The Atom
... mc2 enables us to relate the energy released to the mass loss in the formation of atoms. Use the known values for the mass of a proton, 1.0073 amu, mass of a neutron, 1.0087, and the mass of an electron, 5.486 x 10-4 amu, to show that the mass of a 12C atom is less than the sum of the masses of the ...
... mc2 enables us to relate the energy released to the mass loss in the formation of atoms. Use the known values for the mass of a proton, 1.0073 amu, mass of a neutron, 1.0087, and the mass of an electron, 5.486 x 10-4 amu, to show that the mass of a 12C atom is less than the sum of the masses of the ...
Nucleosynthesis and the death of stars
... • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but the smaller nuclei, but the range of t ...
... • Could stars in principle live forever simply by contracting gravitationally and increasing their temperature to ignite the next heavier source of nuclear fuel whenever they run out? – No. The strong interaction’s range is smaller than the diameters of all but the smaller nuclei, but the range of t ...
Requiem for a Star
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
... Stars Comparable to Sun • M up to about 3 or 4 solar masses • As a Main Sequence star can only use hydrogen as a fuel • When hydrogen is exhausted collapse of interior is inevitable • Increase in temperature caused by collapse suddenly ignites unprocessed hydrogen, causing star to expand to become ...
Learning Objectives Weeks 9-11 . 1. Know that star birth can begin
... white dwarf. A white dwarf is kept from collapsing by the pressure of its degenerate electrons. 11. High-mass stars create heavy elements in their cores. A star of 8 or more solar masses evolves into a supergiant 100 times (or more) larger than the Sun. 12. High-mass stars violently blow apart in su ...
... white dwarf. A white dwarf is kept from collapsing by the pressure of its degenerate electrons. 11. High-mass stars create heavy elements in their cores. A star of 8 or more solar masses evolves into a supergiant 100 times (or more) larger than the Sun. 12. High-mass stars violently blow apart in su ...
Lecture Nine (Powerpoint format) - Flash
... The physics of nuclear burning in stellar interiors can be summarized by energy generation cycles. The basic nuclear physics is very similar to basic chemistry -there is both a product and reactants, and the product and the reactants must “balance”. In the case of basic chemistry, each element ...
... The physics of nuclear burning in stellar interiors can be summarized by energy generation cycles. The basic nuclear physics is very similar to basic chemistry -there is both a product and reactants, and the product and the reactants must “balance”. In the case of basic chemistry, each element ...
Stars: Their Life and Afterlife
... pressure. Having thrown off their outer layers of hydrogen and helium in thermal pulses (forming a so-called “planetary nebula” around the star), these stars become white dwarfs – exposed, hot carbon-oxygen cores that slowly radiate their stored heat energy and cool. We will discuss white dwarfs mor ...
... pressure. Having thrown off their outer layers of hydrogen and helium in thermal pulses (forming a so-called “planetary nebula” around the star), these stars become white dwarfs – exposed, hot carbon-oxygen cores that slowly radiate their stored heat energy and cool. We will discuss white dwarfs mor ...
Why Is the Sun a Star
... discovered a new class of stars that are between 20 – 70 Jupiter masses that are fusing some atoms and radiating some energy, but not in the fantastic amounts like true stars. These stars are known as brown dwarfs since they emit some light but are not as bright as the smallest true stars. They are ...
... discovered a new class of stars that are between 20 – 70 Jupiter masses that are fusing some atoms and radiating some energy, but not in the fantastic amounts like true stars. These stars are known as brown dwarfs since they emit some light but are not as bright as the smallest true stars. They are ...
An Introduction - Solar Physics and Space Weather
... •Protostar: the clump formed from dense and cold nebula under gravitational contraction •The protostar contracts, because the pressure inside is too low to support all the mass. ...
... •Protostar: the clump formed from dense and cold nebula under gravitational contraction •The protostar contracts, because the pressure inside is too low to support all the mass. ...
Class II Supernova
... •Class II can be divided, because of their emission spectra •Unlike a Type I supernova, the mass and brightness can vary •Type 2P has a Very wide wavelength, •A type PL has a somewhat small wavelength, •A rare Type 2N has an extremely narrow wavelength, (thus the “n”) ...
... •Class II can be divided, because of their emission spectra •Unlike a Type I supernova, the mass and brightness can vary •Type 2P has a Very wide wavelength, •A type PL has a somewhat small wavelength, •A rare Type 2N has an extremely narrow wavelength, (thus the “n”) ...
Modelling the Stellar Populations of The Milky Way and Andromeda
... 3. Initialize simulations, embed stellar content into the center of accreted dark matter halo to match a realistic galaxy light profile. ...
... 3. Initialize simulations, embed stellar content into the center of accreted dark matter halo to match a realistic galaxy light profile. ...
– 1 – 1. Cosmochronology
... called the “daughter”), can be measured. After all, the abundance of a decaying radioactive isotope is an negative exponential, Nr (t) = Nr (0) exp(−t/τr ). One looks for an unstable isotope of an element whose production is well understood, one with a suitable lifetime (preferably at least 1 Gyr, i ...
... called the “daughter”), can be measured. After all, the abundance of a decaying radioactive isotope is an negative exponential, Nr (t) = Nr (0) exp(−t/τr ). One looks for an unstable isotope of an element whose production is well understood, one with a suitable lifetime (preferably at least 1 Gyr, i ...
Round 1
... An ’HR diagram’ is a plot of which two quantities. (T (or spectral type) vs. L (or absolute magnitude)) $1200 More luminous stars tend to live this. (shorter lives) $1600 This tells you how much energy is released in the fusion of hydrogen to helium. (E = ∆mc2 where ∆m is the mass difference between ...
... An ’HR diagram’ is a plot of which two quantities. (T (or spectral type) vs. L (or absolute magnitude)) $1200 More luminous stars tend to live this. (shorter lives) $1600 This tells you how much energy is released in the fusion of hydrogen to helium. (E = ∆mc2 where ∆m is the mass difference between ...
strong force
... called isobars, [bar means weight], because they are relatively close in atomic mass. Not exactly because of slightly different n and p masses, AND different binding energies due to structural details. Section 30.1 ...
... called isobars, [bar means weight], because they are relatively close in atomic mass. Not exactly because of slightly different n and p masses, AND different binding energies due to structural details. Section 30.1 ...
Physics in the Balance - Max-Planck
... BREEDING PROCESSES IN STARS MAKE GOLD VALUABLE These so-called waiting point nuclei act like stop signals on the way to even heavier elements. In supernovae, this path is provided by a process to which around half of the elements beyond iron in the chart of nuclides owe their existence. It involves ...
... BREEDING PROCESSES IN STARS MAKE GOLD VALUABLE These so-called waiting point nuclei act like stop signals on the way to even heavier elements. In supernovae, this path is provided by a process to which around half of the elements beyond iron in the chart of nuclides owe their existence. It involves ...
Progenitor stars of supernovae
... NH~ 1.5 x 1021 cm-2 • If reverse shock is in He layers close to C-O boundary (Fransson et al. 2002), then this implies reverse shock mass of ~0.002M-0.8M. ...
... NH~ 1.5 x 1021 cm-2 • If reverse shock is in He layers close to C-O boundary (Fransson et al. 2002), then this implies reverse shock mass of ~0.002M-0.8M. ...
SL2 IIIC Carter 280911 - Particle Solids Interactions group
... • Positive charge in nucleus (1900 – 1920) – Atoms are neutral • positive charge needed to cancel electron’s negative charge • Rutherford atom: positive charge in nucleus ...
... • Positive charge in nucleus (1900 – 1920) – Atoms are neutral • positive charge needed to cancel electron’s negative charge • Rutherford atom: positive charge in nucleus ...
Stellar Metamorphosis: The Nearest Star
... Abstract: In stellar metamorphosis humanities’ closest star is the Earth itself. Explanation is provided. In the so-called “established sciences” the closest star to the Earth is the Sun, and the closest star to Earth besides the Sun is Proxima Centauri. This is not complete. According to stellar me ...
... Abstract: In stellar metamorphosis humanities’ closest star is the Earth itself. Explanation is provided. In the so-called “established sciences” the closest star to the Earth is the Sun, and the closest star to Earth besides the Sun is Proxima Centauri. This is not complete. According to stellar me ...
Biography of a Star - Max-Planck
... to react with the carbon, resulting in neutrons being released. The neutrons are captured by the iron particles that were present in the star in small quantities from the beginning, resulting in the formation of neutron-rich iron isotopes. If too many neutrons accumulate, radioactive beta decay occu ...
... to react with the carbon, resulting in neutrons being released. The neutrons are captured by the iron particles that were present in the star in small quantities from the beginning, resulting in the formation of neutron-rich iron isotopes. If too many neutrons accumulate, radioactive beta decay occu ...
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.