Chapter 17 Solar system.pmd
... (a) directly fall down from the point it is released. (b) hang in space. (c) go up and then come back to the surface of the moon. (d) keep going up never to come back. ...
... (a) directly fall down from the point it is released. (b) hang in space. (c) go up and then come back to the surface of the moon. (d) keep going up never to come back. ...
121mtr
... sized objects in the outer solar system, they are just covered over by lots of earth masses of ice because the ratio of icy material to rocky material is very high. Secondary reasons: formation potential earth size objects near Jupiter or Saturn would have been disrupted by those large bodies. ...
... sized objects in the outer solar system, they are just covered over by lots of earth masses of ice because the ratio of icy material to rocky material is very high. Secondary reasons: formation potential earth size objects near Jupiter or Saturn would have been disrupted by those large bodies. ...
Our Solar System
... Mercury has been known since ancient times. Johann Schroeter (1745 to 1816) was the first to observe the planet Mercury and record detailed drawings of Mercury's surface features. Mercury is the closest planet to our Sun and the fastest moving planet in our Solar System Mercury has a very elliptical ...
... Mercury has been known since ancient times. Johann Schroeter (1745 to 1816) was the first to observe the planet Mercury and record detailed drawings of Mercury's surface features. Mercury is the closest planet to our Sun and the fastest moving planet in our Solar System Mercury has a very elliptical ...
Astrophysics - Student Reference Packet
... known as 2003 UB313, this object was eventually named Eris in 2006. In August 2006, members of the IAU passed a resolution that defined a planet as a celestial body that is in orbit around the Sun; has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydros ...
... known as 2003 UB313, this object was eventually named Eris in 2006. In August 2006, members of the IAU passed a resolution that defined a planet as a celestial body that is in orbit around the Sun; has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydros ...
Planet Hunters
... exoplanet revolution has been the tremendous diversity of our neighboring systems. With only our own solar system as a model, scientists once assumed that most solar systems would consist of small rocky planets near the star and massive gas giants at greater distances, which took decades to round th ...
... exoplanet revolution has been the tremendous diversity of our neighboring systems. With only our own solar system as a model, scientists once assumed that most solar systems would consist of small rocky planets near the star and massive gas giants at greater distances, which took decades to round th ...
Size of Sun and Size of Planets
... 1. Which planet is the largest? _______________________________ 2. Which planet is the smallest? ______________________________ 3. Which two pairs of planets are about the same size? ____________ and ___________ AND ______________ and _______________ Your teacher will fold the earth model in half ...
... 1. Which planet is the largest? _______________________________ 2. Which planet is the smallest? ______________________________ 3. Which two pairs of planets are about the same size? ____________ and ___________ AND ______________ and _______________ Your teacher will fold the earth model in half ...
Some Physics of the Kepler Laws and Orbits Kepler`s First Law
... 3) If E = 2L2/m(GmM)2 < 0, then the eccentricity is zero and we have a circular orbit. 4) If E > 0, the eccentricity is nonzero and we have a hyperbolic orbit. The parabolic and hyperbolic orbits are known are usually referred to as unbounded or open orbits, while the elliptical and circular orbits ...
... 3) If E = 2L2/m(GmM)2 < 0, then the eccentricity is zero and we have a circular orbit. 4) If E > 0, the eccentricity is nonzero and we have a hyperbolic orbit. The parabolic and hyperbolic orbits are known are usually referred to as unbounded or open orbits, while the elliptical and circular orbits ...
lec01_26sep2011
... have surrounded the sun like an atmosphere. The consideration of the planetary motions thus leads us to think that, by virtue of an excessive heat, the solar atmosphere originally extended beyond the orbits of all the planets and that it progressively shrank to its present limits. This might have oc ...
... have surrounded the sun like an atmosphere. The consideration of the planetary motions thus leads us to think that, by virtue of an excessive heat, the solar atmosphere originally extended beyond the orbits of all the planets and that it progressively shrank to its present limits. This might have oc ...
Solar System
... It takes 365.25 days to orbit the Sun 1 time It’s mainly a planet covered with water Earth is the only planet sustaining life Earth’s atmosphere is 78% nitrogen, 21% oxygen, and 1% of other things. The Earth has a moon that orbits every 28 days The Earth is known as The Big Blue Marble ...
... It takes 365.25 days to orbit the Sun 1 time It’s mainly a planet covered with water Earth is the only planet sustaining life Earth’s atmosphere is 78% nitrogen, 21% oxygen, and 1% of other things. The Earth has a moon that orbits every 28 days The Earth is known as The Big Blue Marble ...
14-Habitable zone
... Since life as we know it requires liquid water to exist, we can define the habitable zone around the Sun for which an orbiting terrestrial (or rocky) planets has a surface temperature that allows liquid water to exist on its surface. This is an important qualifier, and is in contrast to studies of o ...
... Since life as we know it requires liquid water to exist, we can define the habitable zone around the Sun for which an orbiting terrestrial (or rocky) planets has a surface temperature that allows liquid water to exist on its surface. This is an important qualifier, and is in contrast to studies of o ...
Our Solar System LEVELED BOOK • S www.readinga-z.com
... Mars is the fourth planet from the Sun. It is known as the red planet because of large amounts of rust-colored dust on its surface. Mars is the most Earth-like of all the planets of our Solar System. Mars has seasons similar to our own, and the soil there is similar to the soil on Earth. But there i ...
... Mars is the fourth planet from the Sun. It is known as the red planet because of large amounts of rust-colored dust on its surface. Mars is the most Earth-like of all the planets of our Solar System. Mars has seasons similar to our own, and the soil there is similar to the soil on Earth. But there i ...
Our Solar System - Mrs. Carter
... Mars is the fourth planet from the Sun. It is known as the red planet because of large amounts of rust-colored dust on its surface. Mars is the most Earth-like of all the planets of our Solar System. Mars has seasons similar to our own, and the soil there is similar to the soil on Earth. But there i ...
... Mars is the fourth planet from the Sun. It is known as the red planet because of large amounts of rust-colored dust on its surface. Mars is the most Earth-like of all the planets of our Solar System. Mars has seasons similar to our own, and the soil there is similar to the soil on Earth. But there i ...
Earth and the Universe Name
... 6. What is the difference between blue and red star? ____________________________________________________. 7. How does our star compare to the blue and red stars based on age?______________________________________. 8. The shape of Earth is _______________________________________________________. 9. ...
... 6. What is the difference between blue and red star? ____________________________________________________. 7. How does our star compare to the blue and red stars based on age?______________________________________. 8. The shape of Earth is _______________________________________________________. 9. ...
Astronomy 1 Study Guide Key 16
... Moon – planet – main sequence star – red giant – supergiant – solar system – galaxy – universe 2. How do we measure distance in space? light year, parsec, or astronomical units 3. If a supernova is 400 light years away, it would take 400 years for us to see it. 4. If a distance is not as large as a ...
... Moon – planet – main sequence star – red giant – supergiant – solar system – galaxy – universe 2. How do we measure distance in space? light year, parsec, or astronomical units 3. If a supernova is 400 light years away, it would take 400 years for us to see it. 4. If a distance is not as large as a ...
The Milky Way
... b. Jupiter swept up so much material that not enough was left to form a planet. c. Mars was once larger and collided with a large planetesimal from the inner Solar System that sent debris outward. *d. Jupiter formed early, and its gravitational influence altered the orbits of nearby accreting planet ...
... b. Jupiter swept up so much material that not enough was left to form a planet. c. Mars was once larger and collided with a large planetesimal from the inner Solar System that sent debris outward. *d. Jupiter formed early, and its gravitational influence altered the orbits of nearby accreting planet ...
What Is a Planet? Pluto and Its Place in the Solar System
... – Orbit only 8x bigger – Closest thing we know of to a ...
... – Orbit only 8x bigger – Closest thing we know of to a ...
Introduction Notes - Sunflower Astronomy
... - uses the scientific method. - involves huge numbers for distances, mass, and time. - involves small numbers for describing phenomena at the atomic level. Overview of the Universe Solar System: Eight (or Nine) planets, Sun, minor planets, moons, comets, meteoroids, and dust. Terrestrial Planets: Me ...
... - uses the scientific method. - involves huge numbers for distances, mass, and time. - involves small numbers for describing phenomena at the atomic level. Overview of the Universe Solar System: Eight (or Nine) planets, Sun, minor planets, moons, comets, meteoroids, and dust. Terrestrial Planets: Me ...
Formation and evolution of the Solar System
The formation of the Solar System began 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the Sun, while the rest flattened into a protoplanetary disk out of which the planets, moons, asteroids, and other small Solar System bodies formed.This widely accepted model, known as the nebular hypothesis, was first developed in the 18th century by Emanuel Swedenborg, Immanuel Kant, and Pierre-Simon Laplace. Its subsequent development has interwoven a variety of scientific disciplines including astronomy, physics, geology, and planetary science. Since the dawn of the space age in the 1950s and the discovery of extrasolar planets in the 1990s, the model has been both challenged and refined to account for new observations.The Solar System has evolved considerably since its initial formation. Many moons have formed from circling discs of gas and dust around their parent planets, while other moons are thought to have formed independently and later been captured by their planets. Still others, such as the Moon, may be the result of giant collisions. Collisions between bodies have occurred continually up to the present day and have been central to the evolution of the Solar System. The positions of the planets often shifted due to gravitational interactions. This planetary migration is now thought to have been responsible for much of the Solar System's early evolution.In roughly 5 billion years, the Sun will cool and expand outward many times its current diameter (becoming a red giant), before casting off its outer layers as a planetary nebula and leaving behind a stellar remnant known as a white dwarf. In the far distant future, the gravity of passing stars will gradually reduce the Sun's retinue of planets. Some planets will be destroyed, others ejected into interstellar space. Ultimately, over the course of tens of billions of years, it is likely that the Sun will be left with none of the original bodies in orbit around it.