ppt
... •Appearance Oscillation can be seen in tagged mode with low background Measure θ23 •More work needed to see if 2nd max can be seen sufficiently well to go beyond osc. to see solar interference CP violation Heirarchy effects. Energy close to Fermi motion limit— can one use C and p or only p? ...
... •Appearance Oscillation can be seen in tagged mode with low background Measure θ23 •More work needed to see if 2nd max can be seen sufficiently well to go beyond osc. to see solar interference CP violation Heirarchy effects. Energy close to Fermi motion limit— can one use C and p or only p? ...
Sakurai`s Object - Department of Physics, HKU
... • But sooner or later, the core helium will be used up, leaving a carbon-oxygen-rich core. ...
... • But sooner or later, the core helium will be used up, leaving a carbon-oxygen-rich core. ...
Star formation jeopardy
... gravitationally collapse, fragments,It heats up and spins faster. When the core temperature reaches 10 mill K, nuclear fusion begins (H into He). When outward pressure equals inward pressure the star enters the main sequence. ...
... gravitationally collapse, fragments,It heats up and spins faster. When the core temperature reaches 10 mill K, nuclear fusion begins (H into He). When outward pressure equals inward pressure the star enters the main sequence. ...
Stellar Evolution and the HR Diagram – Study Guide
... 10. Draw the evolutionary path of our Sun. Start by locating it’s present position on the graph and then indicate where it will be as it ages, and finally what part of the graph it ends in. It would start above Red Dwarfs, but below Giants; it would move down and left to the main sequence (where it ...
... 10. Draw the evolutionary path of our Sun. Start by locating it’s present position on the graph and then indicate where it will be as it ages, and finally what part of the graph it ends in. It would start above Red Dwarfs, but below Giants; it would move down and left to the main sequence (where it ...
Astrophysical explosions: from solar flares to cosmic gamma
... microseconds (or less!) to billions of years. Relevant densities range from nuclear densities of 1014 g cm−3 to the rarified gas between stars with scarcely one particle per cubic centimetre or 10−24 g cm−3 . Atomic, nuclear and plasma physics are all intimately involved. Turbulence and transport—of ...
... microseconds (or less!) to billions of years. Relevant densities range from nuclear densities of 1014 g cm−3 to the rarified gas between stars with scarcely one particle per cubic centimetre or 10−24 g cm−3 . Atomic, nuclear and plasma physics are all intimately involved. Turbulence and transport—of ...
Star Life Cycle Web Activity
... Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element can be used as fuel to burn and equilibriumis reached once again. Eventually the fuel ...
... Stars repeat a cycle of reaching equilibrium and then losing it after burning out one fuel source…then condensing (shrinking) because of gravity, making the core more dense and hotter…so hot that now a new element can be used as fuel to burn and equilibriumis reached once again. Eventually the fuel ...
Space Science cource, Department of Physics, Faculty of
... QuickTimeý Dz TIFFÅià• èkǻǵÅj êLí£ÉvÉçÉOÉâÉÄ Ç™Ç±ÇÃÉsÉNÉ`ÉÉǾå©ÇÈǞǽDžÇÕïKóvÇÇ• ÅB ...
... QuickTimeý Dz TIFFÅià• èkǻǵÅj êLí£ÉvÉçÉOÉâÉÄ Ç™Ç±ÇÃÉsÉNÉ`ÉÉǾå©ÇÈǞǽDžÇÕïKóvÇÇ• ÅB ...
Origin of the Elements and Atomic Structure
... which describes the system in terms of a wavefunction Ψ with energy E. •Explains wave/particle duality and quantized states of electrons in ...
... which describes the system in terms of a wavefunction Ψ with energy E. •Explains wave/particle duality and quantized states of electrons in ...
P-process nucleosynthesis in detonating white dwarfs in the light of
... shock wave is formed which rapidly transforms into a detonation due to the fast and energetic nuclear combustion developed at the rear edge of the shock wave. Soon a ChapmannJouguet self-sustained detonation emerged (see for instance Fig. 4 of GSBW). During its journey the substrate of the detonatio ...
... shock wave is formed which rapidly transforms into a detonation due to the fast and energetic nuclear combustion developed at the rear edge of the shock wave. Soon a ChapmannJouguet self-sustained detonation emerged (see for instance Fig. 4 of GSBW). During its journey the substrate of the detonatio ...
Gravity Defied From Potato Asteroids to Magnetised Neutron Stars
... star never reaches the temperature required to fuse the next element (low mass stars), or because it reaches the end of the fusion chain by producing Fe56 (for stars with M > 8 − 10 M ). When low mass stars stop burning their nuclear fuel, they typically go through a red-giant and a planetary nebul ...
... star never reaches the temperature required to fuse the next element (low mass stars), or because it reaches the end of the fusion chain by producing Fe56 (for stars with M > 8 − 10 M ). When low mass stars stop burning their nuclear fuel, they typically go through a red-giant and a planetary nebul ...
Due: January 14, 2014 Name: White dwarfs are “has been
... The energy radiated from a protostar comes from gravitational potential energy that is converted to kinetic and then thermal energy when the matter within the protostar falls toward the core. The energy radiated by a main-sequence star comes from nuclear fusion. ...
... The energy radiated from a protostar comes from gravitational potential energy that is converted to kinetic and then thermal energy when the matter within the protostar falls toward the core. The energy radiated by a main-sequence star comes from nuclear fusion. ...
Universal Gravitation Worksheet
... (2) A mass m is placed at the center of a thin, hollow, spherical shell of mass M and radius R. (diagram 1) (a) What gravitational force does the mass m experience? (b) What gravitational force does m exert on M? (c) A second mass m is now placed a distance 2R from the center of the shell. (Diagram ...
... (2) A mass m is placed at the center of a thin, hollow, spherical shell of mass M and radius R. (diagram 1) (a) What gravitational force does the mass m experience? (b) What gravitational force does m exert on M? (c) A second mass m is now placed a distance 2R from the center of the shell. (Diagram ...
solution
... I’ll describe three here: 1) One of the binary pair is greater than or about 25 M and undergoes a Type II supernova, resulting in a core remnant that is greater than about 3 M – it thus becomes a black hole; 2) the two stars are a red giant and either of a white dwarf or neutron star, the giant sw ...
... I’ll describe three here: 1) One of the binary pair is greater than or about 25 M and undergoes a Type II supernova, resulting in a core remnant that is greater than about 3 M – it thus becomes a black hole; 2) the two stars are a red giant and either of a white dwarf or neutron star, the giant sw ...
Exam 03
... 32. Determine which of the stars on the table is closest to the Earth, and which star is the farthest. A) Closest = Procyon and farthest = Deneb. B) Closest = Tau Ceti and farthest = Deneb. C) Closest = Deneb and farthest = Tau Ceti. D) Closest = Aldebaran and farthest = Tau Ceti. E) Closest = Spica ...
... 32. Determine which of the stars on the table is closest to the Earth, and which star is the farthest. A) Closest = Procyon and farthest = Deneb. B) Closest = Tau Ceti and farthest = Deneb. C) Closest = Deneb and farthest = Tau Ceti. D) Closest = Aldebaran and farthest = Tau Ceti. E) Closest = Spica ...
Stars - Moodle
... How is the Life cycle of a high mass different???? • Starts the same but burns faster and ends differently ...
... How is the Life cycle of a high mass different???? • Starts the same but burns faster and ends differently ...
NASA`s Chandra Sees Brightest Supernova Ever
... Interestingly, such large masses are consistent with the about 12.5 M⊙ nebula around η Carinae. the pair-instability models of Scannapieco et al. (2005) predict extremely long durations (100 days), slow expansion speeds of 5000 km s−1, and the presence of H in the spectrum, all of which are consis ...
... Interestingly, such large masses are consistent with the about 12.5 M⊙ nebula around η Carinae. the pair-instability models of Scannapieco et al. (2005) predict extremely long durations (100 days), slow expansion speeds of 5000 km s−1, and the presence of H in the spectrum, all of which are consis ...
PHY303 1 TURN OVER PHY303 Data Provided: A formula sheet
... prompt and delayed neutrons, chain reaction and fission fragments. (c) Consider neutrons of energy 0.1 eV incident on a piece of natural uranium. The cross section for fission of 235U at that energy is 250 barns. The amount of 235U in natural uranium is 0.72% and the density of uranium is 19 g cm3. ...
... prompt and delayed neutrons, chain reaction and fission fragments. (c) Consider neutrons of energy 0.1 eV incident on a piece of natural uranium. The cross section for fission of 235U at that energy is 250 barns. The amount of 235U in natural uranium is 0.72% and the density of uranium is 19 g cm3. ...
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.