Efficiency improvement of crystalline silicon solar cells
... increase the yield of solar cell processing. Furthermore, reducing the wafer thickness affects the electrical performance, of solar cells, and a compromise in-between material consumption and power output is needed [5]. The concentration of foreign particles such as oxygen, carbon, and metallic impu ...
... increase the yield of solar cell processing. Furthermore, reducing the wafer thickness affects the electrical performance, of solar cells, and a compromise in-between material consumption and power output is needed [5]. The concentration of foreign particles such as oxygen, carbon, and metallic impu ...
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... of solar coronal processes. Direct measurement of the coronal magnetic field is the most challenging problem in observational solar physics. A major progress here was reached with the deployment of the Coronal Multichannel Polarimeter (CoMP) (Tomczyk et al., 2007, 2008). In order to interpret such t ...
... of solar coronal processes. Direct measurement of the coronal magnetic field is the most challenging problem in observational solar physics. A major progress here was reached with the deployment of the Coronal Multichannel Polarimeter (CoMP) (Tomczyk et al., 2007, 2008). In order to interpret such t ...
arXiv:astro-ph/0411296v1 11 Nov 2004
... and other resulting upper limits on the derived parameters are listed in Table 2 for a distance of 1 kpc. Schönberner (1983) determined lower limits for the mass and luminosity of central stars of PN of approximately 0.55 M⊙ and 2500 L⊙ . If IRAS 19500-1709 is to be this luminous then it must be at ...
... and other resulting upper limits on the derived parameters are listed in Table 2 for a distance of 1 kpc. Schönberner (1983) determined lower limits for the mass and luminosity of central stars of PN of approximately 0.55 M⊙ and 2500 L⊙ . If IRAS 19500-1709 is to be this luminous then it must be at ...
T. Thompson, Jan 2007
... • If GLAST sees a smaller flux from NGC 253: – Either the CRs interact ISM below mean density, rapid escape, – or, < 0.05 less energy per SN to CR protons. – These options can in principle be distinguished by modeling the IC and relativistic bremsstrahlung emission at -ray energies since the la ...
... • If GLAST sees a smaller flux from NGC 253: – Either the CRs interact ISM below mean density, rapid escape, – or, < 0.05 less energy per SN to CR protons. – These options can in principle be distinguished by modeling the IC and relativistic bremsstrahlung emission at -ray energies since the la ...
– 1 – 1. Feedback From The First Stars
... might include the central region of the Milky Way, nearby dwarf spheroidal galaxies, or dark satellites of the Galaxy (small halos that have been accreted to our galaxy, but never formed stars). If annihilation emission is detected, it will help to characterize the nature of the dark matter. The pos ...
... might include the central region of the Milky Way, nearby dwarf spheroidal galaxies, or dark satellites of the Galaxy (small halos that have been accreted to our galaxy, but never formed stars). If annihilation emission is detected, it will help to characterize the nature of the dark matter. The pos ...
Self-similarity in the chemical evolution of galaxies and the delay
... events in galaxies. This is because of the different explosion timescales and yields of different types of supernovae. A direct consequence of this insight is the expectation of a correlation between the ages of stars in galaxies and their [α/Fe] ratios. A recent example is Figure 1 in Chiappini et ...
... events in galaxies. This is because of the different explosion timescales and yields of different types of supernovae. A direct consequence of this insight is the expectation of a correlation between the ages of stars in galaxies and their [α/Fe] ratios. A recent example is Figure 1 in Chiappini et ...
Circumstellar dust shells around long-period variables
... temperature T? , luminosity L? , and the photospheric element abundances i . In order to simulate the interior pulsation of the star, we apply a sinusoidal variation of the velocity with amplitude ∆u and period P at the inner boundary ri of the model. Thus, our models are defined by the prescriptio ...
... temperature T? , luminosity L? , and the photospheric element abundances i . In order to simulate the interior pulsation of the star, we apply a sinusoidal variation of the velocity with amplitude ∆u and period P at the inner boundary ri of the model. Thus, our models are defined by the prescriptio ...
Method of wave equations exact solutions in studies of neutrinos
... perturbation-series expansion techniques. A detailed discussion of the use of this method can be found in [9]. Many processes with electrons under the influence of external electromagnetic fields were investigated using this method. In particular, this method was applied [10] for derivation of an el ...
... perturbation-series expansion techniques. A detailed discussion of the use of this method can be found in [9]. Many processes with electrons under the influence of external electromagnetic fields were investigated using this method. In particular, this method was applied [10] for derivation of an el ...
Lowering the IceCube Detection Threshold by Wavelength
... This is because neutrinos are nearly massless and electrically neutral elementary particles which only interact very weakly with matter. Although they were discovered more than half a century ago, it is still not known whether neutrinos are their own antiparticles or not and what their masses are. H ...
... This is because neutrinos are nearly massless and electrically neutral elementary particles which only interact very weakly with matter. Although they were discovered more than half a century ago, it is still not known whether neutrinos are their own antiparticles or not and what their masses are. H ...
Determination of the distance to the Andromeda Galaxy using variable stars U
... target is to investigate possible cyclic (rotational) variability induced by surface inhomogeneities (e.g., cool spots). No convincing sign of such modulation was found from our Fourier analysis. Three possible explanations can be put forward. First, spot coverage could be too small to observe any r ...
... target is to investigate possible cyclic (rotational) variability induced by surface inhomogeneities (e.g., cool spots). No convincing sign of such modulation was found from our Fourier analysis. Three possible explanations can be put forward. First, spot coverage could be too small to observe any r ...
feps_jan_2007_aas - The Formation & Evolution of Planetary
... distributions (SEDs) from 3-160 microns, as well as obtain high resolution midinfrared spectra. The SEDs yield constraints on the geometric distribution and mass of dust while the spectra enable a search for emission from gas in circumstellar disks as a function of stellar age. Our main goals are to ...
... distributions (SEDs) from 3-160 microns, as well as obtain high resolution midinfrared spectra. The SEDs yield constraints on the geometric distribution and mass of dust while the spectra enable a search for emission from gas in circumstellar disks as a function of stellar age. Our main goals are to ...
Properties of long gamma-ray bursts from massive compact binaries
... We use the binary population of Church et al. [7], within which we searched for double blackhole binaries that satisfy the criterion of Levan et al. [6]. In summary, this requires that the binary be tight enough that, assuming tidal locking, the core is spun up sufficiently that its outer parts form ...
... We use the binary population of Church et al. [7], within which we searched for double blackhole binaries that satisfy the criterion of Levan et al. [6]. In summary, this requires that the binary be tight enough that, assuming tidal locking, the core is spun up sufficiently that its outer parts form ...
Forming Jupiter, Saturn, Uranus and Neptune in Few Million Years
... shorter than the corresponding time scale of orbital decay (Chambers 2006; Brunini & Benvenuto 2008). This situation reverts at r ∼ 20 m. Therefore, the giant planets of the solar system should have formed essentially through accretion of planetesimals larger than r ∼ 30 m, as smaller planetesimals ...
... shorter than the corresponding time scale of orbital decay (Chambers 2006; Brunini & Benvenuto 2008). This situation reverts at r ∼ 20 m. Therefore, the giant planets of the solar system should have formed essentially through accretion of planetesimals larger than r ∼ 30 m, as smaller planetesimals ...
