Craig Miles, The Anthropic and Temporal Conditions for the Mormon
... the water will freeze; if it is too close the water will evaporate. Thus, the planet must have a nearly circular orbit at a proper distance from its star. The gravity at the surface of the planet must not be too large or too small. If it is too large, land masses will not rise above the oceans. Even ...
... the water will freeze; if it is too close the water will evaporate. Thus, the planet must have a nearly circular orbit at a proper distance from its star. The gravity at the surface of the planet must not be too large or too small. If it is too large, land masses will not rise above the oceans. Even ...
Second-Surface Silvered Glass Solar Mirrors of Very
... of thin film dielectric layers between the silver and the glass back surface. Dielectric layers have been designed and used to boost the performance of front-surface silvered mirrors. For example, broad-band boosted coatings for astronomy have been previously described by Macleod in the paper by Son ...
... of thin film dielectric layers between the silver and the glass back surface. Dielectric layers have been designed and used to boost the performance of front-surface silvered mirrors. For example, broad-band boosted coatings for astronomy have been previously described by Macleod in the paper by Son ...
Formation and composition of planets around very low mass stars
... the planetary mass: planets that do not contain a lot of water are generally of lower mass (below ∼ 1M⊕ , although some can be as massive as ∼ 1.5M⊕ ), and planets totally devoid of water are all less massive than 1M⊕ , and even lower than 0.4M⊕ if one does not consider the massive disks. This can b ...
... the planetary mass: planets that do not contain a lot of water are generally of lower mass (below ∼ 1M⊕ , although some can be as massive as ∼ 1.5M⊕ ), and planets totally devoid of water are all less massive than 1M⊕ , and even lower than 0.4M⊕ if one does not consider the massive disks. This can b ...
the light behavior 0807 towards a mirror surface
... used where interference fringes are generated when two spliced light rays from the same light source are slightly phase shifted in time. In time/distance measurements, time and distance are determined separately, then the light velocity is calculated by the common relation v=s/t (see 0101). ...
... used where interference fringes are generated when two spliced light rays from the same light source are slightly phase shifted in time. In time/distance measurements, time and distance are determined separately, then the light velocity is calculated by the common relation v=s/t (see 0101). ...
SPATIAL STUDY WITH THE VERY LARGE TELESCOPE OF A NEW
... 1998), provided by the service mode, and takes into account average IR atmospheric extinction on Paranal (0.11, 0.06, and 0.07 mag per air mass for J, H, and Ks, respectively). We used the same method as described above for our NTT data to produce the resulting color composite image presented in Fig ...
... 1998), provided by the service mode, and takes into account average IR atmospheric extinction on Paranal (0.11, 0.06, and 0.07 mag per air mass for J, H, and Ks, respectively). We used the same method as described above for our NTT data to produce the resulting color composite image presented in Fig ...
Simulations for Multi-Object Spectrograph Planet Surveys
... of a particularly unique design which does not utilise an echelle spectrograph. A prototype of the instrument, called Exoplanet Tracker (ET), was used by van Eyken et al. (2004) to detect the radial velocity signature of the planet orbiting 51 Peg. The Exoplanet Tracker is a fibre-fed dispersed fixe ...
... of a particularly unique design which does not utilise an echelle spectrograph. A prototype of the instrument, called Exoplanet Tracker (ET), was used by van Eyken et al. (2004) to detect the radial velocity signature of the planet orbiting 51 Peg. The Exoplanet Tracker is a fibre-fed dispersed fixe ...
Analysis of white dwarfs with strange-matter cores
... for 10 white dwarfs in visual binaries or common proper-motion systems as well as 11 field white dwarfs. Complementary HST observations have also been made, for example to better determine the spectroscopy for Procyon B [25] and the pulsation of G226-29 [19]. Procyon B at first appeared as a compact ...
... for 10 white dwarfs in visual binaries or common proper-motion systems as well as 11 field white dwarfs. Complementary HST observations have also been made, for example to better determine the spectroscopy for Procyon B [25] and the pulsation of G226-29 [19]. Procyon B at first appeared as a compact ...
pptx - Serbian Virtual Observatory
... - optimisation of performances - cold light from hot atoms and molecules . (white light 3000-5000K, discharge up to 45000K), . high electron density (strong and broad emission in the visible spectrum - Fluorescent lamps: improving efficacity (phosphors) ...
... - optimisation of performances - cold light from hot atoms and molecules . (white light 3000-5000K, discharge up to 45000K), . high electron density (strong and broad emission in the visible spectrum - Fluorescent lamps: improving efficacity (phosphors) ...
Nuclear astrophysics: the unfinished quest for the origin of the
... Most of the ordinary (visible) matter in the Universe, from a tiny terrestrial pebble to a giant star, is composed of protons and neutrons (nucleons). These nucleons can assemble in a suite of different nuclear configurations. The masses of such bound nuclei are actually smaller than the sum of the ...
... Most of the ordinary (visible) matter in the Universe, from a tiny terrestrial pebble to a giant star, is composed of protons and neutrons (nucleons). These nucleons can assemble in a suite of different nuclear configurations. The masses of such bound nuclei are actually smaller than the sum of the ...
Radially and azimuthally polarized beams generated by space
... Singularities in optical fields have received much attention lately.1 Such singularities appear at points or lines where the phase or the amplitude of the wave is undef ined or changes abruptly. One class of dislocation is vortices, which are spiral phase ramps about a singularity. Vortices are H ch ...
... Singularities in optical fields have received much attention lately.1 Such singularities appear at points or lines where the phase or the amplitude of the wave is undef ined or changes abruptly. One class of dislocation is vortices, which are spiral phase ramps about a singularity. Vortices are H ch ...
Why use LEDs? www.vexica.com
... and LM70 which is the ;me it will take a given LED to reach 80% and 70% light output respec;vely, although the higher LM80 standard is fast becoming the norm. The LM80 test procedure addresses o ...
... and LM70 which is the ;me it will take a given LED to reach 80% and 70% light output respec;vely, although the higher LM80 standard is fast becoming the norm. The LM80 test procedure addresses o ...
![arXiv:0705.3323v2 [astro-ph] 12 Oct 2007](http://s1.studyres.com/store/data/014343898_1-81883919b9b58f47cea02891b863ef0c-300x300.png)
arXiv:0705.3323v2 [astro-ph] 12 Oct 2007
... 2007). These are easily affected by smooth changes to the galaxy clustering amplitude as a function of scale. In this paper, we use a more robust approach: the BAO scale is defined via the locations where the BAO cross a smooth fit to the power spectrum. Ideally we would use the BAO within two galax ...
... 2007). These are easily affected by smooth changes to the galaxy clustering amplitude as a function of scale. In this paper, we use a more robust approach: the BAO scale is defined via the locations where the BAO cross a smooth fit to the power spectrum. Ideally we would use the BAO within two galax ...
PowerPoint - Division for Planetary Sciences
... Measuring the Size of Distant Objects • Previous estimates of Eris’ size relied on a combination of observations of its reflected or emitted light and assumptions about its reflectivity or surface temperature • The recent measurements took advantage of a stellar occultation – an event where Eris pa ...
... Measuring the Size of Distant Objects • Previous estimates of Eris’ size relied on a combination of observations of its reflected or emitted light and assumptions about its reflectivity or surface temperature • The recent measurements took advantage of a stellar occultation – an event where Eris pa ...
astro-ph/9704019 2 Apr 1997 - National Optical Astronomy
... have collectively been referred to as the faint blue galaxy problem (Kron 1978). In its simplest manifestation, this is that an apparent excess of faint blue galaxies is seen in the source counts over the number expected on the basis of local galaxy properties. A more specific version of the problem ...
... have collectively been referred to as the faint blue galaxy problem (Kron 1978). In its simplest manifestation, this is that an apparent excess of faint blue galaxies is seen in the source counts over the number expected on the basis of local galaxy properties. A more specific version of the problem ...
A search for nearby counterparts to the moving objects in the Hubble
... Accepted 2000 October 9. Received 2000 October 9; in original form 1999 December 29 ...
... Accepted 2000 October 9. Received 2000 October 9; in original form 1999 December 29 ...
Diffraction
... secondary maxima to the intensity of the central maximum for the single-slit diffraction pattern. ...
... secondary maxima to the intensity of the central maximum for the single-slit diffraction pattern. ...
The Formation of Massive Stars - Max-Planck
... These massive dense clumps have masses between a few 100 and a few 1000 M , sizes on the order of 0.25–0.5 pc, mean densities of 105 cm–3, and temperatures on the order of 16 K. While the masses and densities are typical for highmass star-forming regions, the temperatures derived, for example, from ...
... These massive dense clumps have masses between a few 100 and a few 1000 M , sizes on the order of 0.25–0.5 pc, mean densities of 105 cm–3, and temperatures on the order of 16 K. While the masses and densities are typical for highmass star-forming regions, the temperatures derived, for example, from ...
The mass-loss return from evolved stars to the Large Magellanic Cloud
... The study of Milky Way AGB stars is inhibited by the presence of substantial interstellar extinction, and large uncertainties in distance determinations. The Large Magellanic Cloud (LMC) offers the combination of proximity (∼50 kpc; van Leeuwen et al. 2007), low line-of-sight extinction (E(B − V) ∼ 0 ...
... The study of Milky Way AGB stars is inhibited by the presence of substantial interstellar extinction, and large uncertainties in distance determinations. The Large Magellanic Cloud (LMC) offers the combination of proximity (∼50 kpc; van Leeuwen et al. 2007), low line-of-sight extinction (E(B − V) ∼ 0 ...
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.