The structure of steady detonation waves in Type Ia supernovae
... centre of the core. It therefore seems very likely that detonations play a role in Type Ia supernovae. Khokhlov (1989) investigated the steady one-dimensional structures of nuclear detonations in C±O mixtures and in pure He. In C±O the detonation wave consists of three burning layers: a carbon-burni ...
... centre of the core. It therefore seems very likely that detonations play a role in Type Ia supernovae. Khokhlov (1989) investigated the steady one-dimensional structures of nuclear detonations in C±O mixtures and in pure He. In C±O the detonation wave consists of three burning layers: a carbon-burni ...
The Correlation of Lithium and Beryllium in F and G
... Li-Be correlation we found previously in the temperature regime of 5900–6650 K. The sample size for this temperature range with detectable and (usually) depleted Li and Be is now 88, including Li and Be abundances in both cluster and field stars. Therefore we can now investigate the influence of oth ...
... Li-Be correlation we found previously in the temperature regime of 5900–6650 K. The sample size for this temperature range with detectable and (usually) depleted Li and Be is now 88, including Li and Be abundances in both cluster and field stars. Therefore we can now investigate the influence of oth ...
on the evolution of anomalous x-ray pulsars and soft gamma
... disk turbulence indicates that the fall back disks are active up to a large radius, 1012 cm. We find that transient AXPs and SGRs are likely to be older than their persistent cousins. A fall back disk with mass transfer rates corresponding to the low quiescent X-ray luminosities of the transient so ...
... disk turbulence indicates that the fall back disks are active up to a large radius, 1012 cm. We find that transient AXPs and SGRs are likely to be older than their persistent cousins. A fall back disk with mass transfer rates corresponding to the low quiescent X-ray luminosities of the transient so ...
Evolution of Massive Binary Stars in the LMC and its Implications for
... 4.3) should be un-populated. 'Standard' theory therefore leads to a predicted 'gap' in this region (Tuchman & Wheeler 1990, hereafter TW). Tuchman and Wheeler, however, suggested that these stars are or were members of binary systems which acquired an outer helium-enriched layer through accretion th ...
... 4.3) should be un-populated. 'Standard' theory therefore leads to a predicted 'gap' in this region (Tuchman & Wheeler 1990, hereafter TW). Tuchman and Wheeler, however, suggested that these stars are or were members of binary systems which acquired an outer helium-enriched layer through accretion th ...
Where stars form: inside-out growth and coherent star formation from
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
... 2676 galaxies enabling a division into subsamples based on stellar mass and star formation rate. By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10−18 erg s−1 cm−2 arcsec−2 , allowing us to map the distribution of ionized gas out to greater than 10 kpc for typical L∗ ga ...
UNIVERSITY OF PADUA Master degree in
... ular hydrogen can form. It is however hard to observe molecular hydrogen directly through emission, as molecular hydrogen is homo-nuclear and has no electric dipole moment. This means that the lowest line transition occurs in the rotational-vibrational J = 2 → 0 transition, which is faint because of ...
... ular hydrogen can form. It is however hard to observe molecular hydrogen directly through emission, as molecular hydrogen is homo-nuclear and has no electric dipole moment. This means that the lowest line transition occurs in the rotational-vibrational J = 2 → 0 transition, which is faint because of ...
New brown dwarfs and giant planets
... ~50% trig/50% photo parallaxes Proper motions for all (U, V, W) velocities ...
... ~50% trig/50% photo parallaxes Proper motions for all (U, V, W) velocities ...
evidence for radiogenic sulfur-32 in type ab presolar
... et al. 1999). These stars experience a very-late thermal pulse (VLTP) where convective-reactive nucleosynthesis occurs and unprocessed, H-rich material is convectively mixed into the Heburning zone (Herwig et al. 2011). For the outer He intershell, which extends almost up to the stellar surface, Her ...
... et al. 1999). These stars experience a very-late thermal pulse (VLTP) where convective-reactive nucleosynthesis occurs and unprocessed, H-rich material is convectively mixed into the Heburning zone (Herwig et al. 2011). For the outer He intershell, which extends almost up to the stellar surface, Her ...
Tidal Disruptions of White Dwarfs from Ultra
... incoming star. Thus the disk formed from the tidal debris will have angular momentum that is also misaligned with the BH spin direction (Rees 1988). For thin disks, the BardeenPetterson effect will align the BH spin with the angular momentum of the inner region of the disk (Bardeen & Petterson 1975) ...
... incoming star. Thus the disk formed from the tidal debris will have angular momentum that is also misaligned with the BH spin direction (Rees 1988). For thin disks, the BardeenPetterson effect will align the BH spin with the angular momentum of the inner region of the disk (Bardeen & Petterson 1975) ...
Present-day cosmic abundances - Dr. Karl Remeis
... An ideal alternative to find a reference for the chemical composition of cosmic matter are normal unevolved early B-type stars of ∼8-18 M⊙ , which can provide simultaneously temporal (present-day) and local (birth place) information on chemical abundances. They can be observed not only in the solar ...
... An ideal alternative to find a reference for the chemical composition of cosmic matter are normal unevolved early B-type stars of ∼8-18 M⊙ , which can provide simultaneously temporal (present-day) and local (birth place) information on chemical abundances. They can be observed not only in the solar ...
H 2 O, OH, SiO, NH 3 and CH 3 OH
... [proh-toh-stahr] an early stage in the evolution of a star, after the beginning of the collapse of the gas cloud from which it is formed, but before sufficient contraction has occurred to permit initiation of nuclear reactions at its core. ...
... [proh-toh-stahr] an early stage in the evolution of a star, after the beginning of the collapse of the gas cloud from which it is formed, but before sufficient contraction has occurred to permit initiation of nuclear reactions at its core. ...
Accretion to Stars with Non
... (Donati & Cameron 1997; Donati et al. 1999; Jardine et al. 2002). If the multipolar component dominates in the discaccreting binary systems, then the matter flow to the star and the hot spots will be different from those in the case of a pure dipole field (e.g., Jardine et al. 2006). The dipole magn ...
... (Donati & Cameron 1997; Donati et al. 1999; Jardine et al. 2002). If the multipolar component dominates in the discaccreting binary systems, then the matter flow to the star and the hot spots will be different from those in the case of a pure dipole field (e.g., Jardine et al. 2006). The dipole magn ...
3011800000630
... The zoo of young neutron stars contains a number of categories recognized by the distinct properties of neutron stars discovered or identified in the last decade. The existence of these different types of neutron stars strongly suggests that not all neutron stars are born with the same initial condi ...
... The zoo of young neutron stars contains a number of categories recognized by the distinct properties of neutron stars discovered or identified in the last decade. The existence of these different types of neutron stars strongly suggests that not all neutron stars are born with the same initial condi ...
A HUBBLE SPACE TELESCOPE CENSUS OF
... brightest and hence youngest clusters. In order to get a more representative picture of nuclear star clusters, it is important to study a galaxy sample that is free from selection effects that favor the high end of the nuclear cluster luminosity range. In this paper, we describe the results of an HST ...
... brightest and hence youngest clusters. In order to get a more representative picture of nuclear star clusters, it is important to study a galaxy sample that is free from selection effects that favor the high end of the nuclear cluster luminosity range. In this paper, we describe the results of an HST ...
2. Bright AGN phase
... The contribution to HXRB is dominantly from bright AGNs, but HXRB (especially in ~ 10 1000keV) can constrain accretion history of faint AGNs ...
... The contribution to HXRB is dominantly from bright AGNs, but HXRB (especially in ~ 10 1000keV) can constrain accretion history of faint AGNs ...
Rest of the Universe
... dark matter. WIMPs are heavy particles — about 10 to 100 times heavier than a proton — that were produced during the Big Bang, though just small quantities are left today. These particles interact with normal matter via gravity or the weak nuclear force. More massive WIMPs would move more slowly thr ...
... dark matter. WIMPs are heavy particles — about 10 to 100 times heavier than a proton — that were produced during the Big Bang, though just small quantities are left today. These particles interact with normal matter via gravity or the weak nuclear force. More massive WIMPs would move more slowly thr ...
The interstellar medium and star formation on kpc size scales
... relatively small differences in the gas morphology and temperature distribution, and we have higher resolution here. First, we include feedback using the same method as described in Dobbs et al. (2011), where feedback is instantaneous. We are now including feedback on a much smaller scale (∼pc), so ...
... relatively small differences in the gas morphology and temperature distribution, and we have higher resolution here. First, we include feedback using the same method as described in Dobbs et al. (2011), where feedback is instantaneous. We are now including feedback on a much smaller scale (∼pc), so ...
Modeling the chemical evolution of the Galaxy halo
... the global metallicity (Z), dominated by oxygen. The observational data instead refer to the Fe abundance. Therefore, to compare model results and data, one is forced to adopt a conversion between Z and Fe (see De Lucia & Helmi 2008). In other papers, the Fe evolution was considered, but no Type Ia ...
... the global metallicity (Z), dominated by oxygen. The observational data instead refer to the Fe abundance. Therefore, to compare model results and data, one is forced to adopt a conversion between Z and Fe (see De Lucia & Helmi 2008). In other papers, the Fe evolution was considered, but no Type Ia ...
- Philsci
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
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.