Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... massive cannot support their own weight but collapse to form either Neutron Stars or Black Holes. • This maximum mass is called the Chandrasekhar ...
... massive cannot support their own weight but collapse to form either Neutron Stars or Black Holes. • This maximum mass is called the Chandrasekhar ...
worksheet
... This seems like a small amount of energy but now work out the energy released by 1kg of hydrogen atoms undergoing fusion. (Hint: use percentages) ...
... This seems like a small amount of energy but now work out the energy released by 1kg of hydrogen atoms undergoing fusion. (Hint: use percentages) ...
Natural Radioactivity
... also known as the atomic weight. Nuclei with the same number of protons (same element), but different numbers of neutrons (different atomic weight) are known as isotopes. The atomic weight of an isotope is equal to the number of protons plus the number of neutrons it has. Neutrons and protons can in ...
... also known as the atomic weight. Nuclei with the same number of protons (same element), but different numbers of neutrons (different atomic weight) are known as isotopes. The atomic weight of an isotope is equal to the number of protons plus the number of neutrons it has. Neutrons and protons can in ...
What is a star`s life cycle?
... ____________________ 1. A star changes its heat into energy. ____________________ 2. In 1987, a protostar was observed in the Large Magellanic Cloud. ____________________ 3. During nuclear reactions in large stars, helium is changed into carbon. ____________________ 4. A star stays in the main seque ...
... ____________________ 1. A star changes its heat into energy. ____________________ 2. In 1987, a protostar was observed in the Large Magellanic Cloud. ____________________ 3. During nuclear reactions in large stars, helium is changed into carbon. ____________________ 4. A star stays in the main seque ...
White Dwarf Stars - University of California Observatories
... • A black hole accelerates its surrounding material (often gas from a binary companion) to very high speeds in an accretion disk. • The heat generated by viscosity (friction) in this high speed gas produces X-rays. Some of the gas is ultimately swallowed by the black hole. ...
... • A black hole accelerates its surrounding material (often gas from a binary companion) to very high speeds in an accretion disk. • The heat generated by viscosity (friction) in this high speed gas produces X-rays. Some of the gas is ultimately swallowed by the black hole. ...
Nuclear Reactions Review
... 4.The process by which a nucleus splits into two or more smaller fragments, releasing neutrons and energy is called... A.strong nuclear split C.change reaction ...
... 4.The process by which a nucleus splits into two or more smaller fragments, releasing neutrons and energy is called... A.strong nuclear split C.change reaction ...
Nuclear Reactions Review powerpt
... 4.The process by which a nucleus splits into two or more smaller fragments, releasing neutrons and energy is called... A.strong nuclear split C.change reaction ...
... 4.The process by which a nucleus splits into two or more smaller fragments, releasing neutrons and energy is called... A.strong nuclear split C.change reaction ...
Supernovae - Michigan State University
... presence of 22Ne reduces Ye below 0.5 and therefore the amount of 56Ni produced ...
... presence of 22Ne reduces Ye below 0.5 and therefore the amount of 56Ni produced ...
Life Cycle of the Stars
... • How a star ends its life depends on its mass or how much matter it was born with. • Low and medium mass stars will end up as white dwarfs. • Stars that started with a lot of mass may end their lives as black holes or neutron stars. ...
... • How a star ends its life depends on its mass or how much matter it was born with. • Low and medium mass stars will end up as white dwarfs. • Stars that started with a lot of mass may end their lives as black holes or neutron stars. ...
Chapter 26
... ◦ This is an attractive force that acts between all nuclear particles ◦ The nuclear attractive force is stronger than the Coulomb repulsive force at the short ranges within the nucleus ...
... ◦ This is an attractive force that acts between all nuclear particles ◦ The nuclear attractive force is stronger than the Coulomb repulsive force at the short ranges within the nucleus ...
Problem set #2: AY 254C (Spring 2014) Due March 3, 2014
... Barbara). It covers the physics associated with Type-I X-ray bursts, which we did not cover in detail class. The neutron star in a low-mass x-ray binary accretes hydrogenheliumrich matter from a companion star. This accreted matter winds up getting spread over the surface of the neutron star. As add ...
... Barbara). It covers the physics associated with Type-I X-ray bursts, which we did not cover in detail class. The neutron star in a low-mass x-ray binary accretes hydrogenheliumrich matter from a companion star. This accreted matter winds up getting spread over the surface of the neutron star. As add ...
Stages in the Formation of Stars
... 3. Name the process that causes a star to begin producing vast amounts of energy. _____________________________________________ 4. What two processes balance each other to make a star stable? ...
... 3. Name the process that causes a star to begin producing vast amounts of energy. _____________________________________________ 4. What two processes balance each other to make a star stable? ...
Week 1b_2015
... It is during a supernova explosion that elements heavier than iron are formed by neutron capture. Since the neutron has no charge, it is not repelled by any nucleus it encounters and it can freely enter the nucleus regardless of how slowly it is moving. ...
... It is during a supernova explosion that elements heavier than iron are formed by neutron capture. Since the neutron has no charge, it is not repelled by any nucleus it encounters and it can freely enter the nucleus regardless of how slowly it is moving. ...
Sun: The Nearest Star
... Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F). Corona is the region that prominences appears. Prominences are immense clouds of glowing gas that erupt from the upper chromosphere. The Sun will be for 4.6 billion years and has enough fuel to go on fo ...
... Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F). Corona is the region that prominences appears. Prominences are immense clouds of glowing gas that erupt from the upper chromosphere. The Sun will be for 4.6 billion years and has enough fuel to go on fo ...
Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis
... solar masses. Initially the bounce gives it positive kinetic energy, but for each 0.1 solar masses it traverses and photodisintegrates about 1051 erg of energy is lost. Additional energy is lost to neutrinos as the shock moves to low densities, ρ ≈ 1011 gm cm-3. After about 10 ms the once powerful s ...
... solar masses. Initially the bounce gives it positive kinetic energy, but for each 0.1 solar masses it traverses and photodisintegrates about 1051 erg of energy is lost. Additional energy is lost to neutrinos as the shock moves to low densities, ρ ≈ 1011 gm cm-3. After about 10 ms the once powerful s ...
Atomic/Nuclear
... The binding energy per nucleon versus atomic number graph peaks at iron. Smaller and larger nuclei have less binding energy per nucleon than iron. If a nucleus with an even atomic number 92 or greater and an odd mass number absorbs a neutron, it can be split into two smaller nuclei with about 3 neut ...
... The binding energy per nucleon versus atomic number graph peaks at iron. Smaller and larger nuclei have less binding energy per nucleon than iron. If a nucleus with an even atomic number 92 or greater and an odd mass number absorbs a neutron, it can be split into two smaller nuclei with about 3 neut ...
Lecture 16: Iron Core Collapse, Neutron Stars, and Nucleosynthesis
... ~ 3 MeV (4 kT). Photons further out on the tail have enough energy (~8 MeV) to begin to rip nucleons out of the nucleus (analogue to ionization). The process does not go to completion but about 10% helium by mass is “boiled” out of the iron and this process (photodisintegration) saps energy that mig ...
... ~ 3 MeV (4 kT). Photons further out on the tail have enough energy (~8 MeV) to begin to rip nucleons out of the nucleus (analogue to ionization). The process does not go to completion but about 10% helium by mass is “boiled” out of the iron and this process (photodisintegration) saps energy that mig ...
I. Ch. 21.1 Nuclear Radiation
... Chemical Change – production of ___________ _______________________ with different properties – same elements just rearranged – usually involves valence electrons. ...
... Chemical Change – production of ___________ _______________________ with different properties – same elements just rearranged – usually involves valence electrons. ...
Use this form to take notes in class about stars
... 2. What is the initial reason why the particles within the nebula begin to ...
... 2. What is the initial reason why the particles within the nebula begin to ...
What are stars? - Manhasset Schools
... A giant’s core will continue to contract and become hotter. When it uses up all its helium, it contracts even more. When the temperature reaches 100 million K, helium fuses, forming carbon. Now the star is enormous and its surface is much cooler. Its outer layers escape into space leaving behind a ...
... A giant’s core will continue to contract and become hotter. When it uses up all its helium, it contracts even more. When the temperature reaches 100 million K, helium fuses, forming carbon. Now the star is enormous and its surface is much cooler. Its outer layers escape into space leaving behind a ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.