archive-de.com » DE » G » GEO-LEO.DE

Total: 1104

Choose link from "Titles, links and description words view":

Or switch to "Titles and links view".
  • URL List
    leo de handle 11858 00 1735 0000 0001 BCE4 A http e docs geo leo de handle 11858 00 1735 0000 0001 B91B E http e docs geo leo de handle 11858 00 1735 0000 0001 B878 2 http e docs geo leo de handle 11858 00 1735 0000 0001 34A3 7 http e docs geo leo de handle 11858 00 1735 0000 0001 B98F 8 http e docs geo leo de handle 11858 00 1735 0000 0001 3495 9 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB6 3 http e docs geo leo de handle 11858 00 1735 0000 0001 3489 5 http e docs geo leo de handle 11858 00 1735 0000 0001 3481 6 http e docs geo leo de handle 11858 00 1735 0000 0006 9FAB C http e docs geo leo de handle 11858 00 1735 0000 0022 C200 8 http e docs geo leo de handle 11858 00 1735 0000 0001 345B D http e docs geo leo de handle 11858 00 1735 0000 0009 1FDB 0 http e docs geo leo de handle 11858 00 1735 0000 0006 5D6C 7 http e docs geo leo de handle 11858 00 1735 0000 0006 0D9F 1 http e docs geo leo de handle 11858 00 1735 0000 0006 9FBB A http e docs geo leo de handle 11858 00 1735 0000 0006 0DA1 A http e docs geo leo de handle 11858 00 1735 0000 0006 9FBA C http e docs geo leo de handle 11858 00 1735 0000 0001 345D 9 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB9 E http e docs geo leo de handle 11858 00 1735 0000 0006 0DA3 6 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB7 1 http e docs geo leo de handle 11858 00 1735 0000 0006 0DA0 C http e docs geo leo de handle 11858 00 1735 0000 0006 0DA2 8 http e docs geo leo de handle 11858 00 1735 0000 0006 0DA4 4 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB8 0 http e docs geo leo de handle 11858 00 1735 0000 0001 B9FE 0 http e docs geo leo de handle 11858 00 1735 0000 0006 0DA5 2 http e docs geo leo de handle 11858 00 1735 0000 0001 B9F9 9 http e docs geo leo de handle 11858 00 1735 0000 000C 46D7 B http e docs geo leo de handle 11858 00 1735 0000 0006 0DA6 F http e docs geo leo de handle 11858 00 1735 0000 0006 5E1A 8 http e docs geo leo de handle 11858 00 1735 0000 0006 5E1B 6 http e docs geo leo de handle 11858 00 1735 0000 0001 BA00 9 http e docs geo leo de handle 11858 00 1735 0000 0001 B905 D http e docs geo leo de handle 11858 00 1735 0000 0007 08E9 1 http e docs geo leo de handle 11858 00 1735 0000 0001 3451 1 http e docs geo leo de handle 11858 00 1735 0000 0001 344F 9 http e docs geo leo de handle 11858 00 1735 0000 0001 3466 4 http e docs geo leo de handle 11858 00 1735 0000 0006 9FAC A http e docs geo leo de handle 11858 00 1735 0000 0001 345E 7 http e docs geo leo de handle 11858 00 1735 0000 0006 9FAD 8 http e docs geo leo de handle 11858 00 1735 0000 0006 9FAE 6 http e docs geo leo de handle 11858 00 1735 0000 0006 9FAF 4 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB0 F http e docs geo leo de handle 11858 00 1735 0000 0001 3461 E http e docs geo leo de handle 11858 00 1735 0000 0006 9FB1 D http e docs geo leo de handle 11858 00 1735 0000 0006 9FB2 B http e docs geo leo de handle 11858 00 1735 0000 0006 AB06 0 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB3 9 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB4 7 http e docs geo leo de handle 11858 00 1735 0000 0006 9FB5 5 http e docs geo leo de handle 11858 00 1735 0000 0007 426F E http e docs geo leo de handle 11858 00 1735 0000 0001 344A 4 http e docs geo leo de handle 11858 00 1735 0000 0001 3088 1 http e docs geo leo de handle 11858 00 1735 0000 0006 B916 C http e docs geo leo de handle 11858 00 1735 0000 0001 344B 2 http e docs geo leo de handle 11858 00 1735 0000 0007 3731 6 http e docs geo leo de handle 11858 00 1735 0000 0001 3340 F http e docs geo leo de handle 11858 00 1735 0000 0001 3342 B http e docs geo leo de handle 11858 00 1735 0000 0001 33BE 8 http e docs geo leo de handle 11858 00 1735 0000 000C A080 4 http e docs geo leo de handle 11858 00 1735 0000 0006 C0E9 E http e docs geo leo de handle 11858 00 1735 0000 0007 5E7F 9 http e docs geo leo de handle 11858 00 1735 0000 0007 372B 5 http e docs geo leo de handle 11858 00 1735 0000 0006 C035 2 http e docs geo leo de handle 11858 00 1735 0000 000B 02A9 B http e docs geo leo de handle 11858 00 1735 0000 0001 33F0 1 http e docs geo leo de handle 11858 00 1735 0000 000B 02A8 D http e docs geo leo de handle 11858 00 1735 0000 000B 02A4 6 http e docs geo leo de handle 11858 00 1735 0000 0001 33F1 0 http e docs geo leo de handle 11858 00 1735

    Original URL path: http://e-docs.geo-leo.de/htmlmap?map=5 (2016-02-15)
    Open archived version from archive


  • URL List
    11858 00 1735 0000 0023 B183 5 http e docs geo leo de handle 11858 00 1735 0000 0023 AD19 7 http e docs geo leo de handle 11858 00 1735 0000 0022 AB63 D http e docs geo leo de handle 11858 00 1735 0000 0024 1F16 8 http e docs geo leo de handle 11858 00 1735 0000 0022 AB64 B http e docs geo leo de handle

    Original URL path: http://e-docs.geo-leo.de/htmlmap?map=6 (2016-02-15)
    Open archived version from archive

  • Astronomie, Astrophysik, Weltraumforschung Alle Dokumente nach Erscheinungsdatum
    intergalactic medium IGM is kept at a high photoionisation level by the cosmic UV background radiation field Primarily composed of the integrated contribution of quasars and young Hydrogen deficient central stars of planetary nebulae Todt Helge Univ Potsdam 2009 Central stars of planetary nebulae are low mass stars on the brink of their final evolution towards white dwarfs Because of their surface temperature of above 25 000 K their UV radiation ionizes the surrounding material Heating of the corona in a 3D MHD forward model approach Bingert Sven Univ Freiburg Breisgau 2009 Observations of the solar corona show loop like structures formed by plasma at temperatures of one million degrees and higher Since the solar surface is much cooler than the corona a heating mechanism must be responsible Supernova driven turbulence and magnetic field amplification in disk galaxies Gressel Oliver Univ Potsdam 2009 Supernovae are known to be the dominant energy source for driving turbulence in the interstellar medium Yet their effect on magnetic field amplification in spiral galaxies is still poorly understood Analytical models The upper atmospheric fountain effect in the polar cusp region Rentz Stefanie GFZ Helmholtz Zentrum Potsdam 2009 This thesis examines how the cusp as a feature of the Earth Magnetic Field influences the neutral upper atmospheric dynamics The thermospheric total mass density as derived from CHAMP satellite data shows a distinct Wechselwirkung des Mars mit dem Sonnenwind Hybrid Simulationen mit besonderem Bezug zur Wasserbilanz Bößwetter Alexander Univ Zugl Braunschweig 2009 Seit den 60er Jahren des letzten Jahrhunderts ist Mars immer wieder das Ziel von Raumfahrtmissionen gewesen um unter anderem nach Wasser auf unserem Nachbarplaneten zu suchen Nachdem die bisher analysierten Oberflächenmerkmale Surface spots on cool giant stars probed by spectro astrometry Voigt Boris Univ Hamburg 2009 Spectro astrometry is a technique to obtain information about the structure of an astronomical source on sub diffraction limited spatial scales down to milli or micro arcseconds The method exploits the shift of the The LUCIFER control software operational and observational characteristics and NIR spectroscopy of galaxy centers Knierim Volker Univ Bochum 2009 Die Dissertation behandelt die Konzepte sowie die Implementierung der operativen Aspekte der Kontrollsoftware des LUCIFER Instruments Diese ist in vier Schichten aufgeteilt Die Schnittstelle zwischen Software und Hardware The central parsec of the milky way at 3 8 micrometer Mužić Koraljka Univ Köln 2008 The central part of the Milky Way is a unique environment where an interplay of different astrophysical phenomena can be studied starting from the physics of the interstellar medium stellar physics and star formation Search for neutrino induced cascades with 5 years of the AMANDA II data Actis Oxana Univ Berlin 2008 Das Antarctic Muon And Neutrino Detector Array AMANDA ist ein Cherenkov Detektor der sich im Gletscher der Antarktis am Südpol befindet Wir präsentieren die Analyse von Daten die in den Jahren 2000 bis 2004 gesammelt Non analytical line profiles in stellar atmospheres for planetary host star systems Johnas Christine M S Univ Hamburg 2008 In this work nonanalytical line profiles

    Original URL path: http://e-docs.geo-leo.de/handle/11858/511/browse?order=DESC&rpp=20&sort_by=1&etal=-1&offset=20&type=dateissued (2016-02-15)
    Open archived version from archive

  • Methods for the reconstruction of large scale anisotropies of the cosmic ray flux
    other properties of cosmic ray particles from detected air shower events are reconstructed The question of uniformity in the distribution of arrival directions is of large importance for models that try to explain cosmic radiation In this thesis methods for the reconstruction of parameters of a dipole like flux distribution of cosmic rays from a set of recorded air shower events are studied Different methods are presented and examined by means of detailed Monte Carlo simulations Particular focus is put on the implications of spurious experimental effects Modifications of existing methods and new methods are proposed The main goal of this thesis is the development of the horizontal Rayleigh analysis method Unlike other methods this method is based on the analysis of local viewing directions instead of global sidereal directions As a result the symmetries of the experimental setup can be better utilised The calculation of the sky coverage exposure function is not necessary in this analysis The performance of the method is tested by means of further Monte Carlo simulations The new method performs similarly good or only marginally worse than established methods in case of ideal measurement conditions However the simulation of certain experimental effects can cause substantial

    Original URL path: http://e-docs.geo-leo.de/handle/11858/00-1735-0000-0001-308A-E (2016-02-15)
    Open archived version from archive

  • Properties of quasistellar objects and their progenitors in the radio and mm wavelength regimes in the context of ULIRG-to-QSO evolution
    View Download Kategorien Radioastronomie Sonstige Sternensysteme Astronomie Zur Langanzeige Zusammenfassung The thesis at hand presents the results of a study of galaxies with active galactic nuclei AGN carried out in the radio and mm wavelength regimes at low and high angular resolutions The studied objects cover a broad range of mechanisms responsible for powering the engines of the respective galaxies ULIRGs UltraLuminous Infrared Galaxies a product of mergers between galaxies that are supposedly powered by starbursts AGN or a mixture of the two and QSOs quasi stellar objects which are powered by AGN Since ULIRGs and QSOs show similar properties especially the infrared luminosities it was proposed that they form the early and late phase of an evolutionary sequence where supposedly ULIRGs are the dust enshrouded progenitors of QSOs As a prototypical ULIRG Arp 220 represents an early to intermediate phase object in the scheme of the ULIRG to QSO evolution For this object observations at multiple mm wavelengths and angular resolutions with the IRAM Plateau de Bure Interferometer PdBI are presented and analyzed Arp 220 as a whole is studied in CO emission of the more extended structure Furthermore Arp 220 East is analyzed in more detail in the

    Original URL path: http://e-docs.geo-leo.de/handle/11858/00-1735-0000-0001-3089-0 (2016-02-15)
    Open archived version from archive

  • Masses of small bodies
    11858 00 1735 0000 0001 3088 1 Dateiname Andert2010 pdf PDF 6 0 MB Google View Download Kategorien Radioastronomie Interplanetare Materie Astronomie Zur Langanzeige Zusammenfassung The Radio Science technique enables to estimate the mass and other gravitational parameters of a solar system body from spacecraft observations very precisely It uses the radio link between ground station and spacecraft The frequency shift of the radio signal is proportional to the relative velocity change between spacecraft and ground station If a spacecraft performs a close flyby at a solar system body the velocity of the spacecraft is changed by the gravitational attraction of the body If all other contributions on the radio signal are known the remaining frequency change is solely due to the gravitational attraction A least square fit can be performed on the frequency residuals to derive from it gravitational parameters Within this thesis models were developed and merged into a software package with which it is possible to determine the orbit of a spacecraft precisely and to predict accurately the frequency to be observed at a ground station Models for extracting the frequency shift caused by the propagation of the radio signal through the ionosphere and troposphere of the

    Original URL path: http://e-docs.geo-leo.de/handle/11858/00-1735-0000-0001-3088-1 (2016-02-15)
    Open archived version from archive

  • Radiative transfer in the exosphere of Saturn's moon Titan
    hydrogen in the exosphere of Saturns moon Titan This work is based on measurements performed by the Hydrogen Deuterium Absorption Cell HDAC aboard the Cassini spacecraft that should directly determine the D H ratio from the UV emission of atomic hydrogen and deuterium at 121 567 and 121 533 nm respectively HDAC measurements were performed on December 26 2005 during the ninth Titan flyby of the Cassini orbiter Unfortunately the amount of deuterium in the absorption cell could not be determined Thus the purpose HDAC was designed for could not be achieved For this reason HDAC has performed measurements only once However the amount of atomic hydrogen in the absorption cell is well known hence the data using only the hydrogen cell can be used in order to investigate Titans exosphere This work aims at simulating the HDAC measurements performed in order to investigate Titan rsquo s exosphere e g to determine the distribution of atomic hydrogen A model of Titan rsquo s exosphere including atomic hydrogen and methane has been developed and the transfer of solar radiation is calculated in order to simulate the HDAC measurements The radiative transfer is solved using the Monte Carlo method For the exospheric

    Original URL path: http://e-docs.geo-leo.de/handle/11858/00-1735-0000-0001-3096-3 (2016-02-15)
    Open archived version from archive

  • Heating of the corona in a 3D MHD forward model approach
    Sonne Zur Langanzeige Zusammenfassung Observations of the solar corona show loop like structures formed by plasma at temperatures of one million degrees and higher Since the solar surface is much cooler than the corona a heating mechanism must be responsible for the high temperatures The dissipation of magnetic fields in the corona could provide such a heating mechanism However the process of transforming magnetic energy into thermal energy is still not yet understood in detail To investigate this process and its impact on the heating of the corona we employ a three dimensional magneto hydrodynamical model This numerical model synthesizes the temporal evolution of the magnetic field above an Active Region It includes the solar atmosphere from the photosphere up to the corona The magnetic field in the corona is braided by foot point motions in the photosphere This is done imilarly to the braiding through granulation in reality The stressed agnetic field induces currents which are then dissipated in the corona This dea is known as the DC model direct current and was proposed by Parker in 1972 The model reaches a quasi stationary state i e the energy input by hotospheric motions is counterbalanced by radiative losses in

    Original URL path: http://e-docs.geo-leo.de/handle/11858/00-1735-0000-0001-3094-7 (2016-02-15)
    Open archived version from archive



  •