THE CHEMICAL COMPOSITION AND AGE OF THE METAL
... heaviest stable elements and the radioactive element thorium. However, the other important nuclear chronometer, uranium, has not yet been detected in that star. In this paper we present the results of an extensive series of observations regarding the metal-poor (½Fe=H ¼ 2:1) halo star BD +17 3248 ...
... heaviest stable elements and the radioactive element thorium. However, the other important nuclear chronometer, uranium, has not yet been detected in that star. In this paper we present the results of an extensive series of observations regarding the metal-poor (½Fe=H ¼ 2:1) halo star BD +17 3248 ...
PDF hosted at the Radboud Repository of the Radboud University
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
S T E L L A R
... course on stars at Michigan State University. The only background preparation for this course is undergraduate physics and a course on radiative processes, and so portions of these notes could be useful for upper-level undergraduates. The text layout uses the tufte-book (https://tufte-latex.github.i ...
... course on stars at Michigan State University. The only background preparation for this course is undergraduate physics and a course on radiative processes, and so portions of these notes could be useful for upper-level undergraduates. The text layout uses the tufte-book (https://tufte-latex.github.i ...
Full-Text PDF
... to be the tail of the prompt γ-ray emission. Then it enters a plateau phase and continues as a power law (Wijers et al. [24]) that can some times last up to a few weeks and is most probably associated with an external origin (external shocks, e.g., Meszaros and Rees [22]). Zhang et al. [14] complete ...
... to be the tail of the prompt γ-ray emission. Then it enters a plateau phase and continues as a power law (Wijers et al. [24]) that can some times last up to a few weeks and is most probably associated with an external origin (external shocks, e.g., Meszaros and Rees [22]). Zhang et al. [14] complete ...
Cosmology with objects from the Hamburg Quasar Surveys
... measurement of the primordial deuterium abundance therefore gives the cosmic baryon density Щb. A natural place to look for primordial abundances is in high-redshift, low metal abundance intergalactic clouds where there is little contamination with processed matter ejected by stars where D is destro ...
... measurement of the primordial deuterium abundance therefore gives the cosmic baryon density Щb. A natural place to look for primordial abundances is in high-redshift, low metal abundance intergalactic clouds where there is little contamination with processed matter ejected by stars where D is destro ...
GRAVITATIONAL SETTLING OF 22Ne AND WHITE DWARF
... A ¼ 2Z ) result in a net downward gravitational force and a slow, diffusive settling of 22 Ne in the liquid regions toward the center of the white dwarf. The role of 22 Ne sedimentation in the energetics of crystallizing white dwarfs was first addressed by Isern et al. (1991). The extent to which th ...
... A ¼ 2Z ) result in a net downward gravitational force and a slow, diffusive settling of 22 Ne in the liquid regions toward the center of the white dwarf. The role of 22 Ne sedimentation in the energetics of crystallizing white dwarfs was first addressed by Isern et al. (1991). The extent to which th ...
![arXiv:1604.01613v2 [astro-ph.SR] 23 Aug 2016](http://s1.studyres.com/store/data/015708841_1-69411a0a7e7ee9a8690efbc066a22153-300x300.png)
arXiv:1604.01613v2 [astro-ph.SR] 23 Aug 2016
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
The white dwarf binary pathways survey – I. A sample of FGK stars
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
... SN Ia spectra (Branch et al. 1995). Moreover, there is both theoretical and observational evidence for a large population of close double white dwarf binaries (Yungelson et al. 1994; Nelemans & Tout 2005; Napiwotzki et al. 2001). However, there is some uncertainty as to whether the merger leads to a ...
Chapter 18
... force acts among all or most of the particles. As the nuclei get larger electrostatic repulsion between protons is greater than the strong force, breaking apart the nucleus. 10. How does nuclear binding energy relate to the stability of an atom? The higher the binding energy per nucleon, the more st ...
... force acts among all or most of the particles. As the nuclei get larger electrostatic repulsion between protons is greater than the strong force, breaking apart the nucleus. 10. How does nuclear binding energy relate to the stability of an atom? The higher the binding energy per nucleon, the more st ...
The Stromgren sphere around the highest-redshift QSOs
... accretion process follows a self-similar evolutionary pattern as simple theoretical models predict. • Some other issues deserves of further investigation, such as the long-term evolution of accretion disks, the evolution of BBHs in QSOs/AGNs, coevolution of galaxies and QSOs/AGNs, and the unificatio ...
... accretion process follows a self-similar evolutionary pattern as simple theoretical models predict. • Some other issues deserves of further investigation, such as the long-term evolution of accretion disks, the evolution of BBHs in QSOs/AGNs, coevolution of galaxies and QSOs/AGNs, and the unificatio ...
Hunting for Orphaned Central Compact Objects among Radio Pulsars
... 10−17 (Halpern & Gotthelf 2010; Gotthelf et al. 2013a). Their spin parameters are plotted in the P -Ṗ diagram in Figure 1. These suggest spin-down luminosities of Ė ≡ 4π 2 I Ṗ /P 3 = 1031 –1032 erg s−1 , where I is the neutron star moment of inertia. These values are nearly two orders of magnitud ...
... 10−17 (Halpern & Gotthelf 2010; Gotthelf et al. 2013a). Their spin parameters are plotted in the P -Ṗ diagram in Figure 1. These suggest spin-down luminosities of Ė ≡ 4π 2 I Ṗ /P 3 = 1031 –1032 erg s−1 , where I is the neutron star moment of inertia. These values are nearly two orders of magnitud ...
A self-consistent empirical model atmosphere, abundance and
... Context. Chemically peculiar (CP) stars are unique natural laboratories for the investigation of the microscopic diffusion processes of chemical elements. The element segregation under the influence of gravity and radiation pressure leads to the appearance of strong abundance gradients in the atmosph ...
... Context. Chemically peculiar (CP) stars are unique natural laboratories for the investigation of the microscopic diffusion processes of chemical elements. The element segregation under the influence of gravity and radiation pressure leads to the appearance of strong abundance gradients in the atmosph ...
CPW
... Algol system when their orbits intersected and that due to this encounter Algol B “became part of the Algol system.” Since Student 2 does not state exactly why Algol B became part of the orig ...
... Algol system when their orbits intersected and that due to this encounter Algol B “became part of the Algol system.” Since Student 2 does not state exactly why Algol B became part of the orig ...
Draft paper (submitted to MNRAS)
... particular, since it allows low density gas to accumulate in a galaxy, where it can fuel discrete star formation episodes triggered even by minor accretion events. Ricotti & Gnedin (2005) have also argued, on the basis of numerical simulations, that diversity in dwarf SFHs might actually be a relic ...
... particular, since it allows low density gas to accumulate in a galaxy, where it can fuel discrete star formation episodes triggered even by minor accretion events. Ricotti & Gnedin (2005) have also argued, on the basis of numerical simulations, that diversity in dwarf SFHs might actually be a relic ...
Star Formation: Chemistry as a Probe of Embedded Protostars
... spectrally unresolved.1 I will discuss the CO rotational lines in more detail as an example of both the opportunities and the limitations from the Herschel observations. Rotationally excited CO is ubiquitous in low-mass embedded protostars. Early observations with ground-based sub-millimeter telesco ...
... spectrally unresolved.1 I will discuss the CO rotational lines in more detail as an example of both the opportunities and the limitations from the Herschel observations. Rotationally excited CO is ubiquitous in low-mass embedded protostars. Early observations with ground-based sub-millimeter telesco ...
G0900505-v1 - DCC
... • Nuclear density, temperature below Fermi temperature. • Spin-up during glitch is very fast (<100 s). – NOT electomagnetic torque ...
... • Nuclear density, temperature below Fermi temperature. • Spin-up during glitch is very fast (<100 s). – NOT electomagnetic torque ...
The Milky Way and Andromeda galaxies in a constrained
... imprints of the formation of the LG on their final properties. In particular, we focus on the formation of the main stellar components of the galaxies, and investigate possible correlations between the formation of stellar discs and large-scale effects such as merger events and misalignment between t ...
... imprints of the formation of the LG on their final properties. In particular, we focus on the formation of the main stellar components of the galaxies, and investigate possible correlations between the formation of stellar discs and large-scale effects such as merger events and misalignment between t ...
On the asymmetry of the distribution of observable comets induced
... Using the original Monte Carlo simulation code we calculated the effects of stellar passages for wide ranges of the parameters. The perturber mass varied from 0.5 up to 5 solar masses, the minimum heliocentric distance from 10 000 to 100 000 AU and the stellar perturber velocity from 5 km s−1 to 50 ...
... Using the original Monte Carlo simulation code we calculated the effects of stellar passages for wide ranges of the parameters. The perturber mass varied from 0.5 up to 5 solar masses, the minimum heliocentric distance from 10 000 to 100 000 AU and the stellar perturber velocity from 5 km s−1 to 50 ...
22. Dark Matter and the Fate of the Universe
... • Why can’t neutrinos account for dark matter in galaxies? • Although neutrinos are weakly interacting particles and thus are form of dark matter, they travel too fast/too much energy to be gravitationally bound in galaxies. They could potentially account for some dark matter outside galaxies, but t ...
... • Why can’t neutrinos account for dark matter in galaxies? • Although neutrinos are weakly interacting particles and thus are form of dark matter, they travel too fast/too much energy to be gravitationally bound in galaxies. They could potentially account for some dark matter outside galaxies, but t ...
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.