Exercises
... 10.3 Red giant branch stars (a) Calculate the total energy of the Sun assuming that the density is constant, i.e. using the equation for potential energy Egr = -3/5 GM2 /R. In later phases, stars like the Sun become red giants, with R ≈ 100R . What would be the total energy, if the giant had consta ...
... 10.3 Red giant branch stars (a) Calculate the total energy of the Sun assuming that the density is constant, i.e. using the equation for potential energy Egr = -3/5 GM2 /R. In later phases, stars like the Sun become red giants, with R ≈ 100R . What would be the total energy, if the giant had consta ...
Powerpoint slides - Earth & Planetary Sciences
... Solar System Formation - Overview • Some event (e.g. supernova) triggers gravitational collapse of a cloud (nebula) of dust and gas • As the nebula collapses, it forms a spinning disk (due to conservation of angular momentum) • The collapse releases gravitational energy, which heats the centre • Th ...
... Solar System Formation - Overview • Some event (e.g. supernova) triggers gravitational collapse of a cloud (nebula) of dust and gas • As the nebula collapses, it forms a spinning disk (due to conservation of angular momentum) • The collapse releases gravitational energy, which heats the centre • Th ...
Dec 2016 - Astronomical Society of Northern New England
... After a star the size of our sun runs out of fuel and collapses down to the size of the earth, it becomes 125,000 times denser than steel, so that each cupful of this exotic material would weigh more than a cement truck. However, it is not nearly as dense as a neutron star, where each baseball sized ...
... After a star the size of our sun runs out of fuel and collapses down to the size of the earth, it becomes 125,000 times denser than steel, so that each cupful of this exotic material would weigh more than a cement truck. However, it is not nearly as dense as a neutron star, where each baseball sized ...
Ch_28_-_31_Earths_Role_as_a_Body_in_Space
... The Law of Orbits: All planets move in elliptical orbits, with the sun at one focus. a. An ellipse is … an oval shape centered on two points instead of a single point. b. The orbital period of a planet is … the length of time it takes for it to travel a complete orbit around the sun. c. We call this ...
... The Law of Orbits: All planets move in elliptical orbits, with the sun at one focus. a. An ellipse is … an oval shape centered on two points instead of a single point. b. The orbital period of a planet is … the length of time it takes for it to travel a complete orbit around the sun. c. We call this ...
Coordinates and Time - University of Florida Astronomy
... Now why on the last slide did I write (J2000.0) after the RA and Dec? What that notation means is that these are the coordinates at which you would find the galactic center on the first day of 2000. This is unfortunately necessary because the equatorial coordinates of objects change with time. ...
... Now why on the last slide did I write (J2000.0) after the RA and Dec? What that notation means is that these are the coordinates at which you would find the galactic center on the first day of 2000. This is unfortunately necessary because the equatorial coordinates of objects change with time. ...
Feb 2015 - Bays Mountain Park
... primary duty involved communications with ground control. At some point during the long, grueling day, a short circuit sparked one of the wires in the capsule. This spark eventually led to a raging fire in the 100% high pressure oxygen conditions in the spacecraft. In less than a minute, the men wer ...
... primary duty involved communications with ground control. At some point during the long, grueling day, a short circuit sparked one of the wires in the capsule. This spark eventually led to a raging fire in the 100% high pressure oxygen conditions in the spacecraft. In less than a minute, the men wer ...
Chapter 2 Solar Energy to Earth and the Seasons
... of radiant energy. • Illustrate the interception of solar energy and its uneven distribution at the top of the atmosphere. • Define solar altitude and daylength. • Describe the annual variability of solar altitude, solar declination, and daylength—Earth’s seasonality. © 2015 Pearson Education, In ...
... of radiant energy. • Illustrate the interception of solar energy and its uneven distribution at the top of the atmosphere. • Define solar altitude and daylength. • Describe the annual variability of solar altitude, solar declination, and daylength—Earth’s seasonality. © 2015 Pearson Education, In ...
Astrophysics
... generate huge amounts of heat - but still not enough to last millions of years. (This process is very important in the formation of new stars however.) • The source of the Sun's energy was a mystery until nuclear forces and the relationship between mass and energy were understood. The light we see f ...
... generate huge amounts of heat - but still not enough to last millions of years. (This process is very important in the formation of new stars however.) • The source of the Sun's energy was a mystery until nuclear forces and the relationship between mass and energy were understood. The light we see f ...
Chapter 2: Mercury
... grains became pebbles and boulder-sized crags, which collided and coalesced – a process called accretion - forming larger objects known as planetesimals. These planetesimals eventually accreted to form the planets of the Solar System. The outer gas giant planets, orbiting within the cooler regions o ...
... grains became pebbles and boulder-sized crags, which collided and coalesced – a process called accretion - forming larger objects known as planetesimals. These planetesimals eventually accreted to form the planets of the Solar System. The outer gas giant planets, orbiting within the cooler regions o ...
Huygens` Outline - Académie des Sciences {1666} Leiden
... 1. Find the meridian line and the altitude of the pole of Paris, which are the foundations of all other astronomical observations. 2. Re-establish the [position of the] fixed stars, in which rests all the foundation of astronomy. 3. Measure the diameters of the sun and of the moon in their various d ...
... 1. Find the meridian line and the altitude of the pole of Paris, which are the foundations of all other astronomical observations. 2. Re-establish the [position of the] fixed stars, in which rests all the foundation of astronomy. 3. Measure the diameters of the sun and of the moon in their various d ...
Disk Instability Models
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
Habitability: Good, Bad and the Ugly
... Luminosity of the Sun • Definition of luminosity (watts/m2) • Sun’s luminosity has been changing: earlier in its evolution, luminosity was only 70% of what it is today (how could temperature be maintained over geological time) • Future for luminosity – Remember star sequence from lab and lecture – ...
... Luminosity of the Sun • Definition of luminosity (watts/m2) • Sun’s luminosity has been changing: earlier in its evolution, luminosity was only 70% of what it is today (how could temperature be maintained over geological time) • Future for luminosity – Remember star sequence from lab and lecture – ...
White Dwarfs
... 2. Why can't the lowest-mass stars become giants? a. They never get hot enough for the triple-alpha process. b. Their gravity is too weak to stop them from expanding beyond the giant phase. c. They live so long that none has ever left the main sequence. d. The rate of hydrogen-shell fusion is too sl ...
... 2. Why can't the lowest-mass stars become giants? a. They never get hot enough for the triple-alpha process. b. Their gravity is too weak to stop them from expanding beyond the giant phase. c. They live so long that none has ever left the main sequence. d. The rate of hydrogen-shell fusion is too sl ...
Our Solar System
... particles from the Sun, Jupiter is surrounded by very powerful radiation belts which would kill anyone who entered them. Jupiter's moon Europa is thought to have a giant ocean below its surface Jupiter is by far the largest planet within our Solar System: two and a half times larger than all of the ...
... particles from the Sun, Jupiter is surrounded by very powerful radiation belts which would kill anyone who entered them. Jupiter's moon Europa is thought to have a giant ocean below its surface Jupiter is by far the largest planet within our Solar System: two and a half times larger than all of the ...
... nine planets thought to make up our Solar System. From our early childhood, we have recognized Pluto as the tiniest and the farthest member of the Sun’s immediate family. In 1930, the twenty-two year old American astronomer Clyde Tombaugh discovered Pluto at Lowell Observatory in Arizona. On 24 Augu ...
Crash Test - Eccles Science
... Impacts happen elsewhere in the universe too. Many exoplanets (planets that exist outside our solar system) are surrounded by telltale dust clouds that could have been caused only by collisions, she notes. “If you want to understand the solar system, you want to understand impact events and what the ...
... Impacts happen elsewhere in the universe too. Many exoplanets (planets that exist outside our solar system) are surrounded by telltale dust clouds that could have been caused only by collisions, she notes. “If you want to understand the solar system, you want to understand impact events and what the ...
Antares - Emmi
... Antares is in the constellation scorpio The Scorpio constellations story is an ancient Greek myth. Orion the hunter was the best hunter in the world and the most handsome man. He bragged that he would kill every animal on Earth. Apollo guardian of the cows pleaded with Hera the queen of the gods t ...
... Antares is in the constellation scorpio The Scorpio constellations story is an ancient Greek myth. Orion the hunter was the best hunter in the world and the most handsome man. He bragged that he would kill every animal on Earth. Apollo guardian of the cows pleaded with Hera the queen of the gods t ...
Document
... • Greeks were the first people known to make models of nature. • They tried to explain ...
... • Greeks were the first people known to make models of nature. • They tried to explain ...
The Sun
... on its mass. – It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. – When the hydrogen in its core is gone, a star has a helium center and outer layers made of hydrogen-dominated gas. – Some hydrogen continues to react in a thin ...
... on its mass. – It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. – When the hydrogen in its core is gone, a star has a helium center and outer layers made of hydrogen-dominated gas. – Some hydrogen continues to react in a thin ...
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.