In this paper, an diffusion function which discribes the scattering characteristics of the earth's atmosphere is obtained by fitting a theoretical profile with an aureole intensity profile, observed during a partial eclipse on July 31, 1981. This function may be applied to correction of scattered light in the photometry measurements of sunspots or other active phenomena.
In the highly precise CCD measurement of a stellar image for its position and photometry,some researchers use CCD photometric calibration but the others do not.
The experimental results have revealed that the photometric calibration corrections for a faint star (～16 mag) have nearly 0.2 mag and 0.02 pixel in its photometry and in its position,respectively. These corrections for a bright star (～10 mag),however,decrease to about 0.02 mag and 0.002 pixel in its photometry and its position,respectively.
The long-term light curve in the V-band from 1982 to 2003 for BL Lac object H0323+022 is obtained, and the optical photometry of the sourse,which were observed with the 1 m telescope of Yunnan Astronomical Observatory and 1.56 m telescope of Shanghai Astronomical observatory,is presented.
The aggregation stability of SiO2 (aerosil OX-50), FeOOH, ZrO2 CeO2, and natural diamond sols was studied by photometry over a wide range of KCl and BaCl2 concentrations at pH 6 and 3.
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The influence of short-term heating or cooling and exposure to visible light on the bleaching of a gamma-irradiated glass stored at 20°C is investigated by photometry.
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The photobleaching of the absorption band associated with the hole-type centers in a gamma-irradiated glass of the K2O-PbO-SiO2 system is investigated by photometry.
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Such sources may be used in short-wave pulse photometry, microelectronics, and photo- and biochemistry.
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The photometry of transmitted laser radiation is used to investigate the dynamics of photocurrent fluctuations.
Basic quantities in stellar photographic photometry (in particular, colour index and "effective wavelength") are formulated according to the assumptions that: 1) stellar radiation may be represented by some black body equivalent and 2) within the limits of a single photometric "receiver", intensity-wavelength relationship of the radiation may be taken as linear. Foundations and applicability of these assumptions are examined. On the basis of this the photometric side of the problems of space reddening...
According to the international convention,we have carried out the photographic photometry on the U,B,V system,with the recommended plate-filter combinations:U— Kodak 103a-O+UG2;B—103a-o+GG13 and V—103a-D+GG11.Our telescope is a 15 cm Zeiss astrograph (UV objective).With the data in hand,we cal- culated the effective wave length of the blue combination.(103a-o+GG13)to be 4440A and the yellow combination (103a-D+GG11) 5610A.Both are longer than that of the respective B,V system. When we determine the ma...
The photographic photometry of Nova was observed with three colours—ultraviolet, blue and yellow—from February 17 to November 19,1963.The telescope and plate- filter combinations are the same as those described in a previous paper.Some additional explanation of our magnitude systems has been made.Since the magnitudes of the nearby stars are not suitable for comparison,we have to determine it independently by the usual photographic method.The magnitudes of Nova and comparison stars are given. We discus...
photometry
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