Stonehenge: An Introduction to the concept of the Heaven`s Hinge
... Although science was in its infancy, the people of the time may have felt that they were undergoing the first industrial revolution: Copper was being produced and with the invention of the saw, the size of trees cut down suddenly increased. So did the size of tree-trunks used to make structures. Cor ...
... Although science was in its infancy, the people of the time may have felt that they were undergoing the first industrial revolution: Copper was being produced and with the invention of the saw, the size of trees cut down suddenly increased. So did the size of tree-trunks used to make structures. Cor ...
Luminosity profiles and sizes of massive star clusters in NGC 7252
... far they extend. We were also interested in studying whether the presence or absence of any extended envelope might correlate with the projected distance of clusters from the remnant’s centre, which would be expected if the tidal truncation of clusters in the galaxy potential would already have had ...
... far they extend. We were also interested in studying whether the presence or absence of any extended envelope might correlate with the projected distance of clusters from the remnant’s centre, which would be expected if the tidal truncation of clusters in the galaxy potential would already have had ...
and octa-substituted gallium and indium phthalocyanines
... large pconjugated systems, provides an efficient non-radiative energy relaxation pathway, thereby shortening the excited state lifetimes and greatly reducing the photosensitizing efficiency [20,21]. The nature of peripheral substituents influences the degree of aggregation, with bulky groups reducing thi ...
... large pconjugated systems, provides an efficient non-radiative energy relaxation pathway, thereby shortening the excited state lifetimes and greatly reducing the photosensitizing efficiency [20,21]. The nature of peripheral substituents influences the degree of aggregation, with bulky groups reducing thi ...
Structural and optical properties of visible active
... From the Beer–Lambert’s law, I 5 I0 10–ecd, where e is the extinction coefficient (eD35 5 31300 M1/cm), c the concentration, and d the thickness, the D35 concentration on the WO 3 film was determined to 0.0013 mM, which corresponds to 0.0013 lmol/cm2 or 7.82 1014 molecules/cm2. A Hg arc lamp oper ...
... From the Beer–Lambert’s law, I 5 I0 10–ecd, where e is the extinction coefficient (eD35 5 31300 M1/cm), c the concentration, and d the thickness, the D35 concentration on the WO 3 film was determined to 0.0013 mM, which corresponds to 0.0013 lmol/cm2 or 7.82 1014 molecules/cm2. A Hg arc lamp oper ...
ASTE Simultaneous HCN(4–3) and HCO+(4–3)
... in an AGN, high energy generation efficiency with 6–42% of Mc2 (M is the mass of accreting material; Thorne 1974) is achieved, producing a very high emission surface brightness with >1013 L¯ kpc−2 (Soifer et al. 2000). These differences between a starburst and an AGN could create differences in the ...
... in an AGN, high energy generation efficiency with 6–42% of Mc2 (M is the mass of accreting material; Thorne 1974) is achieved, producing a very high emission surface brightness with >1013 L¯ kpc−2 (Soifer et al. 2000). These differences between a starburst and an AGN could create differences in the ...
Stellar Structure and Evolution
... given for several years to third-year undergraduate students in physics at the University of Aarhus. The goal of the course and the notes is to show how many aspects of stellar evolution can be understood relatively simply in terms of basic physics. Apart from the intrinsic interest of the topic, th ...
... given for several years to third-year undergraduate students in physics at the University of Aarhus. The goal of the course and the notes is to show how many aspects of stellar evolution can be understood relatively simply in terms of basic physics. Apart from the intrinsic interest of the topic, th ...
What does the EUV and thin film group do?
... – interact strongly with all matter – Human hair is 100 micron. – Characteristic absorption length is 0.01 to 0.1 micron – Refractive index is ~1 ...
... – interact strongly with all matter – Human hair is 100 micron. – Characteristic absorption length is 0.01 to 0.1 micron – Refractive index is ~1 ...
Estimating Canopy Light Interception and
... (CR10, Campbell Scienti®c Ltd., Leics, UK) which recorded the radiation every 60 s throughout the day. One sensor was placed horizontally above the canopy to measure incoming PAR. To compare measurements from dierent days, the leaf light interception data were expressed as a fraction of the daily i ...
... (CR10, Campbell Scienti®c Ltd., Leics, UK) which recorded the radiation every 60 s throughout the day. One sensor was placed horizontally above the canopy to measure incoming PAR. To compare measurements from dierent days, the leaf light interception data were expressed as a fraction of the daily i ...
Krypton in presolar mainstream SiC grains from AGB stars
... (80 Kr/82 Kr)G anticorrelation is that AGB stars with an initial mass of 3 M produce coarse SiC grains, whereas AGB stars with an initial mass of 1.5 M produce fine SiC grains. In Fig. 4 we report the Kr−S isotopic ratios predicted at the last third dredge−up episode (25th TP) for an AGB star with ...
... (80 Kr/82 Kr)G anticorrelation is that AGB stars with an initial mass of 3 M produce coarse SiC grains, whereas AGB stars with an initial mass of 1.5 M produce fine SiC grains. In Fig. 4 we report the Kr−S isotopic ratios predicted at the last third dredge−up episode (25th TP) for an AGB star with ...
Chapter 36 . Optical Properties of Semiconductors
... of measurements and physical processes characteristic of various regions of interest involving the optical properties of semiconductors. The electromagnetic spectrum accessible for studies by optical radiation is depicted in Fig. 1a and b where both the photon wavelengths and photon energies, as wel ...
... of measurements and physical processes characteristic of various regions of interest involving the optical properties of semiconductors. The electromagnetic spectrum accessible for studies by optical radiation is depicted in Fig. 1a and b where both the photon wavelengths and photon energies, as wel ...
Properties of Galactic B supergiants
... In contrast, B supergiants have received rather less attention since they are less relevant for energetics of young starbursts. Nevertheless, they are visually bright, typically MV = −7.0 mag, possess larger radii and so are easy to observe individually in nearby galaxies, permitting robust tests of ...
... In contrast, B supergiants have received rather less attention since they are less relevant for energetics of young starbursts. Nevertheless, they are visually bright, typically MV = −7.0 mag, possess larger radii and so are easy to observe individually in nearby galaxies, permitting robust tests of ...
The white dwarf population within 40 pc of the Sun
... smaller than ∼ 10 M⊙ will end their lives as white dwarfs (Garcı́a-Berro et al. 1997; Poelarends et al. 2008). Hence, given the shape of the initial mass function, the local population of white dwarfs carries crucial information about the physical processes governing the evolution of the vast majori ...
... smaller than ∼ 10 M⊙ will end their lives as white dwarfs (Garcı́a-Berro et al. 1997; Poelarends et al. 2008). Hence, given the shape of the initial mass function, the local population of white dwarfs carries crucial information about the physical processes governing the evolution of the vast majori ...
Catalogues of isolated galaxies, isolated pairs, and isolated triplets
... The data is based on the Tenth Data Release of the SDSS (DR10; Ahn et al. 2013). We defined a primary sample composed of galaxies from the main spectroscopic sample (Strauss et al. 2002) with r-band (the deepest SDSS images) model magnitudes in the range 11 ≤ mr ≤ 15.7 (sufficient to develop a homog ...
... The data is based on the Tenth Data Release of the SDSS (DR10; Ahn et al. 2013). We defined a primary sample composed of galaxies from the main spectroscopic sample (Strauss et al. 2002) with r-band (the deepest SDSS images) model magnitudes in the range 11 ≤ mr ≤ 15.7 (sufficient to develop a homog ...
Observational motivation for Dark Matter
... but Baryons and photons are still connected Due to abundance of photons, only when T~eV matter suddenly recombines Transfer from Thomson cross section to neutral Hydrogen makes the universe transparent to photons (but not to electrons!) Requires a full solution of the ionization and ...
... but Baryons and photons are still connected Due to abundance of photons, only when T~eV matter suddenly recombines Transfer from Thomson cross section to neutral Hydrogen makes the universe transparent to photons (but not to electrons!) Requires a full solution of the ionization and ...
Debris disks: seeing dust, thinking of planetesimals and planets
... one or several planets. As Wyatt (2008) pointed out, at the end of the protoplanetary phase, a star is expected to be surrounded by at least one but perhaps all of the following components: various planets from sub-Earth to super-Jupiter size; remnants of the protoplanetary disk, both dust and gas; ...
... one or several planets. As Wyatt (2008) pointed out, at the end of the protoplanetary phase, a star is expected to be surrounded by at least one but perhaps all of the following components: various planets from sub-Earth to super-Jupiter size; remnants of the protoplanetary disk, both dust and gas; ...
Stars: Stellar Evol & “death” Galaxies Astronomy 1 — Elementary Astronomy
... A. It would inevitably get sucked into the black hole with no possibility of escape. B. It would detect the gravitational pull of the black hole and be able to go into orbit around it. C. It would be unable to locate the black hole because it’s, well, black. D. It would be repelled by the black hole ...
... A. It would inevitably get sucked into the black hole with no possibility of escape. B. It would detect the gravitational pull of the black hole and be able to go into orbit around it. C. It would be unable to locate the black hole because it’s, well, black. D. It would be repelled by the black hole ...
How to Build an Astrolabe - St John`s College, Cambridge
... eccentricities, cannot be a truly accurate model. It will become less accurate over time as the earth’s position relative to the stars shifts in small, but perceptible amounts. * the conversion between a date and a point in the Zodiac only allows for non-leap years, so in leap years it will be less ...
... eccentricities, cannot be a truly accurate model. It will become less accurate over time as the earth’s position relative to the stars shifts in small, but perceptible amounts. * the conversion between a date and a point in the Zodiac only allows for non-leap years, so in leap years it will be less ...
Practical Aspects of Mirror Usage in Optical Systems for
... conditions and then to calculate the ...
... conditions and then to calculate the ...
Practical Aspects of Mirror Usage in Optical Systems for
... conditions and then to calculate the ...
... conditions and then to calculate the ...
LATE STAGES OF CLOSE BINARY SYSTEMS 1. Introduction The X
... (1976) show that helium stars more massive than about 3 A f d o not expand to radii larger than about 2R® during helium and carbon burning, whereas helium stars with masses < 2 . 2 5 / ? w i l l , during helium shell burning move to the giant region. Table III, after Arnett (1975) lists the radii of ...
... (1976) show that helium stars more massive than about 3 A f d o not expand to radii larger than about 2R® during helium and carbon burning, whereas helium stars with masses < 2 . 2 5 / ? w i l l , during helium shell burning move to the giant region. Table III, after Arnett (1975) lists the radii of ...
Astronomers` Observing Guides
... leisurely celestial exploration with the telescope. It is estimated that at least 80 percent of the stellar population exists as pairs and multiple groupings. Abounding among the naked-eye stars, they are visible with even the smallest of instruments on all but the worst of nights – even in bright m ...
... leisurely celestial exploration with the telescope. It is estimated that at least 80 percent of the stellar population exists as pairs and multiple groupings. Abounding among the naked-eye stars, they are visible with even the smallest of instruments on all but the worst of nights – even in bright m ...
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.