation through mechanisms that include: (1) catastrophic collisions, (2) rotational disruption, (3) chaotic orbital evolution, and (4) orbital evolution driven by Yarkovsky radiation forces. The time-scales of these loss mechanisms are uncertain and there is a need for more observational constraints. In the inner main belt (IMB), the mean size of the non-family asteroids increases with increasing inclination. Here, we use that observation to show that all IMB asteroids originate from either the known families or from ghost families, that is, old families with dispersed orbital elements. We estimate that the average age of the asteroids in the ghost families is a factor of 1/3 less than the Yarkovsky orbital evolution time-scale. However, this orbital evolution time-scale is a long-term average that must allow for the collisional evolution of the asteroids and for stochastic changes in their spin directions. By applying these constraints on the orbital evolution time-scales to the evolution of the size-frequency distribution of the Vesta asteroid family, we estimate that the age of this family is greater than 1.3 Gyr and could be comparable with the age of the Solar system. By estimating the number of ghost families, we calculate that the number of asteroids that are the root sources of the meteorites and the near-Earth asteroids that originate from the IMB is about 20.
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20

Wallace, Spencer C., Thomas R. Quinn, and Aaron C. Boley. "Collision rates of planetesimals near mean-motion resonances." Monthly Notices of the Royal Astronomical Society 503, no. 4 (March 19, 2021): 5409–24. http://dx.doi.org/10.1093/mnras/stab792.

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ABSTRACT In circumstellar discs, collisional grinding of planetesimals produces second-generation dust. While it remains unclear whether this ever becomes a major component of the total dust content, the presence of such dust, and potentially the substructure within it, can be used to explore a disc’s physical conditions. A perturbing planet produces non-axisymmetric structures and gaps in the dust, regardless of its origin. The dynamics of planetesimals, however, will be very different than that of small dust grains due to weaker gas interactions. Therefore, planetesimal collisions could create dusty disc structures that would not exist otherwise. In this work, we use N-body simulations to investigate the collision rate profile of planetesimals near mean-motion resonances. We find that a distinct bump or dip feature is produced in the collision profile, the presence of which depends on the libration width of the resonance and the separation between the peri- and apocentre distances of the edges of the resonance. The presence of one of these two features depends on the mass and eccentricity of the planet. Assuming that the radial dust emission traces the planetesimal collision profile, the presence of a bump or dip feature in the dust emission at the 2:1 mean-motion resonance can constrain the orbital properties of the perturbing planet. This assumption is valid, so long as radial drift does not play a significant role during the collisional cascade process. Under this assumption, these features in the dust emission should be marginally observable in nearby protoplanetary discs with ALMA.
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21

Muñoz, F., J. Rogan, G. García, J. A. Valdivia, R. Ramírez, and M. Kiwi. "The role of d-orbital polarization on rhodium cluster collisions." European Physical Journal D 64, no. 1 (July 29, 2011): 45–51. http://dx.doi.org/10.1140/epjd/e2011-20052-1.

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22

Micha, David A., and Keith Runge. "Time evolution of orbital polarization in slow ion—atom collisions." Chemical Physics Letters 238, no. 1-3 (May 1995): 132–36. http://dx.doi.org/10.1016/0009-2614(95)00372-x.

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23

Scora, Jennifer, Diana Valencia, Alessandro Morbidelli, and Seth Jacobson. "Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets." Astrophysical Journal 940, no. 2 (November 30, 2022): 144. http://dx.doi.org/10.3847/1538-4357/ac9cda.

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Abstract Rocky planets both in and outside of our solar system are observed to have a range of core-mass fractions (CMFs). Imperfect collisions can preferentially strip mantle material from a planet, changing its CMF, and are therefore thought to be the most likely cause of this observed CMF variation. However, previous work that implements these collisions into N-body simulations of planet formation has struggled to reliably form high CMF super-Earths. In this work, we specify our initial conditions and simulation parameters to maximize the prevalence of high-energy, CMF-changing collisions in order to form planets with highly diverse CMFs. High-energy collisions have a large v imp/v esc ratio, so we maximize this ratio by starting simulations with high eccentricity and inclination disks to increase the difference in their orbital velocities, maximizing v imp. Additionally, we minimize v esc by starting with small embryos. The final planets undergo more high-energy, debris-producing collisions, and experience significant CMF change over their formation. However, we find that a number of processes work together to average out the CMF of a planet over time; therefore, we do not consistently form high CMF, high-mass planets. We do form high CMF planets below 0.5 M ⊕. Additionally, we find, in these highly eccentric environments, loss of debris mass due to collisional grinding has a significant effect on final planet masses and CMFs, resulting in smaller planets and a higher average planet CMF. This work highlights the importance of improving measurements of high-density planets to better constrain their CMFs.
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24

Haghighipour, Nader. "Dynamics, Origin, and Activation of Main Belt Comets." Proceedings of the International Astronomical Union 5, S263 (August 2009): 207–14. http://dx.doi.org/10.1017/s1743921310001766.

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AbstractThe discovery of Main Belt Comets (MBCs) has raised many questions regarding the origin and activation mechanism of these objects. Results of a study of the dynamics of these bodies suggest that MBCs were formed in-situ as the remnants of the break-up of large icy asteroids. Simulations show that similar to the asteroids in the main belt, MBCs with orbital eccentricities smaller than 0.2 and inclinations lower than 25° have stable orbits implying that many MBCs with initially larger eccentricities and inclinations might have been scattered to other regions of the asteroid belt. Among scattered MBCs, approximately 20% reach the region of terrestrial planets where they might have contributed to the accumulation of water on Earth. Simulations also show that collisions among MBCs and small objects could have played an important role in triggering the cometary activity of these bodies. Such collisions might have exposed sub-surface water ice which sublimated and created thin atmospheres and tails around MBCs. This paper discusses the results of numerical studies of the dynamics of MBCs and their implications for the origin of these objects. The results of a large numerical modeling of the collisions of m-sized bodies with km-sized asteroids in the outer part of the asteroid belt are also presented and the viability of the collision-triggering activation scenario is discussed.
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25

Xia, Zonghuang, Demin Wang, and Shigang Wu. "INVESTIGATION OF VACANCY DISTRIBUTION IN C+−B, C+−N, C+−Be andC+−O ION-ATOM COLLISIONS." International Journal of PIXE 06, no. 01n02 (January 1996): 65–69. http://dx.doi.org/10.1142/s0129083596000089.

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The mechanism of vacancy distribution in C +− B , C +− N , C +− Be , and C +− O ion-atom collision process is studied in this paper based on molecular orbital theory. It translates intensity ratio of X-ray and Auger decay in ion-atom collision process.
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26

Hathorn, B. C., B. G. Sumpter, M. D. Barnes, and D. W. Noid. "Molecular dynamics simulation of polymer nanoparticle collisions: orbital angular momentum effects." Polymer 43, no. 10 (May 2002): 3115–21. http://dx.doi.org/10.1016/s0032-3861(02)00030-7.

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27

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 (November 28, 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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28

Guo, D. L., R. T. Zhang, X. L. Zhu, Y. Gao, K. Z. Lin, T. Cao, D. M. Zhao, et al. "Benchmark n ℓ-resolved Cross Sections of Single and Double Charge Exchange Processes in 1.67–20 keV u−1 C4+ Collisions with He." Astrophysical Journal 941, no. 1 (December 1, 2022): 31. http://dx.doi.org/10.3847/1538-4357/ac9d2e.

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Abstract State-resolved charge exchange (CX) cross sections are of the utmost importance for modeling related photon emissions existing in a broad range of astrophysical environments. With the cold-target recoil-ion momentum spectroscopy, we determined with high accuracy the state-resolved single and double CX cross sections at the quantum orbital angular momentum level for solar wind ion C4+ collisions with He in an energy range of 1.67–20 keV u−1, which allow one to benchmark the CX calculations in great detail, and to test the applicability of the analytical n- and ℓ-distribution models widely adopted by the astrophysical community. We found that the present measurements are well reproduced by the most recent state-of-the-art atomic–orbital close-coupling calculations. However, the CX models failed to give a consistent description on the measured ℓ distributions. The present work reveals that the velocity and collision partner species dependence effects as well as electronic correlations for multielectron processes should be included in an improved model. Alternatively, in future modeling to interpret high-resolution astrophysical observations the more elaborate quantum-mechanical calculations may be resorted to with confidence.
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Solanes, J. M., J. D. Perea, and G. Valentí-Rojas. "Timescales of major mergers from simulations of isolated binary galaxy collisions." Astronomy & Astrophysics 614 (June 2018): A66. http://dx.doi.org/10.1051/0004-6361/201832855.

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A six-dimensional parameter space based on high-resolution numerical simulations of isolated binary galaxy collisions has been constructed to investigate the dynamical friction timescales, τmer, for major mergers. Our experiments follow the gravitational encounters between ∼600 pairs of similarly massive late- and early-type galaxies with orbital parameters that meet the predictions of the Λ-cold dark matter (ΛCDM) cosmology. We analyse the performance of different schemes for tracking the secular evolution of mergers, finding that the product of the intergalactic distance and velocity is best suited to identify the time of coalescence. In contrast, a widely used merger-time estimator such as the exhaustion of the orbital spin is shown to systematically underpredict τmer, resulting in relative errors that can reach 60% for nearly radial encounters. We find that the internal spins of the progenitors can lead to total variations in the merger times larger than 30% in highly circular encounters, whereas only the spin of the principal halo is capable of modulating the strength of the interaction prevailing throughout a merger. The comparison of our simulated merger times with predictions from different variants of a well-known fitting formula has revealed an only partially satisfactory agreement, which has led us to recalculate the values of the coefficients of these expressions to obtain relations that fit major mergers perfectly. The observed biases between data and predictions, which do not only apply to the present work, are inconsistent with expectations from differences in the degree of idealisation of the collisions, their metric, spin-related biases, or the simulation set-up. This indicates a certain lack of accuracy of the dynamical friction modelling, arising perhaps from a still incomplete identification of the parameters governing orbital decay.
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30

Fritsch, Wolfgang. "Theoretical study of slow He+–Na(3s, 3p) collisions." Canadian Journal of Physics 74, no. 11-12 (November 1, 1996): 944–49. http://dx.doi.org/10.1139/p96-811.

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Electron transfer processes in He+–Na(3s, 3p) collisions are studied with the semiclassical close-coupling method. The electron dynamics is described with a number of antisymmetrized two-electron configurations of atomic-orbital type. Contrary to assumptions in earlier work, capture to the 31,3L He states is found to be important in the keV energy region. The calculated transfer cross sections agree well with recent data on Na(3p)–Na(3s) cross-section ratios and on the Na(3p0)–Na(3p1) anisotropy parameter.
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31

Voloshin, Sergei A. "Vorticity and particle polarization in heavy ion collisions (experimental perspective)." EPJ Web of Conferences 171 (2018): 07002. http://dx.doi.org/10.1051/epjconf/201817107002.

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The recent measurements of the global polarization and vector meson spin alignment along the system orbital momentum in heavy ion collisions are briefly reviewed. A possible connection between the global polarization and the chiral anomalous effects is discussed along with possible experimental checks. Future directions, in particular those aimed on the detailed mapping of the vorticity fields, are outlined. The Blast Wave model is used for an estimate of the anisotropic flow effect on the vorticity component along the beam direction. We also point to a possibility of a circular pattern in the vorticity field in asymmetric, e.g. Cu+Au, central collisions.
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32

Kley, Wilhelm. "Formation and Orbital Evolution of Planets." Proceedings of the International Astronomical Union 7, S282 (July 2011): 429–36. http://dx.doi.org/10.1017/s1743921311027980.

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AbstractThe formation of planetary systems is a natural byproduct of the star formation process. Planets can form inside the protoplanetary disk by two alternative processes. Either through a sequence of sticking collisions, the so-called sequential accretion scenario, or via gravitational instability from an over-dense clump inside the protoplanetary disk. The first process is believed to have occurred in the solar system. The most important steps in this process will be outlined. The observed orbital properties of exoplanetary systems are distinctly different from our own Solar System. In particular, their small distance from the star, their high eccentricity and large mass point to the existence of a phase with strong mutual excitations. These are believed to be a result of early evolution of planets due to planet-disk interaction. The importance of this process in shaping the dynamical structure of planetary systems will be presented.
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33

BLAND, L. C. "MEASUREMENT OF FORWARD JETS AT RHIC." International Journal of Modern Physics: Conference Series 25 (January 2014): 1460022. http://dx.doi.org/10.1142/s2010194514600222.

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We present first measurements of forward jet production from p↑ + p collisions at [Formula: see text] GeV, including transverse single spin asymmetries. These asymmetries are expected to be sensitive to spin-correlated transverse momentum in the initial state, which is particularly interesting because it is related to orbital angular momentum in the proton.
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34

Wan, Sheng Hui, Jun Ling Song, Jian Chen, and Min Hu. "Hybrid Approach to Optimize the Cluster Flying Orbit for Fractionated Spacecraft Based on PSO-SQP Algorithm." Applied Mechanics and Materials 341-342 (July 2013): 1144–49. http://dx.doi.org/10.4028/www.scientific.net/amm.341-342.1144.

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This template This paper investigates the optimal cluster flight orbit design issue for the fractionated spacecraft according to three main goals: keeping the cluster as stable as possible, preventing the collisions within the cluster, maintaining the inter-satellite distance within the maximum region. Firstly, the relative orbital elements are adopted to describe the relative motion. Then, the formation design requirements are formulated in terms of the relative orbital elements, the constrained optimization problem is solved using the hybrid particle swarm optimization algorithm integrated with sequential quadratic programming local search. The simulation results show that the hybrid PSO-SQP algorithm is effective.
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35

Kimura, M., and C. D. Lin. "Charge transfer and excitation processes inp-He collisions studied using a unified atomic-orbital–molecular-orbital matching method." Physical Review A 34, no. 1 (July 1, 1986): 176–84. http://dx.doi.org/10.1103/physreva.34.176.

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36

Ipatov, Sergei I., and John C. Mather. "Migration of comets to the terrestrial planets." Proceedings of the International Astronomical Union 2, S236 (August 2006): 55–64. http://dx.doi.org/10.1017/s1743921307003067.

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AbstractWe studied the orbital evolution of objects with initial orbits close to those of Jupiter-family comets (JFCs), Halley-type comets (HTCs), and long-period comets, and the probabilities of their collisions with the planets. In our runs the probability of a collision of one object with the Earth could be greater than the sum of probabilities for thousands of other objects. Even without the contribution of such a few objects, the probability of a collision of a former JFC with the Earth during the dynamical lifetime of the comet was greater than 4×10−6. This probability is enough for delivery of all the water to Earth's oceans during the formation of the giant planets. The ratios of probabilities of collisions of JFCs and HTCs with Venus and Mars to the mass of the planet usually were not smaller than that with Earth. Among 30,000 considered objects with initial orbits close to those of JFCs, a few objects got Earth-crossing orbits with semimajor axesa<2 AU and aphelion distancesQ<4.2 AU, or even got inner-Earth (Q<0.983 AU), Aten, or typical asteroidal orbits, and moved in such orbits for more than 1 Myr (up to tens or even hundreds of Myr). From a dynamical point of view, the fraction of extinct comets among near-Earth objects can exceed several tens of percent, but, probably, many extinct comets disintegrated into mini-comets and dust during a smaller part of their dynamical lifetimes.
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37

Antonio, Nicholas W., Corey T. Plowman, Ilkhom B. Abdurakhmanov, Igor Bray, and Alisher S. Kadyrov. "Fully-Stripped Beryllium-Ion Collisions with 2ℓm States of Atomic Hydrogen: Target Excitation and Ionisation cross Sections." Atoms 10, no. 4 (November 10, 2022): 137. http://dx.doi.org/10.3390/atoms10040137.

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The wave-packet convergent close-coupling approach is used to calculate integrated target excitation and ionisation cross sections in bare beryllium-ion collisions with the 2ℓm states of atomic hydrogen (where n, ℓ and m are the principal, orbital angular momentum and magnetic quantum numbers, respectively). The calculations are performed at representative projectile energies between 10 keV/u to 1 MeV/u. The calculated cross sections for collisions with H(2s) are compared with recent theoretical results. Generally, good agreement is observed for the n-partial excitation and total ionisation cross sections. However, a significant discrepancy is found for excitation into the dominant n=3 states at 100 keV/u, where the target excitation cross-section peaks. We also present the first calculations of the excitation and ionisation cross sections for Be4+ collisions with H(2p0) and H(2p±1).
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38

Lin, Douglas N. C., and Ian Dobbs-Dixon. "Diversity of close-in planets and the interactions with their host stars." Proceedings of the International Astronomical Union 3, S249 (October 2007): 131–44. http://dx.doi.org/10.1017/s1743921308016517.

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AbstractShort period planets provide an exciting opportunity of constraining structural properties. Observations have revealed a diverse class of objects, including several at odds with aspects of conventional planet formation theories. Here we present several scenarios that may help in producing the observed diversity. For short period planets in particular, their proximity to their host stars suggests that star-planet interactions may play an important role in their orbital and structural evolution. We first show that the penetration of a non-synchronous stellar magnetic field into short period planets will provide a significant source of energy for planetary expansion and may help stall inward migration. In addition to magnetic dissipation, the intense irradiation from the host star will drive atmospheric flows, whose behaviour is strongly influenced by the opacity of the envelope. Finally, we explore the role of late stage planetesimal and embryo bombardment on the structure of gas-giant planets. Dynamical trapping during migration, followed by orbital destablization during the final stage of gas-giant growth, leads to a surge in the collision rate. Such collisions will lead to preferential core growth and inflated radii. All three of these processes, occurring late in the planetary formation process, will produce a large range in planetary properties and may account for the diversity we see today.
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39

Burns, Joseph A. "Physical Processes on Circumplanetary Dust." International Astronomical Union Colloquium 126 (1991): 341–48. http://dx.doi.org/10.1017/s0252921100067099.

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AbstractThe life cycles of grains in circumplanetary space are governed by various physical processes that alter sizes and modify orbits. Lifetimes are quite short, perhaps 102-104years for typical circumplanetary grains of 1 micron radius. Thus particles must be continually supplied to the circumplanetary complex, probably by the grinding down of larger parent bodies in collisions. Dust is eroded gradually through sublimation and through sputtering by the magnetospheric plasma but also is catastrophically destroyed through hypervelocity impacts with interplanetary micrometeoroids. Orbits evolve through momentum transfer (light drag, plasma or Coulomb drag, and atmospheric drag), and through resonant gravitational and electromagnetic forces. Plasma drag is generally the most effective evolution mechanism, with the possible exceptions of exospheric drag at Uranus and of electromagnetic schemes for some conditions. Since grains become charged (with typical electric potentials of a few volts), they undergo associated orbital perturbations: variable electromagnetic forces can cause the systematic drain of energy (orbital collapse) or, at specific (resonant) orbital locations can force large orbital inclinations/eccentricities. Solar radiation induces a periodic orbital eccentricity that can reach substantial values for 1 micron particles distant from the giant planets.
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40

Lauritsen, J. H. V., J. W. Thomsen, N. Andersen, D. Dowek, J. C. Houver, J. O. P. Pedersen, J. Salgado, and A. Svensson. "Electron transfer in keV collisions: III. Experiments on initial orbital alignment dependence." Journal of Physics B: Atomic, Molecular and Optical Physics 29, no. 5 (March 14, 1996): 1093–100. http://dx.doi.org/10.1088/0953-4075/29/5/017.

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41

Lapicki, G., and William Lichten. "Reconciliation of atomic- and molecular-orbital models in slow and symmetric collisions." Physical Review A 31, no. 3 (March 1, 1985): 1354–61. http://dx.doi.org/10.1103/physreva.31.1354.

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42

Thomsen, J. W., N. Andersen, E. E. B. Campbell, I. V. Hertel, and S. E. Nielsen. "Effects of excitation and orbital alignment on electron transfer in -Na collisions." Journal of Physics B: Atomic, Molecular and Optical Physics 31, no. 15 (August 14, 1998): 3429–37. http://dx.doi.org/10.1088/0953-4075/31/15/014.

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43

Molitoris, J. D., W. E. Meyerhof, Ch Stoller, R. Anholt, D. W. Spooner, L. G. Moretto, L. G. Sobotka, et al. "Molecular-orbital study of late-fission times in deep-inelasticU238+238U collisions." Physical Review Letters 70, no. 5 (February 1, 1993): 537–40. http://dx.doi.org/10.1103/physrevlett.70.537.

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44

Moudry, B. W., O. Yenen, D. H. Jaecks, and J. H. Macek. "Experimental determination of orbital and spin orientation of (Ar+)* formed in collisions." Physical Review A 54, no. 5 (November 1, 1996): 4119–26. http://dx.doi.org/10.1103/physreva.54.4119.

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45

Haro, Sinhué, Juan Antonio Juárez, and Gloria Koenigsberger. "Is there a Connection Between Non-Synchronous Rotation and X-Ray Emission in Massive Binary Systems?" Symposium - International Astronomical Union 215 (2004): 163–65. http://dx.doi.org/10.1017/s0074180900195476.

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A correlation between orbital period and log(LX/Lbol) is found for a sample of B-type binary systems. We suggest that wind-wind collisions are the likely mechanism for generating the X-ray emission, and that the mass-loss rates may be enhanced in non-synchronously rotating systems due to the oscillations that are excited by the tidal forces.
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46

Deng, Jian, Qun Wang, and Hong Zhang. "A topological realization of spin polarization through vortex formation in collisions of Bose–Einstein condensates." Physics of Fluids 34, no. 8 (August 2022): 087118. http://dx.doi.org/10.1063/5.0099125.

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The global spin polarization of hadrons in heavy ion collisions has been measured in the solenoidal tracker at relativistic heavy ion collider experiments, which opens up a new window in the study of the hottest, least viscous, and most vortical fluid that has ever been produced in the laboratory. We present a different approach to spin polarization from conventional ones: a topological realization of spin polarization through quantum vortex formation in collisions of Bose–Einstein condensates. This approach is based on the observation that the vortex is a topological excitation in a superfluid in the presence of local orbital angular momentum and is an analog of spin degrees of freedom. The formation processes of vortices and vortex–antivortex pairs are investigated by solving the Gross–Pitaevskii equation with a large-scale parallel algorithm on a graphics processing unit to very high precision. In a rotating environment, the primary vortex with winding number one is stable against perturbation, which has minimal energy and fixed orbital angular momentum (OAM), but the vortices with larger winding numbers are unstable and will decay into primary vortices through a redistribution of the energy and vorticity. The injection of OAM can also be realized in non-central collisions of self-interacting condensates, part of the OAM of the initial state will induce the formation of vortices through concentration of energy and vorticity density around topological defects. Different from a hydrodynamical description, the interference of the wave function plays an important role in the transport of energy and vorticity, reflecting the quantum nature of the vortex formation process. The study of the vortex formation may shed light on the nature of particle spin and spin–orbit couplings in strong interaction matter produced in heavy-ion collisions.
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47

Souda, Ryutaro. "Band Effects on Ion-Surface Charge Exchange." International Journal of Modern Physics B 11, no. 06 (March 10, 1997): 685–706. http://dx.doi.org/10.1142/s0217979297000393.

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Various aspects of charge exchange between low-energy ions (10 eV–2 keV) and solid surfaces are discussed with particular emphasis placed on the effects of valence orbital hybridization on the electronic transition probabilities, and uniqueness of surface scattering relative to diatomic gas-phase collision is highlighted. Two classes of projectiles are explored, i.e. inert noble-gas ions and a reactive hydrogen ion. One or two core vacancies are created in noble-gas projectiles during collisions with specific target atoms, leading to (re)ionization and autoionization. In contrast to gas-phase collision, it is found that one-electron excitation predominates over simultaneous two-electron excitation. This result is basically ascribed to the band effect of energy-level crossing. Neutralization of the slow hydrogen ion at a surface is rather unique compared to the noble-gas ions and its probability is sensitively dependent upon ionicity of target atoms or the nature of the valence band. This is because a valence electron is captured via a new class of resonance neutralization which is mediated by a short-lived chemisorption state of hydrogen on a surface.
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48

Chemerynska, I. V., M. V. Ishchenko, M. O. Sobolenko, S. A. Khoperskov, and P. P. Berczik. "Kinematic characteristics of the Milky Way globular clusters based on Gaia DR2 data." Advances in Astronomy and Space Physics 12, no. 1-2 (2022): 18–24. http://dx.doi.org/10.17721/2227-1481.18-24.

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Using the data from Gaia (ESA) Data Release 2 we performed the orbital calculations of globular clusters (GCs) of the Milky Way. To explore possible close encounters (or collisions) between the GCs, using our own developed high-order φ-GRAPE code, we integrated backward and forward orbits of 119 objects with reliable positions and proper motions. In the calculations, we adopted a realistic axisymmetric Galactic potential (bulge + disk + halo). Using different impact conditions, we found four pairs of six GCs that may have experienced an encounter within twice the sum of the half-mass radii ('collisions') over the last 5 Gyr: Terzan 3 — NGC 6553, Terzan 3 — NGC 6218, Liller 1 — NGC 6522 and Djorg 2 — NGC 6553.
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Chemerynska, I. V., M. V. Ishchenko, M. O. Sobolenko, S. A. Khoperskov, and P. P. Berczik. "Kinematic characteristics of the Milky Way globular clusters based on Gaia DR2 data." Advances in Astronomy and Space Physics 12, no. 1-2 (2022): 18–24. http://dx.doi.org/10.17721/2227-1481.12.18-24.

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Using the data from Gaia (ESA) Data Release 2 we performed the orbital calculations of globular clusters (GCs) of the Milky Way. To explore possible close encounters (or collisions) between the GCs, using our own developed high-order φ-GRAPE code, we integrated backward and forward orbits of 119 objects with reliable positions and proper motions. In the calculations, we adopted a realistic axisymmetric Galactic potential (bulge + disk + halo). Using different impact conditions, we found four pairs of six GCs that may have experienced an encounter within twice the sum of the half-mass radii ('collisions') over the last 5 Gyr: Terzan 3 — NGC 6553, Terzan 3 — NGC 6218, Liller 1 — NGC 6522 and Djorg 2 — NGC 6553.
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50

Liu, Yongjie, Yu Jiang, and Hengnian Li. "Analytical Propagation of Space Debris Density for Collisions near Sun-Synchronous Orbits." Space: Science & Technology 2022 (September 17, 2022): 1–17. http://dx.doi.org/10.34133/2022/9825763.

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The increasing frequency of human launches has led to a dramatic increase in the amount of space debris, especially near sun-synchronous orbits. Most of the fragments are small in size, which may make tracking difficult. Therefore, characterizing the distribution, evolution, and collision risk of small debris has long been a difficult issue. This paper is aimed at investigating the orbital evolution and global dispersion behavior of debris clouds near sun-synchronous orbits. Firstly, the NASA breakup model is used to provide an initial distribution of small fragments after collision events. Secondly, the continuity equation is adopted to propagate the density variation analytically. Furthermore, we introduce some statistical quantities and the entropy of debris clouds to model the randomness and band formation. A theorem concerning the equivalence of the band formation and maximal entropy is presented. The accuracy of the band formation time estimation is also discussed. For noncatastrophic collisions at an altitude of 800 km due to a projectile with a mass of 100 g and a collision velocity of 1 km/s, we compare the analytical and numerical results of space debris density. The results show that the maximal peak error is within 0.17, and the mean square error is about 0.25 at 400 days. Additionally, the entropy of right ascension of the ascending node is 8.5% less than that for debris clouds near an orbit with the same altitude and an inclination of 30 deg. This indicates the concentrating behavior for debris clouds near sun-synchronous orbits.
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