Galactic Encounters: The Dynamics of Mergers and Satellite Accretion
... galaxies merge, direct hits of stars are very unlikely. This shouldn’t be surprising, considering how small the fraction of the area filled by stars in a galaxy is. For the solar neighbourhood we typically have 20 stars/pc3 and the radius of each star is about 0.2Rsun on average. So the fractional a ...
... galaxies merge, direct hits of stars are very unlikely. This shouldn’t be surprising, considering how small the fraction of the area filled by stars in a galaxy is. For the solar neighbourhood we typically have 20 stars/pc3 and the radius of each star is about 0.2Rsun on average. So the fractional a ...
Observational Lower mass limit on stars
... luminosity, surface temperature and how a star ultimately will end its life. Indirectly knowing a star’s mass can determine the gravitational effects it has on nearby objects such as Earth. High mass stars which end their lives as extravagant explosive events are quit luminous and easy to observe. L ...
... luminosity, surface temperature and how a star ultimately will end its life. Indirectly knowing a star’s mass can determine the gravitational effects it has on nearby objects such as Earth. High mass stars which end their lives as extravagant explosive events are quit luminous and easy to observe. L ...
Section Three: Light and Matter
... first single slit is required only a double slit). The arrangement above is equivalent to two rocks being thrown into a lake, or when sound from two loudspeakers interferes. These two slits have circular waves leaving them because of the diffraction effect. Using the diagrams we can see how an inter ...
... first single slit is required only a double slit). The arrangement above is equivalent to two rocks being thrown into a lake, or when sound from two loudspeakers interferes. These two slits have circular waves leaving them because of the diffraction effect. Using the diagrams we can see how an inter ...
The First Stars in the Universe - Scientific American
... mentioned above showed the formation of clumps with masses of several hundred solar masses or more. Our group’s calculations suggest that the predicted masses of the first star-forming clumps are not very sensitive to the assumed cosmological conditions (for example, the exact nature of the initial ...
... mentioned above showed the formation of clumps with masses of several hundred solar masses or more. Our group’s calculations suggest that the predicted masses of the first star-forming clumps are not very sensitive to the assumed cosmological conditions (for example, the exact nature of the initial ...
EM wave in conductors (note11)
... ρf = ρf (0)e− ε t The free charge ρf (0) dissipates in a characteristic time τ = σε , similar to the static case in which the charge will flow out to the edge of the conductor. If the transient phase is excluded, ρf = 0 can be assumed in a conductor. For simplicity, we shall consider “good” conducto ...
... ρf = ρf (0)e− ε t The free charge ρf (0) dissipates in a characteristic time τ = σε , similar to the static case in which the charge will flow out to the edge of the conductor. If the transient phase is excluded, ρf = 0 can be assumed in a conductor. For simplicity, we shall consider “good” conducto ...
Neutron stars - Institut de Physique Nucleaire de Lyon
... Theory before the discovery T.E.Sterne (1933) – first model EOS (equation of state) of nuclear matter; prediction of the neutronization with increasing density. F.Zwicky [“On collapsed neutron stars,” Astrophys. J. 88 (1938) 522] – estimate of the maximum binding energy of a neutron star; – diffe ...
... Theory before the discovery T.E.Sterne (1933) – first model EOS (equation of state) of nuclear matter; prediction of the neutronization with increasing density. F.Zwicky [“On collapsed neutron stars,” Astrophys. J. 88 (1938) 522] – estimate of the maximum binding energy of a neutron star; – diffe ...
Gamma-ray absorption and pair echos at very high
... with notable differences out to z ∼ 8. However, the effects of further absorption from z > ∼ 8 may be practically indiscernible. Nevertheless, the spectral attenuation feature itself should be observable in high-z gammaray sources by current or future gamma-ray facilities, and possibly distinguishab ...
... with notable differences out to z ∼ 8. However, the effects of further absorption from z > ∼ 8 may be practically indiscernible. Nevertheless, the spectral attenuation feature itself should be observable in high-z gammaray sources by current or future gamma-ray facilities, and possibly distinguishab ...
THE MALAY COLLEGE KUALA KANGSAR INDIVIDUAL
... electronic systems. list and draw symbols for the ...
... electronic systems. list and draw symbols for the ...
A Direct Empirical Proof of the Existence of Dark Matter
... gas (too cool to be visible with Chandra and too dif fuse to have cooled into stars) extending from the cluster at the locations of the weak lensing peaks. To explain the measured surface mass density, such filaments would have to be several Megaparsecs long, very narrow, and oriented exactly along ...
... gas (too cool to be visible with Chandra and too dif fuse to have cooled into stars) extending from the cluster at the locations of the weak lensing peaks. To explain the measured surface mass density, such filaments would have to be several Megaparsecs long, very narrow, and oriented exactly along ...
–1– 28. HIGH-MASS STAR FORMATION: THEORY 28.1. The Effects
... mass range, however, which suggests that competitive accretion does not determine the IMF at lower masses either. Second, competitive accretion is effective only if the virial parameter is much less than observed, as discussed in Lecture 24. The most radical and imaginative model for the formation o ...
... mass range, however, which suggests that competitive accretion does not determine the IMF at lower masses either. Second, competitive accretion is effective only if the virial parameter is much less than observed, as discussed in Lecture 24. The most radical and imaginative model for the formation o ...
The X-ray/hard X-ray/gamma-ray connection of gamma
... On short timescales, this is governed by the accretion rate; this is large if the orbit is eccentric. Alternating systems are a natural consequence. ...
... On short timescales, this is governed by the accretion rate; this is large if the orbit is eccentric. Alternating systems are a natural consequence. ...
Response to Gary Hoge on Whether the Earth can be the Center of
... from the various masses in the system all cancel out, so that if a planet were located at ...
... from the various masses in the system all cancel out, so that if a planet were located at ...
Dark Stars: Dark Matter annihilation can power the first stars
... years with 800 M¤ stars: end up with a donut, i.e., big spherical halo of dark matter with hole in the middle • But, triaxial haloes have all kinds of orbits (box orbits, chaotic orbits) so that much more dark matter is in there. Dark stars can grow much bigger and make supermassive stars, 105-107 ...
... years with 800 M¤ stars: end up with a donut, i.e., big spherical halo of dark matter with hole in the middle • But, triaxial haloes have all kinds of orbits (box orbits, chaotic orbits) so that much more dark matter is in there. Dark stars can grow much bigger and make supermassive stars, 105-107 ...
Can stellar wobble in triple systems mimic a planet?
... 4.1. Planets in binary star systems There are presently around 15 planets detected in binary star systems (Eggenberger et al. 2004). One may wonder to what extent the companion of the target star hosting a planet is a binary system inducing a stellar wobble, imitating the effect of a planet. Since th ...
... 4.1. Planets in binary star systems There are presently around 15 planets detected in binary star systems (Eggenberger et al. 2004). One may wonder to what extent the companion of the target star hosting a planet is a binary system inducing a stellar wobble, imitating the effect of a planet. Since th ...
