Optical Properties of Front and Second Surface Silver-Based
... Houda Ennaceri was born in Morocco. She is currently conducting her PhD research in physics of materials at University Mohammed V-Agdal, Rabat 10000, Morocco, and holds a master’s degree in sustainable energy management in (MSSEM) from Al Akhawayn University in 2013, and a bachelor’s degree in engin ...
... Houda Ennaceri was born in Morocco. She is currently conducting her PhD research in physics of materials at University Mohammed V-Agdal, Rabat 10000, Morocco, and holds a master’s degree in sustainable energy management in (MSSEM) from Al Akhawayn University in 2013, and a bachelor’s degree in engin ...
Sample pages 1 PDF
... black holes and neutron stars, as discussed later in this chapter. The upper end of the relevant temperature range is achieved in the limit of the optically thin emission. It is not unreasonable to link it to the virial temperature of particles near the black hole, kTvir = GMm/r ∝ mc2 /(r/r g ). Unl ...
... black holes and neutron stars, as discussed later in this chapter. The upper end of the relevant temperature range is achieved in the limit of the optically thin emission. It is not unreasonable to link it to the virial temperature of particles near the black hole, kTvir = GMm/r ∝ mc2 /(r/r g ). Unl ...
Why are most molecular clouds not gravitationally bound
... is due to a variety of processes including collisional cooling, gasgrain energy transfer and recombination on grain surfaces. The gas initially lies within a radius of 10 kpc, and has an initial temperature of 700 K. The implementation of stellar feedback will be described in detail in a forthcoming ...
... is due to a variety of processes including collisional cooling, gasgrain energy transfer and recombination on grain surfaces. The gas initially lies within a radius of 10 kpc, and has an initial temperature of 700 K. The implementation of stellar feedback will be described in detail in a forthcoming ...
STELLAR STRUCTURE AND EVOLUTION
... We wish to build a theory of stellar evolution to explain the observational constraints highlighted above. In order to do so we must make some basic assumptions: • stars are considered to be isolated in space, so that their structure and evolution depend only on intrinsic properties (mass and compos ...
... We wish to build a theory of stellar evolution to explain the observational constraints highlighted above. In order to do so we must make some basic assumptions: • stars are considered to be isolated in space, so that their structure and evolution depend only on intrinsic properties (mass and compos ...
The MORGANA model for the rise of galaxies and active nuclei
... into account with simple approximated recipes. The main advantage of these models resides in the possibility of predicting the properties of whole galaxy populations in a short amount of computing time, thus making it possible to achieve a good sampling of the parameter space. However, it has been r ...
... into account with simple approximated recipes. The main advantage of these models resides in the possibility of predicting the properties of whole galaxy populations in a short amount of computing time, thus making it possible to achieve a good sampling of the parameter space. However, it has been r ...
Scaling of collision strengths for highly
... Emission lines from highly-excited states (n ≥ 5) of H- and He-like ions have been detected in astrophysical sources and fusion plasmas. For such excited states, R-matrix or distorted wave calculations for electron-impact excitation are very limited, due to the large size of the atomic basis set nee ...
... Emission lines from highly-excited states (n ≥ 5) of H- and He-like ions have been detected in astrophysical sources and fusion plasmas. For such excited states, R-matrix or distorted wave calculations for electron-impact excitation are very limited, due to the large size of the atomic basis set nee ...
Plasma Diagnostics and Hydrodynamic Evolution of Solar Flares
... cooling model. The model is found to provide a well-defined lower limit to the observed cooling time of a flare, but does not well fit the distribution. The discrepancies between the model and observations are assumed to be due to additional heating which is then compared to the flares’ overall ther ...
... cooling model. The model is found to provide a well-defined lower limit to the observed cooling time of a flare, but does not well fit the distribution. The discrepancies between the model and observations are assumed to be due to additional heating which is then compared to the flares’ overall ther ...
Molecular Clouds and the Onset of Star Formation
... On the giant molecular cloud scale, given an approximate mass one can calculate the gravitational potential energy and find that it is far greater in absolute value than the thermal energy. Thus the clouds are certainly highly gravitationally bound, but in general they are not collapsing. The linewi ...
... On the giant molecular cloud scale, given an approximate mass one can calculate the gravitational potential energy and find that it is far greater in absolute value than the thermal energy. Thus the clouds are certainly highly gravitationally bound, but in general they are not collapsing. The linewi ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... Writing the metric in this form shows that if κ is non-zero, angular lengths are either decreased (for positive curvature) or increased (for negative). Just as importantly, this metric indicates that, like in Minkowski space, time is orthogonal to position (meaning we can foliate the spacetime such ...
... Writing the metric in this form shows that if κ is non-zero, angular lengths are either decreased (for positive curvature) or increased (for negative). Just as importantly, this metric indicates that, like in Minkowski space, time is orthogonal to position (meaning we can foliate the spacetime such ...
Magnetic collapse of a neutron gas: Can magnetars
... which is demanded by Pauli’s principle to guarantee neutron stability), when placed in extremely strong magnetic fields, has a non-linear (ferromagnetic) response to the external field and is also unstable due to the vanishing of the transverse pressure for surface fields strong enough (Bsurf ≥ 1016 G) ...
... which is demanded by Pauli’s principle to guarantee neutron stability), when placed in extremely strong magnetic fields, has a non-linear (ferromagnetic) response to the external field and is also unstable due to the vanishing of the transverse pressure for surface fields strong enough (Bsurf ≥ 1016 G) ...
The dense gas mass fraction in the W51 cloud and its protoclusters
... which effectively smooths the output images from FWHM ≈ 5000 to ≈5400 . See Mangum et al. (2007) for more detail on the on-the-fly mapping technique used here. The Arecibo data were taken at a spectral resolution of 0.68 km s−1 . The spectra were regridded onto a velocity grid from −50 to 150 km s−1 ...
... which effectively smooths the output images from FWHM ≈ 5000 to ≈5400 . See Mangum et al. (2007) for more detail on the on-the-fly mapping technique used here. The Arecibo data were taken at a spectral resolution of 0.68 km s−1 . The spectra were regridded onto a velocity grid from −50 to 150 km s−1 ...
Conceptual Design of the International Axion Observatory (IAXO)
... for the discovery of axions and other ALPs, since it will deeply enter into completely unexplored parameter space. At the very least it will firmly exclude a huge region of this space. Needless to say, the discovery of such particles and the consequent evidence for physics at very high energy scales ...
... for the discovery of axions and other ALPs, since it will deeply enter into completely unexplored parameter space. At the very least it will firmly exclude a huge region of this space. Needless to say, the discovery of such particles and the consequent evidence for physics at very high energy scales ...
Search for Pulsed Very High Energy Gamma Ray
... Pulsars were discovered in 1967, when Hewish and Bell were studying interplanetary scintillations of radio waves. The name pulsar stands for pulsating source of radio which already unveils the most important characteristic: the intensity of the observed emission is regularly pulsing in time. This pu ...
... Pulsars were discovered in 1967, when Hewish and Bell were studying interplanetary scintillations of radio waves. The name pulsar stands for pulsating source of radio which already unveils the most important characteristic: the intensity of the observed emission is regularly pulsing in time. This pu ...
Flare Observations
... describing a syndrome of apparently related processes at various wavelengths. The problem is even more acute in other languages, such as German and French, denoting flares with the equivalent to “eruption”, which may be confused with Coronal Mass Ejections (CMEs) that often happen simultaneously at ...
... describing a syndrome of apparently related processes at various wavelengths. The problem is even more acute in other languages, such as German and French, denoting flares with the equivalent to “eruption”, which may be confused with Coronal Mass Ejections (CMEs) that often happen simultaneously at ...
Microplasma
Microplasmas are plasmas of small dimensions, ranging from tens to thousands of micrometers. They can be generated at a variety of temperatures and pressures, existing as either thermal or non-thermal plasmas. Non-thermal microplasmas that can maintain their state at standard temperatures and pressures are readily available and accessible to scientists as they can be easily sustained and manipulated under standard conditions. Therefore, they can be employed for commercial, industrial, and medical applications, giving rise to the evolving field of microplasmas.