Section 3-3(rev04) 2
... • Small stars can live for about 200 billion years. • Medium stars live for about 10 billion years. • Large stars live for about 10 million years. ...
... • Small stars can live for about 200 billion years. • Medium stars live for about 10 billion years. • Large stars live for about 10 million years. ...
Life Cycle of STARS
... What Causes the Collapse? • What did we say about all matter before? • All matter is attracted to other matter = gravity. ...
... What Causes the Collapse? • What did we say about all matter before? • All matter is attracted to other matter = gravity. ...
Homework 5
... Due November 9, 2012 at 5 p.m., either electronically or on paper. 1. What is a stellar association, how big are they, how many stars do they contain, how long do they last? Finally, what is their fate? ...
... Due November 9, 2012 at 5 p.m., either electronically or on paper. 1. What is a stellar association, how big are they, how many stars do they contain, how long do they last? Finally, what is their fate? ...
Unit E: SPACE EXPLORATION
... • Model of the universe that places the Sun at the centre with the Earth and planets revolving around it • Proposed by Polish astronomer Nicholas Copernicus in 1530 • Could not accurately predict planetary motion ...
... • Model of the universe that places the Sun at the centre with the Earth and planets revolving around it • Proposed by Polish astronomer Nicholas Copernicus in 1530 • Could not accurately predict planetary motion ...
Acting Out the Life Cycle of Stars - University of Texas Astronomy
... so everyone should unbend their arms now. When the star’s envelope expands, it gets cooler and redder and much bigger and the star becomes a red giant. The bright red/orange star in the shoulder of Orion, Betelgeuse, is a red giant. e. For stars that are less than about 8 times the mass of the Sun, ...
... so everyone should unbend their arms now. When the star’s envelope expands, it gets cooler and redder and much bigger and the star becomes a red giant. The bright red/orange star in the shoulder of Orion, Betelgeuse, is a red giant. e. For stars that are less than about 8 times the mass of the Sun, ...
Ch 20-21 Review
... D) it builds up a core of inert helium “ash.” E) it loses all its neutrinos, so fusion must cease. ...
... D) it builds up a core of inert helium “ash.” E) it loses all its neutrinos, so fusion must cease. ...
Lifecycle of Stars
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a personal poster that visually displays the four life cycles. You will work in table teams to complete this process, but you will each create your own mini-poster. 2) Use your n ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a personal poster that visually displays the four life cycles. You will work in table teams to complete this process, but you will each create your own mini-poster. 2) Use your n ...
Unit 8 Astronomy
... A neutron star is an imploded core of an exploded star made up almost entirely of neutrons. A teaspoon of their material would weigh more than all of automobiles in the U.S. together The most massive stars become supernovae and die as: ______________________ BLACK HOLE A black hole is an extremely m ...
... A neutron star is an imploded core of an exploded star made up almost entirely of neutrons. A teaspoon of their material would weigh more than all of automobiles in the U.S. together The most massive stars become supernovae and die as: ______________________ BLACK HOLE A black hole is an extremely m ...
Lecture 15 - Deaths of Stars, Supernovae
... Determining the age of a star cluster • Imagine we have a cluster of stars that were all formed at the same time, but have a variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
... Determining the age of a star cluster • Imagine we have a cluster of stars that were all formed at the same time, but have a variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
Slide 1
... HOW DO STARS DIE ? •Most stars take millions of years to die. When a star like the Sun has burned all of its hydrogen fuel, it expands to become a red giant while the rest of the stars become white dwarfs then cools down and becomes invisible. ...
... HOW DO STARS DIE ? •Most stars take millions of years to die. When a star like the Sun has burned all of its hydrogen fuel, it expands to become a red giant while the rest of the stars become white dwarfs then cools down and becomes invisible. ...
Stellar evolution, II
... tightly bound nucleus. Nuclear reactions to form heavier atoms would use up more energy than they would produce. The outer layers squeeze down onto the iron core and the star explodes as a Type II supernova. ...
... tightly bound nucleus. Nuclear reactions to form heavier atoms would use up more energy than they would produce. The outer layers squeeze down onto the iron core and the star explodes as a Type II supernova. ...
The Technology of Early Exploration
... created by placing the resource of the a mineral called lodestone (a magnetic stone) in the pointer of a compass which magnetically lines up with the magnetic field of the earth. ...
... created by placing the resource of the a mineral called lodestone (a magnetic stone) in the pointer of a compass which magnetically lines up with the magnetic field of the earth. ...
Stellar Evolution Diagram Answer Key:
... spin rapidly and flattens into a disk shape. Protostar: A protostars lifetime is only a few years. As the nebula shrinks a central mass will collect towards the center. It heats up because of the collision of particles and the increase in pressure. A protostar becomes a main sequence star when it re ...
... spin rapidly and flattens into a disk shape. Protostar: A protostars lifetime is only a few years. As the nebula shrinks a central mass will collect towards the center. It heats up because of the collision of particles and the increase in pressure. A protostar becomes a main sequence star when it re ...
Forging the elements
... Evolved stars LOSE about HALF of their MASS through their stellar winds. The winds are mostly made up of hydrogen. Molecules such as H2O (water) and OH (hydroxyl) form in the stellar winds at large distances from the star. Stellar wind ...
... Evolved stars LOSE about HALF of their MASS through their stellar winds. The winds are mostly made up of hydrogen. Molecules such as H2O (water) and OH (hydroxyl) form in the stellar winds at large distances from the star. Stellar wind ...
Pathways to Habitability: from disks to active stars, planets and life
... Planets formed in the gas disk gain large atmospheres made of hydrogen ...
... Planets formed in the gas disk gain large atmospheres made of hydrogen ...
Star Cycle [Recovered]
... Why do larger/hotter stars burn their fuel faster and live shorter lives than the Sun? ...
... Why do larger/hotter stars burn their fuel faster and live shorter lives than the Sun? ...
The perfect K-12 presentation ever (replace this with your title)
... Stellar nebula are clouds of gas and dust that eventually form stars. Stars form through the collapse of stellar nebula The Life Cycle of Stars describes the evolutionary paths for stars. ...
... Stellar nebula are clouds of gas and dust that eventually form stars. Stars form through the collapse of stellar nebula The Life Cycle of Stars describes the evolutionary paths for stars. ...
Stellar Deaths - Mid
... 1) formed at about same time 2) are at about the same distance 3) have same chemical composition The ONLY variable property among stars in a cluster is mass! ...
... 1) formed at about same time 2) are at about the same distance 3) have same chemical composition The ONLY variable property among stars in a cluster is mass! ...
ALMA_stars_summary
... The stellar theme involves different kinds of science, from the Sun to active stars to stellar atmosphere studies to dying stars and dead stars: will utilize the full complement of sensitivity, spatial & spectral resolution, mosaicing capabilities of ALMA ...
... The stellar theme involves different kinds of science, from the Sun to active stars to stellar atmosphere studies to dying stars and dead stars: will utilize the full complement of sensitivity, spatial & spectral resolution, mosaicing capabilities of ALMA ...
Study Notes for Chapter 30: Stars, Galaxies, and the Universe
... 10. After its temperature rises to 10,000,000°C, a protostar becomes a star when nuclear fusion begins. 11. Apparent magnitude is the brightness of a star as it appears from Earth. 12. Astronomers believe that cosmic background radiation formed shortly after the big bang. 13. By analyzing the light ...
... 10. After its temperature rises to 10,000,000°C, a protostar becomes a star when nuclear fusion begins. 11. Apparent magnitude is the brightness of a star as it appears from Earth. 12. Astronomers believe that cosmic background radiation formed shortly after the big bang. 13. By analyzing the light ...
Slide 1
... The Ant Nebula, a cloud of dust and gas whose technical name is Mz3, resembles an ant when observed using ground-based telescopes... The nebula lies within our galaxy between 3,000 and 6,000 light years from earth ...
... The Ant Nebula, a cloud of dust and gas whose technical name is Mz3, resembles an ant when observed using ground-based telescopes... The nebula lies within our galaxy between 3,000 and 6,000 light years from earth ...
Correlation Between Nitrogen and Oxygen Content in Planetary
... exactly alike; this is not hard to see. But the reason for this is harder to explain. Why does an event that happens in the same way under the same types of conditions produce such a different result (in morphology)? Our hypothesis was that the cause of the different morphologies in planetary nebula ...
... exactly alike; this is not hard to see. But the reason for this is harder to explain. Why does an event that happens in the same way under the same types of conditions produce such a different result (in morphology)? Our hypothesis was that the cause of the different morphologies in planetary nebula ...
Star Cycle Notes
... As the star collapses, the particles within the star (now mostly helium) heat up and get squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but much more powerfully this time. The restart of nuclear fusion in the star’s core expands the star ...
... As the star collapses, the particles within the star (now mostly helium) heat up and get squeezed so tightly they begin to fuse and form larger atoms like carbon and oxygen. Nuclear fusion restarts, but much more powerfully this time. The restart of nuclear fusion in the star’s core expands the star ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.