首页 | 本学科首页   官方微博 | 高级检索  
相似文献
 共查询到20条相似文献,搜索用时 31 毫秒
1.
The Schmidt‐Teleskop‐Kamera (STK) is a new CCD‐imager, which is operated since begin of 2009 at the University Observatory Jena. This article describes the main characteristics of the new camera. The properties of the STK detector, the astrometry and image quality of the STK, as well as its detection limits at the 0.9 m telescope of the University Observatory Jena are presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

2.
The night-to-night and short-term variations inUBV light curves of EW Lac which were made during 1982–1984 at Yonsei University Observatory are discussed. The long-term variability in the photometric behaviour of the star is examined with our own data as well as those of Harmanecet al. (1980).Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984.Yonsei University Observatory Contribution No. 23.  相似文献   

3.
The High Efficiency and Resolution Canterbury University Large échelle Spectrograph (HERCULES) a fibre-fed échelle spectrograph that was designed and built at the University of Canterbury and has been in operation at Mt. John University Observatory since April 2001.HERCULES receives light from the f/13.5 Cassegrain focus of the 1 m McLellan telescope. Resolving powers of R = 41 000, 70 000 and 82 000 are available. An R2 200 × 400 mm échelle grating provides dispersion and cross-dispersion uses a large BK7 prism in double pass. The wavelength coverage is designed to be 380–880 nm in a single exposure. The maximum detective quantum efficiency of the fibre, spectrograph and detector system is about 18% in 2 arc second seeing. High wavelength stability (to better than 10 ms-1 in radial velocity) is achieved by installing the whole instrument in a large vacuum tank at 2–4 torr and by there being no moving parts. The tank is in a thermally isolated and insulated environment. The paper describes the design philosophy of HERCULES and its performance during the first year of operation. Now deceased; formerly at This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

4.
The Ku-band polarization identifier (KUPID) will integrate a very low noise 12–18 GHz, correlation polarimeter onto the Crawford Hill seven meter, millimeter-wave antenna. The primary components of the polarimeter will be built at the University of Miami and other key components, including the microwave horn and data acquisition system will be built at the University of Chicago and Princeton University. This project will measure the Q and U Stokes parameters in regions near the north celestial pole, in regions of low galactic contamination, and in regions near the galactic plane. The KUPID survey experiment makes use of many of the techniques employed in the Princeton IQU experiment (PIQUE) that was developed by the members of this collaboration to detect CMB polarization at shorter wavelengths. The KUPID experiment will be constructed in parallel and on the same timescale as the CAPMAP experiment (see Barkats, this volume) which is the follow-on experiment to PIQUE. KUPID will observe on the Crawford Hill antenna from late spring until early autumn, while CAPMAP will observe during the lower water vapor months of late autumn until early spring.  相似文献   

5.
In situ measurements at the lunar surface at millimeter resolution by the Apollo astronauts have been analyzed. Several statistical parameters have been determined for the landing site. The surface roughness has been found to be very nearly gaussian. The root-mean-square slopes have been obtained over scales between 0.5 mm and 5 cm. They steadily decrease with increasing scale length from 58° to 2° and are in reasonable agreement with radar-measured values. The autocorrelation coefficient of the height distribution has also been obtained. It has a scale-length of 0.7 mm.Adjunct Professor at the University of Massachusetts.Visiting Scholar at the University of Massachusetts.  相似文献   

6.
The Dall-Kirkham 1 m Cassegrain reflecting telescope to be installed at Mt. John University Observatory is described.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984.  相似文献   

7.
A discussion of laboratory spectra similar in temperatures and ion abundances to solar flare spectra is given. The laboratory spectra were obtained from high temperature plasmas produced by high power lasers and low inductance vacuum sparks. The current state of knowledge regarding line identifications in laboratory spectra is reviewed, and some of the results are used to identify lines in the high temperature solar flare spectrum in the 100 Å region and in the 1000 Å region. In addition, the physical dimensions and temperatures of the hot regions in the plasmas produced by the low inductance spark were recently measured, and a short summary of the results is given.A review paper given at the IAU Colloquium No. 27 on Ultraviolet and X-Ray Spectroscopy of Astrophysical and Laboratory Plasmas, held at Harvard University, 9–11 September, 1974.On leave from Tel-Aviv University, Tel-Aviv, Israel.  相似文献   

8.
Photoelectric observations of the eclipsing binary V 1073 Cyg have been carried out inB andV colours at the Ege University Observatory. The light curves were analyzed with the Wilson-Devinney approach. A period study reveals that the orbital period of the system is decreasing at the rate of (3.21 ± 0.17) second per century.  相似文献   

9.
We present the archive of the wide‐field plate observations obtained at the University Observatory Jena, which is stored at the Astrophysical Institute of the Friedrich Schiller University Jena. The archive contains plates taken in the period February 1963 to December 1982 with the 60/90/180‐cm Schmidt telescope of the university observatory. A computer‐readable version of the plate metadata catalogue (for 1257 plates), the logbooks, as well as the digitized Schmidt plates in low and high resolution are now accessible to the astronomical community.This paper describes the properties of the archive, as well as the processing procedure of all plates in detail. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

10.
The possibility of the formation of galaxies both during the galactic clustering of small structural units originated earlier and at fragmentation of larger formations is considered. A selfsimilar spectrum of long-wave perturbations is obtained. The results of numerical calculations and conclusions of Press and Schechter's (1974) work are discussed.Translated by Miss Eva Vokálová, Astronomical Institute of Charles University, Prague.  相似文献   

11.
The stratified core sample returned from Mare Crisium by the Luna 24 unmanned space probe is composed primarily of a new variety of subophitic to ophitic basalt with very low contents of TiO2 and MgO. This consists of clinopyroxene, calcic plagioclase, olivine, and minor amounts of silica, chromite, ulvöspinel, ilmenite, troilite, apatite, and Fe-metal. Granular metabasalts have the same bulk composition, but mineral phases exhibit less compositional variation. Fine-grained impact melts have similar compositions and are apparently derived from these basalts. We conclude that the basalts, which are chemically distinct from the very-low-titanium basalts found elsewhere on the Moon, represent the local surface flows of Mare Crisium.Sparse fragments of an olivine vitrophyre that is low in TiO2 but high in MgO and approaches the composition of the Apollo 15 green glasses may be derived from patches of dark mantling materials 20 km from the landing site.Now at Department of Geology, University of California at Davis, Davis, Calif., U.S.A.Now at Department of Geological Sciences, The University of Tennessee, Knoxville, Tenn., U.S.A.  相似文献   

12.
We have measured the motion of facular points and granules in the same region near a decaying sunspot. It is found that both features move away across the moat surrounding the sunspot. The mean speed of facular points is larger than that of granules: 0.65 km s–1 and 0.4 km s–1, respectively. These results are consistent with previous measurements of the speed of bright network features and moving magnetic fields, as well as of non-magnetic photospherical material. They support models in which a decaying sunspot is at the center of a supergranule, whose horizontal motions sweep out granules and magnetic flux tubes associated to the facular points. It is also found that granules are dragged by supergranular motions away of the moat.Contributions from the Kwasan and Hida Observatories, University of Kyoto.A part of this work was done while one of the authors (R.M.) was staying at the Kwasan and Hida Observatories, University of Kyoto, Japan, as a JSPS research fellow.  相似文献   

13.
H. Lundstedt 《Solar physics》1982,81(2):293-301
Lundstedt et al. (1981) showed that the direction of the photospheric magnetic field at the site of a flare is a good predictor of the solar wind velocity observed at Earth four days later. We describe here how the field direction was obtained, and discuss possible errors involved in the determination of the angle. The discussion also includes a characterization of the solar active regions.Now at Institute for Astronomy, Lund University, Lund, Sweden.  相似文献   

14.
The new échelle spectrograph FLECHAS (Fibre Linked ECHelle Astronomical Spectrograph) is in operation at the Nasmyth‐focus of the 0.9 m telescope of the University Observatory Jena. FLECHAS is equipped with a sensitive back‐illuminated and midband coated CCD‐detector, as well as with a calibration unit for flatfield and wavelength‐calibration. The spectrograph covers the spectral range between about 3900 and 8100 Å and exhibits a resolving power of R ∼ 9300. In this article all technical characteristics of FLECHAS are described and examples of the first astronomical observations obtained with the new instrument in July 2013 at the University Observatory Jena are presented, among them the first light spectra taken with FLECHAS, simultaneous imaging and spectroscopic observations, the determination of the detection limit of the instrument, the spectroscopy of stars of different spectral types and of faint extended objects, as well as the Li‐line detection in the spectra of young solar‐like stars. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

15.
A new digital radio spectrograph, the Madurai Solar Radio Spectrograph (MSRS), has been constructed at Madurai Kamaraj University, Madurai, India, and is being operated at the Radio Astronomy Centre, Ooty in southern India to observe solar bursts in the frequency range 30–80 MHz. The operation of the new instrument is briefly described. Observations of solar bursts by this instrument and the results from the preliminary analysis are presented.  相似文献   

16.
Abstract– Klaus Keil ( Fig. 1 ) grew up in Jena and became interested in meteorites as a student of Fritz Heide. His research for his Dr. rer. nat. became known to Hans Suess who––with some difficulty––arranged for him to move to La Jolla, via Mainz, 6 months before the borders of East Germany were closed. In La Jolla, Klaus became familiar with the electron microprobe, which has remained a central tool in his research and, with Kurt Fredriksson, he confirmed the existence of Urey and Craig’s chemical H and L chondrite groups, and added a third group, the LL chondrites. Klaus then moved to NASA Ames where he established a microprobe laboratory, published his definitive paper on enstatite chondrites, and led in the development of the Si(Li) detector and the EDS method of analysis. After 5 years at Ames, Klaus became director of the Institute of Meteoritics at the University of New Mexico where he built up one of the leading meteorite research groups while working on a wide variety of projects, including chondrite groups, chondrules, differentiated meteorites, lunar samples, and Hawai’ian basalts. The basalt studies led to a love of Hawai’i and a move to the University of Hawai’i in 1990, where he has continued a wide variety of meteorite projects, notably the role of volcanism on asteroids. Klaus Keil has received honorary doctorates from Friedrich‐Schiller University, Jena, and the University of New Mexico, Albuquerque. He was President of the Meteoritical Society in 1969–1970 and was awarded the Leonard Medal in 1988.
Figure 1 Open in figure viewer PowerPoint Klaus Keil at the University of Hawai’i at Manoa, 2007.  相似文献   

17.
In this work we present detailed photometric results of the trapezium like galactic nearby OB clusters NGC 1502 and NGC 2169 carried out at the University Observatory Jena. We determined absolute BVRI magnitudes of the mostly resolved components using Landolt standard stars. This multi colour photometry enables us to estimate spectral type and absorption as well as the masses of the components, which were not available for most of the cluster members in the literature so far, using models of stellar evolution. Furthermore, we investigated the optical spectrum of the components ADS 2984A and SZ Cam of the sextuple system in NGC 1502. Our spectra clearly confirm the multiplicity of these components, which is the first investigation of this kind at the University Observatory Jena (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

18.
The time sequence of line profiles of Fe xiv emission obtained at the 1965 solar eclipse is examined for temporal variations of intensity and profile. Although no variations are found in some regions examined, two regions with intensity and profile line width variations are found. A simple temperature wave is consistent with observations.Work performed under the auspices of the U.S. Energy Research and Development Administration.Work accomplished at the Department of Physics and Astronomy, University of Wyoming, Laramie, Wyoming.  相似文献   

19.
A systematic study of the internal horizontal (line-of-sight) motions of quiescent prominences which were observed at the limb has been made by using fourier techniques to analyse the shift of the Ca ii K line as a function of height above the limb. The results indicate that a characteristic size for the velocity elements is present in 70% of the 13 prominences studied. This size of 4700 km is attributed to Alfvén waves induced by horizontal convective motions in the photosphere as previously suggested by Malville. The qualitative aspects of the observations are described by a simple model which is based on this hypothesis.Presently at Department of Astronomy, Pennsylvania State University, 525 Davey Lab., University Park, PA 16802.Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.  相似文献   

20.
This article is essentially the text of lectures presented September 7, 1982 at the Max Born Centenary Conference held in Edinburgh, Scotland and October 21, 1982 at the Max Born Symposium held during the Annual Meeting of the Optical Society of America.Emil Wolf is Wilson Professor of Optical Physics at the University of Rochester. Reprinted fromOptics News, November/December 1983 with permisssion from the author and the Optical Society of America  相似文献   

设为首页 | 免责声明 | 关于勤云 | 加入收藏

Copyright©北京勤云科技发展有限公司  京ICP备09084417号