scholarly journals Slow and Fast Diffusion in Asteroid-Belt Resonances: A Review

1999 ◽  
Vol 172 ◽  
pp. 25-37
Author(s):  
S. Ferraz-Mello
Keyword(s):  
Solar System ◽  
Chaotic Behaviour ◽  
Asteroid Belt ◽  
Fast Diffusion ◽  
Outer Solar System ◽  
Recent Advances ◽  
Short Period ◽  
Hecuba Gap

AbstractThis paper reviews recent advances in several topics of resonant asteroidal dynamics as the role of resonances in the transportation of asteroids and asteroidal debris to the inner and outer solar system; the explanation of the contrast of a depleted 2/1 resonance (Hecuba gap) and a high-populated 3/2 resonance (Hilda group); the overall stochasticity created in the asteroid belt by the short-period perturbations of Jupiter’s orbit, with emphasis in the formation of significant three-period resonances, the chaotic behaviour of the outer asteroid belt, and the depletion of the Hecuba gap.

scholarly journals The origin of inner Solar System water

2017 ◽  
Vol 375 (2094) ◽  
pp. 20150384 ◽  
Author(s):  
Conel M. O'D. Alexander
Keyword(s):  
Solar System ◽  
Classical Model ◽  
Terrestrial Planet ◽  
Asteroid Belt ◽  
Carbonaceous Chondrites ◽  
Outer Solar System ◽  
Isotopic Compositions ◽  
O Isotopes ◽  
N Isotopes

Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H 2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

scholarly journals Resonant trans-Neptunian objects as a source of Jupiter-family comets

2006 ◽  
Vol 2 (S236) ◽  
pp. 31-34
Author(s):  
E. L. Kiseleva ◽  
V. V. Emel'yanenko
Keyword(s):  
Solar System ◽  
Dynamical Evolution ◽  
Early History ◽  
Substantial Contribution ◽  
Outer Solar System ◽  
Symplectic Integrator ◽  
Relative Fraction ◽  
Outward Transport ◽  
Short Period ◽  
History Of

AbstractThe dynamical interrelation between resonant trans-Neptunian objects and short-period comets is studied. Initial orbits of resonant objects are based on computations in the model of the outward transport of objects during Neptune's migration in the early history of the outer Solar system. The dynamical evolution of this population is investigated for 4.5 Gyr, using a symplectic integrator. Our calculations show that resonant trans-Neptunian objects give a substantial contribution to the planetary region. We have estimated that the relative fraction of objects captured per year from the 2/3 resonance to Jupiter-family orbits with perihelion distances q<2.5 AU is 0.4×10−10 near the present epoch.

scholarly journals The Kuiper Belt

1994 ◽  
Vol 160 ◽  
pp. 31-44
Author(s):  
Jane Luu
Keyword(s):  
Solar System ◽  
Kuiper Belt ◽  
Cometary Nucleus ◽  
Outer Solar System ◽  
Short Period Comet ◽  
Short Period ◽  
Lower Limits ◽  
Period Comet

The existence of a belt of comets in the outer solar system (the “Kuiper belt”) has been postulated for a variety of reasons, including the need for a source for the short-period comets. The existence of the belt seems supported by the discoveries of the trans-Neptunian objects 1992 QB1, 1993 FW, 1993 RO, 1993 RP, 1993 SB, and 1993 SC. If these objects are members of the Kuiper belt, crude lower limits on the belt population can be established from the discoveries. The Kuiper belt comets are likely to be primordial remnants of the disk from which the solar system accreted. According to the current theories of cometary nucleus evolution, these objects are expected to possess mantles (“irradiation mantles”) which are different from mantles of comets which have been heated to the point of sublimation (“rubble mantles”). Kuiper belt comets on their way to short-period comet orbits may exist among the Centaur objects.

Near-Simultaneous Optical + NIR Photometry of Interstellar Comet 2I/Borisov

2020 ◽  
Author(s):  
Megan Schwamb ◽  
Michele Bannister ◽  
Michael Marsset ◽  
Wesley Fraser ◽  
Rosemary Pike ◽  
...  
Keyword(s):  
Solar System ◽  
Outer Solar System ◽  
Small Bodies ◽  
Near Ir ◽  
Short Period Comet ◽  
Short Period ◽  
Dust Composition ◽  
Survey Sample ◽  
Dust Coma ◽  
Rare Opportunity

&lt;p&gt;In August 2019, 2I/Borisov, the second interstellar object and first visibly active interstellar comet, was discovered on a trajectory nearly perpendicular to the ecliptic. Observations of planet forming disks and debris disks serve as probes of the ensemble properties of extrasolar planetesimals, but the passage of an active interstellar comet through our Solar System provides a rare opportunity to individually study these small bodies up close in the same ways in which we investigate objects originating from our own Outer Solar System. Ground-based observations of short period comet &lt;span&gt;67P/Churyumov&amp;#8211;Gerasimenko&lt;/span&gt; revealed a coma dust composition indistinguishable from what was measured on its nucleus by the orbiting &lt;em&gt;Rosetta&lt;/em&gt; spacecraft. Therefore when 2/I Borisov had a dust dominated tail, we attempted to study its composition with near-simultaneous griJ photometry with the Gemini North Telescope. We obtained two epochs of GMOS-N and NIRI observations in November 2019, separated by two weeks. We will report on the inferred optical-near-IR colors of 2I/I Borisov&amp;#8217;s dust coma/tail and nucleus. We will compare our measurements to other observations of 2I/Borisov and place the interstellar comet in context with the Col-OSSOS (Colours of the Outer Solar System Survey) sample of small KBOs and interstellar object &lt;span&gt;&amp;#699;Oumuamua&lt;/span&gt; observed in grJ with Gemini North, using the same setup.&lt;/p&gt;

scholarly journals Planetary Trojans – the main source of short period comets?

2010 ◽  
Vol 9 (4) ◽  
pp. 227-234 ◽  
Author(s):  
J. Horner ◽  
P. S. Lykawka
Keyword(s):  
Solar System ◽  
Short Review ◽  
Oort Cloud ◽  
Asteroid Belt ◽  
Exoplanetary Systems ◽  
Short Period ◽  
Proximate Source ◽  
Different Origins ◽  
Near Earth Asteroids ◽  
The Impact

AbstractOne of the key considerations when assessing the potential habitability of telluric worlds will be that of the impact regime experienced by the planet. In this work, we present a short review of our understanding of the impact regime experienced by the terrestrial planets within our own Solar system, describing the three populations of potentially hazardous objects which move on orbits that take them through the inner Solar system. Of these populations, the origins of two (the Near-Earth Asteroids and the Long-Period Comets) are well understood, with members originating in the Asteroid belt and Oort cloud, respectively. By contrast, the source of the third population, the Short-Period Comets, is still under debate. The proximate source of these objects is the Centaurs, a population of dynamically unstable objects that pass perihelion (closest approach to the Sun) between the orbits of Jupiter and Neptune. However, a variety of different origins have been suggested for the Centaur population. Here, we present evidence that at least a significant fraction of the Centaur population can be sourced from the planetary Trojan clouds, stable reservoirs of objects moving in 1:1 mean-motion resonance with the giant planets (primarily Jupiter and Neptune). Focussing on simulations of the Neptunian Trojan population, we show that an ongoing flux of objects should be leaving that region to move on orbits within the Centaur population. With conservative estimates of the flux from the Neptunian Trojan clouds, we show that their contribution to that population could be of order ~3%, while more realistic estimates suggest that the Neptune Trojans could even be the main source of fresh Centaurs. We suggest that further observational work is needed to constrain the contribution made by the Neptune Trojans to the ongoing flux of material to the inner Solar system, and believe that future studies of the habitability of exoplanetary systems should take care not to neglect the contribution of resonant objects (such as planetary Trojans) to the impact flux that could be experienced by potentially habitable worlds.

scholarly journals Jupiter – friend or foe? IV: the influence of orbital eccentricity and inclination

2012 ◽  
Vol 11 (3) ◽  
pp. 147-156 ◽  
Author(s):  
J. Horner ◽  
B. W. Jones
Keyword(s):  
Solar System ◽  
Asteroid Belt ◽  
Slight Reduction ◽  
Orbital Eccentricity ◽  
Orbital Inclination ◽  
The Earth ◽  
Impact Rate ◽  
Impact Flux ◽  
Short Period ◽  
The Impact

AbstractFor many years, it has been assumed that Jupiter has prevented the Earth from being subject to a punishing impact regime that would have greatly hindered the development of life. Here, we present the fourth in a series of dynamical studies investigating this hypothesis. In our earlier work, we examined the effect of Jupiter's mass on the impact rate experienced by the Earth. Here, we extend that approach to consider the influence of Jupiter's orbital eccentricity and inclination on the impact rate from asteroidal bodies and short-period comets. We first considered scenarios in which Jupiter's orbital eccentricity was somewhat higher and somewhat lower than that in our Solar System, for a variety of ‘Jupiter’ masses. We find that Jupiter's orbital eccentricity plays a moderate role in determining the impact flux at Earth, with more eccentric orbits resulting in a noticeably higher impact rate of asteroids than is the case for more circular orbits. This is particularly pronounced at high ‘Jupiter’ masses. For the short-period comets, the same effect is clearly apparent, albeit to a much lesser degree. The flux of short-period comets impacting the Earth is slightly higher for more eccentric Jovian orbits. We also considered scenarios in which Jupiter's orbital inclination was greater than that in our Solar System. Increasing Jupiter's orbital inclination greatly increased the flux of asteroidal impactors upon the Earth. However, at the highest tested inclination, the disruption to the Asteroid belt was so great that the belt would be entirely depleted after an astronomically short period of time. In such a system, the impact flux from asteroid bodies would therefore be very low, after an initial period of intense bombardment. By contrast, the influence of Jovian inclination on impacts from short-period comets was very small. A slight reduction in the impact flux was noted for the moderate and high inclination scenarios considered in this work – the results for inclinations of 5° and 25° were essentially identical.

scholarly journals Near-Earth objects from the cometary flux

2012 ◽  
Vol 10 (H16) ◽  
pp. 153-153
Author(s):  
Vacheslav Emel'yanenko
Keyword(s):  
Solar System ◽  
Outer Solar System ◽  
High Eccentricity ◽  
Earth Space ◽  
Near Earth Space ◽  
Dynamical Characteristics ◽  
Short Period ◽  
Near Earth Objects

AbstractWe analyze the orbital distribution of objects captured to near-Earth space from the flux of comets coming from the outer Solar system. For this purpose, we use the model of the cometary cloud developed earlier (Emelfyanenko, Asher, Bailey, 2007). This model is consistent with the broad dynamical characteristics of observed near-parabolic comets, short-period comets, Centaurs and high-eccentricity trans-Neptunian objects. We show that the observed distributions of both large and small near-Earth objects are different from the modeled distribution formed dynamically by the action of planetary perturbations. In particular, while the distributions of arguments of perihelion for observed Jupiter-family comets and modeled cometary asteroids follow a sinusoidal law with pronounced maxima around 0 and 180 degrees, it is not the case for observed cometary asteroids of any size. We conclude that there exist many unobserved extinct short-period comets among near-Earth objects of various sizes.

scholarly journals Chaotic behaviour in the Solar System

1987 ◽  
Vol 413 (1844) ◽  
pp. 109-129 ◽  
Keyword(s):  
Solar System ◽  
Orbital Evolution ◽  
Chaotic Behaviour ◽  
The Other ◽  
Asteroid Belt ◽  
Essential Ingredient ◽  
The Past

There are several physical situations in the Solar System where chaotic behaviour plays an important role. Saturn’s satellite Hyperion is currently tumbling chaotically. Many of the other irregularly shaped satellites in the Solar System had chaotic rotations in the past. There are also examples of chaotic orbital evolution. Meteorites are most probably transported to Earth from the asteroid belt by way of a chaotic zone. Chaotic behaviour also seems to be an essential ingredient in the explanation of certain non-uniformities in the distribution of asteroids.The long-term motion of Pluto is suspiciously complicated, but objective criteria have not yet indicated that the motion is chaotic.

scholarly journals A scattered Uranus and Neptune, and implications for the asteroid belt

2004 ◽  
Vol 202 ◽  
pp. 241-243
Author(s):  
Edward W. Thommes ◽  
Martin J. Duncan ◽  
Harold F. Levison ◽  
John E. Chambers
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Initial Conditions ◽  
Asteroid Belt ◽  
Outer Solar System ◽  
Wide Range ◽  
Gas Giant ◽  
Gas Accretion ◽  
High Degree

It has been proposed that Uranus and Neptune originated interior to ∽ 10 AU, as potential gas giant cores which were scattered outward when Jupiter won the race to reach runaway gas accretion. We present further numerical simulations of this scenario, which show that it reproduces the present configuration of the outer Solar System with a high degree of success for a wide range of initial conditions. Also, we show that this mechanism may have simultaneously ejected planets from the asteroid belt.

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