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  • MUSE observations of the lensing cluster Abell 1689 - arXiv. org
    of the lensing cluster Abell 1689 (hereafter A1689), as part of MUSE’s commissioning at the ESO Very Large Telescope This cluster has been extensively studied during the past 20 years be-cause it is one of the most e cient strong-lensing clusters cur-rently known Previous analysis of A1689 discovered a large number of multiple images
  • Parameterised models for the lensing cluster Abell 1689
    Parameterised models for the lensing cluster Abell 1689 L J King 1,2 - D I Clowe 2 - P Schneider 2,1 1 - Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Str 1, Garching bei München, Germany 2 - Institut für Astrophysik und Extraterrestrische Forschung der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
  • De Sitter–Schwarzschild metric - Wikipedia
    The metric of any spherically symmetric solution in Schwarzschild form is: = + + (+ ⁡) The vacuum Einstein equations give a linear equation for f(r), which has as solutions: = () =The first is a zero stress energy solution describing a black hole in empty space time, the second (with b positive) describes de Sitter space with a stress-energy of a positive cosmological constant of magnitude 3b
  • Gravitational lens magnification by Abell 1689: distortion of the . . .
    Gravitational lensing magnifies the observed flux of galaxies behind the lens We use this effect to constrain the total mass in the cluster Abell 168 we assume an Einstein-de Sitter universe for reasons of simplicity and because BTP show that this result depends only weakly on the chosen cosmological model Abell 1689 itself can
  • MUSE observations of the lensing cluster Abell 1689
    distant populations of galaxies on the other hand In particular, our current survey of lensing clusters is expected to provide a unique census of sources responsible for the reionization in a representative volume at z ˘47 Key words gravitational lensing: strong – galaxies: high-redshift – galaxies: clusters: individual: Abell 1689 1
  • Gravitational deflection of massive particles in Schwarzschild-de . . .
    the Schwarzschild and de Sitter geometries are still very far away from the gravitational lens, although the value of r cannot exceed the de Sitter radius (rdS = √ 3 Λ) The substitution of Eqs (3)–(4) into the r-component of the Euler-Lagrange equation leads to dr dλ 2 = E2 − 1 − 2M r − Λr2 3 1 + L2 r2, (5) 123
  • DE SITTER AND SCHWARZSCHILD-DE SITTER ACCORDING TO SCHWARZSCHILD AND DE . . .
    some symmetries of the de Sitter vacuum must be broken if we are to understand de Sitter entropy Since dS(IRP3) has a more “normal” (FRW) isometry group than dS(S3), it is reasonable to ask whether dS(IRP3) can lead to a different approach The question of the real significance of de Sitter entropy is one of the deepest in
  • Finite-Distance Gravitational Lensing of a Global Monopole in . . .
    We investigate the gravitational lensing of a Schwarzschild-de Sitter black hole with a global monopole at finite distances In this asymptotically nonflat spacetime, the deflection angle of light is decomposed into two parts: the first derives from the orbit differential equation, and the second originates from the metric itself By absorbing the cosmological constant into the effective
  • [2109. 04147] On the duality of Schwarzschild-de Sitter spacetime and . . .
    The Schwarzschild-de Sitter (SdS) metric is the simplest spacetime solution in general relativity with both a black hole event horizon and a cosmological event horizon Since the Schwarzschild metric is the most simple solution of Einstein's equations with spherical symmetry and the de Sitter metric is the most simple solution of Einstein's equations with a positive cosmological constant, the
  • Finite-Distance Gravitational Lensing of a Global Monopole in . . .
    Abstract We investigate the gravitational lensing of a Schwarzschild-de Sitter black hole with a global monopole at finite distances In this asymptotically nonflat spacetime, the deflection angle of light is decomposed into two parts: the first derives from the orbit differential equation, and the second originates from the metric itself
  • observations: Abell 1689 - arXiv. org
    cluster Abell 1689 (z = 0 182), manifest in the distorted images of background galaxies We start by outlining the observations, and the strategy for obtaining a catalogue of background galaxies for use in the weak lensing analysis Then we describe how this catalogue was used to perform a mass reconstruction of the cluster The M ap statistic of
  • New Hubble view of galaxy cluster Abell 1689 | ESA Hubble
    New Hubble view of galaxy cluster Abell 1689 This new Hubble image shows galaxy cluster Abell 1689 It combines both visible and infrared data from Hubble’s Advanced Camera for Surveys (ACS) with a combined exposure time of over 34 hours (image on left over 13 hours, image on right over 20 hours) to reveal this patch of sky in greater and striking detail than in previous observations





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