Chapter 14
... materials were fused into nuclei around iron, the element with the lowest amount of energy per nucleon and the star used up its energy source. • Larger, more massive dying stars explode into supernovas. Such an explosion releases a flood of neutrons, which bombard medium weight nuclei and build them ...
... materials were fused into nuclei around iron, the element with the lowest amount of energy per nucleon and the star used up its energy source. • Larger, more massive dying stars explode into supernovas. Such an explosion releases a flood of neutrons, which bombard medium weight nuclei and build them ...
The Interstellar Medium (ISM) The Dust The Gas: a. The Hot
... High density: 105 per cm3 molecular hydrogen H2 . Cold Temperature: about 20K Molecular emissions formation of molecules — cool, low energy environment requires dust grains. Types of molecules Organic molecules; pre-biotic? possible detection of amino acid glycine Giant Molecular Clouds Massive, ...
... High density: 105 per cm3 molecular hydrogen H2 . Cold Temperature: about 20K Molecular emissions formation of molecules — cool, low energy environment requires dust grains. Types of molecules Organic molecules; pre-biotic? possible detection of amino acid glycine Giant Molecular Clouds Massive, ...
Stars presentation by lauren
... (apart from the sun) is called Proxima Centauri, and it is 4.3 light years away! It would take us over 1,000 years to get there! It seems impossible, but scientists say we might be able to visit the stars in the future……… ...
... (apart from the sun) is called Proxima Centauri, and it is 4.3 light years away! It would take us over 1,000 years to get there! It seems impossible, but scientists say we might be able to visit the stars in the future……… ...
characteristics of stars/lives of stars
... 7. A star’s brightness as if it were a standard distance from Earth is its 8. A device that breaks light into colors and produces an image is a(n) 9. A unit that is often used to measure distances between stars is a(n) 10. The region of the Hertzsprung-Russell diagram that most stars fall within is ...
... 7. A star’s brightness as if it were a standard distance from Earth is its 8. A device that breaks light into colors and produces an image is a(n) 9. A unit that is often used to measure distances between stars is a(n) 10. The region of the Hertzsprung-Russell diagram that most stars fall within is ...
astr study guide ex 3 s`16
... 32. Why would an isolated black hole in empty intergalactic space be difficult to detect? 33. The material that accretes onto a neutron star or black hole is expected to emit X-rays because 34. What is the difference between a neutron star and a pulsar? 35. What determines the escape velocity of an ...
... 32. Why would an isolated black hole in empty intergalactic space be difficult to detect? 33. The material that accretes onto a neutron star or black hole is expected to emit X-rays because 34. What is the difference between a neutron star and a pulsar? 35. What determines the escape velocity of an ...
powerpoint - Physics @ IUPUI
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
... • This is done by radiation pressure and gas pressure (they counteract gravity). • But to keep this up requires the constant generation of energy in the core. ...
33 Atomic Nucleus and Radioactivity Answers and Solutions for
... 25. When an element emits an alpha particle, atomic number decreases by 2. For emission of a beta particle, atomic number increases by 1. For gamma emission, no change in atomic number. 26. Uranium ultimately transmutes to lead. 27. Ernest Rutherford in 1919 was the first to intentionally transmute ...
... 25. When an element emits an alpha particle, atomic number decreases by 2. For emission of a beta particle, atomic number increases by 1. For gamma emission, no change in atomic number. 26. Uranium ultimately transmutes to lead. 27. Ernest Rutherford in 1919 was the first to intentionally transmute ...
β-Decay Half-Lives of 110 Neutron-Rich Nuclei across the N = 82
... from ðγ; nÞ reactions is minor. These conditions are expected in supersonically expanding neutrino-driven outflow in low-mass supernovae progenitors (e.g., 8 − 12 M⊙ ) or prompt ejecta from neutron star mergers [17]. The final abundance distribution may also be dominated by postprocessing effects su ...
... from ðγ; nÞ reactions is minor. These conditions are expected in supersonically expanding neutrino-driven outflow in low-mass supernovae progenitors (e.g., 8 − 12 M⊙ ) or prompt ejecta from neutron star mergers [17]. The final abundance distribution may also be dominated by postprocessing effects su ...
5Stars_Part_Two
... 16O + 16O = 28Si + 4He 2. Nuclei as heavy as 56Fe and 56Ni can be created if the star core is hot enough. 3. Nucleosynthesis and fusion stop with 56Fe and 56Ni (Binding energy) ...
... 16O + 16O = 28Si + 4He 2. Nuclei as heavy as 56Fe and 56Ni can be created if the star core is hot enough. 3. Nucleosynthesis and fusion stop with 56Fe and 56Ni (Binding energy) ...
Astronomy 100 Name(s):
... systems. For this calculation you will need to count stars (even ones in multiplestar systems) separately. ...
... systems. For this calculation you will need to count stars (even ones in multiplestar systems) separately. ...
The Great Bear and the Little Bear
... • Stars are balls of hot gas. • They are much larger than planets and much further from Earth. • The sun is the closest star to Earth. • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the ...
... • Stars are balls of hot gas. • They are much larger than planets and much further from Earth. • The sun is the closest star to Earth. • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the ...
HS-ESS1 Earth`s Place in the Universe
... The Big Bang theory is supported by observations of distant galaxies receding from our own, of the measured composition of stars and non-stellar gases, and of the maps of spectra of the primordial radiation (cosmic microwave background) that still fills the universe. (HSESS1-2) Other than the hy ...
... The Big Bang theory is supported by observations of distant galaxies receding from our own, of the measured composition of stars and non-stellar gases, and of the maps of spectra of the primordial radiation (cosmic microwave background) that still fills the universe. (HSESS1-2) Other than the hy ...
hot
... stable lifetimes of such stars elements that are more massive than iron form during supernova events ...
... stable lifetimes of such stars elements that are more massive than iron form during supernova events ...
Redshift takes us from 2-D to 3-D
... From average speed of galaxies – the cluster would fly apart From X-ray gas held in – several million degrees and extensive ...
... From average speed of galaxies – the cluster would fly apart From X-ray gas held in – several million degrees and extensive ...
The Universe - IES Alyanub
... (Ceres) is in the asteroid belt. Then there is Pluto, which was a planet for almost 80 years before being reclassified, and finally Eris, which is even further out of the solar system than Pluto is. Solar System Formation Everything has a beginning, and our story begins when the cloud that was the S ...
... (Ceres) is in the asteroid belt. Then there is Pluto, which was a planet for almost 80 years before being reclassified, and finally Eris, which is even further out of the solar system than Pluto is. Solar System Formation Everything has a beginning, and our story begins when the cloud that was the S ...
Document
... low, but the Carbon, Oxygen, and Nitrogen abundance is only about [X/Fe] ~ –2. So this may not be one of the first stars, rather a peculiar star like the l Boo class of objects. ...
... low, but the Carbon, Oxygen, and Nitrogen abundance is only about [X/Fe] ~ –2. So this may not be one of the first stars, rather a peculiar star like the l Boo class of objects. ...
Death - Wayne State University Physics and Astronomy
... • The core, once the size of the Earth, becomes a very stiff neutron star about the size of a small town in less than a second • The in falling outer layers hit the core and heat up to billions of degrees from the impact 12 April 2005 ...
... • The core, once the size of the Earth, becomes a very stiff neutron star about the size of a small town in less than a second • The in falling outer layers hit the core and heat up to billions of degrees from the impact 12 April 2005 ...
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. ...
Other burning stages - Michigan State University
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
Ch 20-21 Review
... B) iron has poor nuclear binding energy. C) iron cannot fuse with other nuclei to produce energy. D) iron supplies too much pressure. E) iron is in the form of a gas, not a solid, in the center of a star. ...
... B) iron has poor nuclear binding energy. C) iron cannot fuse with other nuclei to produce energy. D) iron supplies too much pressure. E) iron is in the form of a gas, not a solid, in the center of a star. ...
GLY 1001 Earth Science Name:__Answers
... Barred spiral – A galaxy having straight arms extending from its nucleus. Big bang theory – The theory that proposes that the universe originated as a single mass which subsequently exploded. Black hole – a massive star that has collapsed to such a small volume that the gravity prevents the escape o ...
... Barred spiral – A galaxy having straight arms extending from its nucleus. Big bang theory – The theory that proposes that the universe originated as a single mass which subsequently exploded. Black hole – a massive star that has collapsed to such a small volume that the gravity prevents the escape o ...
observed
... above my head; and since I had, from boyhood, known all the stars of the heavens perfectly, it was quite evident to me that there had never been any star in that place of the sky, even the smallest, to say nothing of a star so conspicuous and bright as this… A miracle indeed, one that has never been ...
... above my head; and since I had, from boyhood, known all the stars of the heavens perfectly, it was quite evident to me that there had never been any star in that place of the sky, even the smallest, to say nothing of a star so conspicuous and bright as this… A miracle indeed, one that has never been ...
Document
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
... Venn & Lambert (2008) have argued that this may not be the case. Peculiar stars such as post AGB stars and l Boo stars have iron abundances as low as [Fe/H] ~ –5. These are thought to be due to the separation of gas and dust beyond the stellar surface followed by an accretion of the dust-depleted g ...
Physical Science Content Standards
... water and salt, and very large ones, such as carbohydrates, fats, proteins, and DNA. PERIODIC TABLE: 7. The organization of the Periodic Table is based on the properties of the elements and reflects the structure of atoms. As a basis for understanding this concept, students know: a. how to identify ...
... water and salt, and very large ones, such as carbohydrates, fats, proteins, and DNA. PERIODIC TABLE: 7. The organization of the Periodic Table is based on the properties of the elements and reflects the structure of atoms. As a basis for understanding this concept, students know: a. how to identify ...
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.