The Birth of Stars
... Sometimes (especially in spiral arms), the gas is compressed enough that the dust is thick and gravity can collapse knots in these “molecular” clouds to make new stars. ...
... Sometimes (especially in spiral arms), the gas is compressed enough that the dust is thick and gravity can collapse knots in these “molecular” clouds to make new stars. ...
The Superstructure of the Universe
... 1. The Universe is about ____ billion years old. The scientific ________________ that best explains the birth and evolution of the Universe is the ________________ Theory. 2. Evidence for the Big Bang includes a predicted ___ degree Kelvin echo that was discovered ____________ in 1965. The picture r ...
... 1. The Universe is about ____ billion years old. The scientific ________________ that best explains the birth and evolution of the Universe is the ________________ Theory. 2. Evidence for the Big Bang includes a predicted ___ degree Kelvin echo that was discovered ____________ in 1965. The picture r ...
THE NUCLEUS
... Opportunities are usually disguised as hard work, so most people don't recognize them. - Ann Landers ...
... Opportunities are usually disguised as hard work, so most people don't recognize them. - Ann Landers ...
Document
... • Learn some astronomy. The details are not so important, the fact that we have been able to learn so much about the Universe is a more important point. ...
... • Learn some astronomy. The details are not so important, the fact that we have been able to learn so much about the Universe is a more important point. ...
Friday, April 26
... • Light elements (hydrogen, helium) formed in Big Bang • Heavier elements formed by nuclear fusion in stars and thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
... • Light elements (hydrogen, helium) formed in Big Bang • Heavier elements formed by nuclear fusion in stars and thrown into space by supernovae – Condense into new stars and planets – Elements heavier than iron form during supernovae explosions ...
L37 - University of Iowa Physics
... other living thing, but the carbon-14 decays and is not replaced. The carbon-14 decays with its halflife of 5,700 years, while the amount of carbon-12 remains constant in the sample. By looking at the ratio of carbon-12 to carbon-14 in the sample and comparing it to the ratio in a living organism, i ...
... other living thing, but the carbon-14 decays and is not replaced. The carbon-14 decays with its halflife of 5,700 years, while the amount of carbon-12 remains constant in the sample. By looking at the ratio of carbon-12 to carbon-14 in the sample and comparing it to the ratio in a living organism, i ...
Lecture 10: Stellar Evolution
... Role of Mass • A star’s mass determines its entire life story because it determines its core temperature • High-mass stars with >8MSun have short lives, eventually becoming hot enough to make iron, and end in supernova explosions • Low-mass stars with <2MSun have long lives, never become hot e ...
... Role of Mass • A star’s mass determines its entire life story because it determines its core temperature • High-mass stars with >8MSun have short lives, eventually becoming hot enough to make iron, and end in supernova explosions • Low-mass stars with <2MSun have long lives, never become hot e ...
The Death of Stars - Mounds Park Academy Blogs
... Black Holes attract matter and matter attracted to a black hole accelerates as it is pulled toward the hole. Some of the matter is pulled directly into the black hole and is never seen again. Some of the matter goes into a high speed orbit around the ...
... Black Holes attract matter and matter attracted to a black hole accelerates as it is pulled toward the hole. Some of the matter is pulled directly into the black hole and is never seen again. Some of the matter goes into a high speed orbit around the ...
–1– Lecture 21 Review: calculation of mean atomic weight of an
... The result is that as Hydrogen is converted into Helium, the Sun becomes more luminous. Early on, it was 25% less luminous. The faint young Sun paradox is that the early Earth was too cold for liquid water to exist. The most common explanation is that the greenhouse effect kept the surface warmer (t ...
... The result is that as Hydrogen is converted into Helium, the Sun becomes more luminous. Early on, it was 25% less luminous. The faint young Sun paradox is that the early Earth was too cold for liquid water to exist. The most common explanation is that the greenhouse effect kept the surface warmer (t ...
1. setting the scene 2. the cosmic dark ages and the first stars
... Li—these were the only elements synthesised in the Big Bang itself (we’ll return to this point later). All other elements of the Periodic Table, which make our world such an interesting place, were ‘cooked’ later in the interiors of stars or in the supernova explosions which in some cases mark the e ...
... Li—these were the only elements synthesised in the Big Bang itself (we’ll return to this point later). All other elements of the Periodic Table, which make our world such an interesting place, were ‘cooked’ later in the interiors of stars or in the supernova explosions which in some cases mark the e ...
The Hertzsprung – Russell Diagram
... Very bright, red in color, very large, cool in temperature Brightness of stars are due to their enormous size ...
... Very bright, red in color, very large, cool in temperature Brightness of stars are due to their enormous size ...
– 1 – 1. Nucleosynthetic Yields From Various Sources
... early Universe, where 0 metallicity would permit such high mass stars to be formed and to evolve. Such stars, if present, would be tremendously important in chemical evolution because of the very large amount of ejected material. Their nucleosynthesis, first worked out in detail in Heger & Woosley ( ...
... early Universe, where 0 metallicity would permit such high mass stars to be formed and to evolve. Such stars, if present, would be tremendously important in chemical evolution because of the very large amount of ejected material. Their nucleosynthesis, first worked out in detail in Heger & Woosley ( ...
Self Assessment: Life Cycle of a Star
... 6. What event begins the transition from main sequence stage to red giant stage for a sun like star? a) surface cooling that turns the star red b) heating and expansion of the outer envelope c) contraction of the core due to gravity d) beginning of helium fusion 7. What happens during a nova? a) A ...
... 6. What event begins the transition from main sequence stage to red giant stage for a sun like star? a) surface cooling that turns the star red b) heating and expansion of the outer envelope c) contraction of the core due to gravity d) beginning of helium fusion 7. What happens during a nova? a) A ...
N(M)
... Molecules, found in cold regions, typically emit cm or mm-wave radiation ➙ observable with radio-telescopes (large antennas). The most abundant molecule, H2, has very few transitions - in fact v. difficult to observe at any wavelength! On the other hand, CO has a strong line at 2.6 microns - v. conve ...
... Molecules, found in cold regions, typically emit cm or mm-wave radiation ➙ observable with radio-telescopes (large antennas). The most abundant molecule, H2, has very few transitions - in fact v. difficult to observe at any wavelength! On the other hand, CO has a strong line at 2.6 microns - v. conve ...
The age–metallicity distribution of earth-harbouring stars
... • The relation between age and metallicity is very tight and agrees with the general predictions of the chemical evolution theory. • The Sun is more metalrich than 85% of its coeval stars. • Direct spectroscopic findings of terrestrial planets would be more efficient if young stars (having 3 t ...
... • The relation between age and metallicity is very tight and agrees with the general predictions of the chemical evolution theory. • The Sun is more metalrich than 85% of its coeval stars. • Direct spectroscopic findings of terrestrial planets would be more efficient if young stars (having 3 t ...
The Big Bang - Community Resources for Science
... One thing you may notice is that most of the common elements found in the sun can also be found in the human body. So now we have learned that the Big Bang created the first element hydrogen and as the universe expanded stars made of hydrogen were created by gravity and that stars create the element ...
... One thing you may notice is that most of the common elements found in the sun can also be found in the human body. So now we have learned that the Big Bang created the first element hydrogen and as the universe expanded stars made of hydrogen were created by gravity and that stars create the element ...
(No.323)The Genesis of Product Making/The Origin of Iron
... of Universe. It is commonly accepted that the universe was born by an awesome explosion known as the “Big Bang.” The protons and neutrons that are the core constituents of atoms were created by the big bang from a state in which no matter had previously existed. These particles bonded to each other ...
... of Universe. It is commonly accepted that the universe was born by an awesome explosion known as the “Big Bang.” The protons and neutrons that are the core constituents of atoms were created by the big bang from a state in which no matter had previously existed. These particles bonded to each other ...
Document
... big bang? A. Radiation from the big bang might be detected. It was gamma rays 14 billion years ago, but today it is cooler and would look like weak microwaves coming from all of space. B. The Big Bang produced three elements, which might be seen in the oldest stars: 75% hydrogen, 25% helium, 1 part ...
... big bang? A. Radiation from the big bang might be detected. It was gamma rays 14 billion years ago, but today it is cooler and would look like weak microwaves coming from all of space. B. The Big Bang produced three elements, which might be seen in the oldest stars: 75% hydrogen, 25% helium, 1 part ...
Galaxies and Stars Questions KEY
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
CBradleyLoutl
... The radius of the star expands quickly, the temperature of the star drops accordingly, the star becomes a red supergiant. - This is determined primarily by the mass of the star: . <.08 Solar Masses: The temperature and pressure weren’t great enough to cause any hydrogen fusion at all, the star passe ...
... The radius of the star expands quickly, the temperature of the star drops accordingly, the star becomes a red supergiant. - This is determined primarily by the mass of the star: . <.08 Solar Masses: The temperature and pressure weren’t great enough to cause any hydrogen fusion at all, the star passe ...
pps - TUM
... Can we find radioactive s- and r-process isotopes on earth? • Yes, or course: primordial, radioactive isotopes, there are many, few examples: ...
... Can we find radioactive s- and r-process isotopes on earth? • Yes, or course: primordial, radioactive isotopes, there are many, few examples: ...
Astronomy 110G Review Sheet for Exam #3 The
... • Luminous properties of various types of stars are conveniently displayed in the Hertzsprung-Russell diagram. The main sequence is a mass sequence with high mass stars near the top left (high temperature, large luminosity) region. Giants, etc., represent different and later stages in the lives of s ...
... • Luminous properties of various types of stars are conveniently displayed in the Hertzsprung-Russell diagram. The main sequence is a mass sequence with high mass stars near the top left (high temperature, large luminosity) region. Giants, etc., represent different and later stages in the lives of s ...
Nuclear Reactions Radioactive Decay The stability of an isotope
... In other layers helium combine to form beryllium, beryllium combine with helium to form carbon and carbon combine with helium to form oxygen Iron is the most stable atom, so nuclear fission only releases energy for atoms larger than iron. Similarly, nuclear fusion can only occur up to element 26 (ir ...
... In other layers helium combine to form beryllium, beryllium combine with helium to form carbon and carbon combine with helium to form oxygen Iron is the most stable atom, so nuclear fission only releases energy for atoms larger than iron. Similarly, nuclear fusion can only occur up to element 26 (ir ...
ASTRONOMY 120: GALAXIES AND THE UNIVERSE HOMEWORK
... When the Sun becomes a red giant, its luminosity will be about 2000 times greater than it is today. Calculate how long our Sun will be a red giant, assuming: • that this luminosity is caused only by the fusing of hydrogen, • that only 40% of the Sun’s original supply of Hydrogen is fused during the ...
... When the Sun becomes a red giant, its luminosity will be about 2000 times greater than it is today. Calculate how long our Sun will be a red giant, assuming: • that this luminosity is caused only by the fusing of hydrogen, • that only 40% of the Sun’s original supply of Hydrogen is fused during the ...
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.