Peremennye Zvezdy", . ... Min . ... Data . ... min . Comm. ... NSVS 6365610 . ... TYC 2284 00373 1 . ... 11.8 . ... NSVS 6368376 . ... NSVS 3795152 . ... NSVS 3804916 NSVS 6378197 NSVS 6430145 . ... MinII = 14.35, D = 0.07P. The ROTSE data with photometric correction flags (usually rejected) were kept for the analysis. ... A search for variables was carried out in the publicly available data of the Northern Sky Variability Survey (NSVS, Wozniak et al., 2004, also see http://skydot.lanl.gov/nsvs). ...

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• Mercurys Transit: An Unusual Spot on the Sun

... Accurate identification of physical binary star systems has become of increasing interest in recent years. ... Identification of physical binary star systems, with an estimated reliability of such identifications based on the theory of probability, is also important for current and future efforts to find binary star systems that are candidates for observations with the aim of determining their orbits and component masses. ... probability of the proximity of proper motions and ; . ...

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• Modelling Spectro-photometric Characteristics of Eclipsing Binaries
• ESO C Library for an Image Processing Software Environment (eclipse)

... The RS CVn binary HD185510 consists of a K0 III giant which eclipses its faint blue companion every 21 days. The latter has been identified as an sdB star: it is the only such object known in a wide eclipsing binary and can only be observed in the ultraviolet, where its radial velocity amplitude and spectrum have been recorded. A detailed analysis of the orbit from a new ultraviolet light curve and previous radial velocities indicates a low mass (~0.3 solar masses) for the blue star. ...

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• Armagh Observatory
• Solar Eclipse Observed Armagh Observatory
• Lunar Eclipse - January 2000

Next: Accretion Disks with Up: StarsStellar Populations, Previous: Spectroscopic Analysis of . ... We present and discuss spatially resolved spectra of the accretion disk and the gas stream region as a function of distance from disk center, the spectrum of the uneclipsed light, and the radial temperature distribution in the ultraviolet. Keywords: Accretion disks, Cataclysmic variables . ... In this paper we report on the HST spectral mapping of the nova-like UX UMa. ...

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• Results
• HST this week: 335

Catalogue of eclipsing variables (CEV) is the world's principal database of eclipsing binary systems with available classification. CEV contains identifications, classifications, photometry, periods, eclipses data, spectral types, references and notes for 7179 systems. Format of the current CEV . CEV main table (~1.0MB) . ... List of systems, erroneously classified as eclipsing binaries in GCVS (they are not included in the CEV main table) Download all files as a single archive (~0.6MB) . ...

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... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2014 April 30 . A Partially Eclipsed Setting Sun . ... Explanation: If you look closely, you will see something quite unusual about this setting Sun. ... The next solar eclipse will be another partial eclipse , will occur on 2014 October 23, and will be visible from most of North America near sunset. ... About APOD | ...

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• APOD: 2004 June 15 - A Rare Annular Venusian Solar Eclipse
• APOD: 2014 August 24 - Mercury's Transit: An Unusual Spot on the Sun
• APOD: 2006 November 14 - Mercurys Transit: An Unusual Spot on the Sun

... P2456 Date Received: 2008-Dec-02 00:27:59 Technical Page Proposal Type: General Category: Observation Category: Total Time Requested: Minimum Useful Time: Prop osal Title: ABSTRACT: Urgent Pulsars Galactic 3 Hours 20 min Establishing a phase-coherent timing solution for a bright, unusual MSP We have discovered a bright nearby eclipsing millisecond pulsar with a non-degenerate companion, a key "missing link" in the evolution of low-mass X-ray binaries into radio millisecond pulsars. ...

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• Pulsar Highlights - ALFA Finds Youngest Binary Pulsar Ever

... SB, Porb = 55.9212d. V0745 Cas| ... Component B of the double system observed brighter than in the Hipparcos Input Catalogue. ... The variability may be due to the fainter component. ... Type ELL: is also possible. pi Cas| ... Variability type and spectral type (F2/F3Ib/II) do not agree. ... Variability type and spectral type (F3/F5II) do not agree. ... Variability may be due to component B. VZ Pic| ... Variability may be due to component B. V1377 Ori| ... SB, Porb = 9.073d. V0421 Cep|105091| ...

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... Public . Science . ... Science Users Information Science Software Eclipse jump to navigation jump to content . ... Publications with ESO Data . ... Quality Control and Data Processing . ... ESO Science Newsletter . ... The algorithms used in this library have usually nothing specific to astronomy, they gather the know-how in the field of image and signal processing and attempt to make them useful to write astronomical data processing programs. eclipse is not meant to be an interactive facility. ...

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• ArtistтАЩs impression of eclipsing binary
• Explanation of eclipsing binaries
• A Vanishing Star Revisited | ESO

Next: Analysis in the Up: MIDAS utilities for Previous: Fourier analysis . For the detection of smooth signals, e.g. sinusoids, use either SCARGLE/TSA or AOV/TSA with bins. ... SCARGLE/TSA -- . Scargle sine model: This command computes Scargle's (1982) periodogram for unevenly spaced observations x . ... In this way, the command can be used to perform a CLEAN-like analysis manually by removing individual oscillations one by one in the time domain (see Roberts et al. ... AOV/TSA -- . ...

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• A0642 radio identifications
• Principal Components Analysis
• Correspondence Analysis

... The March 20 total solar eclipse was visible over the North Atlantic and Arctic Oceans. ... Solar eclipses are of interest for radio astronomy, as they make it possible to observe individual details on the solar disc (spots, filaments, flocculi, etc.) ... On March 20, 2015 the integrated observations of the solar eclipse were carried out at the RATAN-600 radio telescope at 70 wavelengths simultaneously in the range of 1.65cm to 10cm with the 1% frequency resolution. ...

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• Total solar eclipse broadcast from Kenya with GLORIA
• V1494
• Total Solar Eclipse of 2008 August 1

Next: Caverns in Binary Systems Up: Ejectors in Massive Binary Previous: The Number of Ejectors . In the very first years after the discovery of radiopulsars, it became clear that for some reason they avoid forming binary systems. ... Illarionov and Sunyaev (1975)[ 76 ] noted the fact that coherent radiowaves with a wavelength longer than 75 cm, which make it possible to observe most of the radiopulsars, are absorbed effectively in the stellar wind of a normal star. ...

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• Seminars
• PSR B0042-73 in the Small Magellanic Cloud
• Evolutionary Tracks

... V838 Mon is a member of a new class of eruptive variables which appear as a peculiar novae having late K-M type spectra in their outburst. Before its outburst, it was a wide binary system of B3V type stars. ... The B3V companion was seen in the outburst in the UV spectrum taken with HST (Rauch et al., ... In the latest spectra, the light of B3V companion was predominating in the short-wave photometric bands. ... CCD blue frames of V838 Mon before the eclipse (left) and in the eclipse (right). ...

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• http://mavr.sao.ru/hq/eclipse/eclipse_BTA.html
• Solar eclipse
• GRB follow-up team

Next: Summary of tasks in Up: PROS USERS GUIDE Previous: *qpspec* - Time Resolved . Photons detected with the Einstein IPC and HRI were time-tagged to a precision of 63 sec and 8 sec, respectively. ... The input for most timing tasks is a time-sorted .qp file, which is made from a QPOE file by the task timsort . ... An example of a typical timing analysis . ... calc_bary, apply_bary* - Barycentric Time Corrections . ... fft* - Period search using Fast Fourier Transform . A ``short'' FFT . ...

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• A Preliminary Investigation
• Possible Pitfalls
• Characteristics of the Aurig? System

Educator's Guide to Eclipses . ... In a solar eclipse you observe the Sun (using only safe methods, of course). ... In a lunar eclipse you observe the Moon. ... Because of the geometry described below, you can only view a solar eclipse when the Sun is up, and the Moon is nowhere to be seen. ... Eclipses occur when the Sun, Earth and Moon line up. ... In a solar eclipse the Moon passes directly in front of the Sun. ... In a lunar eclipse the Moon moves into Earth's shadow. ...

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• A Vanishing Star Revisited (ESO Press Release 11/99)
• FEBRUARY 26th 1998 SOLAR ECLIPSE FROM VENEZUELA
• APOD: 2000 July 26 - Lingering Lunar Eclipse

. Next: The Masses of Neutron Up: Binary Neutron Stars Previous: Core-Mass Radius relations . љ . Radio waves absorbed/scattered by companion . Generally bloated low mass stars . hours for some . Orbits not necessarily edge on . Companions are heated on one side by pulsars . љ љ . Figure 49: . љ љ . Figure 50: Off and on pictures of eclipsing pulsars . Jon Bell . Thu Dec 19 15:15:11 GMT 1996

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• Probing the Eclipse Region of a Binary Millisecond Pulsar
• UBV Photometry of the Massive Eclipsing Binary TT Aur
• uvdump

INTEGRAL observations of SS433 : new results Anatol Cherepashchuk Sternberg Astronomical Institute, Moscow University, Russia In collaboration with: Rashid Sunyaev ... Eleonora Antokhina, Nikolai Shakura, Darja Kosenko, Elena Seifina,Sergey Molkov (IKI) 1 Overview · Introduction · · · · Observations Analysis of hard X-ray spectra Analysis of hard X-ray eclipses Discussion and conclusions December 26, 2007 ...

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Hipparchus (and possibly Aristarchus before him) also derived the Moon's distance from the duration of a lunar eclipse . Because the Earth casts a much larger shadow than the Moon, such an eclipse usually darkens the entire Moon, for several hours. ... If the Sun is assumed to be very distant, and if the Moon crosses the middle of the shadow (if not, corrections must be made), the width of the shadow is expected to be about 2r , twice the Earth's radius r . ... Last updated 4 February 1999 Moon. ...

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• The Path of the Sun, the Ecliptic
• Saturn's Possible New Moons

... The goal of this analysis is to determine to what extent the systematic errors affect the measured eclipse depth and time of mid-eclipse. ch1 0.120 0.120 0.300 ch2 0.120 0.120 0.300 0.00213 0 .0 0 0 Tmid Kurtosis Poly Wave MCMC ch1 ch2 9 13 0.06 0.92 1.5 - 0 .2 3 0.00094 0.000 Figure 3: p vs. rank plots showing that with the extra systematic error added the results for the depth in channel 1 (left) and channel 2 (right) become close to Gaussian. ...

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• Example of an OOF analysis for the GBT Bojan Nikolic web pages (r. 329)
• ALMA WVR phase correction algorithms and software Bojan Nikolic web pages (r.

... The Russian TESIS (FIAN) Solar Observatory has transmitted observations back to Earth of the solar eclipse made on July 22nd, 2009. ... On the first occasion, the satellite passed through the eclipse area at 04:30 Moscow time, making it the first on our planet to see the shadow of the Moon, which was still in space and was only approaching the Earth ( film 1.2 MB, wmv format ). ... The first Moon passage over the solar disk (00:30 UT) (Movie wmv; 1.2 MB) . ...

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• The Russian TESIS Observatory will observe two solar eclipses from space
• The culmination of the solar eclipse coincided with the strongest magnetic
• Solar eclipse - the eighth wonder of the world - TESIS photo gallery