... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

... In combining the data, it is assumed that the low resolution image better represents the short spacing data, whereas the high resolution best represents the fine structure. ... Key: out The output image. ... Key: factor The flux calibration factor. ... In practise, the calibration may not be perfect, and an extra calibration factor will be required to align the flux scales. "factor" gives the factor to scale the low resolution image to put it on the same flux scale as the high resolution image. ...

... Moscow, Russia E-mail: krivosheev@iki.rssi.ru Notes: · · The Monte Carlo method (s) is also called the statistical test method An innumerable number of processes can be listed the outcome of which is not determined and has probabilistic nature, but these processes obey statistical laws, so to obtain the result we have to make multiple similar tests, i.e. to use the MC method Because probabilistic processes are widely spread in nature, the MC ...

REPEATABILITY OF THE FOS G130H GRATING EXTERNAL WAVELENGTH ZEROPOINT ANURADHA KORATKAR and IAN EVANS Space Telescope Science Institute,3700 San Martin Drive, Baltimore, MD 21218 Abstract. Measurements of the position of the geo­coronal Lyff are used to determine the repeata­ bility of the G130H grating and the external wavelength zeropoint for the first time since launch. ... The 1oe repeatability of the wavelength calibration is 0.159 љ A (0.64 pixels or 39 kms \Gamma1 ). ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

... Energy . ... The free ions and electrons in a plasma behave the same way. Knowing the temperature of the high atmosphere of Earth, or that of the Sun, we can calculate energies expected of ions and electrons found there. However, ions and electrons actually observed in space are often much, much more energetic, and may move at a respectable fraction of the velocity of light (300,000 km/sec or 186,000 miles/sec). ... Typical energy of an electron in the polar aurora. 40,000 ev . ... 50,000 ev . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... We present the numerical simulations for an electron-beam-driven and loss-cone-driven electron cyclotron maser (ECM) with different plasma parameters and different magnetic field strengths for a relatively small region and short time-scale in an attempt to interpret the recent discovered intense radio emission from ultracool dwarfs. ... A wide frequency band should therefore be covered by future radio observations. ...

... Many scientific institutions maintain bibliographies of articles published by their scientists and monitor references made to these publications; these figures are often used to evaluate the effectiveness of the institution. ... a) Identification of papers that are based, at least partly, on new data Publications based on observations can be subdivided into two groups: those presenting new, previously unreported data, and those that make use of already published data. ... Published by . ...

FLAGGING ANOMALOUS CCDS IN MOS: IN CONTINUATION WITH THE PATH OF EMTAGLENOISE Chandreyee Maitra 2015 EPIC calibrations and operating meeting ESAC, April 9th 2015 1 LOW ENERGY NOISE ON MOD CCDS a.k.a anomalous state in CCDs (Kuntz & Snowden 2008) ! ... 2 LOW ENERGY NOISE ON MOD CCDS Work done by Kuntz & Snowden while modeling the QPB CHARACTERISTICS Enhanced count rate at E < 1 keV and low hardness ratio. Most affected MOS 2 CCD 5 and MOS 1 CCD 4 but found in other CCDs as well. ...