Astronomy Astrophysics
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
The Hamburg/ESO R-process Enhanced Star survey (HERES)
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
Ab Initio Nuclear Structure Calculations for Light Nuclei
... has opened a range of nuclear phenomena for evaluation to high precision using realistic internucleon interactions. The many-body approach adopted in this work is referred to as the no-core full configuration (NCFC) method (1; 2; 3). The NCFC method produces the stationary state solutions of the nuc ...
... has opened a range of nuclear phenomena for evaluation to high precision using realistic internucleon interactions. The many-body approach adopted in this work is referred to as the no-core full configuration (NCFC) method (1; 2; 3). The NCFC method produces the stationary state solutions of the nuc ...
5. cosmic distance ladder ii: standard candles
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
Cosmic Rays and Climate
... Angström exponent: is the aerosol optical thickness dependence of wavelength . The Angström exponent is inversely related to the average size of the particles: the smaller the particles, the larger the exponent. For shorter wave lengths (340,380,440,500 nm) a decrease will mean fewer small particles ...
... Angström exponent: is the aerosol optical thickness dependence of wavelength . The Angström exponent is inversely related to the average size of the particles: the smaller the particles, the larger the exponent. For shorter wave lengths (340,380,440,500 nm) a decrease will mean fewer small particles ...
Learning Objectives
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
... easily calculated. However, some special types of variable and exploding stars do have known, standard luminosities. Consequently, if you can identify a star as being one of these special types, you know its luminosity. Then you only have to measure its brightness to be able to compute its distance. ...
Effects of color superconductivity on the nucleation of
... hadronic compact stars with respect to the conversion to quark stars using different relativistic models for the EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). We have explored the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, fi ...
... hadronic compact stars with respect to the conversion to quark stars using different relativistic models for the EoS: Non Linear Walecka Model (NLWM) & Quark Meson Coupling (QMC). We have explored the effect of different hyperon couplings on the critical mass and on the stellar conversion energy, fi ...
Terzan 5`s Pulsars Fastest
... o Ter5ad is a 716-Hz/1.396-ms eclipsing binary radio pulsar in the rich, dense globular cluster Terzan 5. It is in a highly circular 1.1-day orbit with a > 0.14 Msun companion. o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spi ...
... o Ter5ad is a 716-Hz/1.396-ms eclipsing binary radio pulsar in the rich, dense globular cluster Terzan 5. It is in a highly circular 1.1-day orbit with a > 0.14 Msun companion. o The fast rotation of Ter5ad constrains its radius to be < 16 km, assuming its mass is less than 2 Msun (Fig 1). o The spi ...
Type II SuperNova - University of Dayton
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
... supernova in the last 3 centuries, and for the first time astronomers not only observed the light show, but also detected 19 of the elusive neutrinos (the detectors observed electron anti-neutrinos, to be more precise) produced by the collapse of the star's core. The burst of neutrinos preceded the ...
Globular Clusters - University of Dayton
... Turn Off - As the hydrogen fuel in a star's core runs out the core begins to collapse due to gravity and the star moves away from the main sequence. At the turn off nearly all the central fuel is gone. Red Giant Branch - When the central fuel is gone, hydrogen starts to burn in an envelope around a ...
... Turn Off - As the hydrogen fuel in a star's core runs out the core begins to collapse due to gravity and the star moves away from the main sequence. At the turn off nearly all the central fuel is gone. Red Giant Branch - When the central fuel is gone, hydrogen starts to burn in an envelope around a ...
Electron Firehose instability and acceleration of electrons in solar
... moving MHD waves. Due to a slight overplus in head-on collisions the interaction results in an energy gain for the particle. As in the shock acceleration model, the acceleration by MHD turbulence suffers from an ’injection problem’: Thermal ions and electrons cannot resonate with MHD waves for typic ...
... moving MHD waves. Due to a slight overplus in head-on collisions the interaction results in an energy gain for the particle. As in the shock acceleration model, the acceleration by MHD turbulence suffers from an ’injection problem’: Thermal ions and electrons cannot resonate with MHD waves for typic ...
Star Formation Regions and Planetary Nebulae
... The ubiquity of interstellar regions in which the physics and chemistry are dominated by the effects of far ultra-violet (FUV) photons is now well understood (see, e.g., Hollenbach & Tielens 1997, ARA&A, 35, 179). Such regions, called photodissociation regions, or sometimes photon dominated regions ...
... The ubiquity of interstellar regions in which the physics and chemistry are dominated by the effects of far ultra-violet (FUV) photons is now well understood (see, e.g., Hollenbach & Tielens 1997, ARA&A, 35, 179). Such regions, called photodissociation regions, or sometimes photon dominated regions ...
- The 5th state of matter
... separated against their very strong attraction? Nature separates electric charges, not only in the lightning. E.g. the cosmic rays consist of positive ions and less than 0.1% electrons. Simply, many stars thermally separate electrons from the ions via equ.2 as briefly described below (Körtvélyessy): ...
... separated against their very strong attraction? Nature separates electric charges, not only in the lightning. E.g. the cosmic rays consist of positive ions and less than 0.1% electrons. Simply, many stars thermally separate electrons from the ions via equ.2 as briefly described below (Körtvélyessy): ...
5-th_state_matter - The 5th state of matter
... separated against their very strong attraction? Nature separates electric charges, not only in the lightning. E.g. the cosmic rays consist of positive ions and less than 0.1% electrons. Simply, many stars thermally separate electrons from the ions via equ.2 as briefly described below (Körtvélyessy): ...
... separated against their very strong attraction? Nature separates electric charges, not only in the lightning. E.g. the cosmic rays consist of positive ions and less than 0.1% electrons. Simply, many stars thermally separate electrons from the ions via equ.2 as briefly described below (Körtvélyessy): ...
astrophysics - The University of Sydney
... The cycle then repeats itself. Helium is fused to carbon and oxygen in the star’s core, but eventually the core runs out of helium. Fusion stops, and the core resumes its collapse. This heats up the layer of helium just outside the core, which begins fusing in a shell of its own, inside the hydrogen ...
... The cycle then repeats itself. Helium is fused to carbon and oxygen in the star’s core, but eventually the core runs out of helium. Fusion stops, and the core resumes its collapse. This heats up the layer of helium just outside the core, which begins fusing in a shell of its own, inside the hydrogen ...
more about spectroscopy mportant, less-common
... 1 H z apart will not be clearly distinguishable unless Av of each is less than about 1 Hz, which corresponds to a At, the lifetime of the excited state, of 1/(2n) = 0.16 sec. If AV is 2 2 Hz, lines that are 1 H z apart will be so poorly resolved as to appear as one line (cf. Figure 27-2). A A v of 2 ...
... 1 H z apart will not be clearly distinguishable unless Av of each is less than about 1 Hz, which corresponds to a At, the lifetime of the excited state, of 1/(2n) = 0.16 sec. If AV is 2 2 Hz, lines that are 1 H z apart will be so poorly resolved as to appear as one line (cf. Figure 27-2). A A v of 2 ...
Photoneutron cross sections for samarium isotopes: Toward a
... 3 MeV in the response function. This bump is characteristic of spectra obtained without the C1 collimator, which was confirmed experimentally under the presence and absence of the C1 collimator. The bump corresponds to the laser photons Compton-scattered around 0◦ with large cross sections in the re ...
... 3 MeV in the response function. This bump is characteristic of spectra obtained without the C1 collimator, which was confirmed experimentally under the presence and absence of the C1 collimator. The bump corresponds to the laser photons Compton-scattered around 0◦ with large cross sections in the re ...
The central star of the planetary nebula PB 8: a Wolf-Rayet
... the tip of the asymptotic giant branch (AGB). In the subsequent PN phase it evolves rapidly towards the white dwarf cooling sequence. Most of the CSPNe show a hydrogen-rich surface composition. Among the Galactic central stars, 5-6 % are hydrogendeficient and show emission lines in their spectra (Ty ...
... the tip of the asymptotic giant branch (AGB). In the subsequent PN phase it evolves rapidly towards the white dwarf cooling sequence. Most of the CSPNe show a hydrogen-rich surface composition. Among the Galactic central stars, 5-6 % are hydrogendeficient and show emission lines in their spectra (Ty ...
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.