Review for Midterm 1
... How many stars are typically born in a group and how many groups are typically formed at once? Why? How does spin affect the formation of a star? What are stars formed from and how big is that object? How does the mass of a star affect the time it takes to form? 4. Stellar energy: Where does the ene ...
... How many stars are typically born in a group and how many groups are typically formed at once? Why? How does spin affect the formation of a star? What are stars formed from and how big is that object? How does the mass of a star affect the time it takes to form? 4. Stellar energy: Where does the ene ...
Rare isotopes in the cosmos - National Superconducting Cyclotron
... nature’s chemical elements out of the hydrogen and helium left over from the Big Bang. Fusion reactions in stars drive the formation of elements with atomic numbers up to about that of iron. But fusion does not produce heavier elements; the nuclear binding energy per nucleon is maximal for nuclei ar ...
... nature’s chemical elements out of the hydrogen and helium left over from the Big Bang. Fusion reactions in stars drive the formation of elements with atomic numbers up to about that of iron. But fusion does not produce heavier elements; the nuclear binding energy per nucleon is maximal for nuclei ar ...
Mass-Luminosity Relation for White
... Differing from the usual stars, we have no simple relation between their masses and luminosities in the case of the white-dwarf stars. Namely, the luminosity of a white dwarf frequently differs from that of another with the almost same mass and apparent chemical composition by a factor of one hundre ...
... Differing from the usual stars, we have no simple relation between their masses and luminosities in the case of the white-dwarf stars. Namely, the luminosity of a white dwarf frequently differs from that of another with the almost same mass and apparent chemical composition by a factor of one hundre ...
Stars & Galaxies
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
Gravity simplest fusion
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
... • When a neutron star forms, the pull of gravity is so great that it overrides the electron degeneracy pressure of the atoms of the star. • The electrons are forced into their respective nuclei, where they combine with protons to form neutrons. This greatly decreases the size of each atom, and allow ...
Stellar Masses and the Main Sequence
... integrate reaction rate cross-sections over the Maxwellian distribution. The cross sections are energy dependent, since they depend on momentum and tunneling. ...
... integrate reaction rate cross-sections over the Maxwellian distribution. The cross sections are energy dependent, since they depend on momentum and tunneling. ...
A105 Stars and Galaxies - Indiana University Astronomy
... •The planet needs to have the right mass--too small and the atmosphere escapes--too large and the atmosphere is made of hydrogen •The atmosphere needs to be of the right mix of ...
... •The planet needs to have the right mass--too small and the atmosphere escapes--too large and the atmosphere is made of hydrogen •The atmosphere needs to be of the right mix of ...
solution
... is very long, nearly 107 yr; however, there is a lot of hydrogen out there (see §§22.32, below). 22.13 Many old black-and-white photographs of spiral galaxies were taken using film that was most sensitive to blue light. Explain why the spiral arms were particularly prominent in such photographs.? Th ...
... is very long, nearly 107 yr; however, there is a lot of hydrogen out there (see §§22.32, below). 22.13 Many old black-and-white photographs of spiral galaxies were taken using film that was most sensitive to blue light. Explain why the spiral arms were particularly prominent in such photographs.? Th ...
What is life made of?
... species using the analytical techniques that offer much higher precision than ever before and hope to remedy the lack of quality data for other species (not just humans and bacteria). Widespread studies looking at all forms of life on Earth would be required to work towards our ultimate goal of unde ...
... species using the analytical techniques that offer much higher precision than ever before and hope to remedy the lack of quality data for other species (not just humans and bacteria). Widespread studies looking at all forms of life on Earth would be required to work towards our ultimate goal of unde ...
Semester II: Final Exam Review for Hedden and
... 5. The rate of fusion of high-mass stars greatly exceeds that of low-mass stars. A result is that highmass stars spend less time on the main sequence than low-mass stars ...
... 5. The rate of fusion of high-mass stars greatly exceeds that of low-mass stars. A result is that highmass stars spend less time on the main sequence than low-mass stars ...
PHYS 1400 Sample Exam Questions: Properties of Matter (Atoms) 1
... again after, he was able to show that even though the paper was gone, there was still the same amount of matter in the box. 33. What exactly is Avogadro's Principle? B) Not everything is made of the same number of atoms, but if you isolate equal volumes of different gases, and they are at the same t ...
... again after, he was able to show that even though the paper was gone, there was still the same amount of matter in the box. 33. What exactly is Avogadro's Principle? B) Not everything is made of the same number of atoms, but if you isolate equal volumes of different gases, and they are at the same t ...
Abstract
... and find bright young objects there. Lyman α emitters1 have been recently discovered at redshifts greater than 3 (2.1109 yr after the Big-Bang) and Lyman break galaxies2 are high-redshift star-forming galaxies with the intense ultraviolet radiation from young stars. In the theoretical view point, g ...
... and find bright young objects there. Lyman α emitters1 have been recently discovered at redshifts greater than 3 (2.1109 yr after the Big-Bang) and Lyman break galaxies2 are high-redshift star-forming galaxies with the intense ultraviolet radiation from young stars. In the theoretical view point, g ...
Slide 1
... The sun is only going to have enough pressure to get to the point where it fuses carbon. After it stops, the rest of the sun collapsing down just isn’t hot enough to let it do more fusion. So what happens next? This is where it gets a bit ...
... The sun is only going to have enough pressure to get to the point where it fuses carbon. After it stops, the rest of the sun collapsing down just isn’t hot enough to let it do more fusion. So what happens next? This is where it gets a bit ...
powerpoint - Physics @ IUPUI
... once started at the same point. • This point and time was the big bang. • From the universe know we can retrace the steps to the big bang. • One of the major steps is the time of recombination which created the cosmic microwave background which is now “cooled” to 2.7 K. • From the structure of this ...
... once started at the same point. • This point and time was the big bang. • From the universe know we can retrace the steps to the big bang. • One of the major steps is the time of recombination which created the cosmic microwave background which is now “cooled” to 2.7 K. • From the structure of this ...
Quiz 1: Answers Physics 55: Introduction to
... Circle the letter that best answers each of the following questions. 1. The typical number of stars in a galaxy, the approximate number of galaxies in the observable universe, and the approximate number of neurons in the human brain all have similar values equal to about (a) 106 . (b) 1010 . (c) 102 ...
... Circle the letter that best answers each of the following questions. 1. The typical number of stars in a galaxy, the approximate number of galaxies in the observable universe, and the approximate number of neurons in the human brain all have similar values equal to about (a) 106 . (b) 1010 . (c) 102 ...
How do stars shine?
... Come the twentieth century, and the era of radioactivity and nuclear physics, bringing with it the famous equation E=mc2, and suddenly new possibilities opened up for sources of power. Einstein’s famous equation means we can convert mass into energy, and c, being the speed of light, and a very big ...
... Come the twentieth century, and the era of radioactivity and nuclear physics, bringing with it the famous equation E=mc2, and suddenly new possibilities opened up for sources of power. Einstein’s famous equation means we can convert mass into energy, and c, being the speed of light, and a very big ...
The life-cycle of stars - Young Scientists Journal
... rise as the atoms are crushed together. The repulsive force between the nuclei overcomes gravity and the core recoils out in what we see as a supernova. As the shock wave hits material in the star’s outer layers the material is heated, fusing to form further elements. All heavy elements, including u ...
... rise as the atoms are crushed together. The repulsive force between the nuclei overcomes gravity and the core recoils out in what we see as a supernova. As the shock wave hits material in the star’s outer layers the material is heated, fusing to form further elements. All heavy elements, including u ...
Stars!!!!
... • Super Nova is when a giant or super giant star explodes • What is left over is called a neutron star – Smaller and denser than white dwarfs – They can have the same mass as the sun but can be the size of an asteroid ...
... • Super Nova is when a giant or super giant star explodes • What is left over is called a neutron star – Smaller and denser than white dwarfs – They can have the same mass as the sun but can be the size of an asteroid ...
ppt - Slides by Prof Christian
... WDs with more than ~ 1.4 solar masses can not exist! Chandrasekhar Limit = 1.4 Msun ...
... WDs with more than ~ 1.4 solar masses can not exist! Chandrasekhar Limit = 1.4 Msun ...
Stars & Galaxies
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
... © 2006, TESCCC The content of this multimedia presentation is intended for use by TESCCC subscribers for intra-district professional development ONLY; and may not be used for other purposes, in whole or part, without the expressed written permission of their ESC-TESCCC coordinator for the region han ...
Stellar Evolution
... with spectral types A through K on the main sequence and stars of type O and B on the (super) giant branch. What is the approximate age of the cluster? ...
... with spectral types A through K on the main sequence and stars of type O and B on the (super) giant branch. What is the approximate age of the cluster? ...
Heavy elements game
... unique. Every gold atom has 79 protons in its nucleus. Every carbon atom has 6 protons. The number of protons gives each element its distinctive properties. Stars are the birthplace of all the different types of elements we find on Earth. Through the process of nuclear fusion (the nucleus of two ato ...
... unique. Every gold atom has 79 protons in its nucleus. Every carbon atom has 6 protons. The number of protons gives each element its distinctive properties. Stars are the birthplace of all the different types of elements we find on Earth. Through the process of nuclear fusion (the nucleus of two ato ...
Nucleosynthesis in the Early Universe.
... We can now create deuterons from the protons and neutrons but there are so many photons (with energy greater than 2.233 MeV) that the deuterons break up almost immediately. This is known as the Deuteron Bottleneck- it causes a delay before the light nuclei can be formed. Eventually as T falls the n ...
... We can now create deuterons from the protons and neutrons but there are so many photons (with energy greater than 2.233 MeV) that the deuterons break up almost immediately. This is known as the Deuteron Bottleneck- it causes a delay before the light nuclei can be formed. Eventually as T falls the n ...
The Origin of Light
... oxygen to produce heat and light, and the Sun has predominantly hydrogen with a lesser amount of helium and much smaller quantities of other elements. A nuclear reaction, hydrogen being converted to helium, causes the emission of heat and light. Much research has been carried out by scientists to de ...
... oxygen to produce heat and light, and the Sun has predominantly hydrogen with a lesser amount of helium and much smaller quantities of other elements. A nuclear reaction, hydrogen being converted to helium, causes the emission of heat and light. Much research has been carried out by scientists to de ...
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.