Comparison of electronic structures of mass
... position energy: 2.6 eV)~ At the initial stage of Ag deposi- Decrease of the FWHM of the Ag 3d peaks upon agglomtion, the intensity of the Ag 3d peak grows with increas- eration can be rationalized by the lower surface to volume ing number of deposited clusters without much alteration of ratio of a ...
... position energy: 2.6 eV)~ At the initial stage of Ag deposi- Decrease of the FWHM of the Ag 3d peaks upon agglomtion, the intensity of the Ag 3d peak grows with increas- eration can be rationalized by the lower surface to volume ing number of deposited clusters without much alteration of ratio of a ...
The effect of rotation and tidal heating on the thermal lightcurves of
... radii below 2R⊕ , only a few planets have well-measured masses below 10M⊕ . These low-mass planets exhibit a variety of densities that goes from lower than 1 g/cm3 for Kepler 11 c,e,f (Lissauer et al. 2013) up to 8.8 ± 2.9 g/cm3 for Kepler 10 b ...
... radii below 2R⊕ , only a few planets have well-measured masses below 10M⊕ . These low-mass planets exhibit a variety of densities that goes from lower than 1 g/cm3 for Kepler 11 c,e,f (Lissauer et al. 2013) up to 8.8 ± 2.9 g/cm3 for Kepler 10 b ...
Bismuth-doped optical fibers: a challenging active medium
... near-IR emission from Bi-doped glass: Bi1, Bi clusters, BiO, Bi22/Bi2, Bi22/Bi222, point defects, Bi0 and others have been examined, but none has been directly confirmed to be the defining factor. These hypotheses have been analyzed in detail in Ref. 14. At the same time, the results of extensive re ...
... near-IR emission from Bi-doped glass: Bi1, Bi clusters, BiO, Bi22/Bi2, Bi22/Bi222, point defects, Bi0 and others have been examined, but none has been directly confirmed to be the defining factor. These hypotheses have been analyzed in detail in Ref. 14. At the same time, the results of extensive re ...
properties of the high area-to-mass ratio space debris population in
... The ESA surveys since 1999 provide a large amount of statistical information. By statistical we mean first of all that no attempt was made to catalogue the objects, which would have required follow-up observations for all objects. Objects may therefore have been observed multiple times. The data is ...
... The ESA surveys since 1999 provide a large amount of statistical information. By statistical we mean first of all that no attempt was made to catalogue the objects, which would have required follow-up observations for all objects. Objects may therefore have been observed multiple times. The data is ...
A young protoplanet candidate embedded in the circumstellar disk
... [OI] (Acke & van den Ancker 2006) and OH (Liskowsky et al. 2012) dynamic evidence for such an object was found. In the case of OH the emission is thought to arise from an eccentric inner rim of the outer disk with the eccentricity being introduced by a planet. The outer disk has been resolved at mul ...
... [OI] (Acke & van den Ancker 2006) and OH (Liskowsky et al. 2012) dynamic evidence for such an object was found. In the case of OH the emission is thought to arise from an eccentric inner rim of the outer disk with the eccentricity being introduced by a planet. The outer disk has been resolved at mul ...
CAUTION : Never Look Directly At The Light From A Laser
... with a micrometer caliper. Assuming that the ground edges on the razor blades are alike, the spacing d of the lines is just the thickness of one blade. Mount your double slit in a spring clip in front of the helium-neon laser, with the slits horizontal. Mount the metal plate screen with the millimet ...
... with a micrometer caliper. Assuming that the ground edges on the razor blades are alike, the spacing d of the lines is just the thickness of one blade. Mount your double slit in a spring clip in front of the helium-neon laser, with the slits horizontal. Mount the metal plate screen with the millimet ...
Does feedback help or hinder star formation? The effect of
... the collapse as the gas cools and creates a filamentary structure of dense regions, instead of a centralised collapse. Since we did not want the cloud to be strongly distorted by its turbulence, we removed the lower order modes to avoid the large-scale perturbations. We also used an upper limit, cor ...
... the collapse as the gas cools and creates a filamentary structure of dense regions, instead of a centralised collapse. Since we did not want the cloud to be strongly distorted by its turbulence, we removed the lower order modes to avoid the large-scale perturbations. We also used an upper limit, cor ...
Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... super-Eddington accretion • During this episode a powerful expended evelope was formed • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absorption column, smeared and probably delayed variability of fluoresc ...
... super-Eddington accretion • During this episode a powerful expended evelope was formed • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absorption column, smeared and probably delayed variability of fluoresc ...
Optical Properties of Nanostructures
... • Independent scattering : If there is no interference between the wave scattered by each particle, scattering is independent. The global scattered intensity is the sum of the intensities scattered by each particle. As an approximative criterium, it can be considered that independent scattering occu ...
... • Independent scattering : If there is no interference between the wave scattered by each particle, scattering is independent. The global scattered intensity is the sum of the intensities scattered by each particle. As an approximative criterium, it can be considered that independent scattering occu ...
SpeX Observing Manual - NASA Infrared Telescope Facility
... targets whatever the brightness. This allows any systematic effects in the data to be removed by applying a median combination to the spectra. The most prominent of these effects are the star-like features that are randomly distributed on the array due alpha-particle decays from Thorium used in the ...
... targets whatever the brightness. This allows any systematic effects in the data to be removed by applying a median combination to the spectra. The most prominent of these effects are the star-like features that are randomly distributed on the array due alpha-particle decays from Thorium used in the ...
Part 1
... our advantage, with the goal of getting a better result than would be possible with even a perfectly rigid mask. In this way, our approach is akin to adaptive optics, where the shapes of flexible optical elements are controlled to correct for atmospheric turbulence. With AMM, we seek to measure and ...
... our advantage, with the goal of getting a better result than would be possible with even a perfectly rigid mask. In this way, our approach is akin to adaptive optics, where the shapes of flexible optical elements are controlled to correct for atmospheric turbulence. With AMM, we seek to measure and ...
01.1PART I_Ch1.fm - The Thunderbolts Project
... theory. A mistaken supposition has not only prevented intelligent and sincere investigators from seeing what would otherwise be ...
... theory. A mistaken supposition has not only prevented intelligent and sincere investigators from seeing what would otherwise be ...
Distribution of streaming rates into high
... The ART simulations were run with the AMR code ART (Kravtsov, Klypin & Khokhlov 1997; Kravtsov 2003) with a spatial resolution better than 70 pc in physical units. It incorporates the relevant physical processes for galaxy formation that are: gas cooling, photoionization heating, star formation, met ...
... The ART simulations were run with the AMR code ART (Kravtsov, Klypin & Khokhlov 1997; Kravtsov 2003) with a spatial resolution better than 70 pc in physical units. It incorporates the relevant physical processes for galaxy formation that are: gas cooling, photoionization heating, star formation, met ...
Comprehensive and reliable diagnostics for the corona of laser
... higher plasma density, and longer wavelength is preferred to obtain a significant phase shift in the under-dense region. Relatively large-scale plasma size is required for efficient EUVL sources [9] and laser fusion research, and there is a steep gradient in density profile. The refraction induced b ...
... higher plasma density, and longer wavelength is preferred to obtain a significant phase shift in the under-dense region. Relatively large-scale plasma size is required for efficient EUVL sources [9] and laser fusion research, and there is a steep gradient in density profile. The refraction induced b ...
Comparing Single-Epoch Virial Black Hole Mass Estimators for
... We use a homogeneous sample of 60 intermediate-redshift (z ∼ 1.5 − 2.2) quasars with optical and near-infrared spectra covering CIV through Hα to investigate the relations between single-epoch virial black hole (BH) mass estimators based on different lines. We critically compare restframe UV line es ...
... We use a homogeneous sample of 60 intermediate-redshift (z ∼ 1.5 − 2.2) quasars with optical and near-infrared spectra covering CIV through Hα to investigate the relations between single-epoch virial black hole (BH) mass estimators based on different lines. We critically compare restframe UV line es ...
OGLE 2008–BLG–290: an accurate measurement of the limb
... The first well-documented source-resolving, causticcrossing microlensing event was MACHO Alert 95−30 (Alcock et al. 1997), in which an M4 III giant source star was scanned by the point-like caustic of a single lens. The observations permitted measurement of the source size and detection of its limb ...
... The first well-documented source-resolving, causticcrossing microlensing event was MACHO Alert 95−30 (Alcock et al. 1997), in which an M4 III giant source star was scanned by the point-like caustic of a single lens. The observations permitted measurement of the source size and detection of its limb ...
3 Introduction to Add
... by the two identical gratings. These reflected signals interfere in the 3dB coupler in such a way that the signal is dropped and the back-reflected light intensity arriving at port1 is zero, providing the coupler is well matched (50% splitter). The transmitted wavelengths are made to interfere in th ...
... by the two identical gratings. These reflected signals interfere in the 3dB coupler in such a way that the signal is dropped and the back-reflected light intensity arriving at port1 is zero, providing the coupler is well matched (50% splitter). The transmitted wavelengths are made to interfere in th ...
Theory of Motion of Matter on the Formation of Galaxy and Star
... Way Galaxy will not have been the current state, but a huge solid celestial body formed by the gathering of all material celestial bodies in Milky Way Galaxy. Only the energy change of relative motion among numerous material particles can produce material systems independent to each other. At the in ...
... Way Galaxy will not have been the current state, but a huge solid celestial body formed by the gathering of all material celestial bodies in Milky Way Galaxy. Only the energy change of relative motion among numerous material particles can produce material systems independent to each other. At the in ...
Chapter 2.1 - Focusing Fundamentals
... have plenty of light to work with while you focus, and so does the automatic focuser found in most of today’s cameras. Professional film cameras allow you to focus by looking at a ground glass screen that is conveniently located exactly the same distance from the camera lens as the film. The scene i ...
... have plenty of light to work with while you focus, and so does the automatic focuser found in most of today’s cameras. Professional film cameras allow you to focus by looking at a ground glass screen that is conveniently located exactly the same distance from the camera lens as the film. The scene i ...
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.