Asteroseismic constraints on Asymmetric Dark Matter: Light particles
... eigenfrequency, the different ratios used could in principle be correlated. However, by generating samples of the ratios through the sampling of the observed normally distributed eigenfrequencies, we found that in general the correlation is very small, bellow 0.01. Besides r02 , [49] proposed two ot ...
... eigenfrequency, the different ratios used could in principle be correlated. However, by generating samples of the ratios through the sampling of the observed normally distributed eigenfrequencies, we found that in general the correlation is very small, bellow 0.01. Besides r02 , [49] proposed two ot ...
The Stars education kit - Student activities 11-20
... After the Sun’s core has been completely converted from hydrogen to helium, nuclear fusion reactions will end and the Sun will begin to contract gravitationally, causing the pressure and temperature inside the core to rise. Heat generated by the collapsing core will also spread to the Sun’s other in ...
... After the Sun’s core has been completely converted from hydrogen to helium, nuclear fusion reactions will end and the Sun will begin to contract gravitationally, causing the pressure and temperature inside the core to rise. Heat generated by the collapsing core will also spread to the Sun’s other in ...
Dust in Space - Max-Planck
... quasars flared up. In principle, only supernovas – exploding stars – could be considered candidates here. According to model-based calculations, each supernova would have to deliver around one solar mass of dust in order to explain the quantities that have been observed in the quasars. At the confer ...
... quasars flared up. In principle, only supernovas – exploding stars – could be considered candidates here. According to model-based calculations, each supernova would have to deliver around one solar mass of dust in order to explain the quantities that have been observed in the quasars. At the confer ...
Astro Physics Notes and Study Guide 2015-17
... from fusion reactions is absorbed by atoms throughout the Sun (high KE equals high temperature). This high temperature due to the energetic motion of the atoms of the Sun is able to support it from collapsing due to its massive gravitational. ...
... from fusion reactions is absorbed by atoms throughout the Sun (high KE equals high temperature). This high temperature due to the energetic motion of the atoms of the Sun is able to support it from collapsing due to its massive gravitational. ...
Dark Matter Search
... Rapidly spinning stellar GBM BGO core collapse supernova, with relativistic jets that can produce long GRBs LAT (>1MeV) 31 GeV 0.83 s Constraints on the quantum gravity mass scale (MQG) by direct measurement of photon arrival times, testing Lorentz Compact Merger: Two neutron invariance violation. s ...
... Rapidly spinning stellar GBM BGO core collapse supernova, with relativistic jets that can produce long GRBs LAT (>1MeV) 31 GeV 0.83 s Constraints on the quantum gravity mass scale (MQG) by direct measurement of photon arrival times, testing Lorentz Compact Merger: Two neutron invariance violation. s ...
First Light Sources at the End of the Dark Ages: Direct
... emission detectable by large ground-based telescopes, and possibly a rest-frame ultraviolet continuum observable from the ground and/or with the JWST. By 2016, the JWST and/or ground-based surveys will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and prot ...
... emission detectable by large ground-based telescopes, and possibly a rest-frame ultraviolet continuum observable from the ground and/or with the JWST. By 2016, the JWST and/or ground-based surveys will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and prot ...
The ANTARES telescope turns its gaze to the sky
... in a large instrumented volume of water or ice. These upward going muons result from the interaction of neutrino-muons with the Earth's crust. The typical path of a high energy muon in the rock is a few kilometres so that even a relatively modest sensitive volume (100 m being a typical scale) can in ...
... in a large instrumented volume of water or ice. These upward going muons result from the interaction of neutrino-muons with the Earth's crust. The typical path of a high energy muon in the rock is a few kilometres so that even a relatively modest sensitive volume (100 m being a typical scale) can in ...
Lecture 4
... • Warmest observed stars are low-massive; their neutrino luminosity <= 0.01 of modified Urca • Coldest observed stars are more massive; their neutrino luminosity >= 100 of modified Urca ...
... • Warmest observed stars are low-massive; their neutrino luminosity <= 0.01 of modified Urca • Coldest observed stars are more massive; their neutrino luminosity >= 100 of modified Urca ...
Chapter 15, Galaxies
... Because the mass of white dwarfs when they explode as supernovae is always around 1.0 M⊙, its luminosity is very consistent, and can be used as a standard candle for the measurement of distance to distant galaxies (Chapter 15). The amount of energy produced by white dwarf supernovae and massive star ...
... Because the mass of white dwarfs when they explode as supernovae is always around 1.0 M⊙, its luminosity is very consistent, and can be used as a standard candle for the measurement of distance to distant galaxies (Chapter 15). The amount of energy produced by white dwarf supernovae and massive star ...
Astronomy 114 – Summary of Important Concepts #2 1 Stars: key
... wavelength due to the motion of the source. v is the velocity with which the source is moving with respect to the observer and c is the velocity of light. v can be either positive or negative. A positive value of v corresponds to a source which is moving away from the observer. Negative values of v ...
... wavelength due to the motion of the source. v is the velocity with which the source is moving with respect to the observer and c is the velocity of light. v can be either positive or negative. A positive value of v corresponds to a source which is moving away from the observer. Negative values of v ...
Earth in Space - Learning Outcomes
... A dense star with a sufficiently large mass/small radius could have an escape velocity greater than 3 x 108 m s-1. This means that light emitted from its surface could not escape - hence the name black hole. The physics of the black hole cannot be explained using Newton’s Theory. The correct theory ...
... A dense star with a sufficiently large mass/small radius could have an escape velocity greater than 3 x 108 m s-1. This means that light emitted from its surface could not escape - hence the name black hole. The physics of the black hole cannot be explained using Newton’s Theory. The correct theory ...
The Life of a Star
... of rotation and magnetic elds) and hydrostatic equilibrium. Under these assumptions a star can be described by the run of four structure variables { r, T , P , Lr { with the Lagrangian coordinate m. We will derive the corresponding four partial dierential equations. From the discussion of those se ...
... of rotation and magnetic elds) and hydrostatic equilibrium. Under these assumptions a star can be described by the run of four structure variables { r, T , P , Lr { with the Lagrangian coordinate m. We will derive the corresponding four partial dierential equations. From the discussion of those se ...
Physics case for Antares+
... in ”hidden” regions where the particle accelerators could be located. This concerns, first of all, the regions associated with compact objects - black holes, pulsars, the initial epochs of supernovae explosions, etc. The penetrating potential of neutrinos is important not only for extremely dense en ...
... in ”hidden” regions where the particle accelerators could be located. This concerns, first of all, the regions associated with compact objects - black holes, pulsars, the initial epochs of supernovae explosions, etc. The penetrating potential of neutrinos is important not only for extremely dense en ...
Research proposal uploaded for ESO fellowship
... might be common place at high-redshift (e.g. Shapiro et al. 2009). If these outflows are big enough to compensate for gas accretion onto the galaxy, they could be sufficient to quench star formation. This would imply that supernova driven outflows play an important role in the transition from active ...
... might be common place at high-redshift (e.g. Shapiro et al. 2009). If these outflows are big enough to compensate for gas accretion onto the galaxy, they could be sufficient to quench star formation. This would imply that supernova driven outflows play an important role in the transition from active ...
The Sun Groove– Kyle Chismar (Phys133
... the form of randomly bouncing photons. © 2015 Pearson Education, Inc. ...
... the form of randomly bouncing photons. © 2015 Pearson Education, Inc. ...
Chapter 3 Cosmology 3.1 The Doppler effect
... 2 The luminosity method: type Ia supernovae at peak intensity are known to be 109 times more luminous than the Sun, corresponding to an absolute magnitude of about −18. As you saw in Topic 2.4, type Ia supernovae are distinguished from other types of supernovae by the presence of strong silicon abso ...
... 2 The luminosity method: type Ia supernovae at peak intensity are known to be 109 times more luminous than the Sun, corresponding to an absolute magnitude of about −18. As you saw in Topic 2.4, type Ia supernovae are distinguished from other types of supernovae by the presence of strong silicon abso ...
Solutions for Midterm
... star of radius R* separated by a distance d. Assume that both objects radiate as uniform blackbodies at these temperatures, and that the planet reflects a fraction A of the incident radiation back ...
... star of radius R* separated by a distance d. Assume that both objects radiate as uniform blackbodies at these temperatures, and that the planet reflects a fraction A of the incident radiation back ...
12. Nuclear Reactions in Nature
... production of the massive particles and the hadronic matter condensed into a gas of nucleons and mesons. At this point, the Universe consisted of nucleons, mesons, neutrinos (and antineutrinos), photons, ...
... production of the massive particles and the hadronic matter condensed into a gas of nucleons and mesons. At this point, the Universe consisted of nucleons, mesons, neutrinos (and antineutrinos), photons, ...
Type II supernova
A Type II supernova (plural: supernovae or supernovas) results from the rapid collapse and violent explosion of a massive star. A star must have at least 8 times, and no more than 40–50 times, the mass of the Sun (M☉) for this type of explosion. It is distinguished from other types of supernovae by the presence of hydrogen in its spectrum. Type II supernovae are mainly observed in the spiral arms of galaxies and in H II regions, but not in elliptical galaxies.Stars generate energy by the nuclear fusion of elements. Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans. The degeneracy pressure of electrons and the energy generated by these fusion reactions are sufficient to counter the force of gravity and prevent the star from collapsing, maintaining stellar equilibrium. The star fuses increasingly higher mass elements, starting with hydrogen and then helium, progressing up through the periodic table until a core of iron and nickel is produced. Fusion of iron or nickel produces no net energy output, so no further fusion can take place, leaving the nickel-iron core inert. Due to the lack of energy output allowing outward pressure, equilibrium is broken.When the mass of the inert core exceeds the Chandrasekhar limit of about 1.4 M☉, electron degeneracy alone is no longer sufficient to counter gravity and maintain stellar equilibrium. A cataclysmic implosion takes place within seconds, in which the outer core reaches an inward velocity of up to 23% of the speed of light and the inner core reaches temperatures of up to 100 billion kelvin. Neutrons and neutrinos are formed via reversed beta-decay, releasing about 1046 joules (100 foes) in a ten-second burst. The collapse is halted by neutron degeneracy, causing the implosion to rebound and bounce outward. The energy of this expanding shock wave is sufficient to accelerate the surrounding stellar material to escape velocity, forming a supernova explosion, while the shock wave and extremely high temperature and pressure briefly allow for theproduction of elements heavier than iron. Depending on initial size of the star, the remnants of the core form a neutron star or a black hole. Because of the underlying mechanism, the resulting nova is also described as a core-collapse supernova.There exist several categories of Type II supernova explosions, which are categorized based on the resulting light curve—a graph of luminosity versus time—following the explosion. Type II-L supernovae show a steady (linear) decline of the light curve following the explosion, whereas Type II-P display a period of slower decline (a plateau) in their light curve followed by a normal decay. Type Ib and Ic supernovae are a type of core-collapse supernova for a massive star that has shed its outer envelope of hydrogen and (for Type Ic) helium. As a result, they appear to be lacking in these elements.