Chapter 17 Tour: Formation of the Solar System
... 4. Why does the composition of giant gas planets differ from that of the rocky inner planets? THE OUTER GAS GIANTS ARE MADE OF GAS BECAUSE THEY WERE LOCATED FAR AWAY FROM THE SUN AND COULD COLLECT LOTS OF GAS & DUST. THE INNER PLANETS THAT ARE CLOSER TO THE SUN ARE MADE OF JUST ROCK BECAUSE THE GAS ...
... 4. Why does the composition of giant gas planets differ from that of the rocky inner planets? THE OUTER GAS GIANTS ARE MADE OF GAS BECAUSE THEY WERE LOCATED FAR AWAY FROM THE SUN AND COULD COLLECT LOTS OF GAS & DUST. THE INNER PLANETS THAT ARE CLOSER TO THE SUN ARE MADE OF JUST ROCK BECAUSE THE GAS ...
STICKING THE EARLY PLANETS TOGETHER
... • What was it like during the early stages of formation? (dusty!) • How did our planets form? (by small particles clumping together – accreting). 1. Group students into pairs and allow them to choose colors of Play-Doh®. Encourage students to use at least four different colors to best represent feat ...
... • What was it like during the early stages of formation? (dusty!) • How did our planets form? (by small particles clumping together – accreting). 1. Group students into pairs and allow them to choose colors of Play-Doh®. Encourage students to use at least four different colors to best represent feat ...
Formation of solar system11 Feb Homework 4 • Preparation for Midterm exam (4 March)
... build giant planets. – Gravitational field of giant planets perturbed orbits of remaining planetesimals. ...
... build giant planets. – Gravitational field of giant planets perturbed orbits of remaining planetesimals. ...
The most striking regularity observed in
... disk of gas and dust that surrounded the young Sun (Fig. 1). But do flattened disks of dust and gas inevitably lead to a few massive and widely spaced planets on circular uninclined orbits? Results from numerical simulations discussed at a meeting* in October suggest that, in as far as the inner Sol ...
... disk of gas and dust that surrounded the young Sun (Fig. 1). But do flattened disks of dust and gas inevitably lead to a few massive and widely spaced planets on circular uninclined orbits? Results from numerical simulations discussed at a meeting* in October suggest that, in as far as the inner Sol ...
formation of solar system nebular tx 1112 notes
... points. The change first, under high temperatures because they are the closest to the sun. Eventually, the liquids will change into solids. Light materials (hydrogen and helium) have very low boiling points. They will not change because it does not get cold enough. They are the farthest from the s ...
... points. The change first, under high temperatures because they are the closest to the sun. Eventually, the liquids will change into solids. Light materials (hydrogen and helium) have very low boiling points. They will not change because it does not get cold enough. They are the farthest from the s ...
Astronomy 2291 – Exam 3 Study Guide
... This exam will cover material in Chapters 6 and 8 through 11. The following are the topics we will cover on Exam 3. Note that not all topics on this sheet will necessarily be on the exam. Also, because we are talking about planets, you do need to know some basics of planetary orbits that we’ve been ...
... This exam will cover material in Chapters 6 and 8 through 11. The following are the topics we will cover on Exam 3. Note that not all topics on this sheet will necessarily be on the exam. Also, because we are talking about planets, you do need to know some basics of planetary orbits that we’ve been ...
A glimpse at the formation of our Solar System
... HL Tauri is 450 light-years from Earth and the star is less than a million years old, which makes it pretty young by astronomical standards. The dark rings on the ALMA image may indicate the positions of planets under formation. ALMA is an array of telescopes located in the Atacama desert of Chile a ...
... HL Tauri is 450 light-years from Earth and the star is less than a million years old, which makes it pretty young by astronomical standards. The dark rings on the ALMA image may indicate the positions of planets under formation. ALMA is an array of telescopes located in the Atacama desert of Chile a ...
Formation of planets and debris disks in the terrestrial zone
... • Statistical mechanics approach * collision rate: Nij σ v Fg * Nij bodies of mass Mj * near-circular orbits: eij, iij * multiple annuli (32-64): ai, ∆ai ...
... • Statistical mechanics approach * collision rate: Nij σ v Fg * Nij bodies of mass Mj * near-circular orbits: eij, iij * multiple annuli (32-64): ai, ∆ai ...
Document
... match well with real values • Almost always a close encounter between gas giants • Final orbital configuration sensitive to Saturn-Uranus separation ...
... match well with real values • Almost always a close encounter between gas giants • Final orbital configuration sensitive to Saturn-Uranus separation ...
Nebula Theory - GSHS Mrs. Francomb
... COLD WORLD. As a possible story goes, a nebula collapses under gravity. Particles come together to form larger particles. Planetesimals form which are pre-planets. The spinning attracts more particles until the size grows. The energy released during this collapse is converted into motion. The motion ...
... COLD WORLD. As a possible story goes, a nebula collapses under gravity. Particles come together to form larger particles. Planetesimals form which are pre-planets. The spinning attracts more particles until the size grows. The energy released during this collapse is converted into motion. The motion ...
ASTR 150
... Either icy planetesimals or rocky planetesimals with some water from near the frost line (beyond Mars’ orbit) ...
... Either icy planetesimals or rocky planetesimals with some water from near the frost line (beyond Mars’ orbit) ...
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... Masses and Compositions of the Major Planets • At the location of the terrestrial planets, there was not much mass in the planetesimals, since they were formed of heavier, non-abundant elements • In the outer solar system, there was more mass in the planetesimals, since they were formed of abunda ...
... Masses and Compositions of the Major Planets • At the location of the terrestrial planets, there was not much mass in the planetesimals, since they were formed of heavier, non-abundant elements • In the outer solar system, there was more mass in the planetesimals, since they were formed of abunda ...
Stellar Evolution Stations
... As the disk got thinner and thinner, particles began to stick together and form clumps. Some clumps got bigger, as particles and small clumps stuck to them, eventually forming planets or moons. ...
... As the disk got thinner and thinner, particles began to stick together and form clumps. Some clumps got bigger, as particles and small clumps stuck to them, eventually forming planets or moons. ...
FORMATION OF THE SOLAR SYSTEM
... • Dust grains stick, settle towards disk plane. • Both Size (adhesion) and Gravity enforce pre-planetary Republicanism: the rich (big) get richer (bigger) • PLANETESIMALS grow via ACCRETION of gas and dust; have eccentric and somewhat inclined orbits • Then they COLLIDE: typically bigger ones grow, ...
... • Dust grains stick, settle towards disk plane. • Both Size (adhesion) and Gravity enforce pre-planetary Republicanism: the rich (big) get richer (bigger) • PLANETESIMALS grow via ACCRETION of gas and dust; have eccentric and somewhat inclined orbits • Then they COLLIDE: typically bigger ones grow, ...
Planetary Two-Step Reshaped Solar System, Saved Earth?
... “It’s an exciting model,” says planthe unintuitive ways that gravity shaped rocky planetesimals outward. Moving outward (3), they threw both etary dynamicist William Bottke of the earliest solar system. Both Jupiter sorts of planetesimals inward to form the asteroid belt. SwRI, Boulder, who is not a ...
... “It’s an exciting model,” says planthe unintuitive ways that gravity shaped rocky planetesimals outward. Moving outward (3), they threw both etary dynamicist William Bottke of the earliest solar system. Both Jupiter sorts of planetesimals inward to form the asteroid belt. SwRI, Boulder, who is not a ...
Lecture12
... existence of huge numbers of asteroids and comets and why these small objects reside primarily in the regions we call the asteroid belt, the Kuiper belt, and the Oort cloud. 4. Exceptions to the patterns. Finally, the theory must explain all the general patterns while at the same time making allowan ...
... existence of huge numbers of asteroids and comets and why these small objects reside primarily in the regions we call the asteroid belt, the Kuiper belt, and the Oort cloud. 4. Exceptions to the patterns. Finally, the theory must explain all the general patterns while at the same time making allowan ...
Lecture13
... existence of huge numbers of asteroids and comets and why these small objects reside primarily in the regions we call the asteroid belt, the Kuiper belt, and the Oort cloud. ...
... existence of huge numbers of asteroids and comets and why these small objects reside primarily in the regions we call the asteroid belt, the Kuiper belt, and the Oort cloud. ...
Part 2: Solar System Formation
... another. If the collisions are not too violent material (planetesimals) may stick together. • In the outer parts of the Solar Nebula the planets become large enough to have a significant gravitational pull and collect gas around them. – Ice is ten times more abundant than silicates and iron compound ...
... another. If the collisions are not too violent material (planetesimals) may stick together. • In the outer parts of the Solar Nebula the planets become large enough to have a significant gravitational pull and collect gas around them. – Ice is ten times more abundant than silicates and iron compound ...
Nebular Theory
... Contraction: The cloud starts collapsing under its own gravity; over 100,000 years, it shrinks down to 100 AU, heats up (thermal energy), and compresses in the center. Accretion disk: The matter around the center spins up and flattens into a disk, while heat vaporizes the dust. Protostar: Forms in t ...
... Contraction: The cloud starts collapsing under its own gravity; over 100,000 years, it shrinks down to 100 AU, heats up (thermal energy), and compresses in the center. Accretion disk: The matter around the center spins up and flattens into a disk, while heat vaporizes the dust. Protostar: Forms in t ...
![class16.ppt [Read-Only] - University of Texas Astronomy Home Page](http://s1.studyres.com/store/data/016866176_1-afb2b342fc43676be8b063b94ba751c2-300x300.png)
class16.ppt [Read-Only] - University of Texas Astronomy Home Page
... (star plus accompanying system) must be common ...
... (star plus accompanying system) must be common ...
Chart_set_4
... 3) Gravity-enhanced accretion: objects now have significant gravity. Mutual attraction accelerates accretion. Bigger objects grow faster => a few planet-sized objects. ...
... 3) Gravity-enhanced accretion: objects now have significant gravity. Mutual attraction accelerates accretion. Bigger objects grow faster => a few planet-sized objects. ...
Solar system intro and formation
... Eventually, small-moon sized objects: "planetesimals". 3) Gravity-enhanced accretion: objects now have significant gravity. Mutual attraction accelerates accretion. Bigger objects grow faster => a few planet-sized objects. ...
... Eventually, small-moon sized objects: "planetesimals". 3) Gravity-enhanced accretion: objects now have significant gravity. Mutual attraction accelerates accretion. Bigger objects grow faster => a few planet-sized objects. ...