Series Telescopes INSTRUCTION MANUAL
... A Newtonian reflector uses a single concave mirror as its primary. Light enters the tube traveling to the mirror at the back end. There light is bent forward in the tube to a single point, its focal point. Since putting your head in front of the telescope to look at the image with an eyepiece would ...
... A Newtonian reflector uses a single concave mirror as its primary. Light enters the tube traveling to the mirror at the back end. There light is bent forward in the tube to a single point, its focal point. Since putting your head in front of the telescope to look at the image with an eyepiece would ...
the bible and the pleiades
... view of a basic Bible truth, he carried it too far. As for me, I am not prepared to write a treatise on the stars as found in the Holy Bible. Still, we will see many of these stellar elements in the facts and lore of the Pleiades. But first, a bit about that lovely jewel in the sky. The Pleiades as ...
... view of a basic Bible truth, he carried it too far. As for me, I am not prepared to write a treatise on the stars as found in the Holy Bible. Still, we will see many of these stellar elements in the facts and lore of the Pleiades. But first, a bit about that lovely jewel in the sky. The Pleiades as ...
Electron Shell Contributions to Gamma-ray Spectra of Positron Annihilation in Noble gases" J. Phys. B.: Atomic, Molecular and Optical Physics , 43 , 165207 (2010). Feng Wang, Lalitha Selvam, and C. M. Surko, Gleb F Gribakin, and C. M. Surko (PDF)
... mass of a molecule (or atom) [17]. The annihilation spectral width ε of the noble gases exhibits an opposite trend with respect to size; that is, ε decreases as R2 increases (except for He) or Rnl increases. As observed previously in insulators and metals, as well as noble gases [7], the anni ...
... mass of a molecule (or atom) [17]. The annihilation spectral width ε of the noble gases exhibits an opposite trend with respect to size; that is, ε decreases as R2 increases (except for He) or Rnl increases. As observed previously in insulators and metals, as well as noble gases [7], the anni ...
The Age and Stellar Parameters of the Procyon Binary System
... Procyon B was first detected visually at the end of the 19th century by Schaeberle (1896), and was historically one of the first white dwarfs to be discovered. Even early estimates of the mass (MB ) of the white dwarf component, such as that by Strand (1951), showed that it is much closer to the mea ...
... Procyon B was first detected visually at the end of the 19th century by Schaeberle (1896), and was historically one of the first white dwarfs to be discovered. Even early estimates of the mass (MB ) of the white dwarf component, such as that by Strand (1951), showed that it is much closer to the mea ...
The physics and modes of star cluster formation: observations
... their formation and early evolution, are completely embedded in molecular gas and dust. They are thus obscured from view at optical wavelengths, where the traditional astronomical techniques are most effective. Fortunately, molecular clouds are considerably less opaque at infrared wavelengths and th ...
... their formation and early evolution, are completely embedded in molecular gas and dust. They are thus obscured from view at optical wavelengths, where the traditional astronomical techniques are most effective. Fortunately, molecular clouds are considerably less opaque at infrared wavelengths and th ...
Models of rapidly rotating neutron stars: remnants of accretion
... softest EOS. In addition, they found three models with 0:14 , b , 0:27. Rampp, Müller & Ruffert (1998) subsequently performed 3D simulations of three of these models. They found that the model with b . 0:27 shows a non-linear growth of a nonaxisymmetric dynamical instability dominated by the bar mo ...
... softest EOS. In addition, they found three models with 0:14 , b , 0:27. Rampp, Müller & Ruffert (1998) subsequently performed 3D simulations of three of these models. They found that the model with b . 0:27 shows a non-linear growth of a nonaxisymmetric dynamical instability dominated by the bar mo ...
The maximal runaway temperature of Earth-like planets
... Second, applying the most general assumptions and independently of any particular properties of an absorber, we show that the greenhouse effect saturates and that any Earth-like planet has a maximal temperature which depends on the type of and distance to its main-sequence star, its albedo and the p ...
... Second, applying the most general assumptions and independently of any particular properties of an absorber, we show that the greenhouse effect saturates and that any Earth-like planet has a maximal temperature which depends on the type of and distance to its main-sequence star, its albedo and the p ...
Hipparcos distance estimates of the Ophiuchus and the Lupus cloud
... not included in the error estimate quoted above). For Ophiuchus, we find some evidence that the streamers are closer to us than the core. The method applied in this paper is currently limited to nearby molecular clouds, but it will find many natural applications in the GAIA-era, when it will be poss ...
... not included in the error estimate quoted above). For Ophiuchus, we find some evidence that the streamers are closer to us than the core. The method applied in this paper is currently limited to nearby molecular clouds, but it will find many natural applications in the GAIA-era, when it will be poss ...
Water in star-forming regions with Herschel (WISH): II. Evolution of
... with the Heterodyne Instrument for the Far-Infrared (HIFI; de Graauw et al. 2010) on the Herschel Space Observatory (Pilbratt et al. 2010), see Table 1 for an overview of the sources. Observations were performed as single-pointing observations in either dual-beam-switch mode with a chop of 3′ or pos ...
... with the Heterodyne Instrument for the Far-Infrared (HIFI; de Graauw et al. 2010) on the Herschel Space Observatory (Pilbratt et al. 2010), see Table 1 for an overview of the sources. Observations were performed as single-pointing observations in either dual-beam-switch mode with a chop of 3′ or pos ...
ph709-15
... planet-metallicity correlation at all stellar masses; this argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." BUT: Neptune-mass planets form preferentially around metal-poor stars, in contrast to stars with giant planets 3) Some planet have ...
... planet-metallicity correlation at all stellar masses; this argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." BUT: Neptune-mass planets form preferentially around metal-poor stars, in contrast to stars with giant planets 3) Some planet have ...
High spectral resolution multiplex CARS spectroscopy using chirped
... Coherent Anti-stokes Raman Scattering (CARS) is a nonlinear process wherein the interaction of three beams, ωp, the pump (which is usually degenerate) and ωs (the Stokes beam) generates the anti-Stokes signal at the frequency ωas = 2ωp - ωs. By tuning the energy difference ωp - ωs into a molecular r ...
... Coherent Anti-stokes Raman Scattering (CARS) is a nonlinear process wherein the interaction of three beams, ωp, the pump (which is usually degenerate) and ωs (the Stokes beam) generates the anti-Stokes signal at the frequency ωas = 2ωp - ωs. By tuning the energy difference ωp - ωs into a molecular r ...
Evolutionary paths among different red galaxy types at 0.3< z< 1.5
... checked that all galaxies in our mass-limited red sample exhibit apparent magnitudes brighter than this limit. We have used the color-color diagram shown in Fig. 1 to remove stars from the sample. It represents the I − Ks vs. V − I distribution for all the sources in the mass-limited red galaxy samp ...
... checked that all galaxies in our mass-limited red sample exhibit apparent magnitudes brighter than this limit. We have used the color-color diagram shown in Fig. 1 to remove stars from the sample. It represents the I − Ks vs. V − I distribution for all the sources in the mass-limited red galaxy samp ...
Shock interactions, turbulence and the origin of the stellar mass
... On the largest galactic scales (several kpc), the overall structure of the shock-dominated, diffuse ISM of the Galaxy is seen in the neutral hydrogen (H I) gas observations such as the Canadian Galactic Plane Survey [14]. These 21 cm maps of radio emission show that the diffuse ISM is highly filamen ...
... On the largest galactic scales (several kpc), the overall structure of the shock-dominated, diffuse ISM of the Galaxy is seen in the neutral hydrogen (H I) gas observations such as the Canadian Galactic Plane Survey [14]. These 21 cm maps of radio emission show that the diffuse ISM is highly filamen ...
Chapter 12 Pre-supernova evolution of massive stars
... Pre-supernova evolution of massive stars We have seen that low- and intermediate-mass stars (with masses up to ≈ 8 M⊙ ) develop carbonoxygen cores that become degenerate after central He burning. As a consequence the maximum core temperature reached in these stars is smaller than the temperature req ...
... Pre-supernova evolution of massive stars We have seen that low- and intermediate-mass stars (with masses up to ≈ 8 M⊙ ) develop carbonoxygen cores that become degenerate after central He burning. As a consequence the maximum core temperature reached in these stars is smaller than the temperature req ...
Galaxy morphology, luminosity, and environment in the SDSS DR7
... and colour. The smoothed bootstrap method is used to calculate confidence regions of the derived luminosity functions. Results. We find a strong environmental dependency for the LF of elliptical galaxies. The LF of spiral galaxies is almost environment independent, suggesting that spiral galaxy form ...
... and colour. The smoothed bootstrap method is used to calculate confidence regions of the derived luminosity functions. Results. We find a strong environmental dependency for the LF of elliptical galaxies. The LF of spiral galaxies is almost environment independent, suggesting that spiral galaxy form ...
Heriot-Watt University Mode-resolved 10
... Fourier-transform spectrometer stage over 10 cm is shown in Fig. 4. The measurement time was 1.5 seconds and the OPD was calibrated using a simultaneously recorded HeNe laser interferogram. For the purposes of calculating the comb spectrum, the interferogram was windowed to an optical path length of ...
... Fourier-transform spectrometer stage over 10 cm is shown in Fig. 4. The measurement time was 1.5 seconds and the OPD was calibrated using a simultaneously recorded HeNe laser interferogram. For the purposes of calculating the comb spectrum, the interferogram was windowed to an optical path length of ...
Effect of the stellar spin history on the tidal evolution of close
... Methods. We used a standard equilibrium tidal model to compute the orbital evolution of single planets orbiting both Sun-like stars and very low-mass stars (0.1 M ). We tested two stellar spin evolution profiles, one with fast initial rotation (1.2 day rotation period) and one with slow initial rot ...
... Methods. We used a standard equilibrium tidal model to compute the orbital evolution of single planets orbiting both Sun-like stars and very low-mass stars (0.1 M ). We tested two stellar spin evolution profiles, one with fast initial rotation (1.2 day rotation period) and one with slow initial rot ...
22 Years of a Pulsar
... • Use scintillation/ emission measure properties to probe inhomogeneities in disk/wind (e.g. McClure Griffiths et al. 1996) ...
... • Use scintillation/ emission measure properties to probe inhomogeneities in disk/wind (e.g. McClure Griffiths et al. 1996) ...
VLBA imaging of the Gamma-ray Emission Regions in
... ⇒ Sometimes upstream of 43 GHz core ⇒ Often in or downstream of 43 GHz core • Intra-day γ-ray/optical variability can occur in mm-wave regions ⇒ The highest-Γ jets are very narrow, < 1°, so at 10 pc from the ...
... ⇒ Sometimes upstream of 43 GHz core ⇒ Often in or downstream of 43 GHz core • Intra-day γ-ray/optical variability can occur in mm-wave regions ⇒ The highest-Γ jets are very narrow, < 1°, so at 10 pc from the ...
Li K-edge XANES and Li(1s) XPS Spectra of Lithium Compounds
... resemble those of alkaline-earth metal elements rather than other alkali metal elements. For a peculiar property of lithium, many researchers have extensively studied on lithium [3, 4]. However, there are no suitable analytical methods to get easily important information on the electronic states of ...
... resemble those of alkaline-earth metal elements rather than other alkali metal elements. For a peculiar property of lithium, many researchers have extensively studied on lithium [3, 4]. However, there are no suitable analytical methods to get easily important information on the electronic states of ...
October 2013 - Skyscrapers, Inc.
... was good to me, however. He uncharacteristically dispatched with his business promptly, and I gleefully made a beeline back to the television, and a front row seat to history. Ah, but for fortune. This October 12th marks the “International Observe the Moon Night”, an annual event dedicated to encour ...
... was good to me, however. He uncharacteristically dispatched with his business promptly, and I gleefully made a beeline back to the television, and a front row seat to history. Ah, but for fortune. This October 12th marks the “International Observe the Moon Night”, an annual event dedicated to encour ...
Visible to near-infrared optical properties of pure synthetic olivine
... As discussed above, the absorption features in the acquired reflectance spectra were quantified with the Modified Gaussian Model (MGM). Each spectrum was modeled with a series of four standard “fits,” where a “fit” refers to a particular starting condition. Because MGM model results can be sensitive ...
... As discussed above, the absorption features in the acquired reflectance spectra were quantified with the Modified Gaussian Model (MGM). Each spectrum was modeled with a series of four standard “fits,” where a “fit” refers to a particular starting condition. Because MGM model results can be sensitive ...
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.