Search Publications
The mass and angular momentum loss from the edge of the accretion disk and the evolution of cataclysmic binaries
Yu, K. N.; Huang, Run-qian
We give the mass and angular momentum loss from the edge of the accretion disk of a cataclysmic binary and model theoretically the effect of these losses on the evolution of the system. The results of the calculation show that the high-velocity mass outflows observed by IUE come from the edge of the disk and the angular momentum loss there could b…
A model for the accretion disk in the dwarf nova AB Draconis
Li, Zong-yun; Zhu, Ci-sheng; Ding, Yue-rong
A least squares fit to the dwarf nova AB Dra shows that the continuum spectrum predicted by a blackbody accretion disk model can roughly account for the IUE observations during the time of the explosion, while small discrepancies can be attributed to recombination radiation of an optically thin atmosphere and/or blackbody radiation from hot spots.…
A new γ-ray pulsar: PSR 0740-28
Lu, Tan; Ma, Yu-qian; Song, Li-ming
We made a period folding analysis on two sets of COS-B observations and obtained a clearly pulsed phase structure in the γ-ray photons from the direction of PSR 0740-28. The phase diagrams from the two different data sets have a similar structure and the period and period rate are close to radio expectations. The probability of the two phase struc…
The establishment of a continuous declination system with photoelectric astrolabe Mark I—An international cooperation between Lintong and Irkutsk
Xu, Jia-yan; Wang, Zheng-ming
We propose a cooperative observational project of using the photo-electric astrolabe Mark I of Shaanxi Observatory in Irkutsk. As the instrument will be equipped with a Z = 45° angle prism, it will have no blind zone when used at latitude ( φ = 52°. Important contribution can be expected to the establishing of fundamental reference system and the …
Variation of QSO color indices with redshift
Fan, Xiao-hui; Chen, Jian-sheng
In this paper we discuss the effect of features in the spectrum of QSOs on their color indices and the consequent variation of the latter with the redshift. As the redshift increases, the various absorption features shortwards of the Lyα emission line enter into the visible region and alter the way in which the color indices vary with the redshift…
A morphological study of the circumstellar dust shell of Herbig Ae/Be stars
Wang, Jun-jie; Hu, Jing-yao
In this paper the Kurucz stellar atmosphere model is fitted to the observed IUE, IRAS, ground-based optical and near-infrared data of 22 Herbig Ae/Be stars. A statistical analysis is made based on energy balance between the central star and the circumstellar shell. It is concluded that the shells are disk-shaped.
COS-B identification of the new γ pulsar PSR 1055-52
Lu, Tan; Song, Li-ming
Using COS-B data we analyzed the timing parameters of PSR 1055-52, the newly discovered γ-ray pulsar by CGRO. We found a significant and similar pulsed structure, thus confirming the CGRO discovery. A comparison of this pulsar with 5 previously known ones is made.
Analysis of COS-B and HEAO-B satellite data of the pulsar Geminga
Wu, Mei; Ma, Lin; Ma, Yu-qian +4 more
We have made timing and spectral analyses of COS-B and HEAO-B satellite data of the pulsar Geminga and our results further confirm that Geminga is a pulsar with a strong γ emission and a weak X emission.
PSR 1820-11 : A binary gamma-ray pulsar
Wu, Mei; Li, Ti-pei
Significant pulsation structure in phase distribution in the 50-6000MeV gamma-rays from the direction of the binary radio pulsar PSR 1820-11 in the COS-B data was obtained using the folding algorithm. Besides the period search, a spatial analysis was Bade and a clear point-like gamma-ray image was found at the pulsar's position.
High energy gamma-rays from cygnus X-3
Wu, Mei; Li, Tipei
Simultaneous observations by the ESA satellite COS-B show that the 2-12 keV X-rays and 150-5000 MeV gamma-rays of Cyg X-3 are negatively correlated. A clear gamma-ray image of Cyg X-3 can be obtained between June 1977 and June 1980, when the X-ray emission was low, to yield a flux of P(E > 100MeV) ~ 1 × 10 -6cm -2s -1…