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http://www.sao.ru/Doc-en/Science/Public/Conf/magstars-2010/p153.pdf.

1. http://www.sao.ru/Doc-en/Science/Public/Conf/magstars-2010/p153.pdf
Magnetic Stars, 2011, pp. 153 ­ 156 Ab out the Dep endence of the Rotation Velo city of CP Stars on the Magnetic Field Glagolevskij Yu. ... Based on the observational data of the average magnitudes of the surface magnetic field strength Bs for a number of chemically peculiar stars we investigate the dependence of the rotation period on the magnetic field. ... Now the periods of rotation P and the average values of the surface magnetic field Bs are known for more than 50 magnetic stars. ...
[ Текст ]  Ссылки http://www.sao.ru/Doc-en/Science/Public/Conf/magstars-2010/p153.pdf -- 95.3 Кб -- 11.08.2011
[ Текст ]  Ссылки http://mavr.sao.ru/Doc-en/Science/Public/Conf/magstars-2010/p153.pdf -- 95.3 Кб -- 11.08.2011
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2. Is the Crab Pulsar Showing A 60-second Periodic Modulation?
... We Fourier analysed Hubble Telescope Crab pulsar data obtained with the High Speed Photometer in October 1993. A weak modulation at frequency Hz is detected. We found a strong correlation between this result and the Fourier transform result of stroboscopic Crab pulsar data obtained in December 1994 at the 1.82m telescope of Asiago observatory (University of Padua, Italy). ... We found that both data show a weak modulation at the period of 60 seconds. ... The corresponding frequency is Hz . ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/stsci/meetings/shst2/cadeza.html -- 12.0 Кб -- 15.06.2005
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3. http://mavr.sao.ru/hq/lizm/conferences/pdf/1991/1992_2_p12-p16.pdf
... SHTOL ' Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz 357147, Russia The investigation of such a phenomenon as the magnetic field variability at long times (years - decennials) is very interesting. If the explanation of the magnetic field variability with rotation period by the oblique rotator model is evident, then the reason of the long-period variability is not clear yet, despite the existence of some assumptions on its nature. ... Fig.2. ... 213 Fig.3. ...
[ Текст ]  Ссылки http://mavr.sao.ru/hq/lizm/conferences/pdf/1991/1992_2_p12-p16.pdf -- 57.5 Кб -- 24.02.2010
[ Текст ]  Ссылки http://www.sao.ru/hq/lizm/conferences/pdf/1991/1992_2_p12-p16.pdf -- 57.5 Кб -- 24.02.2010
[ Текст ]  Ссылки http://jet.sao.ru/hq/lizm/conferences/pdf/1991/1992_2_p12-p16.pdf -- 57.5 Кб -- 24.02.2010
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4. Concerning Steady State Corotation of the Io Plasma Torus
... In recent years, substantial information concerning the Io torus has been published. ... Explaining the observed steady state rotation of the torus seems to be difficult. The angular velocity of the torus must be in accordance with the celestial mechanics laws, of the same orders as Io's one. ... We wish to straighten out the situation describing the main geometric and kinematic features of the Io torus using a steady state model based on some of Alfven's ideas [Alfven, 1981]. ...
[ Сохраненная копия ]  Ссылки http://www.iki.rssi.ru/vprokhor/papers/iotor/iotor.htm -- 9.5 Кб -- 02.02.1999
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5. http://www.ipa.nw.ru/conference/2002/sovet/PS/GUSEV2.PS
... 8, ``Celestial Mechanics'', 2002 FCN -- period dependence on dynamic characteristics of a lunar core A. Gusev 1 , N. Petrova 1 , N. Kawano 2 , and RISE group 2 1 Kazan State University, Kazan, Russia 2 National Astronomical Observatory, Mizusawa, Iwate, Japan Two modes in a polar oscillation are obtained when a free rotation of the two--layer Moon was studied: 1 PCW = 2\Omega A Am p fffi ё 1 74yr 1 P FCN = \ Gamma \Omega A 2Am ` C c \ ...
[ Текст ]  Ссылки http://www.ipa.nw.ru/conference/2002/sovet/PS/GUSEV2.PS -- 40.0 Кб -- 19.08.2002
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6. Correlating Spectral Data with Spatial Gain Variations
Next: Quantum Efficiency Correction (a.k.a. Up: ROSAT HRI Recipes Previous: Appearance of new HRI . The mean pulse height analyzer channel (PHA) of a spectral distribution will vary depending on its location on the detector. Below is a method to compare observed data with that of preflight calibration measurements. ... For temporal gain variations, see The HRI Calbration Report . ... Retrieve the gain maps (mean PHA) from anonymous ftp at SAO. ... But don't forget temporal gain variations!] ...
[ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/PROS/PUG/node206.html -- 8.2 Кб -- 01.10.2012
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7. Armagh Observatory
... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... The formation process of a MBF and the associated BP (No. 1 in Table 1), which is formed by bipolar emergence. The top row gives the BP region as seen in AIA 193 at the indicated time. ... The bottom row shows the normalised AIA 193 lightcurve (left), and the positive (middle) and negative (right) magnetic fluxes obtained in the blue and yellow boxes marked in the top two rows. ...
[ Сохраненная копия ]  Ссылки http://star.arm.ac.uk/highlights/2015/685.html -- 6.8 Кб -- 18.01.2016
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8. Magnetic mapping
The magnetic mapping is fulfilled by the magnetic field line tracing from the satellite position up to the Ionosphere (stop trace at the altitude 110 km). ... As a rule the Tsyganenko [1987] external magnetic field model and IOPT = 3 (Kp = 2) are used. ... The output file includes the following information: . ... For example the file with name aa9610d1.geo contains the information corresponding to the aposteriory magnetic mapping for INTERBALL Auroral Probe for the first decade of October 1996. ...
[ Сохраненная копия ]  Ссылки http://www.iki.rssi.ru/vprokhor/descr/mapping.htm -- 4.6 Кб -- 12.05.1999
[ Сохраненная копия ]  Ссылки http://www.cosmos.ru/vprokhor/descr/mapping.htm -- 4.6 Кб -- 12.05.1999
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9. Processing OM Image mode data
... OM grism data are obtained as image mode data. However the different nature of this type of data, spectra of the objects in the field of view instead of their "sky" image, makes that a special processing must be applied to the grism images. ... They are concatenated in a perl script, omgchain , which works in a similar way to the image and fast mode chains. ... All necessary corrections are applied to the grism data files. ... As we have pointed out OM grism data are image mode data. ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/7.0.0/documentation/threads/omg_thread.html -- 15.4 Кб -- 21.08.2006
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10. Polarization properties (transmitted radiation)
Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...
[ Сохраненная копия ]  Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node5.html -- 24.1 Кб -- 19.11.2010
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11. http://www.izmiran.rssi.ru/~ichertok/Forbush/ECRC12_paper.pdf
... We analyze relations between characteristics of an extended ensemble of Forbush decreases (FDs) caused by CMEs from the central zone of the solar disk during the 23rd solar cycle, on the one hand, and such solar eruption parameter as a summarized unsigned magnetic flux of CME-associated EUV dimmings and arcades, on the other hand. ... FD magnitude Figure 1a shows the relationship between the magnetic flux and the FD magnitude AF for events unambiguously identified with concrete solar eruption. ...
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