Nuclear Reactions and Superfluid Time Dependent Density
... theorem proves that if two N -fermion systems evolve from the same initial state, but are subject to two different time-dependent potentials, their respective time-dependent densities will be different [29]. There is however an important problem which troubled TDDFT over many years and is related to t ...
... theorem proves that if two N -fermion systems evolve from the same initial state, but are subject to two different time-dependent potentials, their respective time-dependent densities will be different [29]. There is however an important problem which troubled TDDFT over many years and is related to t ...
Stellar Spectra Classification
... Included in this activity is a table of simulated stellar spectra on page 5. Your first task is to sort the spectra by creating a classification scheme. As with real stellar spectra, you will never find two exactly the same. The thickness of each line represents how much light is received at a parti ...
... Included in this activity is a table of simulated stellar spectra on page 5. Your first task is to sort the spectra by creating a classification scheme. As with real stellar spectra, you will never find two exactly the same. The thickness of each line represents how much light is received at a parti ...
The Sun
... The Sun’s Life Cycle • What happens during a star’s life cycle depends on its mass. – It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. – When the hydrogen in its core is gone, a star has a helium center and outer layers made ...
... The Sun’s Life Cycle • What happens during a star’s life cycle depends on its mass. – It takes about 10 billion years for a star with the mass of the Sun to convert all of the hydrogen in its core into helium. – When the hydrogen in its core is gone, a star has a helium center and outer layers made ...
the holifield radioactive ion beam facility at the oak ridge
... sections of the machine, changing the SF6 insulating gas pressure, or suffering catastrophic transmission losses. Experiments with 16O indicate that the transmission losses at 1 MV are only factors of two lower than those for 25-MV terminal operation. Further improvements in transmission efficiency ...
... sections of the machine, changing the SF6 insulating gas pressure, or suffering catastrophic transmission losses. Experiments with 16O indicate that the transmission losses at 1 MV are only factors of two lower than those for 25-MV terminal operation. Further improvements in transmission efficiency ...
Time evolution of the particle distribution function in a high
... colliding particles. For proton-proton collisions there are not only the Coulomb forces but also the nuclear forces, which become important once kT> 1 MeV. The total cross section of elastic proton-proton scattering in the energy interval 10-300 MeV can be well approximated in the form7 o,,N=o,,N=10 ...
... colliding particles. For proton-proton collisions there are not only the Coulomb forces but also the nuclear forces, which become important once kT> 1 MeV. The total cross section of elastic proton-proton scattering in the energy interval 10-300 MeV can be well approximated in the form7 o,,N=o,,N=10 ...
Radio and X-ray signatures of merging neutron stars
... this is that the light cylinder radius for the magnetar magnetosphere (or `magnetarsphere'!) is , c=V , 5 1011 cm P=100 s; so that all of our subsequent discussion concerns processes occurring deep within the closed region of this magnetosphere. This will hold true right up to the point of a mer ...
... this is that the light cylinder radius for the magnetar magnetosphere (or `magnetarsphere'!) is , c=V , 5 1011 cm P=100 s; so that all of our subsequent discussion concerns processes occurring deep within the closed region of this magnetosphere. This will hold true right up to the point of a mer ...
NEW PARTICLES FROM NUCLEAR REACTIONS IN THE SUN Max
... cross section is estimated to be less than about 10-36 cm 2. In fig. 2 we show estimates of cross sections for various possibly significant processes at E a = 5.5 MeV. The largest type of absorption cross section is the analog of photo dissociation, a + nucleus -+ nuclear fragments. However, among t ...
... cross section is estimated to be less than about 10-36 cm 2. In fig. 2 we show estimates of cross sections for various possibly significant processes at E a = 5.5 MeV. The largest type of absorption cross section is the analog of photo dissociation, a + nucleus -+ nuclear fragments. However, among t ...
The Helium Flash • When the temperature of a stellar core reaches T
... thick helium burning shell will form. The energy generated in this shell will push the adjacent material outward, thereby lowering the temperature and density of the hydrogen burning shell. As a result, the outer envelope will contract and the star will move blueward in the HR diagram. Shortly there ...
... thick helium burning shell will form. The energy generated in this shell will push the adjacent material outward, thereby lowering the temperature and density of the hydrogen burning shell. As a result, the outer envelope will contract and the star will move blueward in the HR diagram. Shortly there ...
ES Chapter 30
... – Energy produced in the core of the Sun gets to the surface through two zones in the solar interior. • In the radiative zone, which is above the core, energy is transferred from particle to particle by radiation, as atoms continually absorb energy and then re-emit it. • Above the radiative zone, in ...
... – Energy produced in the core of the Sun gets to the surface through two zones in the solar interior. • In the radiative zone, which is above the core, energy is transferred from particle to particle by radiation, as atoms continually absorb energy and then re-emit it. • Above the radiative zone, in ...
Cygnus X-1
... a very inconsistent source for X-ray emissions. The emissions of X-rays for Cygnus X-1 flicker in hundredth of a second bursts. It is also been proven that Cygnus X-1 is smaller than the Earth. Strangely enough, Cygnus X-1 has a companion star called HDE 226868. HDE 226868 is a supergiant with a tem ...
... a very inconsistent source for X-ray emissions. The emissions of X-rays for Cygnus X-1 flicker in hundredth of a second bursts. It is also been proven that Cygnus X-1 is smaller than the Earth. Strangely enough, Cygnus X-1 has a companion star called HDE 226868. HDE 226868 is a supergiant with a tem ...
Electromagnetic pulse from final gravitational stellar collapse
... What is the measurable signal for gravitational collapse? It certainly produces gravitational waves, but unfortunately these have shown to be undetectable so far. However, there is another signal. Since the star has a sizable magnetic field, and since we expect this field to get quenched very rapidl ...
... What is the measurable signal for gravitational collapse? It certainly produces gravitational waves, but unfortunately these have shown to be undetectable so far. However, there is another signal. Since the star has a sizable magnetic field, and since we expect this field to get quenched very rapidl ...
Betelgeuse
... Its explosion into a supernova would be so bright; it would be visible even in daylight This is expected in the next 1000 years or so, though Betelgeuse’s actual fate is still a mystery ...
... Its explosion into a supernova would be so bright; it would be visible even in daylight This is expected in the next 1000 years or so, though Betelgeuse’s actual fate is still a mystery ...
Shape of a slowly rotating star measured by asteroseismology
... scale as T −3/2 times the noise-to-signal ratio of the periodic oscillations (15), and thus, the mode frequencies can be determined with astounding precision. In the p-mode frequency band, Kurtz et al. (12) report frequency errors between 5 × 10−7 day−1 and 10−4 day−1. The stellar model that best ex ...
... scale as T −3/2 times the noise-to-signal ratio of the periodic oscillations (15), and thus, the mode frequencies can be determined with astounding precision. In the p-mode frequency band, Kurtz et al. (12) report frequency errors between 5 × 10−7 day−1 and 10−4 day−1. The stellar model that best ex ...
Active Galactic Nuclei: are they important?
... Why I started to be interested in AGN? •Active Galactic Nuclei are fantastic subject for somebody who likes to apply GR •They consist of a massive black hole surrounded by plentiful material flowing in and out •This material emits radiation so we can trace what is happening close to a black hole ...
... Why I started to be interested in AGN? •Active Galactic Nuclei are fantastic subject for somebody who likes to apply GR •They consist of a massive black hole surrounded by plentiful material flowing in and out •This material emits radiation so we can trace what is happening close to a black hole ...
Summary of Astronomy
... by Ned Rozell The recent discovery of three planets orbiting a sun-like star once again raises one of mankind's favorite questions: can life exist on other planets? Someday, the aurora might help find an answer, according to Syun-Ichi Akasofu, director of both the Geophysical Institute and the Inter ...
... by Ned Rozell The recent discovery of three planets orbiting a sun-like star once again raises one of mankind's favorite questions: can life exist on other planets? Someday, the aurora might help find an answer, according to Syun-Ichi Akasofu, director of both the Geophysical Institute and the Inter ...
T. Thompson, Jan 2007
... – Because from secondary electrons/positrons, another process (not synchrotron) must dominate CR electron cooling. ...
... – Because from secondary electrons/positrons, another process (not synchrotron) must dominate CR electron cooling. ...
News from high-mass twin stars
... - higher order NJL - piecewise polytrope - density functional HMTs require stiff hadronic and quark matter EoS with a strong phase transition (PT) Existence of HMTs can be verified, e.g., by precise compact star mass and radius observations (and a bit of good luck) → Indicator for strong PT !! Extre ...
... - higher order NJL - piecewise polytrope - density functional HMTs require stiff hadronic and quark matter EoS with a strong phase transition (PT) Existence of HMTs can be verified, e.g., by precise compact star mass and radius observations (and a bit of good luck) → Indicator for strong PT !! Extre ...
Lecture5
... Otherwise, only the maximum mass can be found. • If both a1 and a2 (or their ratio a1/a2) are found (can happen for some of all binary kinds), then Eqns (20a)(20b) give mass of both ...
... Otherwise, only the maximum mass can be found. • If both a1 and a2 (or their ratio a1/a2) are found (can happen for some of all binary kinds), then Eqns (20a)(20b) give mass of both ...
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.