Orbital evolution of Mars-crossing asteroids

2020 ◽  
Vol 500 (3) ◽  
pp. 3569-3578
Author(s):  
I Wlodarczyk
Keyword(s):  
Solar System ◽  
Significant Influence ◽  
Orbital Evolution ◽  
The Sun ◽  
Lyapunov Time ◽  
Near Earth Objects ◽  
Orbital Analysis ◽  
Asteroid Families

ABSTRACT This study is an orbital analysis of the interesting Mars-crossing asteroids (MCAs), also known as Mars-crosser (MC) asteroids or Mars-crossers (MCs). We computed that after 100 million years (Myr), approximately 66 ${{\ \rm per\ cent}}$ of all known MCs are ejected out of the Solar System by collision with the Sun, the planets, Ceres, Pallas, Vesta, or Hygiea. The rate of MC migration is high. Thus, this population of MCs would be supplied by just as many asteroids from outside the Solar System. We estimated the rate at which near-Earth objects were created from MCs throughout a 100 Myr period, with Atiras accounting for nearly 3 ${{\ \rm per\ cent}}$ of these objects, over 2 ${{\ \rm per\ cent}}$ were Atens, nearly 7.5 ${{\ \rm per\ cent}}$ were Apollos, approximately 9${{\ \rm per\ cent}}$ were Amors, and nearly 0.4 ${{\ \rm per\ cent}}$ became Centaurs. These results were calculated with 10 000 yr output intervals. Furthermore, 0.028${{\ \rm per\ cent}}$ of all the starting MCs were in retrograde orbits for at least 10 000 yr. We found that majority of the remaining MCs have migrated into the region of three asteroid families: Phocaea, Hungaria, and Flora. We calculated a small but significant influence of Ceres, Pallas, Vesta, and Hygiea on the orbital evolution of the MCs. From the AstDys catalogue, we found that the largest number of studied numbered MCs have their Lyapunov time (LT) in the range 2–4 kyr. Using the orbfit software, we computed the LT of selected MCs in retrograde orbits, and obtained an LT of between 540 yr (asteroid 2016 DR1) and 71 000 yr (asteroid 42887 1999 RV155).

scholarly journals Observational data and orbits of the asteroids discovered at the Molėtai Observatory in 2010–2012

2017 ◽  
Vol 26 (1) ◽  
Author(s):  
Ireneusz Włodarczyk ◽  
Kazimieras Černis ◽  
Justas Zdanavičius
Keyword(s):  
Observational Data ◽  
Orbital Evolution ◽  
Astronomical Observatory ◽  
The Earth ◽  
Lyapunov Time ◽  
Near Earth Objects ◽  
Orbital Analysis

AbstractThis paper is devoted to the discovery of asteroids at the Molėtai Astronomical Observatory (MAO) in 2010- 2012 together with the orbital analysis of two dynamically interesting Near Earth Objects (NEOs) discovered at the MAO, namely 2006 SF77 and 2010 BT3. We used the OrbFit software v.5.0 to compute orbits and to analyze orbital evolution of 2006 SF77 and 2010 BT3. We computed value of the Lyapunov time: 830 years for 2006 SF77 and 1650 year for 2010 BT3.We also searched for possible impacts of 2006 SF77 and 2010 BT3 with the Earth, Venus and Mars in the next 15000 years.

Dynamical evolution of near-Earth objects

2020 ◽  
Author(s):  
Athanasia Toliou ◽  
Mikael Granvik
Keyword(s):  
Semimajor Axis ◽  
Dynamical Evolution ◽  
Orbital Evolution ◽  
Derived Categories ◽  
Asteroid Belt ◽  
The Sun ◽  
Escape Route ◽  
Perihelion Distance ◽  
Main Asteroid Belt ◽  
Near Earth Objects

<p><span>An apparent discrepancy between the number of observed near-Earth objects (NEOs) with small perihelion distances (q) and the number of objects that models <br />predict, has led to the conclusion that asteroids get destroyed at non-trivial distances from the Sun. Consequently, there must be a, possibly thermal, <br />mechanism at play, responsible for breaking up asteroids asteroids in such orbits.<br /><br />We studied the dynamical evolution of ficticious NEOs whose perihelion distance reaches below the average disruption distance q_dis=0.076 au, as suggested by <br />Granvik et al. (2016). To that end, we used the orbital integrations of objects that escaped from the main asteroid belt (Granvik et al. 2017), and entered the <br />near-Earth region (Granvik et al. 2018). First, we investigated a variety of mechanisms that can lower the perihelion distance of an object to a small-enough <br />value. In particular, we considered mean-motion resonances with Jupiter, secular resonances with Jupiter and Saturn (v_5 and v_6) and also the Kozai resonance.<br /><br />We developed a code that calculates the evolution of the critical argument of all the relevant resonances and identifies librations during the last stages of <br />an object's orbital evolution, namely, just before q=q_dis. Any subsequent evolution of the object was disregarded, since we considered it disrupted. The <br />accuracy of our model is ~96%.<br /><br />In addition, we measured the dynamical 'lifetimes' of NEOs when they orbit the innermost parts of the inner Solar System. More precisely, we calculated the <br />total time it takes for the q of each object to go from 0.4 au to q_dis (τ_lq). The outer limit of this range was chosen such because it is a) the approximate <br />semimajor axis of Mercury, and b) an absence of sub-meter-sized boulders with q smaller than this distance has been proposed by Wiegert et al (2020). Combining <br />this measure with the recorded resonances, we can get a sense of the timescale of each q-lowering mechanism.<br /><br />Next, for a more rigorous study of the evolution of the NEOs with q<0.4 au, we divided this region in bins and measured the relevant time they spend at <br />different distances from the Sun. Together with the total time spent in each bin, we kept track of the number of times that q entered one of the bins. <br />Finally, we computed the actual time each object spends in each bin during its evolution, i.e., the total time it spends in a specific range in radial <br />heliocentric distance.<br /><br />By following this approach, we derived categories of typical evolutions of NEOs that reach the average disruption distance. In addition, since we have the <br />information concerning the escape route from the main asteroid belt followed by each NEO, we linked the q-lowering mechanism and the associated orbital <br />evolutions in the range below the orbit of Mercury, to their source regions and thus were able to draw conclusions abour their physical properties.</span></p>

scholarly journals On the orbital evolution of 2020 AV2, the first asteroid ever observed to go around the Sun inside the orbit of Venus

2020 ◽  
Vol 494 (1) ◽  
pp. L6-L10 ◽  
Author(s):  
C de la Fuente Marcos ◽  
R de la Fuente Marcos
Keyword(s):  
Orbital Evolution ◽  
Gravitational Perturbation ◽  
The Sun ◽  
Moon System ◽  
Resonant Orbit ◽  
The Earth ◽  
Short Period ◽  
Orbital Periods ◽  
Near Earth Objects

ABSTRACT The innermost section of the Solar system has not been extensively studied because minor bodies moving inside Earth’s orbit tend to spend most of their sidereal orbital periods at very low solar elongation, well away from the areas more frequently observed by programs searching for near-Earth objects. The survey carried out from the Zwicky Transient Facility (ZTF) is the first one that has been able to detect multiple asteroids well detached from the direct gravitational perturbation of the Earth–Moon system. ZTF discoveries include 2019 AQ3 and 2019 LF6, two Atiras with the shortest periods among known asteroids. Here, we perform an assessment of the orbital evolution of 2020 AV2, an Atira found by ZTF with a similarly short period but following a path contained entirely within the orbit of Venus. This property makes it the first known member of the elusive Vatira population. Genuine Vatiras, those long-term dynamically stable, are thought to be subjected to the so-called von Zeipel–Lidov–Kozai oscillation that protects them against close encounters with both Mercury and Venus. However, 2020 AV2 appears to be a former Atira that entered the Vatira orbital domain relatively recently. It displays an anticoupled oscillation of the values of eccentricity and inclination, but the value of the argument of perihelion may circulate. Simulations show that 2020 AV2 might reach a 3:2 resonant orbit with Venus in the future, activating the von Zeipel–Lidov–Kozai mechanism, which in turn opens the possibility to the existence of a long-term stable population of Vatiras trapped in this configuration.

scholarly journals OSSOS

2019 ◽  
Vol 621 ◽  
pp. A102 ◽  
Author(s):  
Nahuel Cabral ◽  
Aurélie Guilbert-Lepoutre ◽  
Wesley C. Fraser ◽  
Michaël Marsset ◽  
Kathryn Volk ◽  
...  
Keyword(s):  
Solar System ◽  
Giant Planet ◽  
Orbital Evolution ◽  
Outer Solar System ◽  
The Sun ◽  
Point Spread Functions ◽  
Water Ice ◽  
Point Spread ◽  
Size Estimates ◽  
Cometary Activity

Context. Centaurs are icy objects in transition between the trans-Neptunian region and the inner solar system, orbiting the Sun in the giant planet region. Some centaurs display cometary activity, which cannot be sustained by the sublimation of water ice in this part of the solar system, and has been hypothesized to be due to the crystallization of amorphous water ice. Aims. In this work, we investigate centaurs discovered by the Outer Solar System Origins Survey (OSSOS) and search for cometary activity. Tentative detections would improve understanding of the origins of activity among these objects. Methods. We search for comae and structures by fitting and subtracting both point spread functions and trailed point-spread functions from the OSSOS images of each centaur. When available, Col-OSSOS images were used to search also for comae. Results. No cometary activity is detected in the OSSOS sample. We track the recent orbital evolution of each new centaur to confirm that none would actually be predicted to be active, and we provide size estimates for the objects. Conclusions. The addition of 20 OSSOS objects to the population of ~250 known centaurs is consistent with the currently understood scenario, in which drastic drops in perihelion distance induce changes in the thermal balance prone to trigger cometary activity in the giant planet region.

scholarly journals Lunar-like silicate material forms the Earth quasi-satellite (469219) 2016 HO3 Kamoʻoalewa

2021 ◽  
Vol 2 (1) ◽  
Author(s):  
Benjamin N. L. Sharkey ◽  
Vishnu Reddy ◽  
Renu Malhotra ◽  
Audrey Thirouin ◽  
Olga Kuhn ◽  
...  
Keyword(s):  
Solar System ◽  
Reflectance Spectrum ◽  
Space Weathering ◽  
The Sun ◽  
Silicate Material ◽  
Lunar Material ◽  
The Earth ◽  
Solar System Bodies ◽  
Near Earth Objects

AbstractLittle is known about Earth quasi-satellites, a class of near-Earth small solar system bodies that orbit the sun but remain close to the Earth, because they are faint and difficult to observe. Here we use the Large Binocular Telescope (LBT) and the Lowell Discovery Telescope (LDT) to conduct a comprehensive physical characterization of quasi-satellite (469219) Kamoʻoalewa and assess its affinity with other groups of near-Earth objects. We find that (469219) Kamoʻoalewa rotates with a period of 28.3 (+1.8/−1.3) minutes and displays a reddened reflectance spectrum from 0.4–2.2 microns. This spectrum is indicative of a silicate-based composition, but with reddening beyond what is typically seen amongst asteroids in the inner solar system. We compare the spectrum to those of several material analogs and conclude that the best match is with lunar-like silicates. This interpretation implies extensive space weathering and raises the prospect that Kamo’oalewa could comprise lunar material.

scholarly journals Extraterrestrial Influences on Remote Sensing in the Earth’s Atmosphere

2021 ◽  
Vol 13 (5) ◽  
pp. 890
Author(s):  
Aleksandra Nina ◽  
Milan Radovanović ◽  
Luka Č. Popović
Keyword(s):  
Remote Sensing ◽  
Solar System ◽  
Solar Radiation ◽  
Significant Influence ◽  
Coming Out ◽  
Outer Space ◽  
Signal Propagation ◽  
Atmospheric Parameters ◽  
Atmospheric Disturbances ◽  
Propagation Paths

Atmospheric properties have a significant influence on electromagnetic (EM) waves, including the propagation of EM signals used for remote sensing. For this reason, changes in the received amplitudes and phases of these signals can be used for the detection of the atmospheric disturbances and, consequently, for their investigation. Some of the most important sources of the temporal and space variations in the atmospheric parameters come from the outer space. Although the solar radiation dominates in these processes, radiation coming out of the solar system also can induces enough intensive disturbance in the atmosphere to provide deflections in the EM signal propagation paths. The aim of this issue is to present the latest research linking events and processes in outer space with changes in the propagation of the satellite and ground-based signals used in remote sensing.

scholarly journals The Principle of Least Interaction Action

1974 ◽  
Vol 3 ◽  
pp. 489-489
Author(s):  
M. W. Ovenden
Keyword(s):  
Solar System ◽  
Planetary System ◽  
Satellite System ◽  
Asteroid Belt ◽  
Correct Prediction ◽  
The Sun ◽  
Approximate Methods ◽  
Satellites Of Jupiter ◽  
History Of ◽  
Minimum Interaction

AbstractThe intuitive notion that a satellite system will change its configuration rapidly when the satellites come close together, and slowly when they are far apart, is generalized to ‘The Principle of Least Interaction Action’, viz. that such a system will most often be found in a configuration for which the time-mean of the action associated with the mutual interaction of the satellites is a minimum. The principle has been confirmed by numerical integration of simulated systems with large relative masses. The principle lead to the correct prediction of the preference, in the solar system, for nearly-commensurable periods. Approximate methods for calculating the evolution of an actual satellite system over periods ˜ 109 yr show that the satellite system of Uranus, the five major satellites of Jupiter, and the five planets of Barnard’s star recently discovered, are all found very close to their respective minimum interaction distributions. Applied to the planetary system of the Sun, the principle requires that there was once a planet of mass ˜ 90 Mθ in the asteroid belt, which ‘disappeared’ relatively recently in the history of the solar system.

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