Origin of Terrestrial Planets and-the Earth
... shock dissipation. The forces between particles thus include attraction due to gravity, which acts inversely with the squared distance between particles, and a repulsive pressure for adjacent particles closer than approximately the sum of their smoothing lengths. The equation of state relates a part ...
... shock dissipation. The forces between particles thus include attraction due to gravity, which acts inversely with the squared distance between particles, and a repulsive pressure for adjacent particles closer than approximately the sum of their smoothing lengths. The equation of state relates a part ...
Chapter 15 The Formation of Planetary Systems
... • Large interstellar cloud of gas and dust starts to contract, heating as it does so. ...
... • Large interstellar cloud of gas and dust starts to contract, heating as it does so. ...
Origin of Terrestrial Planets and the Earth-Moon System - U
... random particle velocities arise from the planetesimals' orbital eccentricities and inclinations and are analogous to the random thermal velocities of gas molecules confined to some volume. As this simple expression shows, the rate of collisions, and therefore of accretional growth, depends on the l ...
... random particle velocities arise from the planetesimals' orbital eccentricities and inclinations and are analogous to the random thermal velocities of gas molecules confined to some volume. As this simple expression shows, the rate of collisions, and therefore of accretional growth, depends on the l ...
Nebula Theory
... of the gas is lower, the density of solids is enhanced with rocky and icy planetesimals. • Such an enhancement of the solid density may cause collisional accumulation of solids and results in runaway growth to a mass of approximately10 Earth-masses in 0.5-1 million years. • These bodies may accrete ...
... of the gas is lower, the density of solids is enhanced with rocky and icy planetesimals. • Such an enhancement of the solid density may cause collisional accumulation of solids and results in runaway growth to a mass of approximately10 Earth-masses in 0.5-1 million years. • These bodies may accrete ...
Lecture 7 Formation of the Solar System Nebular Theory
... Flattening of the Solar Nebula • As the nebula collapses, clumps of gas collide & merge. • Their random velocities average out into the nebula’s direction of rotation. => Orderly motion • The spinning nebula assumes the shape of a disk. ...
... Flattening of the Solar Nebula • As the nebula collapses, clumps of gas collide & merge. • Their random velocities average out into the nebula’s direction of rotation. => Orderly motion • The spinning nebula assumes the shape of a disk. ...
Origin of the Solar System
... Formation of the solar system! • A collapsing gas cloud naturally tends to heat up, spin faster, and flatten out as it shrinks in size. ! • Thus, our solar system began as a spinning disk of gas. ! ...
... Formation of the solar system! • A collapsing gas cloud naturally tends to heat up, spin faster, and flatten out as it shrinks in size. ! • Thus, our solar system began as a spinning disk of gas. ! ...
Document
... potassium-40, half of which decays into argon-40 every 1.25 billion years. You open the rock and find 15 atoms of argon-40 for every atom of potassium-40. How long ago did the rock form? a) ...
... potassium-40, half of which decays into argon-40 every 1.25 billion years. You open the rock and find 15 atoms of argon-40 for every atom of potassium-40. How long ago did the rock form? a) ...
Birth of the Solar System
... Planets orbit in same direction as Sun rotates (prograde) Most planets rotate in same direction as they orbit with axial tilts less than 30 (Venus and Uranus are exceptions) Separation between orbits increases with distance from Sun Multitude of smaller bodies (asteroids, KBOs, comets) with ...
... Planets orbit in same direction as Sun rotates (prograde) Most planets rotate in same direction as they orbit with axial tilts less than 30 (Venus and Uranus are exceptions) Separation between orbits increases with distance from Sun Multitude of smaller bodies (asteroids, KBOs, comets) with ...
Lesson 2
... Today, we know that the orbits of the planets are only slightly elliptical, but the orbits of objects such as Pluto and comets are highly elliptical. Kepler found that a planet moves slower at aphelion, sweeping out a narrow sector on the ellipse. Conversely, a planet moves faster at perihelion, swe ...
... Today, we know that the orbits of the planets are only slightly elliptical, but the orbits of objects such as Pluto and comets are highly elliptical. Kepler found that a planet moves slower at aphelion, sweeping out a narrow sector on the ellipse. Conversely, a planet moves faster at perihelion, swe ...
File
... dust grains containing heavier elements produced by earlier stars and supernovas. 2) Shockwaves from supernovas may have triggered the collapse of the nebular cloud, which rotated faster as it contracted in order to conserve angular momentum. 3) The inward pull of gravity along with the outward push ...
... dust grains containing heavier elements produced by earlier stars and supernovas. 2) Shockwaves from supernovas may have triggered the collapse of the nebular cloud, which rotated faster as it contracted in order to conserve angular momentum. 3) The inward pull of gravity along with the outward push ...
ppt version
... From Grains to Planetesimals Grains that have low-velocity collisions can stick together, forming bigger grains. • Beyond the “frost line”, get additional growth by condensing ices onto the grains. ...
... From Grains to Planetesimals Grains that have low-velocity collisions can stick together, forming bigger grains. • Beyond the “frost line”, get additional growth by condensing ices onto the grains. ...
Lesson 2 Power Notes Outline
... Friction from matter that fell into the disk heated its center to millions of degrees, resulting in the fusion of hydrogen atoms into helium atoms. ...
... Friction from matter that fell into the disk heated its center to millions of degrees, resulting in the fusion of hydrogen atoms into helium atoms. ...
Life in the Universe Lecture (G 345U)
... What we know comes from meteorites and modeling. Only hard evidence is from chrondrite meteorites. Chrondites are pieces of asteroid that gathered up the solids of the nebula and never got “processed”. Inner solar disk hotter and outer is cooler. Makes a difference on planet formation. Inner terres ...
... What we know comes from meteorites and modeling. Only hard evidence is from chrondrite meteorites. Chrondites are pieces of asteroid that gathered up the solids of the nebula and never got “processed”. Inner solar disk hotter and outer is cooler. Makes a difference on planet formation. Inner terres ...
How Planets Form (990L)
... In addition, all the planets proceed along their orbits in the same direction. It's not that some go clockwise and others go counterclockwise. They're like horses on a carousel, all aimed the same way. These facts convince astronomers that the solar system began when a large, cold lump of interstell ...
... In addition, all the planets proceed along their orbits in the same direction. It's not that some go clockwise and others go counterclockwise. They're like horses on a carousel, all aimed the same way. These facts convince astronomers that the solar system began when a large, cold lump of interstell ...
2785
... Introduction: Collisions that deform and disrupt both target and projectile bodies change the configuration of the original system. It produces remnant bodies that may differ in composition, angular momentum and orbit. These can span a large size range, from the target body itself, to smaller satell ...
... Introduction: Collisions that deform and disrupt both target and projectile bodies change the configuration of the original system. It produces remnant bodies that may differ in composition, angular momentum and orbit. These can span a large size range, from the target body itself, to smaller satell ...
Parallels: Proto-Planetary Disks and rings
... • Regular planet orbits: same plane, direction, almost circular • Planets are closely spaced • Terrestrial and Jovian planets – Small, rocky planets near sun – Gas giant planets further out ...
... • Regular planet orbits: same plane, direction, almost circular • Planets are closely spaced • Terrestrial and Jovian planets – Small, rocky planets near sun – Gas giant planets further out ...
Remnants of Rock and Ice (Chapter 12) Asteroids (small rocky
... asteroids would only form an object 2000 km in diameter if combined together. The few largest asteroids may be spherical and differentiated into a mantle and a core, but most are rugged, undifferentiated lumps. Most asteroids orbit in the Asteroid Belt between Mars and Jupiter. Orbital resonances wi ...
... asteroids would only form an object 2000 km in diameter if combined together. The few largest asteroids may be spherical and differentiated into a mantle and a core, but most are rugged, undifferentiated lumps. Most asteroids orbit in the Asteroid Belt between Mars and Jupiter. Orbital resonances wi ...
Formation of the Solar System
... The Sun and the planets formed from a rotating disk of dust and gas. As the speed of rotation increased, the center of the disk flattened out and matter became more concentrated in the center of the disk, where the Sun eventually formed. The growth of the planets began as solid bits of matter began ...
... The Sun and the planets formed from a rotating disk of dust and gas. As the speed of rotation increased, the center of the disk flattened out and matter became more concentrated in the center of the disk, where the Sun eventually formed. The growth of the planets began as solid bits of matter began ...
The Solar System and its Origin
... • Vesc = sqrt(2 GM / R) – Massive/compact objects have high surface ...
... • Vesc = sqrt(2 GM / R) – Massive/compact objects have high surface ...
1-1 Origin of the Earth Motion NOTES blanks
... Refractory elements, such as iron, comprise the terrestrial planets, which are close to the Sun. Volatile elements, such as ices and gases like hydrogen, comprise the planets further from the Sun, where it is cool. ...
... Refractory elements, such as iron, comprise the terrestrial planets, which are close to the Sun. Volatile elements, such as ices and gases like hydrogen, comprise the planets further from the Sun, where it is cool. ...
Solar System/Planet Formation
... • Sun and planets rotate in same direction • disks seen around other stars • terrestrial planets and asteroids found near Sun • jovian planets, icy moons, comets found farther away ...
... • Sun and planets rotate in same direction • disks seen around other stars • terrestrial planets and asteroids found near Sun • jovian planets, icy moons, comets found farther away ...
Astronomy Library wk5.cwk (WP)
... It is thought that the Solar System formed from a cloud of dust and gas about 4.5 billion years ago. Cloud collapses under its own gravity. The central region collapses to form the sun. As the cloud collapses its spin rate increases: ...
... It is thought that the Solar System formed from a cloud of dust and gas about 4.5 billion years ago. Cloud collapses under its own gravity. The central region collapses to form the sun. As the cloud collapses its spin rate increases: ...
16gasgiants2s
... All of the outer planets (not just Saturn have ring systems) rings composed of small particles ...
... All of the outer planets (not just Saturn have ring systems) rings composed of small particles ...