ppt
... Massive stars (M > 8 solar masses) will complete all their stages of evolution and then collapse to a black hole or neutron star. They expel nearly all of their core energy (resulting from gravity) by emitting 1057 (1053 ergs of) neutrinos in ~10 seconds. ...
... Massive stars (M > 8 solar masses) will complete all their stages of evolution and then collapse to a black hole or neutron star. They expel nearly all of their core energy (resulting from gravity) by emitting 1057 (1053 ergs of) neutrinos in ~10 seconds. ...
Comparison of atmospheric neutrino flux calculations at low energies
... with a low normalization relative to which there is an excess of electrons could also be consistent with an interpretation in terms of a neutron-induced background masquerading as interactions of n e @10#. Of the four calculations we consider, three are completely independent of one another. The ind ...
... with a low normalization relative to which there is an excess of electrons could also be consistent with an interpretation in terms of a neutron-induced background masquerading as interactions of n e @10#. Of the four calculations we consider, three are completely independent of one another. The ind ...
PowerPoint Presentation - Isolated Neutron Stars, solid crust
... emission from neutron stars and to search for features in their spectrum. Isolated neutron stars play a key role in compact objects astrophysics: these are the only sources in which we can see directly the surface of the compact star. ...
... emission from neutron stars and to search for features in their spectrum. Isolated neutron stars play a key role in compact objects astrophysics: these are the only sources in which we can see directly the surface of the compact star. ...
Chapter17.2
... end in supernova explosions. • Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs. • Intermediate-mass stars can make elements heavier than carbon but end as white dwarfs. © 2010 Pearson Education, Inc. ...
... end in supernova explosions. • Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as white dwarfs. • Intermediate-mass stars can make elements heavier than carbon but end as white dwarfs. © 2010 Pearson Education, Inc. ...
White dwarfs from GAIA: The 7th dimension
... There is a plethora of other science that will come out of the GAIA WD sample: constraints on the existence of WIMPS and alternative theories of gravitation, identify remnant planetary systems, probe the physics of dense plasmas, understand the origin of strongly magnetic white dwarfs... ...
... There is a plethora of other science that will come out of the GAIA WD sample: constraints on the existence of WIMPS and alternative theories of gravitation, identify remnant planetary systems, probe the physics of dense plasmas, understand the origin of strongly magnetic white dwarfs... ...
Resolved SPs : simulations
... (evaluate crowding conditions: if there is more than 1 star per resolution element the photometry is bad; crowding condition depends on sampled luminosity, size of the resolution element and star’s magnitude) ...
... (evaluate crowding conditions: if there is more than 1 star per resolution element the photometry is bad; crowding condition depends on sampled luminosity, size of the resolution element and star’s magnitude) ...
Experimental and numerical study of modulation of ionization front propagation velocity in ?s helium plasma gun discharge with nitrogen admixture
... The key role of penning reaction on the discharge features has been checked from model calculations, as presented in figure 6, comparing electron density patterns with or without accounting for penning reactions in the model kinetic scheme. When penning reactions are artificially suppressed, the pla ...
... The key role of penning reaction on the discharge features has been checked from model calculations, as presented in figure 6, comparing electron density patterns with or without accounting for penning reactions in the model kinetic scheme. When penning reactions are artificially suppressed, the pla ...
Presentation in PDF format.
... A reaction i(j,k)l destroys species i and j, and creates species k,l at a rate rij. The rate of change of abundance of species i will then be given (in mass fraction) by dxi/dt = - (1+δij) rij / NA Where the bracket allows for more than one particle of species I being destroyed in a reaction. Thus f ...
... A reaction i(j,k)l destroys species i and j, and creates species k,l at a rate rij. The rate of change of abundance of species i will then be given (in mass fraction) by dxi/dt = - (1+δij) rij / NA Where the bracket allows for more than one particle of species I being destroyed in a reaction. Thus f ...
ISOCAM 4 m imaging of the nuclear starburst in M83
... the mechanism that governs the magnitude of the burst in the central regions of galaxies and the way it may propagate, are important issues because they relate to the more general questions of the origin of the AGNs and their occurence since Sanders et al.(1988) proposed that the most important star ...
... the mechanism that governs the magnitude of the burst in the central regions of galaxies and the way it may propagate, are important issues because they relate to the more general questions of the origin of the AGNs and their occurence since Sanders et al.(1988) proposed that the most important star ...
Evolution of supermassive stars as a pathway to black hole formation
... Supermassive stars, with masses & 106 M⊙ , are possible progenitors of supermassive black holes in galactic nuclei. Because of their short nuclear burning timescales, such objects can be formed only when matter is able to accumulate at a rate exceeding ∼ 1M⊙ yr−1 . Here we revisit the structure and ...
... Supermassive stars, with masses & 106 M⊙ , are possible progenitors of supermassive black holes in galactic nuclei. Because of their short nuclear burning timescales, such objects can be formed only when matter is able to accumulate at a rate exceeding ∼ 1M⊙ yr−1 . Here we revisit the structure and ...
30.4 Gravitational collapse & early protostellar evolution I (HB)
... Mass-radius relation - Initial size unknown, but that does not matter since it quickly converges. - Adding additional infalling mass shells, the protostar can be described by its entropy profile s(Mr), reflecting the changing conditions at the accretion shock. - Since s represents heat content of e ...
... Mass-radius relation - Initial size unknown, but that does not matter since it quickly converges. - Adding additional infalling mass shells, the protostar can be described by its entropy profile s(Mr), reflecting the changing conditions at the accretion shock. - Since s represents heat content of e ...
Massive star evolution: luminous blue variables as unexpected
... rare LBV phase in many aspects, such as spectral appearance, proximity to the Eddington limit, and chemical abundances at the surface. One may wonder why the rotating model explodes as an LBV, while the corresponding non-rotating model 20 M does not evolve back to the blue and explodes as a RSG, sh ...
... rare LBV phase in many aspects, such as spectral appearance, proximity to the Eddington limit, and chemical abundances at the surface. One may wonder why the rotating model explodes as an LBV, while the corresponding non-rotating model 20 M does not evolve back to the blue and explodes as a RSG, sh ...
Diffuse TeV Emission from the Galactic Center
... Flares occur on average once per day Average L ~ 1035 ergs s-1, but last for a few thousand seconds. The constant luminosity of IGR J17456-2901 cannot result from successive flares ...
... Flares occur on average once per day Average L ~ 1035 ergs s-1, but last for a few thousand seconds. The constant luminosity of IGR J17456-2901 cannot result from successive flares ...
Document
... Inner vs. Outer Abundance Results There is a larger dispersion for outer halo abundances. ...
... Inner vs. Outer Abundance Results There is a larger dispersion for outer halo abundances. ...
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.