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http://mavr.sao.ru/hq/lizm/conferences/pdf/1987/1987_p41-p41.pdf.

1. http://mavr.sao.ru/hq/lizm/conferences/pdf/1987/1987_p41-p41.pdf
... An attempt is made to explain light variations in the blue region of the magnetic star CQ UMa by means of a simple oblique rotator model with one extensive circular dark spot centred to the south magnetic pole; Observed variations in v and colours may be explained by a spot covering about 69 percent of a hemisphere, the ratios of luminances (brightness densities) inside and outside the spot being 0.77 and 0 . ...
[ Текст ]  Ссылки http://mavr.sao.ru/hq/lizm/conferences/pdf/1987/1987_p41-p41.pdf -- 13.5 Кб -- 24.02.2010
[ Текст ]  Ссылки http://www.sao.ru/hq/lizm/conferences/pdf/1987/1987_p41-p41.pdf -- 13.5 Кб -- 24.02.2010
[ Текст ]  Ссылки http://jet.sao.ru/hq/lizm/conferences/pdf/1987/1987_p41-p41.pdf -- 13.5 Кб -- 24.02.2010
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2. Low Surface Brightness Galaxy Gallery
In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...
[ Сохраненная копия ]  Ссылки http://zebu.uoregon.edu/sb2.html -- 4.8 Кб -- 26.05.2000
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3. APOD: 2006 September 5 - Bright Cliffs Across Saturns Moon Dione
... 2006 September 5 . Bright Cliffs Across Saturn's Moon Dione . Credit: Cassini Imaging Team , SSI , JPL , ESA , NASA . Explanation: What causes the bright streaks on Dione? Recent images of this unusual moon by the robot Cassini spacecraft now orbiting Saturn are helping to crack the mystery. ... The bright ice-cliffs run across some of Dione 's many craters, indicating that the process that created them occurred later than the impacts that created those craters. ... About APOD | ...
[ Сохраненная копия ]  Ссылки http://www.sai.msu.su/apod/ap060905.html -- 5.5 Кб -- 02.10.2012
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4. WFPC2 Instrument Handbook Update
... To be read in conjunction with Section 4.11 of the WFPC2 Instrument Handbook , -Version 4.0. ... 1 The second study found evidence that CTE loss for faint stars has increased with time (Whitmore, 1998). The primary observational consequence of CTE loss is that a point source at the top of the chip appears to be fainter than if observed at the bottom of the chip, due to the loss of electrons as the star is read out down the chip (see Figure 1 ). ... Last updated: 06/16/98 10:38:00 . ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/instrument-news/handbooks/wfpc2/98update/update0698.fm1.html -- 6.8 Кб -- 23.06.1998
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5. XWare > APOD
... IC 405: The Flaming Star Nebula . ... A Superwind from the Cigar Galaxy . ... This composite image was made from 22 separate pictures of the Moon and Sun all taken from Chisamba, Zambia during the total phase of the 2001 June 21 solar eclipse. ... Leonids Over Indian Cove . ... Canis Major Dwarf: A New Closest Galaxy . ... For many years astronomers thought the Large Magellan Cloud (LMC) was closest, but its title was supplanted in 1994 by the Sagittarius dwarf galaxy. Leonids from Leo . ...
[ Сохраненная копия ]  Ссылки http://www.astronet.ru/db/xware/apod.html?page=314&d=2012-06 -- 14.6 Кб -- 13.04.2016
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6. Analysis of very bright sources
XMM-Newton Science Analysis System . ... A different approach is done via the setting withctisrcpos =Y: all event energy corrections do not use the actual RAWY coordinate but the corresponding RAWY location of the source ( SRCPOS ) as determined by the task epframes (either automatically or via setting withsrccoords =Y). ... The task epchain may be used with the setting ccds =4 withctisrcpos =Y to process only the CCD 4 where usually the bright source is located that causes the Out-of-Time events. ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/7.0.0/doc/epevents/node8.html -- 4.8 Кб -- 28.06.2006
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7. HIPASS Bright Galaxy Catalog
... The two plots below illustrate two of the selection criteria: velocity width (limited by the channel width) and the HIPASS peak flux. Zoom-in on Figure 3a. The two plots below give some idea of the shape of the HI spectra. ... For Gaussian HI spectra the difference is slightly more, but for irrgeular galaxies, pairs and groups many different shapes are observed. ... Some trend towards detecting more narrow-width galaxies at higher velocities is visible. ...
[ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/people/bkoribal/BGals/comparisons.html -- 2.8 Кб -- 23.12.2007
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8. http://www.izmiran.rssi.ru/~obridko/papers/2004IAUS_223_371B.pdf
... It is found that the correlation coefficients between these two parameters calculated separately inside and outside the sunspot formation zone ±30 have cyclic variation and occur in anti-phase. This suggests different mechanisms of formation of the corona in the fields of small, medium, and large scales. ... The relationship between the coronal green line brightness (CGLB) and the magnetic field strength (MFS) has been investigated by constructing the corresponding synoptic maps for the 1977-2001. ...
[ Текст ]  Ссылки http://www.izmiran.rssi.ru/~obridko/papers/2004IAUS_223_371B.pdf -- 73.7 Кб -- 17.11.2015
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9. M. de Groot, Senior Research Associate
... In collaboration with Drs Van Genderen (Leiden, Holland) and Sterken (Brussels, Belgium) papers XV and XVI in the series `Light Variations of Massive Stars' were published. These dealt with the brightness variations of several massive stars in the two nearest neighbour galaxies, namely six stars (R85, R99, R103, R110, R123 and R128) in the Large Magellanic Cloud (LMC) and two (R42 and R45) in the Small Magellanic Cloud (SMC). ...
[ Сохраненная копия ]  Ссылки http://star.arm.ac.uk/annrep/annrep98/node8.html -- 7.2 Кб -- 14.12.1999
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10. ALMA Phase Calibration Techniques at the Cavendish Astrophysics Group
ALMA | ... In this section, we explain why we need to correct phase fluctuations and ALMA's strategy to do this. Rapid fluctuations will be corrected with water vapour radiometers (WVRs). The Cavendish Astrophysics Group was also a leading contributor to the ALMA prototype WVRs, which were put through their paces in tests at the Submillimeter Array (SMA). ... The Cavendish Astrophysics Group in partnership with the Onsala Space Observatory built two prototype WVRs for the ALMA project. ...
[ Сохраненная копия ]  Ссылки http://www.mrao.cam.ac.uk/projects/alma/fp6/wvr.html -- 11.0 Кб -- 29.03.2012
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11. http://www.sao.ru/Doc-en/Science/Public/Bulletin/V1-57/38.pdf
... 38 CONTENTS Karachentsev I.D., Kopylov A.I., Kopylova F. G. Distance moduli in M 101 group from brightest stars .. Tikhonov N.A., Karachentsev I.D. Maffei 2, a nearby galaxy shielded by the Milky Way.. ... Zhuravkov A.V. , Bartolini C., Guarnieri A., Piccioni A., Zampieri G. Optical behaviour of GRO J0422+32 in different brightness levels ............................................................................. telescope .. ... Cas OB5 .. ... Instrumental facilities of the 6 m telescope .. ...
[ Текст ]  Ссылки http://www.sao.ru/Doc-en/Science/Public/Bulletin/V1-57/38.pdf -- 15.1 Кб -- 26.12.2008
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12. Mars pictures from Stellafane by Paul Valleli
Images and text 2003 Paul Valleli . While up at Stellafane for pre-convention preparations, I spent some early morning times, experimenting with different videography setups on the 13" F/10 Schupmann at the McGregor Observatory. ... Mars was too bright and would have required neutral density filters. ... Next time, I will try 12mm and 9mm projections. ... I aquired about ten thousand frames by 3AM, at which time a breeze picked up and the seeing went to Hellas! ... 2003 P