PDF only - at www.arxiv.org.
... minimize the reflection of light that couples from (low-index) air to a relatively high-index medium (glass, semiconductors, etc.). As result, advances in optically-smooth AR coatings cannot be applied to the reciprocal geometry, where the light couples from a high-index media [such as (O)LEDs or sc ...
... minimize the reflection of light that couples from (low-index) air to a relatively high-index medium (glass, semiconductors, etc.). As result, advances in optically-smooth AR coatings cannot be applied to the reciprocal geometry, where the light couples from a high-index media [such as (O)LEDs or sc ...
Toward $ ab\, initio $ extremely metal poor stars
... We ray-traced ionizing radiation from the star particle to compute the dynamical expansion of the HII region over the star’s lifetime of 3.5 Myr. The ionization state and temperature along each separate ray in the HII region interior were evaluated by interpolating from values pre-computed with the ...
... We ray-traced ionizing radiation from the star particle to compute the dynamical expansion of the HII region over the star’s lifetime of 3.5 Myr. The ionization state and temperature along each separate ray in the HII region interior were evaluated by interpolating from values pre-computed with the ...
Hubble Space Telescope snapshot survey of 3CR quasars: The Data
... NOTES.ÈCol. (1) : 3CR source designation. Col. (2) : number of separate exposures each with the exposure time in listed in col. (3). The total integration time is given by multiplying cols. (2) and (3). Col. (3) : integration time in seconds per exposure. Col. (4) : date of observation. The two expo ...
... NOTES.ÈCol. (1) : 3CR source designation. Col. (2) : number of separate exposures each with the exposure time in listed in col. (3). The total integration time is given by multiplying cols. (2) and (3). Col. (3) : integration time in seconds per exposure. Col. (4) : date of observation. The two expo ...
Using Parallax to Measure the Distance of Stars
... One of the most difficult problems in astronomy is determining the distances to objects in the sky. There are four basic methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby ...
... One of the most difficult problems in astronomy is determining the distances to objects in the sky. There are four basic methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby ...
Introduction to Astronomy
... out to be false. But other knowledge, including advanced math and the rational thought, were used as the skills needed to allow modern western culture to expand The Catholic Church accepted the ancient philosophies of the Universe, including Ptolemy’s theory that the sun orbited the earth and that t ...
... out to be false. But other knowledge, including advanced math and the rational thought, were used as the skills needed to allow modern western culture to expand The Catholic Church accepted the ancient philosophies of the Universe, including Ptolemy’s theory that the sun orbited the earth and that t ...
stellar diameters and temperatures. iii. main-sequence a, f, g
... uniform disk θUD and limb-darkened θLD angular diameter functions, as defined in Hanbury Brown et al. (1974). We use a nonlinear least-squares fitting routine written in IDL to solve for each value of θUD and θLD as well as the errors, assuming a reduced χ 2 = 1. In order to correct for limbdarkenin ...
... uniform disk θUD and limb-darkened θLD angular diameter functions, as defined in Hanbury Brown et al. (1974). We use a nonlinear least-squares fitting routine written in IDL to solve for each value of θUD and θLD as well as the errors, assuming a reduced χ 2 = 1. In order to correct for limbdarkenin ...
Comets review.fm - Journals at the University of Arizona
... “Interrelations.” Every part contains several excellent reviews of related topics, for a total of 37 papers. Most of the papers contain numerous black-and-white illustrations that are very useful in following the general arguments. There is also a section with color diagrams and pictures at the end ...
... “Interrelations.” Every part contains several excellent reviews of related topics, for a total of 37 papers. Most of the papers contain numerous black-and-white illustrations that are very useful in following the general arguments. There is also a section with color diagrams and pictures at the end ...
Comparison of the Phenomena of Light Refraction and Gravitational
... In 1916 Einstein realized that it was also necessary to scale the unit of radial distance [16]. This development was key to his successful prediction of the angle of displacement of star images during solar eclipses. Failure to scale the radial distance as well leads to exactly half the correct valu ...
... In 1916 Einstein realized that it was also necessary to scale the unit of radial distance [16]. This development was key to his successful prediction of the angle of displacement of star images during solar eclipses. Failure to scale the radial distance as well leads to exactly half the correct valu ...
WIND-INTERACTION MODELS FOR THE EARLY AFTERGLOWS
... at lower frequencies should be the same as that of the R-band at the break, namely about 0.83 mJy, which is well below the 86 GHz measurement. This discrepancy was also noted by Pandey et al. (2002). The relatively high 86 GHz flux is not a problem for our model, where the transition to slow cooling ...
... at lower frequencies should be the same as that of the R-band at the break, namely about 0.83 mJy, which is well below the 86 GHz measurement. This discrepancy was also noted by Pandey et al. (2002). The relatively high 86 GHz flux is not a problem for our model, where the transition to slow cooling ...
Wave Optics
... the same place, the resultant disturbance is the sum of the disturbances from the individual waves. In the chapter 17 context, we were talking about mechanical waves. But the principle holds for electromagnetic waves as well. ...
... the same place, the resultant disturbance is the sum of the disturbances from the individual waves. In the chapter 17 context, we were talking about mechanical waves. But the principle holds for electromagnetic waves as well. ...
Wave Optics
... the same place, the resultant disturbance is the sum of the disturbances from the individual waves. In the chapter 17 context, we were talking about mechanical waves. But the principle holds for electromagnetic waves as well. ...
... the same place, the resultant disturbance is the sum of the disturbances from the individual waves. In the chapter 17 context, we were talking about mechanical waves. But the principle holds for electromagnetic waves as well. ...
Active Control of Rogue Waves for Stimulated Supercontinuum
... Corning HNL ZD 1550) with very low dispersion at 1550 nm. The pump pulses are 3:7 ps in duration, as determined by autocorrelation. A weak seed pulse (0.01% of the pump intensity) derived from the same source, but with a shifted center frequency (1630 nm), is produced by broadening a portion of th ...
... Corning HNL ZD 1550) with very low dispersion at 1550 nm. The pump pulses are 3:7 ps in duration, as determined by autocorrelation. A weak seed pulse (0.01% of the pump intensity) derived from the same source, but with a shifted center frequency (1630 nm), is produced by broadening a portion of th ...
General law of universal gravitation (PDF Available)
... value is approximately 9.80 m/s2 [1]. 2.3. The Gravitational Field Some scientists asked Newton “how is it possible for masses or objects to interact when they were not in contact with each other such as the sun and planets around the sun”. In fact, Newton was not able to answer this question [1]. T ...
... value is approximately 9.80 m/s2 [1]. 2.3. The Gravitational Field Some scientists asked Newton “how is it possible for masses or objects to interact when they were not in contact with each other such as the sun and planets around the sun”. In fact, Newton was not able to answer this question [1]. T ...
30.4 Gravitational collapse & early protostellar evolution I (HB)
... the protostar can be described by its entropy profile s(Mr), reflecting the changing conditions at the accretion shock. - Since s represents heat content of each added mass shell, an increase of s(MR) causes a swelling of the protostar. - In the absence of nuclear burning, an increasing s(Mr) arises ...
... the protostar can be described by its entropy profile s(Mr), reflecting the changing conditions at the accretion shock. - Since s represents heat content of each added mass shell, an increase of s(MR) causes a swelling of the protostar. - In the absence of nuclear burning, an increasing s(Mr) arises ...
The star formation histories of two northern LMC fields
... the star formation rate in these fields, beginning approximately 2.5 Gyr ago, with the current metallicity in the region being Fe=H 20:38 ^ 0:10: The two fields have had very similar star formation rates until 200 Myr ago, at which point one shows a large increase. Key words: Magellanic Clouds ± ...
... the star formation rate in these fields, beginning approximately 2.5 Gyr ago, with the current metallicity in the region being Fe=H 20:38 ^ 0:10: The two fields have had very similar star formation rates until 200 Myr ago, at which point one shows a large increase. Key words: Magellanic Clouds ± ...
CoRoT pictures transiting exoplanets
... gaseous planets, whose transits (1-3% deep, 2-3 hour long) were easily detected from ground-based telescopes of small size (typically less than 1m). In this article, we will review the findings of the CoRoT mission in its search for exoplanets. After describing the mission concept and instrument, we ...
... gaseous planets, whose transits (1-3% deep, 2-3 hour long) were easily detected from ground-based telescopes of small size (typically less than 1m). In this article, we will review the findings of the CoRoT mission in its search for exoplanets. After describing the mission concept and instrument, we ...
Introduction to Diffraction Grating
... layer of aluminum by vacuum deposition. Parallel, equally spaced grooves are ruled in a groove profile. The ruling engine must be able to retrace the exact path of the diamond forming tool on each stroke and to index (advance) the substrate a predetermined amount after each cut. Numerous test gratin ...
... layer of aluminum by vacuum deposition. Parallel, equally spaced grooves are ruled in a groove profile. The ruling engine must be able to retrace the exact path of the diamond forming tool on each stroke and to index (advance) the substrate a predetermined amount after each cut. Numerous test gratin ...
Conference title, upper and lower case, bolded, 18 point type
... scales, while periodic on a larger scale [6–15] (typically on the order of a micron). The largescale periodicity provides a finite computational cell for calculations, making such structures amenable to simulation and optimization. Theoretically, it has been predicted that structures with optimized ...
... scales, while periodic on a larger scale [6–15] (typically on the order of a micron). The largescale periodicity provides a finite computational cell for calculations, making such structures amenable to simulation and optimization. Theoretically, it has been predicted that structures with optimized ...
Magnetic fields in O-, B- and A-type stars on the main sequence
... and when emerging at the surface would produce hot bright spots at the surface of massive stars. So far there are no direct observations of these fields because they lead to small-scaled structure of weak strengths. However, there is increasing evidence of indirect observations of such fields in hot s ...
... and when emerging at the surface would produce hot bright spots at the surface of massive stars. So far there are no direct observations of these fields because they lead to small-scaled structure of weak strengths. However, there is increasing evidence of indirect observations of such fields in hot s ...
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.