Rotational spin-up in the 30-Myr
... According to WFI ETC, this range can be covered in a 300 sec single exposure. We will adopt the same observational strategy as we used for the h Per cluster, that allowed us to successfully measure rotational periods for nearly 600 of its low-mass members (Moraux et al. 2013). Namely, we will monito ...
... According to WFI ETC, this range can be covered in a 300 sec single exposure. We will adopt the same observational strategy as we used for the h Per cluster, that allowed us to successfully measure rotational periods for nearly 600 of its low-mass members (Moraux et al. 2013). Namely, we will monito ...
Astronomy Exam #2 for the 10
... and two of the four electrons are combined to form two neutrons that are found in the helium nucleus. The two neutrinos are sub-atomic particles with almost no mass that travel near light-speed and only weakly interact with matter. They are created with the two neutrons as a by-product of the fusion ...
... and two of the four electrons are combined to form two neutrons that are found in the helium nucleus. The two neutrinos are sub-atomic particles with almost no mass that travel near light-speed and only weakly interact with matter. They are created with the two neutrons as a by-product of the fusion ...
Neutron Degeneracy Pressure
... interaction. Solving these problems gave atomic physicists a closer approximation of the energy, for example, of non-Hydrogen like atoms. This idea of energy state filling becomes crucial when discussing degeneracy pressure. The Pauli Exclusion Principle can also be applied to further our understan ...
... interaction. Solving these problems gave atomic physicists a closer approximation of the energy, for example, of non-Hydrogen like atoms. This idea of energy state filling becomes crucial when discussing degeneracy pressure. The Pauli Exclusion Principle can also be applied to further our understan ...
Living alongside Monsters: Matter around Central Massive Black Holes Q. Daniel Wang
... • The mass-loaded hot gas undergoes outflows, affecting the global ecosystem of the galaxies. • We aim to understand the formation modes of massive stars and their interplay with the extreme environment in galactic nuclei. ...
... • The mass-loaded hot gas undergoes outflows, affecting the global ecosystem of the galaxies. • We aim to understand the formation modes of massive stars and their interplay with the extreme environment in galactic nuclei. ...
DOC file
... Shells: property of fragments (2-center shell model), favour fission channels; vanish with E*. Nuclide distribution: superposition of fission from different nuclei at different E*. ...
... Shells: property of fragments (2-center shell model), favour fission channels; vanish with E*. Nuclide distribution: superposition of fission from different nuclei at different E*. ...
transmutation of nuclides
... nuclide, because this nuclide no longer exists in the planet Earth. Studies of radioactive decays led to theories of nuclear stability and nuclear structure. Some of these theories will be examined as we take a closer look at atomic nuclei. Concepts such as energy states of nucleons, angular momentu ...
... nuclide, because this nuclide no longer exists in the planet Earth. Studies of radioactive decays led to theories of nuclear stability and nuclear structure. Some of these theories will be examined as we take a closer look at atomic nuclei. Concepts such as energy states of nucleons, angular momentu ...
Life Stages of High
... requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
... requires higher temperatures than hydrogen fusion—larger charge leads to greater repulsion Fusion of two helium nuclei doesn’t work, so helium fusion must combine three He nuclei to make carbon ...
Massive star formation in 100000 years from turbulent and
... where kB is Boltzmann’s constant and fgas is the fraction of the cloud’s mass that is in gas, as opposed to stars. They have power-law density profiles10 ρ ∝ r−kρ , with kρ ≃ 1.5 ± 0.5. Molecular clouds are observed to be inhomogeneous on a wide range of scales, and numerical simulations show that t ...
... where kB is Boltzmann’s constant and fgas is the fraction of the cloud’s mass that is in gas, as opposed to stars. They have power-law density profiles10 ρ ∝ r−kρ , with kρ ≃ 1.5 ± 0.5. Molecular clouds are observed to be inhomogeneous on a wide range of scales, and numerical simulations show that t ...
Good Vibrations and Stellar Pulsations - Physics
... diminishing it during expansion. That is the first alternative we considered. But it would come to the same thing if we varied the leak, stopping the leak during compression and increasing it during expansion. To apply this method we must make the star more heat-tight when compressed than when expan ...
... diminishing it during expansion. That is the first alternative we considered. But it would come to the same thing if we varied the leak, stopping the leak during compression and increasing it during expansion. To apply this method we must make the star more heat-tight when compressed than when expan ...
Stellar Evolution 1
... into Helium in core of a star? 6. As a result of the increase in the rate of nuclear energy generation, what happens to the Luminosity a) It increases b) It remains the same (until the pressure outside the core builds up enough to make the surrounding envelope expand which reduces the insulation and ...
... into Helium in core of a star? 6. As a result of the increase in the rate of nuclear energy generation, what happens to the Luminosity a) It increases b) It remains the same (until the pressure outside the core builds up enough to make the surrounding envelope expand which reduces the insulation and ...
Stars part 2
... Stellar Formation and Life Cycle Stars are theorized to evolve through six stages of development… 1. Protostar Stage – the gravitational collapse of a gaseous cloud mass. • The collapse may be triggered by the passing of, the eruption of, or the explosion of a near-by star. • Energy production is d ...
... Stellar Formation and Life Cycle Stars are theorized to evolve through six stages of development… 1. Protostar Stage – the gravitational collapse of a gaseous cloud mass. • The collapse may be triggered by the passing of, the eruption of, or the explosion of a near-by star. • Energy production is d ...
Dark Matter in the Milky Way - how to find it using Gaia and other
... The only way we’ve detected dark matter is through it’s gravitational effects We can find the dark matter density by finding the gravitational potential (and subtracting off the baryonic bit) ...
... The only way we’ve detected dark matter is through it’s gravitational effects We can find the dark matter density by finding the gravitational potential (and subtracting off the baryonic bit) ...
Neutron Stars, Pulsars, Magnetars – the “corpses” of medium
... Credit: NASA, ESA, Spacetelescope.org ...
... Credit: NASA, ESA, Spacetelescope.org ...
A Simple Model for r-Process Scatter and Halo Evolution
... 3. The placement of a star between these extremes quantifies a admixture of nucleosynthesis sources recorded in the star. Thus, (a) at the very earliest times, when single SN events are really all that contaminate a given star, the r/Fe scatter should only populate the extremes. (b) At later times, ...
... 3. The placement of a star between these extremes quantifies a admixture of nucleosynthesis sources recorded in the star. Thus, (a) at the very earliest times, when single SN events are really all that contaminate a given star, the r/Fe scatter should only populate the extremes. (b) At later times, ...
Higgs Portal VDM and Indirect Signature
... • The previous symmetry can be identified as the lepton number. • It can also serve as the source for type-I seesaw mechanism. • If it is only associated with one generation of leptons, DM then decays solely to that generation lepton pair. ...
... • The previous symmetry can be identified as the lepton number. • It can also serve as the source for type-I seesaw mechanism. • If it is only associated with one generation of leptons, DM then decays solely to that generation lepton pair. ...
Dark Matter in the Universe:
... Most (> 90%) of this mass is in the Dark Halo of the Galaxy, which extends out over 500,000 light-years from the center of the Galaxy -much further than the visible disk ...
... Most (> 90%) of this mass is in the Dark Halo of the Galaxy, which extends out over 500,000 light-years from the center of the Galaxy -much further than the visible disk ...
Omega Centauri
... These anticorrelations are present in Carretta et al. 2010 all clusters analyzed so far. ...
... These anticorrelations are present in Carretta et al. 2010 all clusters analyzed so far. ...
Medical Physics #2
... Positrons are produced by Beta decay - in order to gain a more stable ratio of protons to neutrons in the nucleus. Positrons are found when a proton disintegrates to form a neutron and a positron. E.g. Decay of Carbon-11 to Boron-11: ...
... Positrons are produced by Beta decay - in order to gain a more stable ratio of protons to neutrons in the nucleus. Positrons are found when a proton disintegrates to form a neutron and a positron. E.g. Decay of Carbon-11 to Boron-11: ...
Equations of State for White Dwarfs Elena Heikkilä Kandidaatin
... White dwarfs are classified as compact objects, meaning that their life begins when a star dies. Star death is a point where the most of its nuclear fuel has been consumed. Like other compact objects such as black holes and neutron stars, white dwarfs have small radii, relatively large mass (in comp ...
... White dwarfs are classified as compact objects, meaning that their life begins when a star dies. Star death is a point where the most of its nuclear fuel has been consumed. Like other compact objects such as black holes and neutron stars, white dwarfs have small radii, relatively large mass (in comp ...
Radioactive Decays – transmutations of nuclides
... nuclide, because this nuclide no longer exists in the planet Earth. Studies of radioactive decays led to theories of nuclear stability and nuclear structure. Some of these theories will be examined as we take a closer look at atomic nuclei. Concepts such as energy states of nucleons, angular momentu ...
... nuclide, because this nuclide no longer exists in the planet Earth. Studies of radioactive decays led to theories of nuclear stability and nuclear structure. Some of these theories will be examined as we take a closer look at atomic nuclei. Concepts such as energy states of nucleons, angular momentu ...
1) P - UCSD Physics
... Which requires the most work, to move a positive charge from P to points 1, 2, 3 or 4 ? All points are the same distance from P. ...
... Which requires the most work, to move a positive charge from P to points 1, 2, 3 or 4 ? All points are the same distance from P. ...
Cos. Won edu 2 - Adler Planetarium
... stars are much smaller and may last trillions of years. Throughout their lifespan, stars create energy by converting hydrogen to helium through the process of nuclear fusion in their cores. This process of fusion generates energy and heat, which in turn produce pressure within the star that pushes o ...
... stars are much smaller and may last trillions of years. Throughout their lifespan, stars create energy by converting hydrogen to helium through the process of nuclear fusion in their cores. This process of fusion generates energy and heat, which in turn produce pressure within the star that pushes o ...
Insights into thermonuclear supernovae from the incomplete Si
... method of Wagoner with adaptive time steps. The iterative procedure ends when the relative variation in the molar abundances is smaller than 10−6 , taking only those nuclei with molar abundance Y > 10−14 mol g−1 into account. The number of iterations is limited to 7, and if this limit is reached a n ...
... method of Wagoner with adaptive time steps. The iterative procedure ends when the relative variation in the molar abundances is smaller than 10−6 , taking only those nuclei with molar abundance Y > 10−14 mol g−1 into account. The number of iterations is limited to 7, and if this limit is reached a n ...
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.