Ay123 Fall 2011 STELLAR STRUCTURE AND EVOLUTION Problem Set 2
... carbon white dwarf. Plot the following three white dwarfs on your graph: (1) Sirius B, M = 1.053 M⊙ , R = 0.0074 R⊙ ; (2) 40 Eri B, M = 0.48 M⊙ , R = 0.0124 R⊙ ; (3) Stein 2051, M = 0.50 M⊙ or 0.72 M⊙ , R = 0.0115 R⊙ , and try to infer their compositions. e. The results you have derived above should ...
... carbon white dwarf. Plot the following three white dwarfs on your graph: (1) Sirius B, M = 1.053 M⊙ , R = 0.0074 R⊙ ; (2) 40 Eri B, M = 0.48 M⊙ , R = 0.0124 R⊙ ; (3) Stein 2051, M = 0.50 M⊙ or 0.72 M⊙ , R = 0.0115 R⊙ , and try to infer their compositions. e. The results you have derived above should ...
The interstellar medium
... Other discoveries that provided evidence that there was material distributed between the stars: 1847 – W. Struve publishes Etudes d'Astronomie Stellaire. From the number of stars per magnitude bin, he concludes that there must be something distributed through space that is dimming starlight 1904 – ...
... Other discoveries that provided evidence that there was material distributed between the stars: 1847 – W. Struve publishes Etudes d'Astronomie Stellaire. From the number of stars per magnitude bin, he concludes that there must be something distributed through space that is dimming starlight 1904 – ...
Two Simplified Algorithms for maintaining Order in a List
... The Order-Maintenance Problem is to maintain a total order subject to the following operations: • Insert (X,Y): Insert a new element Y immediately after element X in the total Order. • Delete (X): Remove an element X from the total order. • Order (X,Y): Determine whether X precedes Y in the total or ...
... The Order-Maintenance Problem is to maintain a total order subject to the following operations: • Insert (X,Y): Insert a new element Y immediately after element X in the total Order. • Delete (X): Remove an element X from the total order. • Order (X,Y): Determine whether X precedes Y in the total or ...
File
... Smaller, cooler main sequence stars achieve this via the proton-proton chain reactions where protons are added successively to produce the helium. This reaction is the starting point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse h ...
... Smaller, cooler main sequence stars achieve this via the proton-proton chain reactions where protons are added successively to produce the helium. This reaction is the starting point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse h ...
Oxygen production on the AGB and the relevance of planetary
... • After each He-shell flash, the base of the envelope may “dredge” into the intershell region " third dredge-up • This can lead to carbon star production, where C/O > 1 at the stellar surface • Correlated with an enrichment of heavy elements (s-process) Standard picture: Dominant process in stars ...
... • After each He-shell flash, the base of the envelope may “dredge” into the intershell region " third dredge-up • This can lead to carbon star production, where C/O > 1 at the stellar surface • Correlated with an enrichment of heavy elements (s-process) Standard picture: Dominant process in stars ...
Section 14
... If the white dwarf is part of a system of two or more stars, it can lead to an interesting effect. As the non-white dwarf star produces energy, it is also emitting mass. This mass can accumulate on the surface of the white dwarf. If enough mass accumulates, it can lead to fusion processes within it ...
... If the white dwarf is part of a system of two or more stars, it can lead to an interesting effect. As the non-white dwarf star produces energy, it is also emitting mass. This mass can accumulate on the surface of the white dwarf. If enough mass accumulates, it can lead to fusion processes within it ...
Solar Lithium Mystery Solved
... conducted a survey of 500 stars, nearly 25% of which are like our own sun (Nature 2009, 462, 189). Seventy of the sunlike stars are known to have planetary systems. Most of the stars that host planets have on average one-tenth the amount of lithium of sunlike stars without planets. The researchers s ...
... conducted a survey of 500 stars, nearly 25% of which are like our own sun (Nature 2009, 462, 189). Seventy of the sunlike stars are known to have planetary systems. Most of the stars that host planets have on average one-tenth the amount of lithium of sunlike stars without planets. The researchers s ...
transcript
... 03:33 Ones we will call terrestrial, which are rocky planets like our earth and the others we will call gases, like Jupiter and Saturn because they are mostly made of gas. So rocky planets reside closer to the star [our sun] so we have four planets residing close to our sun because rocky material ca ...
... 03:33 Ones we will call terrestrial, which are rocky planets like our earth and the others we will call gases, like Jupiter and Saturn because they are mostly made of gas. So rocky planets reside closer to the star [our sun] so we have four planets residing close to our sun because rocky material ca ...
Lailaigib Lifecycle Of A Star
... http://www.universetoday.com/wpcontent/uploads/2008/05/foxneutronartwork.jpg ...
... http://www.universetoday.com/wpcontent/uploads/2008/05/foxneutronartwork.jpg ...
A-105 Homework 1
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
... 2. (1 pt.) How can the contraction of an inert helium core trigger the ignition of a hydrogen-fusion shell? ...
The World Year of Physics is a worldwide celebration of physics
... Roughly once per century in a typical galaxy, a massive star ends its life in a spectacular explosion that shines with the brilliance of all the billions of other stars in the galaxy combined. These explosions are called supernovae, and their fleeting presence in the night sky has been recorded sinc ...
... Roughly once per century in a typical galaxy, a massive star ends its life in a spectacular explosion that shines with the brilliance of all the billions of other stars in the galaxy combined. These explosions are called supernovae, and their fleeting presence in the night sky has been recorded sinc ...
Ch.21 Stars, Galaxies, and the Universe Section 3: Lives of Stars
... High-mass stars quickly evolve into brilliant supergiants When a supergiant runs out of fuel, it can explode suddenly The supernovas can become part of a nebula This nebula can then contract to form a new, partly recycled star o Neutron Stars: are the remains of high-mass stars They are ev ...
... High-mass stars quickly evolve into brilliant supergiants When a supergiant runs out of fuel, it can explode suddenly The supernovas can become part of a nebula This nebula can then contract to form a new, partly recycled star o Neutron Stars: are the remains of high-mass stars They are ev ...
Chapter 21 Notes
... 21.4 The Formation of the Elements The last nucleus in the alpha-particle chain is nickel-56, which is unstable and quickly decays to cobalt-56 and then to iron56. Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron captur ...
... 21.4 The Formation of the Elements The last nucleus in the alpha-particle chain is nickel-56, which is unstable and quickly decays to cobalt-56 and then to iron56. Iron-56 is the most stable nucleus, so it neither fuses nor decays. However, within the cores of the most massive stars, neutron captur ...
ASTRONOMY 1 ... You may use this only this study guide for reference... No electronic devises: I pads, lap tops, phones, etc.
... 20. Why are Star clusters important to our study of stars ? See figure 3 pg. 235 21. What is the approximate age of the star cluster in the HR diagram below? (Hint: Main Sequence Stars of spectral between types A and B core supply of hydrogen is sufficient to last about 250 million years. Between A ...
... 20. Why are Star clusters important to our study of stars ? See figure 3 pg. 235 21. What is the approximate age of the star cluster in the HR diagram below? (Hint: Main Sequence Stars of spectral between types A and B core supply of hydrogen is sufficient to last about 250 million years. Between A ...
Big Bang, 429
... 20. Why are Star clusters important to our study of stars ? See figure 3 pg. 235 21. What is the approximate age of the star cluster in the HR diagram below? (Hint: Main Sequence Stars of spectral between types A and B core supply of hydrogen is sufficient to last about 250 million years. Between A ...
... 20. Why are Star clusters important to our study of stars ? See figure 3 pg. 235 21. What is the approximate age of the star cluster in the HR diagram below? (Hint: Main Sequence Stars of spectral between types A and B core supply of hydrogen is sufficient to last about 250 million years. Between A ...
Probing the first stars through the abundance of metal poor stars
... 2) Systematic discrepancy between direct and indirect measurements of the high redshift star formation rate 3)Lack of surviving globular clusters that formed at high metallicity and high redshift 4) More rapid rise in the metallicity of cosmic gas than is predicted by current simulations 5) Enhancem ...
... 2) Systematic discrepancy between direct and indirect measurements of the high redshift star formation rate 3)Lack of surviving globular clusters that formed at high metallicity and high redshift 4) More rapid rise in the metallicity of cosmic gas than is predicted by current simulations 5) Enhancem ...
Lesson 2 | The Sun and Other Stars
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
... Directions: On the line before each definition, write the letter of the term that matches it correctly. Each term is used only once. ...
Stars: Their Life and Afterlife
... too light to reach the temperatures required to burn neon, oxygen, and heavier elements, so after burning carbon they are finished with fusion and evolve similarly to lighter white dwarfs. White dwarfs have a mass of ~1.2 MŸ or less. This limit is imposed by two conditions. First, if the mass were ...
... too light to reach the temperatures required to burn neon, oxygen, and heavier elements, so after burning carbon they are finished with fusion and evolve similarly to lighter white dwarfs. White dwarfs have a mass of ~1.2 MŸ or less. This limit is imposed by two conditions. First, if the mass were ...
The slow-neutron capture process at low metallicity
... • It is puzzling how CEMP-s/r could have formed in such large numbers • Given that the s and r-processes are thought to occur in independent events ...
... • It is puzzling how CEMP-s/r could have formed in such large numbers • Given that the s and r-processes are thought to occur in independent events ...
ASTRONOMY WEBQUEST…… EXPLORE THE UNIVERSE
... 11. What happened following the Big Bang to allow protons and neutrons to come together to form atoms and eventually atoms to come together to form different elements? __________________________________________________________________________________ http://map.gsfc.nasa.gov/universe/bb_tests.html ...
... 11. What happened following the Big Bang to allow protons and neutrons to come together to form atoms and eventually atoms to come together to form different elements? __________________________________________________________________________________ http://map.gsfc.nasa.gov/universe/bb_tests.html ...
What is a Star? - Lisle CUSD 202
... explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. ...
... explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. ...
Origins of nuclear science
... times – result is about $1 with 24 zeroes after it (a $T has only 12 zeroes !) • To understand the very large (force of nuclear weapons – Crossroads Baker) • To see features in the still photo of Crossroads Baker test ...
... times – result is about $1 with 24 zeroes after it (a $T has only 12 zeroes !) • To understand the very large (force of nuclear weapons – Crossroads Baker) • To see features in the still photo of Crossroads Baker test ...
Nucleosynthesis
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. It was then that hydrogen and helium formed to become the content of the first stars, and this primeval process is responsible for the present hydrogen/helium ratio of the cosmos.With the formation of stars, heavier nuclei were created from hydrogen and helium by stellar nucleosynthesis, a process that continues today. Some of these elements, particularly those lighter than iron, continue to be delivered to the interstellar medium when low mass stars eject their outer envelope before they collapse to form white dwarfs. The remains of their ejected mass form the planetary nebulae observable throughout our galaxy.Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28). Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the R process) in the period of a few seconds during the explosion. The elements formed in supernovas include the heaviest elements known, such as the long-lived elements uranium and thorium.Cosmic ray spallation, caused when cosmic rays impact the interstellar medium and fragment larger atomic species, is a significant source of the lighter nuclei, particularly 3He, 9Be and 10,11B, that are not created by stellar nucleosynthesis.In addition to the fusion processes responsible for the growing abundances of elements in the universe, a few minor natural processes continue to produce very small numbers of new nuclides on Earth. These nuclides contribute little to their abundances, but may account for the presence of specific new nuclei. These nuclides are produced via radiogenesis (decay) of long-lived, heavy, primordial radionuclides such as uranium and thorium. Cosmic ray bombardment of elements on Earth also contribute to the presence of rare, short-lived atomic species called cosmogenic nuclides.