The Binary Populations of Eight Globular Clusters in the Outer Halo
... ∼40% in the cluster core. However, our results do not support a significant correlation with the cluster age as suggested in the literature. In most GCs, binaries are more centrally concentrated than single stars. If the fraction of binaries is normalised to the core binary fraction the radial densi ...
... ∼40% in the cluster core. However, our results do not support a significant correlation with the cluster age as suggested in the literature. In most GCs, binaries are more centrally concentrated than single stars. If the fraction of binaries is normalised to the core binary fraction the radial densi ...
Mark Correlations: Relating Physical Properties to Spatial Distributions
... representative of the whole castle distribution in Italy. That means in particular that, if the Gonzaga castles are clustered, so are the Sforza ones. Before we turn to applications, we have to develop practical test quantities in order to test for segregation effects in real data and to describe th ...
... representative of the whole castle distribution in Italy. That means in particular that, if the Gonzaga castles are clustered, so are the Sforza ones. Before we turn to applications, we have to develop practical test quantities in order to test for segregation effects in real data and to describe th ...
Microlensing Events by Proxima Centauri in 2014 and 2016
... the 2MASS source catalog for the infrared magnitudes of the sources. The 2MASS catalog shows a single source at this position, with magnitudes of J = 16.089, H = 15.436, and Ks = 15.764, and uncertainties of about ±0.07 mag. These magnitudes most likely represent the combined light of both backgroun ...
... the 2MASS source catalog for the infrared magnitudes of the sources. The 2MASS catalog shows a single source at this position, with magnitudes of J = 16.089, H = 15.436, and Ks = 15.764, and uncertainties of about ±0.07 mag. These magnitudes most likely represent the combined light of both backgroun ...
Multidimensional Vibrational Spectroscopy of Hydrogen Bonds in
... donor forms a covalent bond with the hydrogen atom whereas the interaction between the hydrogen atom and the acceptor is often considerably weaker∗ [1]. Despite its simplicity, the relevance of hydrogen bonds in nature can hardly be overestimated. It is a unique interaction that is strong enough to ...
... donor forms a covalent bond with the hydrogen atom whereas the interaction between the hydrogen atom and the acceptor is often considerably weaker∗ [1]. Despite its simplicity, the relevance of hydrogen bonds in nature can hardly be overestimated. It is a unique interaction that is strong enough to ...
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... presence of the coordinated OH group, obtained by hydrolysis of one chlorine atom in basic medium [13-15]. Magnetic and Electronic Spectral Data The electronic absorption spectra are often very helpful in the evaluation of the results provided by other methods of structural investigation. The electr ...
... presence of the coordinated OH group, obtained by hydrolysis of one chlorine atom in basic medium [13-15]. Magnetic and Electronic Spectral Data The electronic absorption spectra are often very helpful in the evaluation of the results provided by other methods of structural investigation. The electr ...
Soliton Self-Frequency Shift Cancellation in
... large variety of fundamental processes in many natural and artificially created nonlinear systems, such as the sea surface, nerve fibers, superconducting transmission lines, optical fibers, elementary particles, and outer space (1). Optical solitons are self-localized pulses or beams of light with t ...
... large variety of fundamental processes in many natural and artificially created nonlinear systems, such as the sea surface, nerve fibers, superconducting transmission lines, optical fibers, elementary particles, and outer space (1). Optical solitons are self-localized pulses or beams of light with t ...
Understanding Resolution
... aperture and the wavelength of the light observed. As aperture increases, angular size of the Airy disk decreases. Also, the size of the Airy disk varies as wavelength varies. Second, the magnitude of the observed star has an affect on the appearance of the Airy disk. A very bright star puts so much ...
... aperture and the wavelength of the light observed. As aperture increases, angular size of the Airy disk decreases. Also, the size of the Airy disk varies as wavelength varies. Second, the magnitude of the observed star has an affect on the appearance of the Airy disk. A very bright star puts so much ...
The effects of longitudinal chromatic aberration and a shift in the
... shown that for color vision there is little variation in the optimal values of the peak of the spectral function with different natural illuminants. In addition, we could have used other data to estimate reflectances in natural scenes, but again Lewis and Zhaoping (2006), find that using different refl ...
... shown that for color vision there is little variation in the optimal values of the peak of the spectral function with different natural illuminants. In addition, we could have used other data to estimate reflectances in natural scenes, but again Lewis and Zhaoping (2006), find that using different refl ...
400 YEARS OF STELLAR ROTATION - DFTE
... In 1592 Galileo moves to Padua university which was a thriving economic resource for the city and the Venetian Republic itself, both through student tuition fees and ancillary expenses. In Padua and Venice the freedom to teach was generally guaranteed, even though occasionally some heretic condemned ...
... In 1592 Galileo moves to Padua university which was a thriving economic resource for the city and the Venetian Republic itself, both through student tuition fees and ancillary expenses. In Padua and Venice the freedom to teach was generally guaranteed, even though occasionally some heretic condemned ...
The physics of star formation
... Star formation occurs as a result of the action of gravity on a wide range of scales, and different mechanisms may be important on different scales, depending on the forces opposing gravity. On galactic scales, the tendency of interstellar matter to condense under gravity into star-forming clouds is ...
... Star formation occurs as a result of the action of gravity on a wide range of scales, and different mechanisms may be important on different scales, depending on the forces opposing gravity. On galactic scales, the tendency of interstellar matter to condense under gravity into star-forming clouds is ...
G 3 Geochemistry Geophysics
... hydrothermal vent environments where targets of interest such as high-temperature vent fluids, fragile chimney structures and bacterial mats may be either too hot for contact analysis or altered when brought to the surface for ship- or shore-based analysis. Raman spectroscopy has been widely used in ...
... hydrothermal vent environments where targets of interest such as high-temperature vent fluids, fragile chimney structures and bacterial mats may be either too hot for contact analysis or altered when brought to the surface for ship- or shore-based analysis. Raman spectroscopy has been widely used in ...
Yellow supergiants as supernova progenitors: an indication of
... HRD of the progenitor. One of the most important physical process governing the evolution of massive stars is mass loss. Combined with rotation, it changes the evolution of the star radically (see the review by Maeder & Meynet 2011). However, the mass-loss rates inferred observationally or theoretic ...
... HRD of the progenitor. One of the most important physical process governing the evolution of massive stars is mass loss. Combined with rotation, it changes the evolution of the star radically (see the review by Maeder & Meynet 2011). However, the mass-loss rates inferred observationally or theoretic ...
Article PDF - IOPscience
... The recent discovery of a neutron star accretor in the ultra-luminous X-ray (ULX) source M82 X-2 challenges our understanding of high-mass X-ray binary formation and evolution. By combining binary population synthesis and detailed mass-transfer models, however, we show that the binary parameters of ...
... The recent discovery of a neutron star accretor in the ultra-luminous X-ray (ULX) source M82 X-2 challenges our understanding of high-mass X-ray binary formation and evolution. By combining binary population synthesis and detailed mass-transfer models, however, we show that the binary parameters of ...
Understanding Microscopy And Filtering Techniques
... 10mm Adapter to attach the objective (this adapter adds 10mm of length and adapts the M26 thread to a C-thread). An additional 76.5mm of space between the tube lens and objective is optimal, but it is common to only use about 56.5mm of space between #55-743 and #58-329 since each adapter adds about ...
... 10mm Adapter to attach the objective (this adapter adds 10mm of length and adapts the M26 thread to a C-thread). An additional 76.5mm of space between the tube lens and objective is optimal, but it is common to only use about 56.5mm of space between #55-743 and #58-329 since each adapter adds about ...
Observation of light below Cerenkov threshold in a 1.5 meter long
... length counter implies that a particle with a given velocity, #c, will emit light at angles both smaller and larger than the nominal Cerenkov angle. Although it is implicit in the diffraction formula, it is not generally realized that the same effect implies that light will be emitted below Cerenkov ...
... length counter implies that a particle with a given velocity, #c, will emit light at angles both smaller and larger than the nominal Cerenkov angle. Although it is implicit in the diffraction formula, it is not generally realized that the same effect implies that light will be emitted below Cerenkov ...
Early-time dynamics of the photoexcited hydrated electron
... explained using a model in which the transition dipole moment of the electron increases after the excitation due the strong coupling to the solvent molecules. Furthermore, it is shown that the effect is librational in nature. Finally, we demonstrate that a simple model based on wave packet dynamics ...
... explained using a model in which the transition dipole moment of the electron increases after the excitation due the strong coupling to the solvent molecules. Furthermore, it is shown that the effect is librational in nature. Finally, we demonstrate that a simple model based on wave packet dynamics ...
10-draft-EPS-238
... Higher-order corrections may be obtained to account for interference from strong atmospheric absorption (e.g., by O3 in the UV Huggins bands) as I 0 I 0e I 0 (1 2 / 2 ), and forming an orthogonal set of correction spectra using a Gram-Schmidt orthogonalization process. For GOME, this ...
... Higher-order corrections may be obtained to account for interference from strong atmospheric absorption (e.g., by O3 in the UV Huggins bands) as I 0 I 0e I 0 (1 2 / 2 ), and forming an orthogonal set of correction spectra using a Gram-Schmidt orthogonalization process. For GOME, this ...
Population synthesis for double white dwarfs-II. Semi
... dwarfs In Fig. 1 we show the limiting mass ratio for dynamically stable mass transfer (Eq. (4)) as the upper solid line, with ζ(m) derived from Eq. (5). The initial masstransfer rates, as given by Eq. (3), can be higher than the Eddington limit of the accretor (Tutukov & Yungelson 1979). The matter ...
... dwarfs In Fig. 1 we show the limiting mass ratio for dynamically stable mass transfer (Eq. (4)) as the upper solid line, with ζ(m) derived from Eq. (5). The initial masstransfer rates, as given by Eq. (3), can be higher than the Eddington limit of the accretor (Tutukov & Yungelson 1979). The matter ...
Title The Correlation between Dispersion Measure and X
... where me and e are electron mass and charge, respectively, and c is the speed of light. Most free electrons in our Galaxy are found in the hot phase of the ISM, including H ii regions ionized by UV radiation from hot O or B type stars and the shock-heated interior of supernova remnants (SNRs). These ...
... where me and e are electron mass and charge, respectively, and c is the speed of light. Most free electrons in our Galaxy are found in the hot phase of the ISM, including H ii regions ionized by UV radiation from hot O or B type stars and the shock-heated interior of supernova remnants (SNRs). These ...
Chapter15 - cloudfront.net
... while traveling along the same medium. The interference of waves causes the medium to take on a shape that results from the net effect of the two individual waves upon the particles of the medium ...
... while traveling along the same medium. The interference of waves causes the medium to take on a shape that results from the net effect of the two individual waves upon the particles of the medium ...
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.