the instability of venus trojans
... elongations, and the few surveys have not yet found any. Numerical studies of the long-term stability of putative Venus Trojans (Mikkola & Innanen 1992; Tabachnik & Evans 2000) are limited in time and cover a period of up to 100 Myr. This time span is not long enough to answer the critical question ...
... elongations, and the few surveys have not yet found any. Numerical studies of the long-term stability of putative Venus Trojans (Mikkola & Innanen 1992; Tabachnik & Evans 2000) are limited in time and cover a period of up to 100 Myr. This time span is not long enough to answer the critical question ...
DYNAMICS OF THE GIANT PLANETS OF THE SOLAR SYSTEM IN
... periods of Saturn and Jupiter was initially slightly less than 2, so that the planets were close to their mutual 1: 2 MMR; Uranus and Neptune were supposedly orbiting the Sun a few AU beyond the gas giants, and a massive planetesimal disk extended from about 1.5 AU beyond the last planet up to 30Y35 ...
... periods of Saturn and Jupiter was initially slightly less than 2, so that the planets were close to their mutual 1: 2 MMR; Uranus and Neptune were supposedly orbiting the Sun a few AU beyond the gas giants, and a massive planetesimal disk extended from about 1.5 AU beyond the last planet up to 30Y35 ...
Strange Lights in the Sky - Beck-Shop
... my first look at Comet West, the first look of many. To someone who lived his whole life to that point on a “2-D planet,” like most of us beset by issues of daily life, this was a dose of sudden magic. Who knew that you could simply walk out and so easily see such a range of incredible sights in the u ...
... my first look at Comet West, the first look of many. To someone who lived his whole life to that point on a “2-D planet,” like most of us beset by issues of daily life, this was a dose of sudden magic. Who knew that you could simply walk out and so easily see such a range of incredible sights in the u ...
The Comparative Exploration of the Ice Giant Planets with
... The planets of our Solar System are divided into two main classes: the terrestrial planets, populating the inner Solar System, and the giant planets, which dominate the outer Solar System. The giant planets, in turn, can be divided into the gas giants Jupiter and Saturn, whose mass is mostly constit ...
... The planets of our Solar System are divided into two main classes: the terrestrial planets, populating the inner Solar System, and the giant planets, which dominate the outer Solar System. The giant planets, in turn, can be divided into the gas giants Jupiter and Saturn, whose mass is mostly constit ...
On the chaotic orbit of comet 29P/Schwassmann
... the angle librates, during a long period. However, we found that θ varied from 0o to 360o during the last 10 000 years when calculated for the MMRs 5:4, 6:5 and 11:9 with Jupiter and 1:2 with Saturn. Obviously, 29P is not in any MMR with the first or second giant planet. We also investigate if 29P i ...
... the angle librates, during a long period. However, we found that θ varied from 0o to 360o during the last 10 000 years when calculated for the MMRs 5:4, 6:5 and 11:9 with Jupiter and 1:2 with Saturn. Obviously, 29P is not in any MMR with the first or second giant planet. We also investigate if 29P i ...
Early Dynamical Evolution of the Solar System: Pinning Down the
... which is both efficient and reasonable, is resonant capture (Masset & Snellgrove 2001). When a newly formed gaseous planet reaches a critical mass of ∼ 1MJ , it opens a gap in the proto-planeatary disk. Incidentally, the planet continues to interact with the disk via various resonances. Summed toget ...
... which is both efficient and reasonable, is resonant capture (Masset & Snellgrove 2001). When a newly formed gaseous planet reaches a critical mass of ∼ 1MJ , it opens a gap in the proto-planeatary disk. Incidentally, the planet continues to interact with the disk via various resonances. Summed toget ...
Primordial Excitation and Depletion of the Main Belt
... fragments of larger asteroids destroyed in a collision. Only the largest asteroids retain characteristics that relate to the formation of the asteroid belt and that were not drastically changed by the later evolution. Asteroids with diameters D > 50 km have a collisional lifetime of the order of the ...
... fragments of larger asteroids destroyed in a collision. Only the largest asteroids retain characteristics that relate to the formation of the asteroid belt and that were not drastically changed by the later evolution. Asteroids with diameters D > 50 km have a collisional lifetime of the order of the ...
![ori pro 02 semifin [sfn] - SwRI-Boulder`s](http://s1.studyres.com/store/data/005475037_1-57bfe7f4854fb7170a370f2b1ee14ae6-300x300.png)
ori pro 02 semifin [sfn] - SwRI-Boulder`s
... of the belt that strike each of the terrestrial planets as a function of time during the LHB? Bodies can be transported inward from the belt both by “powerful resonances,” such as the ν6 secular resonance and the 3:1 mean-motion resonance with Jupiter, and by numerous weak “diffusive resonances” (Mo ...
... of the belt that strike each of the terrestrial planets as a function of time during the LHB? Bodies can be transported inward from the belt both by “powerful resonances,” such as the ν6 secular resonance and the 3:1 mean-motion resonance with Jupiter, and by numerous weak “diffusive resonances” (Mo ...
The Cosmic Perspective Asteroids, Comets, and Dwarf Planets
... • Much smaller than the terrestrial or jovian planets • Not a gas giant like other outer planets • Has an icy composition like a comet • Has a very elliptical, inclined orbit • Has more in common with comets than with the eight major planets ...
... • Much smaller than the terrestrial or jovian planets • Not a gas giant like other outer planets • Has an icy composition like a comet • Has a very elliptical, inclined orbit • Has more in common with comets than with the eight major planets ...
Comets- Visitors from the Frozen Edge of the Solar System
... the nucleus is affected by the radiation pressure of the sunlight. This primarily acts on the smaller and thus lighter of the solid grains, spreading them out into more of a curvy or fan-shaped tail, rendered visible by the way the grains reflect sunlight to appear with a yellowish colour. Larger du ...
... the nucleus is affected by the radiation pressure of the sunlight. This primarily acts on the smaller and thus lighter of the solid grains, spreading them out into more of a curvy or fan-shaped tail, rendered visible by the way the grains reflect sunlight to appear with a yellowish colour. Larger du ...
ORIGIN AND EVOLUTION OF THE SOLAR SYSTEM: An overview
... ∗ The observation of disks around stars ∗ The protoplanetary disk: physical features ∗ Accretion of grains into planetesimals and growth to planets ∗ Planet migration and scattering of residual planetesimals ∗ Some reflections about the discovered extrasolar systems ∗ Residual populations: comets, a ...
... ∗ The observation of disks around stars ∗ The protoplanetary disk: physical features ∗ Accretion of grains into planetesimals and growth to planets ∗ Planet migration and scattering of residual planetesimals ∗ Some reflections about the discovered extrasolar systems ∗ Residual populations: comets, a ...
The 11th Sci-Tech Talk in English
... Solar System Built + operated by students at University of ...
... Solar System Built + operated by students at University of ...
Trans-Neptunian Objects as Natural Probes to the Unknown Solar System
... Abstract Trans-Neptunian objects (TNOs) are icy/rocky bodies that move beyond the orbit of Neptune in a region known as the trans-Neptunian belt (or Edgeworth-Kuiper belt). TNOs are believed to be the remnants of a collisionally, dynamically and chemically evolved protoplanetary disk composed of bil ...
... Abstract Trans-Neptunian objects (TNOs) are icy/rocky bodies that move beyond the orbit of Neptune in a region known as the trans-Neptunian belt (or Edgeworth-Kuiper belt). TNOs are believed to be the remnants of a collisionally, dynamically and chemically evolved protoplanetary disk composed of bil ...
Chapter12.2
... • Much smaller than the terrestrial or jovian planets • Not a gas giant like other outer planets • Has an icy composition like a comet • Has a very elliptical, inclined orbit • Has more in common with comets than with the eight major planets © 2010 Pearson Education, Inc. ...
... • Much smaller than the terrestrial or jovian planets • Not a gas giant like other outer planets • Has an icy composition like a comet • Has a very elliptical, inclined orbit • Has more in common with comets than with the eight major planets © 2010 Pearson Education, Inc. ...
An “Asteroid Garden” for the Gainesville Solar Walk And an Asteroid
... are numbered and often named.) For comparison, the Moon and Earth are about 2,160 and 7,920 miles across respectively. Ceres, scaled to the dimensions of the Gainesville Solar Walk would be less than 0.01 inches across! (Note: Some astronomers now consider Ceres large enough to be called a dwarf pla ...
... are numbered and often named.) For comparison, the Moon and Earth are about 2,160 and 7,920 miles across respectively. Ceres, scaled to the dimensions of the Gainesville Solar Walk would be less than 0.01 inches across! (Note: Some astronomers now consider Ceres large enough to be called a dwarf pla ...
Growing the Terrestrial Planets from the Gradual
... because of electrostatic forces. Once particles become large enough so that their Stokes numbers (τ ≡ ts ΩK , where ts is the stopping time due to aerodynamic drag and ΩK is the orbital frequency) are between ∼ 10−3 and 1, depending on the model, these so-called ‘pebbles’ can be concentrated by aero ...
... because of electrostatic forces. Once particles become large enough so that their Stokes numbers (τ ≡ ts ΩK , where ts is the stopping time due to aerodynamic drag and ΩK is the orbital frequency) are between ∼ 10−3 and 1, depending on the model, these so-called ‘pebbles’ can be concentrated by aero ...
Effects of Planetary Migration on Natural Satellites of the Outer Planets
... and their orbits are characterized by large eccentricities and/or inclinations. In most cases the orbits are retrograde. In principle, their dynamical properties are not very compatible with formation from the primordial disk, unless latter evolutionary mechanisms can account for their present orbit ...
... and their orbits are characterized by large eccentricities and/or inclinations. In most cases the orbits are retrograde. In principle, their dynamical properties are not very compatible with formation from the primordial disk, unless latter evolutionary mechanisms can account for their present orbit ...
Make a Comet Motion Flip Book
... the Sun and quickly when it is near to the Sun. It is easy to understand why, if we look at how the pull of gravity between the Sun and the comet works. Gravity is the force that makes any object attract all other objects. The pull of the Earth’s gravity keeps you attached to the Earth and the Sun’s ...
... the Sun and quickly when it is near to the Sun. It is easy to understand why, if we look at how the pull of gravity between the Sun and the comet works. Gravity is the force that makes any object attract all other objects. The pull of the Earth’s gravity keeps you attached to the Earth and the Sun’s ...
Inner versus Outer Planets
... Jupiter, Saturn, Uranus, and Neptune are the outer planets of our solar system. These are the four planets farthest from the Sun. The outer planets are much larger than the inner planets. Since they are mostly made of gases, they are also called gas giants. Pictured below are the relative sizes of t ...
... Jupiter, Saturn, Uranus, and Neptune are the outer planets of our solar system. These are the four planets farthest from the Sun. The outer planets are much larger than the inner planets. Since they are mostly made of gases, they are also called gas giants. Pictured below are the relative sizes of t ...
Jupiter: Cosmic Jekyll and Hyde - Mary Ann Liebert, Inc. publishers
... from 10 million (Chen and Benton, 2012) to as much as 30 million (Sahney and Benton, 2008) years to rebound. If impact events were larger or more frequent, Earth’s biosphere might be radically different from today, perhaps even nonexistent. Some have claimed that Jupiter serves in the role as a cosm ...
... from 10 million (Chen and Benton, 2012) to as much as 30 million (Sahney and Benton, 2008) years to rebound. If impact events were larger or more frequent, Earth’s biosphere might be radically different from today, perhaps even nonexistent. Some have claimed that Jupiter serves in the role as a cosm ...
The potential meteoroid streams crossing the orbits of terrestrial
... A collision of meteoroid particle with the Earth’s atmosphere is detectable if the impact velocity, vi , is high enough. It has been found that the intensity of light from a meteor is proportional to ∝ vi5 . When we aim to find the candidates for the parents of observable meteor showers, we must the ...
... A collision of meteoroid particle with the Earth’s atmosphere is detectable if the impact velocity, vi , is high enough. It has been found that the intensity of light from a meteor is proportional to ∝ vi5 . When we aim to find the candidates for the parents of observable meteor showers, we must the ...
The Potato Radius: a Lower Minimum Size for Dwarf Planets
... the ratio of angular momentum to energy, L/E, increases. The result is a disk (e.g. plane of the Milky Way, ecliptic plane of our Solar System, protoplanetary accretion disks and the rings of Saturn, see Fig. 1, fourth column). Protoplanetary accretion disks are hot and export energy efficiently, bu ...
... the ratio of angular momentum to energy, L/E, increases. The result is a disk (e.g. plane of the Milky Way, ecliptic plane of our Solar System, protoplanetary accretion disks and the rings of Saturn, see Fig. 1, fourth column). Protoplanetary accretion disks are hot and export energy efficiently, bu ...
SR 52(9) 29-32
... existence of an unknown Clyde Tombaugh, the discoverer of Pluto, planet beyond Neptune in at the Lowell Observatory in Arizona. 1905 from odd deviations co-planar. Pluto’s Composite image of Pluto and Charon, released by NASA on 13 July 2015. he observed in the orbits of Neptune orbit is also highly ...
... existence of an unknown Clyde Tombaugh, the discoverer of Pluto, planet beyond Neptune in at the Lowell Observatory in Arizona. 1905 from odd deviations co-planar. Pluto’s Composite image of Pluto and Charon, released by NASA on 13 July 2015. he observed in the orbits of Neptune orbit is also highly ...
A two-stage formation process for the Oort comet cloud and its
... Following the calculations presented above, between 0.15 M⊕ and 0.43 M⊕ should be deposited in the outer cloud by expansion of the innermost cloud over about 4 Gyr through the peturbations of passing stars. In addition, the giant planets deposit some of the material from the disc outside Neptune in ...
... Following the calculations presented above, between 0.15 M⊕ and 0.43 M⊕ should be deposited in the outer cloud by expansion of the innermost cloud over about 4 Gyr through the peturbations of passing stars. In addition, the giant planets deposit some of the material from the disc outside Neptune in ...
Scattered disc
The scattered disc (or scattered disk) is a distant region of the Solar System that is sparsely populated by icy minor planets, a subset of the broader family of trans-Neptunian objects. The scattered-disc objects (SDOs) have orbital eccentricities ranging as high as 0.8, inclinations as high as 40°, and perihelia greater than 30 astronomical units (4.5×109 km; 2.8×109 mi). These extreme orbits are thought to be the result of gravitational ""scattering"" by the gas giants, and the objects continue to be subject to perturbation by the planet Neptune.Although the closest scattered-disc objects approach the Sun at about 30–35 AU, their orbits can extend well beyond 100 AU. This makes scattered objects among the most distant and coldest objects in the Solar System. The innermost portion of the scattered disc overlaps with a torus-shaped region of orbiting objects traditionally called the Kuiper belt, but its outer limits reach much farther away from the Sun and farther above and below the ecliptic than the Kuiper belt proper.Because of its unstable nature, astronomers now consider the scattered disc to be the place of origin for most periodic comets in the Solar System, with the centaurs, a population of icy bodies between Jupiter and Neptune, being the intermediate stage in an object's migration from the disc to the inner Solar System. Eventually, perturbations from the giant planets send such objects towards the Sun, transforming them into periodic comets. Many Oort cloud objects are also thought to have originated in the scattered disc. Detached objects are not sharply distinct from scattered disc objects, and some such as Sedna have sometimes been considered to be included in this group.