1 - Piscataway High School
... of the gas would weigh more than an automobile. In this degenerate matter, the pressure does not depend on temperature, and that means the pressure–temperature thermostat does not regulate energy production. When the temperature becomes hot enough, helium fusion begins to make energy, and the temper ...
... of the gas would weigh more than an automobile. In this degenerate matter, the pressure does not depend on temperature, and that means the pressure–temperature thermostat does not regulate energy production. When the temperature becomes hot enough, helium fusion begins to make energy, and the temper ...
Neutrino Physics and Astrophysics with SuperKamiokande Jordan A
... Can we detect them? In 1934 Bethe & Peierls calculated the cross section for neutrino interaction of 10-44 cm2. Nature (London) 133, 532(1934) “It is therefore absolutely impossible to observe processes of this kind with neutrinos created in nuclear transformations” “… one can conclude that t ...
... Can we detect them? In 1934 Bethe & Peierls calculated the cross section for neutrino interaction of 10-44 cm2. Nature (London) 133, 532(1934) “It is therefore absolutely impossible to observe processes of this kind with neutrinos created in nuclear transformations” “… one can conclude that t ...
The Aurora
... EXPERIMENTS - IMAGE Imager for Magnetopause-to-Aurora Global Exploration Launch: 25 March 2000 ...
... EXPERIMENTS - IMAGE Imager for Magnetopause-to-Aurora Global Exploration Launch: 25 March 2000 ...
Stellar Population Modeling of Galaxies in Nearby Groups
... measurements of star formation rate (SFR) as a function of age and metallicity using multi-color photometry of the resolved stars in the galaxy. Simultaneous metallicity determination gives us chemical enrichment in the process of the galaxy evolution. Relatively simple systems (for example, globula ...
... measurements of star formation rate (SFR) as a function of age and metallicity using multi-color photometry of the resolved stars in the galaxy. Simultaneous metallicity determination gives us chemical enrichment in the process of the galaxy evolution. Relatively simple systems (for example, globula ...
Electric Field Driven Torque in ATP Synthase Miller, J.H., Jr
... Figure 2 shows cross-sections of the resulting equipotential surfaces (black lines) and tangential electric field components (red arrows), superimposed on an idealized cross section of the c-ring (yellow) and a-subunit (green). The proton channel cross sections in the a-subunit are colored to depict ...
... Figure 2 shows cross-sections of the resulting equipotential surfaces (black lines) and tangential electric field components (red arrows), superimposed on an idealized cross section of the c-ring (yellow) and a-subunit (green). The proton channel cross sections in the a-subunit are colored to depict ...
Analysis of white dwarfs with strange-matter cores
... Indeed, in [24] it was concluded that an iron core might be required to provide the required compactness as illustrated in figure 1. On the other hand, other stars (e.g., Sirius B, Procyon B and 40 Eri B) fall nicely along the normal white-dwarf mass–radius relation. Hence, there is a hint of eviden ...
... Indeed, in [24] it was concluded that an iron core might be required to provide the required compactness as illustrated in figure 1. On the other hand, other stars (e.g., Sirius B, Procyon B and 40 Eri B) fall nicely along the normal white-dwarf mass–radius relation. Hence, there is a hint of eviden ...
MACHOs
... the two values is due to dark matter 99% of matter in the galaxy is dark matter 1 – study how certain stars are moving around an intense source of radio emission really far away we’re 25,000 light years away from radio emission 1. Calculate velocity with which stars are moving o take coordinat ...
... the two values is due to dark matter 99% of matter in the galaxy is dark matter 1 – study how certain stars are moving around an intense source of radio emission really far away we’re 25,000 light years away from radio emission 1. Calculate velocity with which stars are moving o take coordinat ...
Head-On Collision of Neutron Stars As A Thought Experiment
... energy. The configuration is not in equilibrium following the passage of the initial recoil shocks, but undergoes oscillations, damped by acoustic (viscous) dissipation and gravitational radiation reaction forces. Only a small fraction of the total rest mass escapes from the system and an even small ...
... energy. The configuration is not in equilibrium following the passage of the initial recoil shocks, but undergoes oscillations, damped by acoustic (viscous) dissipation and gravitational radiation reaction forces. Only a small fraction of the total rest mass escapes from the system and an even small ...
The Celestial Origin of Atoms
... neutron star very compact star composed mainly of neutrons nucleon proton or neutron nucleosynthesis production of atomic nuclei in the Universe quintessence substrate exerting a gravitational repulsion scalar field a non-directional type of field required in cosmology and particle physics supernova s ...
... neutron star very compact star composed mainly of neutrons nucleon proton or neutron nucleosynthesis production of atomic nuclei in the Universe quintessence substrate exerting a gravitational repulsion scalar field a non-directional type of field required in cosmology and particle physics supernova s ...
The Etherino and/or the Neutrino Hypothesis
... general belief that this is due to the very low value of the cross section between neutrinos and other particles casts shadows on the theory rather than resolving the conceptual uneasiness here considered. (2) The fundamental reaction for the production of the (electron) neutrino, Eq. (1.2), violate ...
... general belief that this is due to the very low value of the cross section between neutrinos and other particles casts shadows on the theory rather than resolving the conceptual uneasiness here considered. (2) The fundamental reaction for the production of the (electron) neutrino, Eq. (1.2), violate ...
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... move faster as they are squeezed into a very small space. • As a white dwarf's mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar lim ...
... move faster as they are squeezed into a very small space. • As a white dwarf's mass approaches 1.4MSun, its electrons must move at nearly the speed of light. • Because nothing can move faster than light, a white dwarf cannot be more massive than 1.4MSun, the white dwarf limit (or Chandrasekhar lim ...
protostellar disks under the influence of winds and uv radiation
... radiation. The central stars themselves can have a stellar wind and may produce sufficient UV and X-ray to ultimately destroy their surrounding disks. Here we describe the results of numerical simulations of the influence that an external UV source and a central star’s wind can have on its circumste ...
... radiation. The central stars themselves can have a stellar wind and may produce sufficient UV and X-ray to ultimately destroy their surrounding disks. Here we describe the results of numerical simulations of the influence that an external UV source and a central star’s wind can have on its circumste ...
Numerical Evolu4on of Soliton Stars
... fields. These par.cles could clump together by a Jeans instability mechanism to form stars called soliton stars. • There are also scalar par.cles that can be described by complex scalar fields (also possible dark maPer candidates) that could form stars by the same mechanism. Such hypothe.cal st ...
... fields. These par.cles could clump together by a Jeans instability mechanism to form stars called soliton stars. • There are also scalar par.cles that can be described by complex scalar fields (also possible dark maPer candidates) that could form stars by the same mechanism. Such hypothe.cal st ...
Nuclear structure and excitations by large
... Level density in nuclear shellmodel calc. • Level density ⇒ count the number of eigenvalues of huge sparse matrix in a certain energy region • Lanczos method for highly-excited states ⇒ difficult due to slow convergence, ...
... Level density in nuclear shellmodel calc. • Level density ⇒ count the number of eigenvalues of huge sparse matrix in a certain energy region • Lanczos method for highly-excited states ⇒ difficult due to slow convergence, ...
The Deaths of Very Massive Stars
... degeneracy linger, however, on up to at least 30 M⊙ at oxygen ignition, and to still heavier masses for silicon burning. Even at 80 M⊙ , the center of a massive star has become degenerate by silicon depletion. Were the core fully degenerate and composed of nuclei with equal numbers of neutrons and p ...
... degeneracy linger, however, on up to at least 30 M⊙ at oxygen ignition, and to still heavier masses for silicon burning. Even at 80 M⊙ , the center of a massive star has become degenerate by silicon depletion. Were the core fully degenerate and composed of nuclei with equal numbers of neutrons and p ...
Asteroseismic constraints on Asymmetric Dark Matter: Light particles
... present solar fraction of the number of trapped DM particles in the ADM scenario relative to the WIMP picture. The number of ADM particles trapped inside the Sun is greater than that of WIMPs by a factor of a few for hσA vi ∼ 10−33 cm3 /s and by 104 relative to the natural scale of annihilation for ...
... present solar fraction of the number of trapped DM particles in the ADM scenario relative to the WIMP picture. The number of ADM particles trapped inside the Sun is greater than that of WIMPs by a factor of a few for hσA vi ∼ 10−33 cm3 /s and by 104 relative to the natural scale of annihilation for ...
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.