共查询到20条相似文献，搜索用时 203 毫秒
1.
Dzh. A. Stepanyan V. A. Lipovetskii V. O. Chavushyan L. K. Erastova A. I. Shapovalova 《Astrophysics》1991,34(3):163-170
Byurakan Astrophysical Observatory; Special Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 3, pp. 315–325, May–June, 1991. 相似文献
2.
Stepanyan Dzh A. Lipovetskii V. A. Chavushyan V. O. Erastova L. K. Shapovalova A. I. 《Astrophysics》1991,34(1):1-6
Byurakan Astrophysical Observatory; Special Astrophysical Observatory, USSR Academy of Sciences. Translated from Astrofizika, Vol. 34, No. 1, pp. 5–12, January–February, 1991. 相似文献
3.
《Astronomische Nachrichten》2011,332(7)
Light curve with the flare observed in the Pleiades cluster with the Schmidt‐Teleskop‐Kamera at the University Observatory Jena (see M. Moualla et al., this issue, p. 661). 相似文献
4.
V. A. Lipovetskii Dzh. A. Stepanyan L. K. Erastova A. I. Shapovalova 《Astrophysics》1988,29(3):747-751
Special Astrophysical Observatory, USSR Academy of Sciences; Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 29, No. 3, pp. 548–555, November–December, 1988. 相似文献
5.
J. Y. Hu 《Astrophysics and Space Science》1994,217(1-2):53-54
A high spatial resolution near infrared imaging system is being developed at Beijing Observatory. It is a joint-project with Institute of Optics and Electronics, CSA, and National Astronomical Observatory, Japan. The system contains a 512 × 512 PtSi CSD near infrared camera and a 21-element adaptive optics system and will be operated at Coudé focus of the 2.16 meter telescope at Xinglong Station, Beijing Observatory. The infrared camera will be fixed at Cassegrain focus with focus reducers too. 相似文献
6.
《Astronomische Nachrichten》2014,335(8)
TIGRE at La Luz Observatory, Guanajuato, Mexico (see J.H.M.M. Schmitt et al., this issue, p. 787). (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
7.
Photoelectric measurements of the night sky brightness and the light pollution of Kottamia Observatory have been carried out and the deduced results are expressed in mag/sec2. The maximum brightness of the sky in the direction of Cairo city at zenith distance 45° and azimuth 70° when the sun is almost 60° below the horizon are 22.68; 21.54 and 19.82 mag/sec2 for blue, yellow and red colours respectively. The corresponding values of night sky background are 22.94; 21.85 and 20.14 mag/sec2 respectively.The isophotes of the sky brightness at Kottamia Observatory have been drawn for blue, yellow and red colours. The variations of the night sky brightness and the (B-V) colour index with altitude of the observed point have been studied.The light pollution and the night sky brightness at the site of Kottamia Observatory is compared with that deduced by different investigators at other sites. It has been shown that the sky brightness at zenith distance 45° at Kottamia Observatory site is similar to Kitt Peak and Palomar Observatory sites. Kottamia Observatory site is slightly brighter than Junipero Serra while it is darker than Mount Hamilton and San Jose sites. The comparative results have been carried out at blue and yellow colours. No comparison is obtained at red as there is no data published for the red colour. 相似文献
8.
Elchanan Almoznino & Noah Brosch 《Monthly notices of the Royal Astronomical Society》1998,298(3):920-930
We selected samples of late-type dwarf galaxies in the Virgo cluster with H i information. The galaxies were observed at the Wise Observatory using several broad-band and Hα bandpasses. UV measurements were carried out with the IUE Observatory from VILSPA, and with the FAUST shuttle-borne UV telescope. We describe the observations in detail, paying particular attention to the determination of measurement errors, and present the observational results together with published data and far-infrared information from IRAS . The sample will be analysed in subsequent papers, in order to study star formation mechanisms in galaxies. 相似文献
9.
A set of close binaries have been observed using the same instrumental configuration at Kitt Peak National Observatory, USA. The rotation velocities for 99 components in 75 binaries, derived by two methods, are given here, including 55 components for the first time. These high-accuracy velocities provide a reliable observational basis for investigating synchronism in binaries and the various synchronizing mechanisms. 相似文献
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In this review, we consider all aspects of the development of heliometric and positional observations of the Moon and the investigation of its figure, rotation (physical libration), and gravitational field as well as other similar questions at the Engelhard Astronomical Observatory (EAO) and the Kazan Municipal Astronomical Observatory (KMAO) at Kazan University. 相似文献
14.
Dzh A. Stepanyan V. A. Lipovetskii A. I. Shapovalova L. K. Erastova V. O. Chavushyan 《Astrophysics》1990,33(2):411-418
Byurakan Astrophysical Observatory; Special Astrophysical Observatory, USSR Academy of Sciences. Translated from Astrofizika, Vol. 33, No. 2, pp. 199–212, September–October, 1990. 相似文献
15.
The linear polarization of the reflection nebula R Mon/NGC 2261 has been observed since November 1991 with a multi-channel polarimeter at Dodaira Observatory, one of the branches of the National Astronomical Observatory of Japan. Results of the observations are reported. 相似文献
16.
The paper describes the design and the realization of a multiple-function photoelectric photometer made by Trieste Observatory
for Torino Observatory. The system design shows a two-beam, sequential multiband photon counting and analog photoelectric
photometer configuration based on a PDP8/E computer for the control and data acquisition and elaboration. The actual realization
of the system and the use of it in the one-beam configuration operating now at torino Observatory shows the advantages of
such a solution and the easiness in modifying and determining the system functions by software programs rather than by hardware
specials.
Work supported by Consiglio Nazionale delle Ricerche, Gruppo Nazionale di Astronomia, Settore Tecnologie Astronomiche. The
realization of the machine was fully supported by Torino Observatory. Trieste Observatory-Instruments and Data Processing
Group (5/76). 相似文献
17.
Dzh A. Stepanyan V. A. Lipovetskii A. I. Shapovalova L. K. Erastova 《Astrophysics》1990,33(1):344-354
Byurakan Astrophysical Observatory; Special Astrophysical Observatory, USSR Academy of Sciences. Translated from Astrofizika, Vol. 33, No. 1, pp. 89–105, July–August, 1990. 相似文献
19.
B. R. Pettersen M. K. Tsvetkov S. L. Hawley L. A. Coleman A. S. Amirkhanyan 《Astrophysics》1988,29(1):445-449
Institute of theoretical Astrophysics, Oslo, Norway; Department of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences; Department of Astronomy and McDonald Observatory, Austin, Texas, USA; Department of Physics and Astronomy, University of Arkansas at Little Rock, Arkansas, USA; Byurakan Astrophysical Observatory Armenian Academy of Sciences, USSR. Published in English in Astrofizika, Vol. 19, No. 1, 67–73, July–August, 1988. 相似文献
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