The e-Science in the Transient Radio Sky Soon
... Spectral slope is fastly evolved from negative, flat to positive, even within a week or two. The cause for turnover is in dispute. ...
... Spectral slope is fastly evolved from negative, flat to positive, even within a week or two. The cause for turnover is in dispute. ...
Device for projecting and viewing stereoscopic pictures
... ing to the invention use is made not only of the backward rays, but also of the lateral sess the disadvantage that they have a right rays which are usually lost. In this manner and a wrong side, one of theends having about twice as many rays are utilized and to be placed before the eyes: if the othe ...
... ing to the invention use is made not only of the backward rays, but also of the lateral sess the disadvantage that they have a right rays which are usually lost. In this manner and a wrong side, one of theends having about twice as many rays are utilized and to be placed before the eyes: if the othe ...
Document
... – An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). • What is the significance of the main sequence? – Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram. – A star's mass determines its position along t ...
... – An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). • What is the significance of the main sequence? – Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram. – A star's mass determines its position along t ...
Bamberg_VanGrootel - ORBi
... i.e., stars that experience a delayed He-flash during contraction, at higher Teff, after leaving the RGB before tip (H-burning shell stops due to strong mass loss on RGB) D’Cruz et al. (1996) showed that such stars populate the EHB, with similar ...
... i.e., stars that experience a delayed He-flash during contraction, at higher Teff, after leaving the RGB before tip (H-burning shell stops due to strong mass loss on RGB) D’Cruz et al. (1996) showed that such stars populate the EHB, with similar ...
pyrene on Au(111) - American Chemical Society
... II spectra that were measured during the growth of the NP film. The bottom spectrum is the clean Au(111) film on mica. Subsequent depositions of the aromatic molecule show the valence states of the gold are gradually replaced by the spectrum of the organic film. No gas-phase photoelectron data for N ...
... II spectra that were measured during the growth of the NP film. The bottom spectrum is the clean Au(111) film on mica. Subsequent depositions of the aromatic molecule show the valence states of the gold are gradually replaced by the spectrum of the organic film. No gas-phase photoelectron data for N ...
Simultaneous Generation of Different Types of Ion Pairs upon
... decay upon ultrafast recombination.23 The discrepancy with the original study was due to two factors: (1) better time resolution (100 fs vs 30-50 ps) and (2) the possibility of calibrating the transient absorption signal arising from Pe•+ by independent photoconductivity measurements. This calibrati ...
... decay upon ultrafast recombination.23 The discrepancy with the original study was due to two factors: (1) better time resolution (100 fs vs 30-50 ps) and (2) the possibility of calibrating the transient absorption signal arising from Pe•+ by independent photoconductivity measurements. This calibrati ...
Steepening of the 820 μm continuum surface brightness profile
... the observed dispersion in each of the bins. These σi correspond to the error on the averaged real visibilities and follow from the dispersion of the data points in the bin divided by the square root of the number of data points. Any undetected asymmetric structures also contribute to σi , which ran ...
... the observed dispersion in each of the bins. These σi correspond to the error on the averaged real visibilities and follow from the dispersion of the data points in the bin divided by the square root of the number of data points. Any undetected asymmetric structures also contribute to σi , which ran ...
optically active substances.
... Quest: What about superposition of two circularly polarized light (RCP and LCP) beams with same amplitude and wavelength. Any plane polarized light wave can be obtained as a superposition of a left circularly polarized and a right circularly polarized light wave, whose amplitude is identical. This ...
... Quest: What about superposition of two circularly polarized light (RCP and LCP) beams with same amplitude and wavelength. Any plane polarized light wave can be obtained as a superposition of a left circularly polarized and a right circularly polarized light wave, whose amplitude is identical. This ...
Gas giants in hot water: inhibiting giant planet
... form planets via gravitational instability or core accretion. In fact, I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–170 K (Podolak & Zucker 2004; Lecar et al. 2006). Because the discs equil ...
... form planets via gravitational instability or core accretion. In fact, I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–170 K (Podolak & Zucker 2004; Lecar et al. 2006). Because the discs equil ...
Transit Lightcurve Signatures of Artificial Objects
... Fig.2 shows that the triangle transit lightcurve cannot exactly be fitted by a spherical nor an oblate body with zero or 90◦ obliquity, and that the fit residuals are symmetrical suggesting a non-spherical zero-obliquity symmetrical transiting body. Our fit gives residuals are of the order of 10−4 , ...
... Fig.2 shows that the triangle transit lightcurve cannot exactly be fitted by a spherical nor an oblate body with zero or 90◦ obliquity, and that the fit residuals are symmetrical suggesting a non-spherical zero-obliquity symmetrical transiting body. Our fit gives residuals are of the order of 10−4 , ...
The ages of pre-main-sequence stars
... The position of pre-main-sequence or protostars in the Hertzsprung±Russell diagram is often used to determine their mass and age by comparison with pre-main-sequence evolution tracks. On the assumption that the stellar models are accurate, we demonstrate that, if the metallicity is known, the mass o ...
... The position of pre-main-sequence or protostars in the Hertzsprung±Russell diagram is often used to determine their mass and age by comparison with pre-main-sequence evolution tracks. On the assumption that the stellar models are accurate, we demonstrate that, if the metallicity is known, the mass o ...
X-ray activity cycle on the active ultra
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
Stellar interactions in dense and sparse star clusters
... Olczak et al. 2008; Pfalzner et al. 2008). However, investigating one model star cluster is not sufficient to draw general conclusions – in fact, one could not answer questions as: How would things change in a denser cluster? Would a higher density inevitably imply that stellar encounters play a more ...
... Olczak et al. 2008; Pfalzner et al. 2008). However, investigating one model star cluster is not sufficient to draw general conclusions – in fact, one could not answer questions as: How would things change in a denser cluster? Would a higher density inevitably imply that stellar encounters play a more ...
astro-ph/0303282 PDF
... sensitivity does not vary as a function of azimuth – though sensitivity is significantly lower in the northern offset field of Epsilon Eridani due to poor conditions. The Vega sensitivity limits come from the offset image, which has comparable sensitivity as a function of radius to the centered imag ...
... sensitivity does not vary as a function of azimuth – though sensitivity is significantly lower in the northern offset field of Epsilon Eridani due to poor conditions. The Vega sensitivity limits come from the offset image, which has comparable sensitivity as a function of radius to the centered imag ...
Neutron stars: the densest state of condensed matter
... discovered by James Chadwick. He was awarded the Nobel prize in 1935. Talk of D. G. Yakovlev from Ioffe Institute in St Perterburg ...
... discovered by James Chadwick. He was awarded the Nobel prize in 1935. Talk of D. G. Yakovlev from Ioffe Institute in St Perterburg ...
Optical Properties of Solids
... Great Clarendon Street, Oxford OX2 6DP Oxford University Press is a department of the University of Oxford. It furthers the University's objective of excellence in research, scholarship, and education by publishing worldwide in ...
... Great Clarendon Street, Oxford OX2 6DP Oxford University Press is a department of the University of Oxford. It furthers the University's objective of excellence in research, scholarship, and education by publishing worldwide in ...
Chapter 9 Post-main sequence evolution through helium burning
... intermediate-mass stars ignite helium stably in a non-degenerate core, but after central He burning they develop a degenerate carbon-oxygen core. They have masses between MHeF and Mup ≈ 8 M⊙ . Both low-mass and intermediate-mass stars shed their envelopes by a strong stellar wind at the end of their ...
... intermediate-mass stars ignite helium stably in a non-degenerate core, but after central He burning they develop a degenerate carbon-oxygen core. They have masses between MHeF and Mup ≈ 8 M⊙ . Both low-mass and intermediate-mass stars shed their envelopes by a strong stellar wind at the end of their ...
1 Distance: A History of Parallax and Brief Introduction to Standard
... invisible concentric spheres, but used them only as geometrical models to describe the observations [Hirshfeld 4]. One major problem with all these nested spheres is that no solution would permit the other planets from varying their distance from Earth [Hoskin 36]. ...
... invisible concentric spheres, but used them only as geometrical models to describe the observations [Hirshfeld 4]. One major problem with all these nested spheres is that no solution would permit the other planets from varying their distance from Earth [Hoskin 36]. ...
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.