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Birriel, J. J.; Adkins, J. K. |
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Title |
Sky Brightness at Zenith During the January 2019 Total Lunar Eclipse |
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2019 |
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The Journal of the American Association of Variable Star Observers |
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47 |
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1 |
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94 |
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Skyglow |
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Abstract |
Lunar eclipses occur during the full moon phase when the moon is obscured by Earth's shadow. During these events, the night sky brightness changes as the full moon rises and then passes first into the penumbral and then the umbral shadow. We acquired sky brightness data at zenith using a Unihedron Sky Quality Meter during the 20-21 January 2019 total lunar eclipse as seen from Morehead, Kentucky. The resulting sky brightness curve shows an obvious signature when the moon enters the umbral (partial) eclipse phases and the total eclipse phase. During the total eclipse phase, the brightness curve is flat and measures 19.1 ± 0.1 mag / arcsec2. The observed brightness at totality is close to typical new moon in January night at our location, which measures 19.3 ± 0.1 mag / arcsec2. The partial eclipse phase is symmetric on either side of totality. The penumbral phase is more difficult to identify in the plot, without comparison to a typical full moon night. There is a clear asymmetry in the curve just before and just after the umbral phase. This asymmetry is probably due to changes in terrestrial atmospheric conditions, such as high altitude clouds. |
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2647 |
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Author |
Elvey, C.T.; Roach, F.E. |
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Title |
A Photoelectric Study of the Light from the Night Sky |
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1937 |
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The Astrophysical Journal |
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ApJL |
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85 |
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213 |
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Instrumentation; Sky Brightness |
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0004-637X |
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2399 |
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Gartlein, C.W. |
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Title |
Request for Auroral Observations |
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1939 |
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Journal of the Royal Astronomical Society of Canada |
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33 |
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46-50 |
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Skyglow |
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Author |
Treanor, P. J. |
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Title |
A simple propagation law for artificial night-sky illumination |
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1973 |
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The Observatory |
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93 |
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117-120 |
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Skyglow |
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The problem of locating new large astronomical observatories in sites which have a suitably dark night sky (artificial excess of the order of omi) is becoming increasingly difficult in Europe and the United States, on account of extensive urban development, the high luminous efficiency of modern discharge lighting, and the scattering of light in an atmosphere contaminated by aerosols. To investigate the artificial illumination of the sky over large regions on the basis of necessarily limited observations, one needs an expression for the zenith brightness produced by towns of known site and distance.
The exact derivation of such a law is exceedingly complex, involving the computation of the radiation transfer in an atmosphere with absorption, multiple scattering, and complicated physical and geometrical parameters. Notwithstanding these difficulties, it is possible to obtain a useful physical insight into the general form of this law by considering a very simplified model, consisting of a homogeneous atmosphere, in which vertical heights are small in relation to the horizontal distances between town and observatory, and which the scattering is limited to a cone of small angle whose axis lies in the direction of the incident beam. The limited scale height and optical thickness of the real atmosphere, and the forward-scattering characteristics of aerosols lend some plausibility to these simplifications. |
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IDA @ intern @ |
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2633 |
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Author |
Garstang, R. H. |
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Title |
Improved scattering formula for calculations of artificial night-sky illumination |
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1984 |
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The Observatory |
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104 |
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196-197 |
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In recent years there has been increased interest in measuring the artificial illumination produced in the night sky cities of various sizes at a range of distances from the observer. Examples of such measurements include the work of Treanor on three Italian cities, that of Walker on the cities of various sized in California, and a study by Berry of light pollution in Southern Ontario. There seem to have been few attempts to provide theoretical interpretations of these measurements other than that contained in the paper by Treanor. He developed a simple empirical formula (his equation (6)) for the zenith brigthness due to a distant city as a function of the distance of the observer from the city. Treanor's formula was used by Berry, with a modification which we mention later.
Treanor based his formula on a very ingenious method of estimating the contribution to the zenith brightness of aerosol scattering between the city, treated as a point source, and an element of the atmosphere in the direction of the observer's zenith. Readers are referred to Treanor's paper for details of his derivation. We give here a simple extension of his work which leads to a scattering formula valid under less restrictive assumptions. |
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IDA @ intern @ |
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2638 |
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