The birth rate of subluminous and overluminous type Ia supernovae
... Gap (HG), and then a stable RLOF occurs. The primary loses its hydrogen-rich envelope and then becomes a helium star, where mass ratio reverses at a point. The helium star may fill its Roche lobe again after its central helium is exhausted, where the RLOF is also dynamically stable for a low-mass ra ...
... Gap (HG), and then a stable RLOF occurs. The primary loses its hydrogen-rich envelope and then becomes a helium star, where mass ratio reverses at a point. The helium star may fill its Roche lobe again after its central helium is exhausted, where the RLOF is also dynamically stable for a low-mass ra ...
Chapter 7 in the LSST Science Book
... to form within dark matter halos that are themselves growing through gravitational collapse and mergers. In fact, we are very fortunate to live in a hierarchical Universe where the LV galaxies contain the signatures not only of their own formation, but also of the hundreds of galaxies that they accr ...
... to form within dark matter halos that are themselves growing through gravitational collapse and mergers. In fact, we are very fortunate to live in a hierarchical Universe where the LV galaxies contain the signatures not only of their own formation, but also of the hundreds of galaxies that they accr ...
evidence for radiogenic sulfur-32 in type ab presolar
... The Astrophysical Journal Letters, 776:L29 (6pp), 2013 October 20 ...
... The Astrophysical Journal Letters, 776:L29 (6pp), 2013 October 20 ...
Book of Abstracts - University of Sheffield
... rare collisions with WIMP particles. The TPC detection principle allows for measurements of WIMP-induced recoils through two signals: a prompt scintillation signal and an ionization signal. In previous XENON100 analyses the recoil energy was determined using the size of the scintillation signal. WIM ...
... rare collisions with WIMP particles. The TPC detection principle allows for measurements of WIMP-induced recoils through two signals: a prompt scintillation signal and an ionization signal. In previous XENON100 analyses the recoil energy was determined using the size of the scintillation signal. WIM ...
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... A twofold model of turbulent accretion for massive star formation was proposed by Krumholz et al. (2006), where Bondi accretion is assumed, with the Bondi velocity dispersion set either to the turbulent velocity dispersion or to the velocity dispersion due to vorticity. Models of accretion onto a st ...
... A twofold model of turbulent accretion for massive star formation was proposed by Krumholz et al. (2006), where Bondi accretion is assumed, with the Bondi velocity dispersion set either to the turbulent velocity dispersion or to the velocity dispersion due to vorticity. Models of accretion onto a st ...
3011800000630
... prescription given by Vrtilek et al. (1990). To estimate the temperatures, both Hulleman et al. (2000) and Perna et al. (2000) assumed the same particular irradiation efficiency, and found that their estimated optical flux values lie well above the values indicated by the observations of the AXPs 4U ...
... prescription given by Vrtilek et al. (1990). To estimate the temperatures, both Hulleman et al. (2000) and Perna et al. (2000) assumed the same particular irradiation efficiency, and found that their estimated optical flux values lie well above the values indicated by the observations of the AXPs 4U ...
Chapter 1
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
... ratios are higher than a cooler nebula. This is because to produce [O iii] λ4363 an electron needs to be excited to 5.3 eV, which requires more energy than for 4959/5007 which result from decay from 1 D2 level, 2.5 eV above the ground-state (see Figure 2.2). Therefore, these ratios can be used to co ...
Hot and Dense Matter in Compact Stars – From Nuclei to Quarks
... However, already at T = 0.8 MeV the typical weak reaction rates fall below the expansion rate of the universe, and thus weak equilibrium is not established any more. As the neutron lifetime is rather long, τn ∼ 890 s, at this temperature the neutron abundance freezes out with a value nn /np ∼ 0.2. A ...
... However, already at T = 0.8 MeV the typical weak reaction rates fall below the expansion rate of the universe, and thus weak equilibrium is not established any more. As the neutron lifetime is rather long, τn ∼ 890 s, at this temperature the neutron abundance freezes out with a value nn /np ∼ 0.2. A ...
D-particles
... (i) consider a microscopic model of flavour vacua, with Dynamical determination of cutoff (if possible) (ii) Incorporate the Lorentz symmetry breaking of the Atcondensate present only effectivearguments FIELD TEORY Flavour byTOY microscopic in vacuo models of flavour states constructed in this frame ...
... (i) consider a microscopic model of flavour vacua, with Dynamical determination of cutoff (if possible) (ii) Incorporate the Lorentz symmetry breaking of the Atcondensate present only effectivearguments FIELD TEORY Flavour byTOY microscopic in vacuo models of flavour states constructed in this frame ...
Multi-dimensional models of circumstellar shells around evolved
... Results. As the fast Wolf-Rayet wind expands, it creates a dense shell of swept up material that expands outward, driven by the high pressure of the shocked Wolf-Rayet wind. These shells are subject to a fair variety of hydrodynamic-radiative instabilities. If the Wolf-Rayet wind is expanding into t ...
... Results. As the fast Wolf-Rayet wind expands, it creates a dense shell of swept up material that expands outward, driven by the high pressure of the shocked Wolf-Rayet wind. These shells are subject to a fair variety of hydrodynamic-radiative instabilities. If the Wolf-Rayet wind is expanding into t ...
STRUCTURAL CHARACTERISTICS AND STELLAR
... 1991). The area weighted colors are less a ected and should be more representative of the underlying stellar population. Indeed, this is a much greater concern for broad band colors of HSB disks, where the star formation rate and H II region covering factor are higher. Due to bad weather, some galax ...
... 1991). The area weighted colors are less a ected and should be more representative of the underlying stellar population. Indeed, this is a much greater concern for broad band colors of HSB disks, where the star formation rate and H II region covering factor are higher. Due to bad weather, some galax ...
