... NGC 6357s Cathedral to Massive Stars . ... Credit Copyright: NASA , ESA and J. M. Apellюniz ( IAA , Spain) Explanation: How massive can a normal star be? Estimates made from distance, brightness and standard solar models had given one star in the open cluster Pismis 24 over 200 times the mass of our Sun, nearly making it the record holder. ... Publications with keywords: massive stars . Publications with words: massive stars . ... A Massive Star in NGC 6357 . ... Massive Stars Of 30 Doradus . ...

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• Massive Stars in Open Cluster Pismis 24
• Астронет > Massive Stars in Open Cluster Pismis 24
• NGC 6357: Cathedral to Massive Stars

... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2012 November 18 . NGC 6357: Cathedral to Massive Stars . Image Credit: NASA , ESA and Jes s Ma z Apell niz ( IAA , Spain) . Explanation: How massive can a normal star be? ... Toward the bottom of the image, stars are still forming in the associated emission nebula NGC 6357 . ... About APOD | ... A service of: ASD at NASA / GSFC . ...

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• APOD: 2008 October 26 - Massive Stars in Open Cluster Pismis 24
• APOD: 2006 December 19 - Massive Stars in Open Cluster Pismis 24
• APOD: 2008 December 1 - Massive Stars Resolved in the Carina Nebula

... The hot component shows very spectacular activity: irregular outbursts accompanied by fast, massive outflows and jets. ... Diffraction-limited images for both components of CH Cyg binary system were reconstructed using visible speckle interferometry at BTA 6-m telescope (Fig.1). The orbital period 15.6 years and masses: 2.0 Msun and 0.7 Msun for red giant and white dwarf, respectively were derived from angular distance (0.042") and magnitude difference (2 m ) of the components. ... Fig.1. ...

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• Detection of unique bright radio flare of X-ray binary
• Galaxy sector, archive 2006
• Galaxy sector, archive 2009

A New Mass Model For The JVAS Gravitational Lens B1030+074. ... University of Manchester, Jodrell Bank, U.K. B1030+074 is a double image gravitational lens, which was dis- covered during the Jodrell Bank VLA Astrometric Survey (JVAS). ... HST WFPC2 observations have revealed the lensing galaxy, which lies close to component B. The redshifts of the lensing galaxy and the background source have also been obtained and are 0.599 and 1.535 respectively. ...

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• Bojan Nikolic -- 90 GHz Continuum Observations of Messier 66
• G41.1-0.3

Next: Pass band integrations Up: Fit scenarios Previous: Triple with velocity curves Contents . Fit all three masses, as well as the inclination of one of the pairs. That not any combination of orbital inclinations is allowed can be seen from the fact that the triple consists of two double-lined binaries and only one mass solution exists for a given inclination. ... Christian Hummel 2015-04-28 ...

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• Masses
• The format of STARTABLE
• ESO - Thesis Topic: Magnetic fields in massive stars

... Called Gliese 623b or Gl623b, the diminutive star (right of center) is ten times less massive than the Sun and 60,000 times fainter. ... The image file is on oposite.stsci.edu in the directory /pubinfo/gif: PR# GIF File Caption text Object STScI-PRC94-54 Gl623b.gif G1623b.txt Dwarf Star Gliese 623b The photo release text is in the directory /pubinfo/press-releases: PR# PR text STScI-PRC94-54 PR-54.txt Another directory, /pubinfo/latest, contains all of the files relevant to the latest releases. ...

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• APOD: October 2, 1999 - Phi Persei: Double Star
• APOD: October 18, 1999 - NGC 3603: An Active Star Cluster
• Hubble Uncovers Dust Disk Around a Massive Black Hole (STScI-PRC98-22) A

B?rbel Koribalski (ATNF) + HIPASS and ZOA teams . The properties shown below were derived from the measurd HI properties. Displayed here are the Local Group velocities of all sources from -300 to +8000 km/s (bins are 100 km/s). Displayed here are the distances of all sources (assuming Ho = 75 km/s/Mpc). ... Displayed here are the HI masses of all sources (assuming point source distribution). Extended galaxies and pairs/groups need to be re-measured. ...

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• UBV Photometry of the Massive Eclipsing Binary TT Aur
• casacore: components/ComponentModels.h Source File
• casacore: components package (libcasa_components)

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Lightcurve of HW Vir from images obtained using the Faulkes Telescope South, operated by Las Cumbres Observatory . The blue triangles show the difference between two stars whose brightness is constant. ... This shows the value of the Faulkes Telescopes in the follow-up observations of eclipsing binaries with the aim to detect and characterise additional circumbinary companions. ...

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• Armagh Observatory
• Homepage of "Jorick Vink"
• M. de Groot, Senior Research Associate

... Tonight's Sky . ... Behemoth black hole found in an unlikely place . ... Ancient super-bright quasar with massive black hole found . ... Quasars supermassive black holes found at the center of distant massive galaxies are the most luminous beacons in the sky. ... An international team of astronomers, including Carnegie s Yuri Beletsky, has discovered the brightest quasar ever found in the early universe, which is powered by the most massive black hole observed for an object from that time. ...

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• The most massive star | Astronomy.com
• What factors determine if a massive star (say, 100 solar masses) forms instead
• XMM-Newton's massive discovery | Astronomy.com

Text of these problems is available also in other languages : . ... What can one see in the Moon's sky more often - the Sun or the Earth? ... There are about of 250 millions of stars in the elliptical galaxy M32 (a satellite of Andromeda galaxy). ... The masses of Capella's components. ... You are proposed to estimate the masses of Capella's components, using our observational data. ... A galaxy's mass. ... Estimate the mass of FGC 1908 and compare it to the mass of our galaxy. ...

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... What are the fluxes of the stars? ... Volume sampled is no longer 4/3 pi r cubed due to curved space-time Want to derive population properties brightness, size, etc - as function of distance (therefore, cosmic time) But - biases in sample Biases NUMBER OF STARS VS MASS Eddington Bias: in astronomy, there are always more little faint things than big bright things. ... Suppose there are 10 stars of mass 0.5 and 100 stars of mass 0.4, and you have a 20 percent error on measuring the mass. ...

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• PAUL J. GREEN - Contributing ConcepTests
• The AstroStat Slog massive data
• Characteristics of the Aurig? System

... (Roettgering+, 1994) ============================================================================ Samples of ultra-steep spectrum radio sources ROETTGERING H.J.A., LACY M., MILEY G.K., CHAMBERS K.C., SAUNDERS R. 15mJy z: A bright serendipitous source in the VLA field ---------------------------------------------------------------------------- Notes on individual sources : 0141+356 A serendipitous double ... 1718+630 Component '1' serendipitous or related to double radio source? ...

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• Sky models
• Current star formation rate
• A deep 38-MHz radio survey

... Stars . ... Cepheid variable stars have been known since the 18th century. ... Regularly brightening to a peak over days, weeks or months before fading these variable stars were remarkable curiosities to astronomers in past centuries.€а The term Cepheid is taken from the star Delta Cephei in the constellation of Cepheus, which was identified as variable€а in 1784 by the teenaged prodigy John Goodricke (1764-96). ... Tweets that mention Cepheids: Inconstant Stars which break the rules | ...

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• Orion, mighty hunter of the winter sky | Astronotes
• Stargazing in July | Astronotes
• Exploring Icy Moons in Search of Life | Astronotes

The black hole. ... The black holes are generated in the result of a collapse of giant stars with the mass more than three Sun's masses. ... And moreover the gas near the neutron star or the black hole will get hot and will become a source of high energetic electromagnetic radiation in X-rays and gamma range. ... In the majority of double systems, being the sources of X-rays radiation, the invisible component mass does not exceed the two solar masses, so it is a neutron star. ...

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• bliznetsie

Properties of the interstellar gas clouds . ... The angular resolution of this Survey was 2.4' x 130', velocity resolution was 6.3 km/s, r.m.s. fluctuations of antenna temperature (T a ) was 0.25 K. All clouds with kinematical distances r a Some selection effects were discovered and our statistic results were corrected for them. Figure 1. ... In the very high mass range the number of neutral gas clouds may be decreased because of gravitational instability or/and molecularization. ...

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• Results scientific researchs 5
• Olga Maryeva homepage
• Bispectrum Speckle Interferometry of the Massive Protostellar Object S140 IRS

HIGH RESOLUTION IONOSPHERIC MASS SPECTROMETER P-11 . ... Onboard mass-spectrometric equipment for study of neutral and ionized components of Earth upper atmosphere. Mass-spectrometer P-11 is one of P-series modifications of the on board radio-frequency monopole spectrometers. ... The instruments of P-series have passed successful approbation in space experiments aboard geophysical rockets MP-12, launched for investigation of Earth upper atmosphere (Ref. ... Measured mass number range, AMU - 1.. ...

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• Extragalactic Astronomy
• Stellar Astronomy
• Solar Physics

... 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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• ADASS 2003 Conference Proceedings
• Application of the Minimum Determination Algorithm to the Study of the Fine
• Calculating the Position and Velocity Components of HST

... Phase light curves of binary model that consists of a primary component with mass M 1 and a secondary component with mass M 2 . ... The input parameters of the problem are the accretion rate onto the binary components ( ), the component mass ratio q = M 2 /M 1 , the orbital inclination to the line of sight , the eccentricity e, the rotation angle of the apsidal line relative to the observer , and the parameter c characterizing viscosity. ...

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• Conferences
• Articles

NMW survey overview . Access image archive . ... The New Milky Way survey aims to detect bright (V<13.5) optical transients near the Galactic plane using an automated wide-field (8x6 deg.) system capable of surveying the whole Milky Way area visible from the observing site in one night. ... All images obtained during the transient search survey are available online (please use the image archive access form ). ... Images per field: . ... Images per night: . ... Milky Way imaging time: . ...

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The HI Mass Function: Open Questions Stephen Schneider University of Massachusetts The Evolution of Galaxies through the Neutral Hydrogen Window 1 February 2008 HI Mass Functions = ­1.5 = ­1.2 Is the bright end variable? Is There One HI Mass Function? ... Also face flux-bias problems when hunting close to noise: promote more weak sources than lose stronger sources Arecibo Slice AGES HI Mass Function to Date The slope is relatively flat for the first 142 galaxies detected. ...

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• http://www.naic.edu/~astro/hiconference/hiconf_pdfs/baker_0802naic.pdf
• http://www.naic.edu/vscience/schedule/tpfiles/FreiretagP2391tp.ps
• http://www.naic.edu/~gibson/cv/granada.pdf