Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System Characteristics Formation Exosolar Planets Class 3 Stars The Sun Stellar Evolution of Low and High Mass Stars Deaths of Stars Exotic Stars Class 4 Galaxies Galaxy Classification Formation of Galaxies Galactic Evolution ... So far, one planet has been studied by this method. ...

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• Amateur Astronomers Association of New York ? Amateur Astronomers Association
• Central Park ? Solar Observing ? Amateur Astronomers Association of New York
• AAA Urban Starfest in Central Park ? Amateur Astronomers Association of New...

EVOLUTION OF GALACTIC DISCS: TWO MODES OF STAR FORMATION ABSTRACT We develop the model of the evolution of surface gas density, stellar density, star formation rates and chemical composition of galactic disc taking into account the gravitational instability of rotating gaseous layer in the scales of several kpc. ... In the model we took into account the gas return from evolved stars, a radial movement of the gas in a spiral arms and accretion of the gas into the galactic disc. ...

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• Molecular Masers
• Astronomical Circular - Contents

Yu.V.Lunyova, A.F.Kholtygin . Chemical evolution of the system of galactic planetrary nebulae , Astrophysics , 45 , 451-463 (2002) . Chemical evolution of the system of galactic planetary nebulae beginning from the early age of the Galaxy is investigated. We calculate radial and vertical abundance gradients of C, N, O, Ne, Ar, Cl and S depending of different ages of the central star of the nebula. It have been founded statistically significant dependence of abundance gradients with the age of central star.

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• Broawn et al., MN, V. 352 (2004)
• Kholtygin, Astrophysics (2000)
• Vladimir P. Reshetnikov's Home Page

As an example for an observation of a stellar corona, a simulation of the response of RGS was performed. The input spectrum was a two component Mewe-Kaastra plasma, with solar abundance, and temperatures of 0.35 and 2 keV. ... The following image shows an intensity display of the measured spectrum with dispersion coordinate as measured in the spatial dimension on the RGS Focal Camera (RFC) along the abscissa, and the energy response of the CCDs along the ordinate. ...

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• XMM Science Objectives

... Future seminars . P a s t seminars . Seminar council . ... A.F. Zakharov (Institute of Theoretical and Experimental Physics) . ... Different regimes of gravitational lensing depend on masses of lens and correspond roughly an angular distance between images. If a gravitational lens has a typical stellar mass, this regime is named as microlensing because a typical angular distance between images is about microarcseconds in the case if sources and lenses are located at cosmological distances. ...

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• Electricity as a Fluid
• (Q-8) Quantum Tunneling
• Main results of the experimental and theoretical research completed in 2010

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

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• Central meridian positions for physical observations of Saturn for Computer
• Central meridian positions for physical observations of Uranus for Computer
• Central meridian positions for physical observations of Neptune for Computer

Gas outflows and stellar populations in powerful quasars Carolin Villforth University of St Andrews ! Paul Hewett, Vivienne Wild, James Allen Do quasar outflows depend on host stellar populations? Do quasar outflows depend on host stellar populations? Outflows Measure outflows in [OIII] Relatively Easy Do quasar outflows depend on host stellar populations? Outflows Measure outflows in [OIII] Relatively Easy Stellar populations Do quasar outflows depend on host stellar populations? ...

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• http://www.arcetri.astro.it/~palla/ANDREAIMMAGINI/ISM/Trifid.txt
• The relationship between NSs and SNRs (Elba, June 1-4,1998)
• The Mystery of the Lonely Neutron Star (ESO Press Release 19/00)

You Can Make Stellar Images Brighter . Articles | ... A few months ago I wrote an article titled "You Can’t Make Them Brighter". So why am I now writing that you can make them brighter. ... The image of a focused star is actually a small disk called the Airy disk, named after the 19 th century scientist Sir George Airy. ... For a given aperture, a smaller Airy disk means that the light is focused to a smaller disk and is therefore brighter. ... www.astronomy.net . About Astronomy Net | ...

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• Depends - an Astronomy Net Education Forum Message
• Depends - an Astronomy Net ATM Forum Message
• Amateur Astronomers Of Central Iowa, AstroGuide Listing

... Previous: Substepping and its Application to HST Imaging . ... This is a preliminary report on an application of the co-addition technique based upon the Richardson-Lucy algorithm. The combination of high signal-to-noise ground-based images obtained with the ESO NTT using SUSI with high angular resolution HST FOC f/96 images gives new insights on the properties of galaxy cores and their potential time variability. Cores of galaxies are one of the main thrusts of present extragalactic research. ...

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• Chandra X-Ray Observatory - First Year Science Highlights
• ADASS 2003 Conference Proceedings
• Using Massively Parallel Processing of a NLTE Spectrum Synthetic Code and an

... Sources of the quantum theory. ... Wave function and their physical interpretation. Schroedinger equation as a constraint on the physical state. Feynman's formulation of the quantum mechanics (path integration) and classical limit. Quantum mechanics postulates. States and observables, measurable physical values. ... State vector. ... Amplitude and crossection of scattering. ... M.: Nauka, 1974. ... Iroshnikov G.S. Path integral and coherent states in quantum mechanics and field theory. ...

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Pulsars (from PULSAting stARs) were discovered, albeit accidentally, by Jocelyn Bell at Cambridge in 1967. ... In addition, some pulsars are known to be members of binary systems in which the companion is another neutron star, a white dwarf and even a main sequence star. ... PSR B1913+16: . ... Although subsequent pulsar surveys with better sensitivity to short period objects have found a large number of similar objects, for 24 years PSR B1937+21 stayed as the most rapidly rotating neutron star known. ...

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• Slide 11
• Pleiades VLA Survey Area Comparisons
• Arp220

Gamma-rays from the GC . M.Chernyakova (DIAS), D.Malyshev (DIAS), F.Aharonian (DIAS, MPIK), R.M.Crocker(MPIK), D.I.Jones(MPIK) 1 10°x10° Count and TS maps (>300 GeV) Gamma-rays from the GC 2 TS maps of the GC at different energies 300 MeV ­ 3GeV 3 GeV ­ 30 GeV 30 GeV ­ 300 GeV Gamma-rays from the GC 3 4 Gamma-rays from the GC Lightcurve 5 Gamma-rays from the GC Source spectrum Model X-ray and low-energy emission come from the central object, probably SMBH accretion disk. ...

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• z90-program

UPPER PANEL: The gas surface density map in log scale. The red circle in the center represents the central protostar. The development of spiral structure in the protostellar disk is evident. Dense protostellar/protoplanetary clumsp form within the spiral arms and are driven into the protostar by the action of gravitational torques. LOWER PANEL: The mass accretion rate onto the protostar as a function of time. The mass accretion rate is characterized by very short ( . ...

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• http://ip.rsu.ru/~vorobyov/shells.pdf

... The Co­Addition Technique Applied to Images of Galaxy Cores W. W. Zeilinger Institut f˜ur Astronomie, University of Vienna, T˜urkenschanzstraúe 17, A­1180 Wien, Austria P. Crane, P. GrosbÜl and A. Renzini European Southern Observatory, Karl­Schwarzschild Straúe 2, D­85748 Garching, Germany Abstract. ... One may therefore take full advantage of the high resolution FOC images by co­adding them with (high signal­to­noise) ground­ based data. ... References Crane, P. et al. ...

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• ESLAB 2007
• NICMOS Science
• HST NICMOS Observations of Circumstellar Matter Around CYG X-3

... Ïîäïèñêà íà ðàññûëêó îáçîðîâ astro-ph íà Subscribe.Ru . ... Îáçîðû ÓÔÍ . ... Ðåçóëüòàòû WMAP . Èçó÷åíèå öåíòðà íàøåé Ãàëàêòèêè . ... Ðàçðûâ Âñåëåííîé" . ... çâåçäû , . ... Êîðîòêîå ýññå îá ýëåêòðîííûõ ïðåïðèíòàõ . ... Ñàìûå èíòåðåñíûå ïðåïðèíòû astro-ph ÿíâàðÿ 2003 ãîäà ïî ìàòåðèàëàì îáçîðîâ Àðõèâà íà ñàéòå Scientiic.Ru " . ... Authors: A. M. Ghez et al. astro-ph/0306220 Ãåîìåòðè÷åñêîå îïðåäåëåíèå ðàññòîÿíèÿ äî öåíòðà Ãàëàêòèêè (A Geometric Determination of the Distance to the Galactic Center) . ...

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• Íîâîñòè íàóêè
• Scientific.ru Îáùèé ôîðóì

... S. G. Pugacheva. Sternberg State Astronomical Institute, Moscow, 119899, Russia, pugach@sai.msu.ru . ... Sternberg State Astronomical Institute, Moscow University, Russia, pugach@sai.msu.ru . ... Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., ... Sternberg State Astronomical Institute, Lomonosov Moscow State University, Universitetskii pr. ... S. G. Pugacheva and V. V. Shevchenko, Sternberg State Astronomical Institute, Moscow University, 13 Universitetsky pr., ...

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... Dept. for Physics of Stars&Galaxies . ... Astronomical Calendar . ... History of MAO . ... Á€“ 2013. ... Zakhozhay O. and Vorobyov E.I. The signatures of disk fragmentation in spectral energy distributions // Proceedings of the conference Hot Planets and Cool Stars, Garching, November 12-16, 2012. ... Zakhozhay O.V., Vorobyov E.I. Spectral energy distributions of fragmenting protostellar disks // Formation, detection, and characterization of extrasolar habitable planets Proceedings IAU Symposium No....

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• Olga V. Zakhozhay

... We consider the astrophysical evolution of the Galaxy over large time scales, from early stages (an age of ~10 8 yrs) to the end of traditional stellar evolution (~10 11 yrs). ... In the model considered, the basic stages of Galactic evolution are as follows. ... Essentially all other basic parameters of the Galaxy vary little. ... The final "stellar epoch" in the life of the Galaxy is completed ~10 13 yrs after its formation, when the evolution of the least massive stars comes to an end. ...

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... The circumnuclear GASEOUS disks are often decoupled from the circumnuclear stellar disks and are even stronger inclined to the outer disk planes; in fact, we have found a considerable `population' of inner polar rings. Inner gas polar rings are found as in spiral galaxies with the massive outer gas disks co-planar to the main symmetry planes (e.g. NGC 2841, Sil'chenko et al. 1997, and NGC 7217, Sil'chenko & Afanasiev 2000) as well in many lenticular galaxies (Fig. ...

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• http://sn.sai.msu.ru/~sil/preprints/postbr2.pdf
• Olga Silchenko

... MASTER Net is 56 square degrees per 1 exposition . ... 06 Dec 2015: GRB 151205B: MASTER-NET early optical observations GCN18665 . ... 18 Nov 2015: GRB 151118A: MASTER-NET optical observations GCN18613 . ... 12 Nov 2015: GRB 151112A: MASTER-NET optical limit GCN18591 . ... 07 Nov 2015: GRB 151107A: MASTER-NET optical observations GCN18565 . ... 31 Oct 2015: Five OTs detected by Global Robotic MASTER Net ATel8232 . ... 02 Oct 2015: GRB 151001B: MASTER-NET early optical observations GCN18380 . ...

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• Îáñåðâàòîðèÿ