Journal of Non-Crystalline Solids 114 (1989) 813-815
... Where I is the size of the domains, and Pa is the fraction of a-Si. This equation is valid for c~-a~
... Where I is the size of the domains, and Pa is the fraction of a-Si. This equation is valid for c~-a~
SimulationDatabases
... Data sets are often very large, often far away (makes them even larger!) To analyse remote datasets, one needs to be able to bring the analysis to the data. “Standard” approach using flat files and C/IDL/etc code sub-optimal To analyse very large datasets we also need advanced methods of dat ...
... Data sets are often very large, often far away (makes them even larger!) To analyse remote datasets, one needs to be able to bring the analysis to the data. “Standard” approach using flat files and C/IDL/etc code sub-optimal To analyse very large datasets we also need advanced methods of dat ...
Diapositiva 1 - Yale University
... 1838: Bessel determines the trigonometric parallax of 61 Cyg 1887: The photographic plate is adopted as a detector 1989: ESA launches the Hipparcos satellite * There is some evidence indicating that it was actually Nicholas of Cusa (circa 1400) who first mentioned the proper motion of stars ...
... 1838: Bessel determines the trigonometric parallax of 61 Cyg 1887: The photographic plate is adopted as a detector 1989: ESA launches the Hipparcos satellite * There is some evidence indicating that it was actually Nicholas of Cusa (circa 1400) who first mentioned the proper motion of stars ...
The Chemical Composition of Exoplanet
... (exoplanets.eu, as of November 2013), there are currently 1039 known exoplanets, composing 787 planetary systems. There have been several methods developed to detect these exoplanets, each method providing different types of information regarding the planetary systems (Perryman, 2011). Three of the ...
... (exoplanets.eu, as of November 2013), there are currently 1039 known exoplanets, composing 787 planetary systems. There have been several methods developed to detect these exoplanets, each method providing different types of information regarding the planetary systems (Perryman, 2011). Three of the ...
Section IV High-Energy Astrophysics and Cosmology
... emission line at a half of height in the radiation spectrum, i.e. FWHM. The BLR radius RBLR is usually determined by the reverberation method, i.e. with time delay between continuum and emission line variations. Determination of the f value is strongly depending on accepted BLR model. Labita et al. ...
... emission line at a half of height in the radiation spectrum, i.e. FWHM. The BLR radius RBLR is usually determined by the reverberation method, i.e. with time delay between continuum and emission line variations. Determination of the f value is strongly depending on accepted BLR model. Labita et al. ...
Sample Return from Primitive Asteroids and Comets
... These enigmatic outer-belt asteroids are important because they preserve unique records of the transition between the Solar System starting materials and the origins of the planets. Key questions to be addressed by a sample return from an outer belt or comet-like asteroid: • What processes drive the ...
... These enigmatic outer-belt asteroids are important because they preserve unique records of the transition between the Solar System starting materials and the origins of the planets. Key questions to be addressed by a sample return from an outer belt or comet-like asteroid: • What processes drive the ...
Variable Blue Stragglers in M67
... Complete photometric study has been finished for S1282, S1280 and S1284; physical parameters for the 3 variable BSs are determined, evolutionary status and probable formation mechanism are discussed; S1036 and S1082; waiting for more observations. ...
... Complete photometric study has been finished for S1282, S1280 and S1284; physical parameters for the 3 variable BSs are determined, evolutionary status and probable formation mechanism are discussed; S1036 and S1082; waiting for more observations. ...
PDF file
... 3) Bound vs. unbound clusters. While many young stars are born in groups and clusters, most disperse rapidly; few clusters remain bound over timescales > 10 Myr. The conditions under which bound clusters are produced are not clear. Studies of older, widely-spread low-mass stars around young cluster ...
... 3) Bound vs. unbound clusters. While many young stars are born in groups and clusters, most disperse rapidly; few clusters remain bound over timescales > 10 Myr. The conditions under which bound clusters are produced are not clear. Studies of older, widely-spread low-mass stars around young cluster ...
Part 9: Story of the Universe
... Finkelstein, S. L. et al. Nature 502, 524–527 (2013); see also Riecher 24 October 2013, Nature, 502, 459 Atoms to Astronomy ...
... Finkelstein, S. L. et al. Nature 502, 524–527 (2013); see also Riecher 24 October 2013, Nature, 502, 459 Atoms to Astronomy ...
Goal: To understand how to find the brightness of stars and what
... USA for 3 million years!). • The earth in the infrared has an absolute brightness of about 1 * 1024 erg/sec (which is still enough energy to power the USA for a day). ...
... USA for 3 million years!). • The earth in the infrared has an absolute brightness of about 1 * 1024 erg/sec (which is still enough energy to power the USA for a day). ...
Spectral and Hydrodynamic Modeling of X-Ray Michael Rosenberg
... as thorough a treatment. Many objects of current astrophysical interest, including x-ray binaries and active galactic nuclei, produce massive regions of photoionized plasmas. By achieving a better understanding of the spectra of photoionized plasmas, conditions in these extreme environments may b e ...
... as thorough a treatment. Many objects of current astrophysical interest, including x-ray binaries and active galactic nuclei, produce massive regions of photoionized plasmas. By achieving a better understanding of the spectra of photoionized plasmas, conditions in these extreme environments may b e ...
Paper
... Dirac pulse (10 s), applied after 2 ms of ballistic expansion. The copies, with momentum pr , moved away from the zero momentum peak for time t before an identical pulse recombined them with the original. This type of interferometer has three readout ports, with momenta 0, pr . The straightline ...
... Dirac pulse (10 s), applied after 2 ms of ballistic expansion. The copies, with momentum pr , moved away from the zero momentum peak for time t before an identical pulse recombined them with the original. This type of interferometer has three readout ports, with momenta 0, pr . The straightline ...
Lecture 1
... coupled time-varying electric and magnetic fields that satisfy a wave equation (which itself can be derived from Maxwell’s equations): ...
... coupled time-varying electric and magnetic fields that satisfy a wave equation (which itself can be derived from Maxwell’s equations): ...
A simple tool for assessing the completeness in apparent magnitude
... the limiting apparent magnitude (Hubble 1926). This test, which presupposes that the galaxies population does not evolve with time and is homogeneously distributed in space, is however not very efficient. It is difficult to decide in practice whether the deviation of the counts law is due to the pre ...
... the limiting apparent magnitude (Hubble 1926). This test, which presupposes that the galaxies population does not evolve with time and is homogeneously distributed in space, is however not very efficient. It is difficult to decide in practice whether the deviation of the counts law is due to the pre ...
L117 SHOCK-HEATED NH3 IN A MOLECULAR JET ASSOCIATED
... limits at other wavelengths, Hofner et al. interpreted this source as emission from an ionized jet. The lack of a detectable H ii region indicates that the central object is probably a high-mass protostar. In contrast to the weak centimeter emission, the source is detected at all wavelengths in the ...
... limits at other wavelengths, Hofner et al. interpreted this source as emission from an ionized jet. The lack of a detectable H ii region indicates that the central object is probably a high-mass protostar. In contrast to the weak centimeter emission, the source is detected at all wavelengths in the ...
Strong period decrease in the Mira star S Sex: a possible helium
... perhaps due to the faintness of S Sex. These data were therefore not included in the detailed study of the period change, although they will be discussed in the final section in order to give an overview of the temporal evolution of S Sex. Fig. 1 shows the light curve from JD2442000 to JD2451340. We ...
... perhaps due to the faintness of S Sex. These data were therefore not included in the detailed study of the period change, although they will be discussed in the final section in order to give an overview of the temporal evolution of S Sex. Fig. 1 shows the light curve from JD2442000 to JD2451340. We ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.