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Information (Word Doc)
... Once a medium size star (such as our Sun) has reached the red giant phase, its outer layers continue to expand, but it’s core contracts, the result being that helium atoms together to form carbon. This fusion releases new energy but only for a few minutes! The core is now stable and the end is near. ...
... Once a medium size star (such as our Sun) has reached the red giant phase, its outer layers continue to expand, but it’s core contracts, the result being that helium atoms together to form carbon. This fusion releases new energy but only for a few minutes! The core is now stable and the end is near. ...
Life Cycle of a Star - Intervention Worksheet
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
Life Cycle of a Star
... _______________ cloud of gas and dust from which our solar system formed _______________ the life cycle of a star _______________ an explosion of a star that emits large amounts of matter and energy Stellar Evolution (video or transcript) Put the steps in order: ______ A nebula condenses into small ...
... _______________ cloud of gas and dust from which our solar system formed _______________ the life cycle of a star _______________ an explosion of a star that emits large amounts of matter and energy Stellar Evolution (video or transcript) Put the steps in order: ______ A nebula condenses into small ...
PHYS 2410 General Astronomy Homework 7
... 20. We know that the central object in a planetary nebula has a surface temperature of at least _________ because the nebula contains large amounts of ionized hydrogen. ...
... 20. We know that the central object in a planetary nebula has a surface temperature of at least _________ because the nebula contains large amounts of ionized hydrogen. ...
The Interstellar Medium (ISM)
... Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but emit few UV photons. Why “H II Region”? H I: Hydrogen atom H I ...
... Hot, massive stars produce huge amounts of these. Such short-lived stars spend all their lives in the stellar nursery of their birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but emit few UV photons. Why “H II Region”? H I: Hydrogen atom H I ...
Science Quiz
... The Big Bang- five basic steps of the big bang, when it happened, what does the future of our universe look like? Galaxies-three main shapes, what is our galaxy named and what shape is it? Be able to put space objects in order from biggest to smallest (use the galactic address info) Stars-What is a ...
... The Big Bang- five basic steps of the big bang, when it happened, what does the future of our universe look like? Galaxies-three main shapes, what is our galaxy named and what shape is it? Be able to put space objects in order from biggest to smallest (use the galactic address info) Stars-What is a ...
Explore the Galaxy - Museum of Science, Boston
... Nebula- An interstellar cloud of dust and gas (predominantly hydrogen and helium). Nebulae are commonly thought of as places where stars and planets are being actively formed, but they can also describe other astronomical phenomena. A planetary nebula is the gaseous shell released upon the death of ...
... Nebula- An interstellar cloud of dust and gas (predominantly hydrogen and helium). Nebulae are commonly thought of as places where stars and planets are being actively formed, but they can also describe other astronomical phenomena. A planetary nebula is the gaseous shell released upon the death of ...
Star Formation
... Stars not yet on the main sequence – find a cluster in which the massive stars are already on the main sequence, but the low-mass stars are not yet there. This is because their gravity is weaker, and they collapse somewhat more slowly as they form! T Tauri stars – young stars, including some called ...
... Stars not yet on the main sequence – find a cluster in which the massive stars are already on the main sequence, but the low-mass stars are not yet there. This is because their gravity is weaker, and they collapse somewhat more slowly as they form! T Tauri stars – young stars, including some called ...
This link is in pdf format for ease of reading
... Eventually, all stars run out of fuel in their cores. They lose their equilibrium as the force of gravity comes to dominate. Different-mass stars end their lives differently. Low-mass stars die quietly as their nuclear fires dwindle. The core in a Sun-like star collapses rapidly into an Earth-size w ...
... Eventually, all stars run out of fuel in their cores. They lose their equilibrium as the force of gravity comes to dominate. Different-mass stars end their lives differently. Low-mass stars die quietly as their nuclear fires dwindle. The core in a Sun-like star collapses rapidly into an Earth-size w ...
ASTR 1120H – Spring Semester 2010 Exam 2 – Answers The
... H II regions (also known as emission nebulae) are regions of gas that have been ionized by UV radiation from nearby hot stars. The hydrogen nuclei (i.e., protons) and electrons recombine in excited energy states and when the electron cascades back down toward the ground state, the transition from n ...
... H II regions (also known as emission nebulae) are regions of gas that have been ionized by UV radiation from nearby hot stars. The hydrogen nuclei (i.e., protons) and electrons recombine in excited energy states and when the electron cascades back down toward the ground state, the transition from n ...
HEIC0619: EMBARGOED UNTIL: 19:30 (CET)/01:30 PM EST 11
... now, Pismis 24-1, a bright young star that lies in the core of the small open star cluster Pismis 24 (the bright stars in the Hubble image) about 8,000 light-years away from Earth. Pismis 24-1 was thought to have an incredibly large mass of 200 to 300 solar masses. This would have made it by far the ...
... now, Pismis 24-1, a bright young star that lies in the core of the small open star cluster Pismis 24 (the bright stars in the Hubble image) about 8,000 light-years away from Earth. Pismis 24-1 was thought to have an incredibly large mass of 200 to 300 solar masses. This would have made it by far the ...
Life Cycle 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 large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
Life Cycle of a Star
... All stars start as a nebula. A nebula is a large cloud of gas and dust. Gravity can pull some of the gas and dust in a nebula together. The contracting cloud is then called a protostar. A protostar is the earliest stage of a star’s life. A star is born when the gas and dust from a nebula become so h ...
... All stars start as a nebula. A nebula is a large cloud of gas and dust. Gravity can pull some of the gas and dust in a nebula together. The contracting cloud is then called a protostar. A protostar is the earliest stage of a star’s life. A star is born when the gas and dust from a nebula become so h ...
Life Cycle of a Star - Intervention Worksheet
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
Stars Life Cycle WS
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
... After the star explodes, some of the materials from the star are left behind. This material may form a neutron star. Neutron stars are the remains of high-mass stars. The most massive stars become black holes when they die. After a large mass star explodes, a large amount of mass may remain. The gra ...
Star - Holy Family Regional School
... Star Classifications The mass of a star determines what kind of main sequence star it is. The more massive the star, the hotter it is. The brightest stars are at the top, with the dimmer ones at the bottom. The hottest stars are on the left, and the coolest ones are on the right. ...
... Star Classifications The mass of a star determines what kind of main sequence star it is. The more massive the star, the hotter it is. The brightest stars are at the top, with the dimmer ones at the bottom. The hottest stars are on the left, and the coolest ones are on the right. ...
Stellar Fusion
... together (mostly H being fused to form He). 5. Other element fusion? Yes, eventually helium, carbon, neon, magnesium and silicon can form. All of the naturally occurring elements in the universe are created by fusion reactions in stars. ...
... together (mostly H being fused to form He). 5. Other element fusion? Yes, eventually helium, carbon, neon, magnesium and silicon can form. All of the naturally occurring elements in the universe are created by fusion reactions in stars. ...
unit notes filled out
... expanding, the MS star can lose mass to the WD. The WD will ignite the mass in an eruption that cause the WD to temporarily “flair up” (10 magnitudes higher or more), this is called a nova and the process can be reoccurring. The most massive stars can get hot enough to fuse carbon and other elemen ...
... expanding, the MS star can lose mass to the WD. The WD will ignite the mass in an eruption that cause the WD to temporarily “flair up” (10 magnitudes higher or more), this is called a nova and the process can be reoccurring. The most massive stars can get hot enough to fuse carbon and other elemen ...
Handout 30
... The band that runs diagonally through the Hertzsprung-Russell diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. ...
... The band that runs diagonally through the Hertzsprung-Russell diagram and extends from cool, dim, red stars at the lower right to hot, bright, blue stars at the upper left. ...
Life Cycle of the Stars
... • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the dust and gas. ...
... • When the core of the matter becomes hot enough, thermonuclear fusion begins. • This means that there is enough heat to turn hydrogen to helium. • Once this has happened a true star has been born. • The star shines with its own light. • A solar wind then blows away the rest of the dust and gas. ...
a starry night - University of Florida Astronomy
... Wanderers in the Celestial Sphere & Beyond Dr. Stephen Kane, University of Florida. ...
... Wanderers in the Celestial Sphere & Beyond Dr. Stephen Kane, University of Florida. ...
Ch. 14 Formation of Stars
... energy so that it neither expands or contracts too much? • If the star begins producing more energy, then it expands. This results in a lower central temperature and density and slows nuclear fusion until the star regained stability. • The same process works in reverse: if less energy were generated ...
... energy so that it neither expands or contracts too much? • If the star begins producing more energy, then it expands. This results in a lower central temperature and density and slows nuclear fusion until the star regained stability. • The same process works in reverse: if less energy were generated ...
F03HW12
... RQ 12: How can we understand the Algol paradox? Answer: Algol is a binary star composed of a five solar mass main sequence star and a one solar mass giant. This presents a paradox because massive stars evolve faster than low mass stars, so the five solar mass stars should leave the main sequence bef ...
... RQ 12: How can we understand the Algol paradox? Answer: Algol is a binary star composed of a five solar mass main sequence star and a one solar mass giant. This presents a paradox because massive stars evolve faster than low mass stars, so the five solar mass stars should leave the main sequence bef ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
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.