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Enrique Pérez Rosa M. González-Delgado Clive Tadhunter Zlatan Tsvetanov 《Astrophysics and Space Science》1990,171(1-2):71-75
We present new narrow band images of NGC 4151, taken in excellent seeing conditions with the 4.2-m William Herschel Telescope on La Palma. These reveal a wealth of detail that can be used to test models for the anisotropy of the narrow-line region.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain. 相似文献
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The Discovery of a Second Field Methane Brown Dwarf from Sloan Digital Sky Survey Commissioning Data
Tsvetanov ZI Golimowski DA Zheng W Geballe TR Leggett SK Ford HC Davidsen AF Uomoto A Fan X Knapp GR Strauss MA Brinkmann J Lamb DQ Newberg HJ Rechenmacher R Schneider DP York DG Lupton RH Pier JR Annis J Csabai I Hindsley RB Ivesic Z Munn JA Thakar AR Waddell P 《The Astrophysical journal》2000,531(1):L61-L65
We report the discovery of a second field methane brown dwarf from the commissioning data of the Sloan Digital Sky Survey (SDSS). The object, SDSS J134646.45-003150.4 (hereafter SDSS 1346-00), was selected because of its very red color and stellar appearance. Its spectrum between 0.8 and 2.5 μm is dominated by strong absorption bands of H2O and CH4 and closely mimics those of Gliese 229B and SDSS 162414.37+002915.6 (hereafter SDSS 1624+00), two other known methane brown dwarfs. SDSS 1346-00 is approximately 1.5 mag fainter than Gliese 229B, suggesting that it lies about 11 pc from the Sun. The ratio of flux at 2.1 μm to that at 1.27 μm is larger for SDSS 1346-00 than for Gliese 229B and SDSS 1624+00, which suggests that SDSS 1346-00 has a slightly higher effective temperature than the others. Based on a search area of 130 deg2 and a detection limit of z*=19.8, we estimate a space density of 0.05 pc-3 for methane brown dwarfs with Teff approximately 1000 K in the 40 pc3 volume of our search. This estimate is based on small-sample statistics and should be treated with appropriate caution. 相似文献
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The magnitude and frequency of coastal storms are expected to increase with rising global sea levels, which necessitates evaluating coastal flood adaptation measures. This study examines an important issue in the context of coastal flood protection, namely, the decision when to adopt protection measures. For any given coastal region, our benefit-cost framework allows us to determine the optimal timing of initiating protection that maximizes expected net benefits. We present an application of this framework to a coastal area in Connecticut. Our results suggest that the optimal timing of adopting protection may vary across different census blocks within the study area. We find that using a relatively low discount rate in the benefit-cost analysis implies greater heterogeneity in the timing decisions and earlier overall adoption, whereas, with higher discount rates, the timing decisions are reduced to a choice between early protection and no protection at all. If possible negative environmental and aesthetic impacts of sea barriers are taken into account, delaying protection would become more desirable, with the extent of delay being sensitive to the relative magnitude of one-time costs (e.g., loss of ocean view and recreational opportunities) vs. continuous costs (e.g., shoreline erosion and loss of wetlands). 相似文献
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J. W. Atkinson J. L. Collett A. Marconi D. J. Axon A. Alonso-Herrero D. Batcheldor J. J. Binney A. Capetti C. M. Carollo L. Dressel H. Ford J. Gerssen M. A. Hughes D. Macchetto W. Maciejewski M. R. Merrifield C. Scarlata W. Sparks M. Stiavelli Z. Tsvetanov R. P. van der Marel 《Monthly notices of the Royal Astronomical Society》2005,359(2):504-520
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By considering the consecutive effects of synchrotron reabsorption, Compton scattering and other kinds of energy losses of relativistic electrons, it may be possibile to form a universal distribution of electrons in the region of reabsorption (synchrotron reactor). This will be either a power law with a power index of the energy spectrumn
r=3–5, or a relativistic Maxwell distribution with an electron temperatureT
e=4T
b(1+), where is the ratio of Compton (or other losses) to synchrotron losses, andT
bis the brightness temperature of the radiation. Since the total energy losses of electrons in the reactor is equal to zero, this ensures the continuous existence and accumulation of relativistic electrons in the region of reabsorption and their associated hard scattered radiation. Multiple Compton scattering produces a specific stepped power distribution of scattered radiation by which we can identify the reactor. In the nuclei of quasars W
Hand, therefore,n
r=3; hence the spectral index of scattered radiation in the corresponding ranges (optical, UV, X- and -ray) is
.Consideration of other kinds of losses and gains of energy by electrons can lead to the dependencen
=3–5(E) — where (E) may have either positive or negative values—which, in turn, leads to the frequency dependence of the spectral index of scattered radiation
= 1 – (), |()| < 1, |(E)| < 1.Within the framework of the model being considered, the physical parameters of the nucleus of quasar 3C 273 are calculated. 相似文献
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