Physics 2028: Great Ideas in Science II: The Changing Earth Module
... sometimes destroying each other, sometimes sticking together to form even bigger planetesimals =⇒ this is a process known as accretion. ...
... sometimes destroying each other, sometimes sticking together to form even bigger planetesimals =⇒ this is a process known as accretion. ...
lecture9 Solar System1
... grew larger gravity captured hydrogen & helium composition similar to Sun gaseous accretion disk forms around planet Moons form in disk around planet ...
... grew larger gravity captured hydrogen & helium composition similar to Sun gaseous accretion disk forms around planet Moons form in disk around planet ...
Planet formation - problems and future
... For about 300 years, from the middle of the seventeenth century to the middle of the twentieth, there were two fundamentally different, competing scenarios. The nebular hypothesis argued for the formation of planets from residual (or, in earlier versions, spin-ejected) circumstellar material and sug ...
... For about 300 years, from the middle of the seventeenth century to the middle of the twentieth, there were two fundamentally different, competing scenarios. The nebular hypothesis argued for the formation of planets from residual (or, in earlier versions, spin-ejected) circumstellar material and sug ...
The Planets of the Solar System
... • In addition to the 8 major planets, there are at least 100 moons in our solar system. • While some of these moons are spherical, most look roughly like potatoes. • There is still minor debris left over from the formation of the solar system: – asteroids and comets. ...
... • In addition to the 8 major planets, there are at least 100 moons in our solar system. • While some of these moons are spherical, most look roughly like potatoes. • There is still minor debris left over from the formation of the solar system: – asteroids and comets. ...
Document
... • Rock & Metals form where T < 1300 K • Carbon grains & ices where T(gas) < 300 K • Inner planets and asteroids: Rocky and metallic • Snow line • Outer Jovian systems: Gaseous giants, carbon ices • Dust grains and ices collide, accrete, and eventually grow bigger gravitationally into planetesimals b ...
... • Rock & Metals form where T < 1300 K • Carbon grains & ices where T(gas) < 300 K • Inner planets and asteroids: Rocky and metallic • Snow line • Outer Jovian systems: Gaseous giants, carbon ices • Dust grains and ices collide, accrete, and eventually grow bigger gravitationally into planetesimals b ...
PLANETARY MOTION
... If used in the classroom this advanced use case requires mathematical skills. The geometry of ellipses has to be well understood and it is required to understand the fitting procedure of data points to a linear relation. The use case is therefore suggested for students at college level. ...
... If used in the classroom this advanced use case requires mathematical skills. The geometry of ellipses has to be well understood and it is required to understand the fitting procedure of data points to a linear relation. The use case is therefore suggested for students at college level. ...
PLANETARY MOTION G. Iafrate(a) and M. Ramella(a) (a) INAF
... If used in the classroom this advanced use case requires mathematical skills. The geometry of ellipses has to be well understood and it is required to understand the fitting procedure of data points to a linear relation. The use case is therefore suggested for students at college level. ...
... If used in the classroom this advanced use case requires mathematical skills. The geometry of ellipses has to be well understood and it is required to understand the fitting procedure of data points to a linear relation. The use case is therefore suggested for students at college level. ...
General Proper es of the Terrestrial Planets
... • The apparent moCon of the planets in the sky is called “retrograde” moCon. As it is seen from Earth, all the planets appear to change their posiCon in the sky periodically. • It is because bo ...
... • The apparent moCon of the planets in the sky is called “retrograde” moCon. As it is seen from Earth, all the planets appear to change their posiCon in the sky periodically. • It is because bo ...
Intro To The Solar System
... Earth has diameter 0.3 mm. Sun: ~ size of a small plum. Mercury, Venus, Earth, Mars: ~ size of a grain of salt. Jupiter: ~ size of an apple seed. Saturn: ~ slightly smaller than Jupiter’s “apple seed”. ...
... Earth has diameter 0.3 mm. Sun: ~ size of a small plum. Mercury, Venus, Earth, Mars: ~ size of a grain of salt. Jupiter: ~ size of an apple seed. Saturn: ~ slightly smaller than Jupiter’s “apple seed”. ...
The Origin of Our Solar System
... – Planetesimals were made of a mixture of ices and rocky materials, which could become bigger • Protoplanets could have captured an envelope of gas – Gas atoms, hydrogen and helium, were moving slowly in the outer region and so easily captured by the gravity of the massive cores. – this is called co ...
... – Planetesimals were made of a mixture of ices and rocky materials, which could become bigger • Protoplanets could have captured an envelope of gas – Gas atoms, hydrogen and helium, were moving slowly in the outer region and so easily captured by the gravity of the massive cores. – this is called co ...
"It`s increasingly seeming that the solar system is
... orbits around sun-like stars. And finding bigger planets like the ones in the outer solar system will require more time. One of the main techniques to detect planets-which Kepler and TESS use, for example - is to look for the slight dimming of starlight when a planet passes in front of it. But becau ...
... orbits around sun-like stars. And finding bigger planets like the ones in the outer solar system will require more time. One of the main techniques to detect planets-which Kepler and TESS use, for example - is to look for the slight dimming of starlight when a planet passes in front of it. But becau ...
Homework 4 1 Chapter 3 October 4, 2011
... warmer only the rock and metal could condense and eventually form planets made of those materials. But, farther away the hydrogen and helium condensed as well, so planets in that region are composed of these elements as well (in fact their composition is dominated by these elements since they were m ...
... warmer only the rock and metal could condense and eventually form planets made of those materials. But, farther away the hydrogen and helium condensed as well, so planets in that region are composed of these elements as well (in fact their composition is dominated by these elements since they were m ...
Origin of the Solar System – Notes Rings encircle Jupiter, Saturn
... Temperature plays a major role in determining whether the materials of which planets are made exist as solids, liquids, or gases. Hydrogen and helium are gaseous except at extremely low temperatures. By contrast, rockforming substances such as iron and silicon are solids except at temperatures well ...
... Temperature plays a major role in determining whether the materials of which planets are made exist as solids, liquids, or gases. Hydrogen and helium are gaseous except at extremely low temperatures. By contrast, rockforming substances such as iron and silicon are solids except at temperatures well ...
AST 301—Review for Exam 3 Consult “Guide to Reading and Study
... that there are several techniques that could be used to detect extrasolar planets, but that basically only one has been so far successful (with a few recent detections using another technique). Can you explain why that is? (We also went over this in class.) Of the numerous extrasolar planets that ha ...
... that there are several techniques that could be used to detect extrasolar planets, but that basically only one has been so far successful (with a few recent detections using another technique). Can you explain why that is? (We also went over this in class.) Of the numerous extrasolar planets that ha ...
Exoplanets
... All (or almost all?) are gas or ice giants • Masses from 7ME up to > 13MJ (MJ = 320 ME) Orbits are mostly unlike the Solar System • “Hot Neptunes” & “Hot Jupiters” (a < 0.4 AU) are ...
... All (or almost all?) are gas or ice giants • Masses from 7ME up to > 13MJ (MJ = 320 ME) Orbits are mostly unlike the Solar System • “Hot Neptunes” & “Hot Jupiters” (a < 0.4 AU) are ...
Observational Constraints The Nebular Hypothesis
... 1. Small dust grains grow into larger—but still relatively small—asteroid-like bodies called planetesimals. 2. Planetesimals repeated crash into each other, resulting in increasingly large planetesimals. Some of these objects grow large enough to be called protoplanets. 3. As the protoplanets grow t ...
... 1. Small dust grains grow into larger—but still relatively small—asteroid-like bodies called planetesimals. 2. Planetesimals repeated crash into each other, resulting in increasingly large planetesimals. Some of these objects grow large enough to be called protoplanets. 3. As the protoplanets grow t ...
What is Pluto?
... What is Pluto? • Strange object; located far out from the Sun with gas giants but small size and very elliptical and highly inclined orbit • Pluto is a mixture of ices and rocks • composition similar to satellites of giant planets • Could be captured Kuiper Belt Object (e.g. comet)? ...
... What is Pluto? • Strange object; located far out from the Sun with gas giants but small size and very elliptical and highly inclined orbit • Pluto is a mixture of ices and rocks • composition similar to satellites of giant planets • Could be captured Kuiper Belt Object (e.g. comet)? ...
Intelligent life in the Universe
... Physics • The molecules of life are large. • Thermodynamics almost explicitly forbids making living molecules in equilibrium. • Sustained energy flow into the environment is NECESSARY, we do not know what is the SUFFICIENT condition ...
... Physics • The molecules of life are large. • Thermodynamics almost explicitly forbids making living molecules in equilibrium. • Sustained energy flow into the environment is NECESSARY, we do not know what is the SUFFICIENT condition ...
Our Solar System
... same size as Earth, and it is rocky. The similarities end there. Venus can become very hot, reaching about 460°C (860°F). It is even hotter than Mercury because Venus’s thick ...
... same size as Earth, and it is rocky. The similarities end there. Venus can become very hot, reaching about 460°C (860°F). It is even hotter than Mercury because Venus’s thick ...
File
... and Mars. These planets are all made of rock and have a solid surface. Mercury is the planet closest to the sun, and it is the smallest of the eight planets. Because it is so close to the sun, from Earth it can only be seen at sunrise in the east and sunset in the west. This makes the planet seem li ...
... and Mars. These planets are all made of rock and have a solid surface. Mercury is the planet closest to the sun, and it is the smallest of the eight planets. Because it is so close to the sun, from Earth it can only be seen at sunrise in the east and sunset in the west. This makes the planet seem li ...
Pythagoras Eudoxus of Cnidus Aristotle Eratosthenes Hipparchus
... telescope. Galileo designed and built his own, much larger, telescope and turned it toward the sky. He observed the Moon and several “planets” circling Jupiter (he later identified these as moons). Galileo noticed that Venus had phases just like the moon. This observation gave him the first proof th ...
... telescope. Galileo designed and built his own, much larger, telescope and turned it toward the sky. He observed the Moon and several “planets” circling Jupiter (he later identified these as moons). Galileo noticed that Venus had phases just like the moon. This observation gave him the first proof th ...
The Solar System
... planets orbiting the Sun: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune. Our Solar System began to form about five billion years ago from a cloud of dust and gas. This dust and gas began to spin and flatten out into a disc shape. In the centre of the disc the Sun was formed and the p ...
... planets orbiting the Sun: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune. Our Solar System began to form about five billion years ago from a cloud of dust and gas. This dust and gas began to spin and flatten out into a disc shape. In the centre of the disc the Sun was formed and the p ...
Class 11 and 12 lecture slides (giant planets)
... • Uranus and Neptune didn’t acquire so much gas because they were further out and accreted more slowly • Planets will have initially been hot (gravitational energy) and subsequently cooled and contracted • We can investigate how rapidly they are cooling at the present day . . . ...
... • Uranus and Neptune didn’t acquire so much gas because they were further out and accreted more slowly • Planets will have initially been hot (gravitational energy) and subsequently cooled and contracted • We can investigate how rapidly they are cooling at the present day . . . ...
Planetary Diversity - MIT Computer Science and Artificial
... gin. Stability prompts the question, Is the body able to sur- even though it includes most of the periodic table. Revive a long time-say, billions of years? Cosmochemistry markably, nuclear physics orders the elements according prompts the question, Is the body's composition plausible, to abundance ...
... gin. Stability prompts the question, Is the body able to sur- even though it includes most of the periodic table. Revive a long time-say, billions of years? Cosmochemistry markably, nuclear physics orders the elements according prompts the question, Is the body's composition plausible, to abundance ...
Planet
A planet (from Ancient Greek ἀστήρ πλανήτης (astēr planētēs), or πλάνης ἀστήρ (plánēs astēr), meaning ""wandering star"") is an astronomical object orbiting a star, brown dwarf, or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science, mythology, and religion. Several planets in the Solar System can be seen with the naked eye. These were regarded by many early cultures as divine, or as emissaries of deities. As scientific knowledge advanced, human perception of the planets changed, incorporating a number of disparate objects. In 2006, the International Astronomical Union (IAU) officially adopted a resolution defining planets within the Solar System. This definition is controversial because it excludes many objects of planetary mass based on where or what they orbit. Although eight of the planetary bodies discovered before 1950 remain ""planets"" under the modern definition, some celestial bodies, such as Ceres, Pallas, Juno, Vesta (each an object in the solar asteroid belt), and Pluto (the first trans-Neptunian object discovered), that were once considered planets by the scientific community are no longer viewed as such.The planets were thought by Ptolemy to orbit Earth in deferent and epicycle motions. Although the idea that the planets orbited the Sun had been suggested many times, it was not until the 17th century that this view was supported by evidence from the first telescopic astronomical observations, performed by Galileo Galilei. By careful analysis of the observation data, Johannes Kepler found the planets' orbits were not circular but elliptical. As observational tools improved, astronomers saw that, like Earth, the planets rotated around tilted axes, and some shared such features as ice caps and seasons. Since the dawn of the Space Age, close observation by space probes has found that Earth and the other planets share characteristics such as volcanism, hurricanes, tectonics, and even hydrology.Planets are generally divided into two main types: large low-density giant planets, and smaller rocky terrestrials. Under IAU definitions, there are eight planets in the Solar System. In order of increasing distance from the Sun, they are the four terrestrials, Mercury, Venus, Earth, and Mars, then the four giant planets, Jupiter, Saturn, Uranus, and Neptune. Six of the planets are orbited by one or more natural satellites.More than a thousand planets around other stars (""extrasolar planets"" or ""exoplanets"") have been discovered in the Milky Way: as of 1 October 2015, 1968 known extrasolar planets in 1248 planetary systems (including 490 multiple planetary systems), ranging in size from just above the size of the Moon to gas giants about twice as large as Jupiter. On December 20, 2011, the Kepler Space Telescope team reported the discovery of the first Earth-sized extrasolar planets, Kepler-20e and Kepler-20f, orbiting a Sun-like star, Kepler-20. A 2012 study, analyzing gravitational microlensing data, estimates an average of at least 1.6 bound planets for every star in the Milky Way.Around one in five Sun-like stars is thought to have an Earth-sized planet in its habitable zone.