White Dwarf star. Are
... of energy, it is finished. Our sun will run out of energy and it will be finished too. But this will not happen for another 5 billion years! ...
... of energy, it is finished. Our sun will run out of energy and it will be finished too. But this will not happen for another 5 billion years! ...
Comets and Asteroids
... reflect sufficient light to be detectable at large distances, and because their stable orbit do not bring them closer to the Sun. • Total number of comets in the sphere of influence of our Sun could be of the order of 1013! • Represents a mass the order of 1000 Earths. ...
... reflect sufficient light to be detectable at large distances, and because their stable orbit do not bring them closer to the Sun. • Total number of comets in the sphere of influence of our Sun could be of the order of 1013! • Represents a mass the order of 1000 Earths. ...
Integrative Studies 410 Our Place in the Universe
... • The energy of the electron depends on orbit • When an electron jumps from one orbital to another, it emits (emission line) or absorbs (absorption line) a photon of a certain energy • The frequency of emitted or absorbed photon is related to its energy ...
... • The energy of the electron depends on orbit • When an electron jumps from one orbital to another, it emits (emission line) or absorbs (absorption line) a photon of a certain energy • The frequency of emitted or absorbed photon is related to its energy ...
Extrasolar Planetary Systems » American Scientist
... One modern theory for how a planet, say a gas giant like Jupiter, forms from a protostellar disk of gas and dust hinges ongravitational instability. Simply put, as the density of the protostellar disk increases, it starts to clump here and there in response to self-gravitation. Simultaneously, the p ...
... One modern theory for how a planet, say a gas giant like Jupiter, forms from a protostellar disk of gas and dust hinges ongravitational instability. Simply put, as the density of the protostellar disk increases, it starts to clump here and there in response to self-gravitation. Simultaneously, the p ...
butoday20050915
... 2003UB313, the heavenly body is a member of the Kuiper Asteroid Belt. It’s the farthestknown object in the solar system, and bigger than Pluto, which was spotted by astronomers in 1930 and named the solar system’s ninth planet. ...
... 2003UB313, the heavenly body is a member of the Kuiper Asteroid Belt. It’s the farthestknown object in the solar system, and bigger than Pluto, which was spotted by astronomers in 1930 and named the solar system’s ninth planet. ...
Kepler`s Laws Powerpoint
... “Heavenly Spheres”, revolved around the Sun in circular orbits and the Earth spun on its axis. The stars were also much farther from the Sun than the planets. ...
... “Heavenly Spheres”, revolved around the Sun in circular orbits and the Earth spun on its axis. The stars were also much farther from the Sun than the planets. ...
the moons of jovian planets.
... d) comets that were trapped by Jupiter’s gravitational field. Explanation: Asteroids, meteoroids, and comets may have not changed at all since the solar system formed. ...
... d) comets that were trapped by Jupiter’s gravitational field. Explanation: Asteroids, meteoroids, and comets may have not changed at all since the solar system formed. ...
Reading exercise
... no air or water. Plants and animals can’t live there either. Astronauts first landed on the Moon in 1969. After that, there were six more trips to the Moon. They brought back Moon rocks, which scientists are still studying. There are holes, or craters, all over the Moon’s surface. Scientists believe ...
... no air or water. Plants and animals can’t live there either. Astronauts first landed on the Moon in 1969. After that, there were six more trips to the Moon. They brought back Moon rocks, which scientists are still studying. There are holes, or craters, all over the Moon’s surface. Scientists believe ...
Star Life Cycles
... After becoming a planetary nebula, the remains of the core of the star become a white dwarf. A white dwarf is a star that has exhausted most or all of its nuclear fuel and has collapsed to a very small size; such a star is near its final stage of life. White dwarfs eventually become black dwarfs ...
... After becoming a planetary nebula, the remains of the core of the star become a white dwarf. A white dwarf is a star that has exhausted most or all of its nuclear fuel and has collapsed to a very small size; such a star is near its final stage of life. White dwarfs eventually become black dwarfs ...
Star Formation: Interstellar Gas and Dust
... • Eddington limit. Radiation pressure on gas exceeds gravitational attraction of star. • Blows away gas trying to fall onto forming star. ...
... • Eddington limit. Radiation pressure on gas exceeds gravitational attraction of star. • Blows away gas trying to fall onto forming star. ...
Denver Public Schools
... show how different kinds of dinosaurs were adapted to fill the very same niches in nature that modern animals occupy today. How did it all come to an end for these magnificent creatures? Several theories including some that point to a cosmic culprit are presented. ...
... show how different kinds of dinosaurs were adapted to fill the very same niches in nature that modern animals occupy today. How did it all come to an end for these magnificent creatures? Several theories including some that point to a cosmic culprit are presented. ...
Volcanoes and Igneous Activity Earth
... MOTIONS OF THE EARTH-MOON SYSTEM • Phases of the Moon • When viewed from above the North Pole, the Moon orbits Earth in a counterclockwise (eastward) direction • The relative positions of the Sun, Earth, and Moon ...
... MOTIONS OF THE EARTH-MOON SYSTEM • Phases of the Moon • When viewed from above the North Pole, the Moon orbits Earth in a counterclockwise (eastward) direction • The relative positions of the Sun, Earth, and Moon ...
The Sun and Moon powerpoint.
... OUR STAR • 1.4 million km diameter • 750 times the mass of all of the solar system’s planets put together ...
... OUR STAR • 1.4 million km diameter • 750 times the mass of all of the solar system’s planets put together ...
bYTEBoss lesson 3 life of star
... The end of the life cycle of really massive stars is different to that of massive stars. After a really massive red giant collapses in a supernova explosion, it leaves a star so dense that not even light can escape its gravitational pull. This is called a black hole! Some scientists believe that the ...
... The end of the life cycle of really massive stars is different to that of massive stars. After a really massive red giant collapses in a supernova explosion, it leaves a star so dense that not even light can escape its gravitational pull. This is called a black hole! Some scientists believe that the ...
SKYTRACK Glossary of Terms
... same position along the ecliptic, such as a solstice or equinox. The mean interval between two vernal equinoxes is 365.242 days long. The tropical year differs from the solar year by one part in about 26,000, since this is the period of the Earth's precession about its rotational axis combined with ...
... same position along the ecliptic, such as a solstice or equinox. The mean interval between two vernal equinoxes is 365.242 days long. The tropical year differs from the solar year by one part in about 26,000, since this is the period of the Earth's precession about its rotational axis combined with ...
87 Sr
... • When the bodies reach sizes of approximately one kilometer, then they can attract each other directly ...
... • When the bodies reach sizes of approximately one kilometer, then they can attract each other directly ...
Kepler`s Laws of Planetary Motion
... By the end of this presentation, students will be able to • Describe how the orbits of planets are defined using Kepler’s laws. • Evaluate the period of an orbit or the relative distance of a planet using Kepler’s Law of ...
... By the end of this presentation, students will be able to • Describe how the orbits of planets are defined using Kepler’s laws. • Evaluate the period of an orbit or the relative distance of a planet using Kepler’s Law of ...
THE ROTATION OF THE SUN
... that case. The spots seem to move more or less from east to west if we use the terrestrial point of view. But if we look at the Sun as we do with geographical map (view from space), we have to change our reference frame: the spots seem to move from the Westside to the eastside, the same as our plane ...
... that case. The spots seem to move more or less from east to west if we use the terrestrial point of view. But if we look at the Sun as we do with geographical map (view from space), we have to change our reference frame: the spots seem to move from the Westside to the eastside, the same as our plane ...
Astronomy 4 Test #3 Practice 2. How were the rings of Uranus
... b. In order for Io to be as massive as it is, the collision that formed the Galilean moons must have ejected a lot of material from Jupiter, but since Jupiter is still so big, it must have a very high mass. c. Since Io’s orbit was `circularized’ by tidal forces from Jupiter, Jupiter must be extremel ...
... b. In order for Io to be as massive as it is, the collision that formed the Galilean moons must have ejected a lot of material from Jupiter, but since Jupiter is still so big, it must have a very high mass. c. Since Io’s orbit was `circularized’ by tidal forces from Jupiter, Jupiter must be extremel ...
Research Information for Space Bodies Project
... is much smaller than a planet (smaller even than Earth's moon), but it is not a moon. Pluto is the best known of the dwarf planets. 10 Need-to-Know Things About Dwarf Planets: 1. If the sun were as tall as a typical front door, Earth would be the size of a nickel and dwarf planets Pluto and Eris, fo ...
... is much smaller than a planet (smaller even than Earth's moon), but it is not a moon. Pluto is the best known of the dwarf planets. 10 Need-to-Know Things About Dwarf Planets: 1. If the sun were as tall as a typical front door, Earth would be the size of a nickel and dwarf planets Pluto and Eris, fo ...
The Sun - SCHOOLinSITES
... radiative zone - the zone of the sun’s interior that is between the core and the convective zone and in which energy moves by radiation – surrounds the core. – The temperature of the radiative zone ranges from about 2,000,000ºC to 7,000,000 ºC . – energy moves outward in the form of ...
... radiative zone - the zone of the sun’s interior that is between the core and the convective zone and in which energy moves by radiation – surrounds the core. – The temperature of the radiative zone ranges from about 2,000,000ºC to 7,000,000 ºC . – energy moves outward in the form of ...
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.