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  • 1
    Monograph available for loan
    Monograph available for loan
    Planetary magnetism (2010)
    New York, NY [u.a.] : Springer
    Associated volumes
    Details Availability
    Call number: 5/M 18.91371
    In: Space science series of ISSI
    Type of Medium: Monograph available for loan
    Pages: 664 Seiten , Ill., graph. Darst., Kt. , 235 mm x 155 mm
    ISBN: 9781441959003
    Series Statement: Space Sciences Series of ISSI 33
    URL: Inhaltsverzeichnis
    Classification:
    Geomagnetism, Geoelectromagnetism
    Language: English
    Note: Planetary magnetism : foreword / A. Balogh ... [et al.] -- Space exploration of planetary magnetism / N.F. Ness -- Planetary magnetic field measurements : missions and instrumentation / A. Balogh -- Current systems in planetary magnetospheres and ionospheres / W. Baumjohann ... [et al.] -- Separation of the magnetic field into external and internal parts / N. Olsen, K.-H. Glassmeir, X. Jia -- The magnetic field of planet Earth / G. Hulot ... [et al.] -- Crustal magnetic fields of terrestrial planets / B. Langlais ... [et al.] -- Magnetic fields of the outer planets / C.T. Russell, M.K. Dougherty -- Magnetic fields of the satellites of Jupiter and Saturn / X. Jia ... [et al.] -- The magnetic field of mercury / B.J. Anderson ... [et al.] -- Paleomagnetic records of meteorites and early planetesimal differentiation / B.P. Weiss ... [et al.] -- Induced magnetic fields in solar system bodies / J. Saur, f.M. Neubauer, K.-H. Glassmeier -- The interior structure, composition, and evolution of giant planets / J.J. Fortney, N. Nettelmann -- Thermal evolution and magnetic field generation in terrestrial planets and satellites / D. Breuer, S. Labrosse, T. Spohn -- Theory and modeling of planetary dynamos / J. Wicht, A. Tilgner -- Laboratory dynamo experiments / G. Verhille ... [et al.] -- Dynamo scaling laws and applications to the planets / U.R. Christensen -- The solar dynamo / C.A. Jones, M.J. Thompson, S.M. Tobias -- Dynamo models for planets other than Earth / S. Stanley, G.A. Glatzmaier -- Planetary magnetic fields : achievements and prospects / D.J. Stevenson..
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  • 2
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    Cluster observations of surface waves in the ion jets from magnetotail reconnection (2011)
    Wiley
    Details
    Publication Date: 2011-12-28
    Description: We present a Cluster spacecraft investigation of plasma sheet-confined waves and the associated Poynting flux in strong ion jets near a reconnection region in the geomagnetic tail at ∼−17 Re. Using phase lag analysis, we determine from multispacecraft measurements the phase front, wavelength, and phase velocity of the waves with spacecraft frame frequencies from 0.03 Hz to 1 Hz. The wave phase velocities were found to be directed nearly perpendicular to the local magnetic field laying in the plasma sheet plane. The strong evidence that the waves were driven by ion velocity shears has been provided. The waves are confined by the plasma sheet and their amplitude diminishes in the tail lobes. The δE/δB ratios are mostly on the order of the Alfven speed. The observed wave characteristics are different from plasma sheet flapping observed at the same time. The field-aligned Poynting flux was found to be directed away from the reconnection region. The values of earthward Poynting flux (100 ergs/cm2s or 0.1 W/m2) and longitudinal scales (10–100 km) mapped to the auroral ionosphere suggest that the observed waves may provide energy needed to accelerate auroral particles and may drive observed motions in auroral curls.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
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    A study of the changes of the near-Earth plasma sheet and lobe driven by multiple substorms: Comparison with a full particle simulation of reconnection (2012)
    Wiley
    Details
    Publication Date: 2012-01-31
    Description: Comparisons of multispacecraft observations and full-particle simulations are used to understand magnetotail changes during substorms and the related cross-tail current disruptions/reductions. We first show that the electric field accompanying current disruptions can be measured in the tail lobe from the drift velocity of oxygen beams. A stormy period is studied here with a fleet of spacecraft including the four Cluster spacecraft and the Double Star spacecraft TC-1 in the tail, ACE and Geotail respectively in the solar wind and magnetosheath, and five LANL geostationary satellites, thus allowing the determination of the direction of propagation of the substorm disturbances. Each substorm here corresponds to an energy-loading period followed by a dipolarization of the magnetic field seen from 11 to 18 RE. Plasma sheet thinning inside 12 RE occurs during energy loading and is enhanced at the onset of strong dissipations of magnetic energy, which precede by several minutes particle injections at 6.6 RE. Dipolarizations coincide with an increase of the lobe electric field, up to several mV/m. This study shows that the onset of the magnetic energy conversion occurs at about ∼10–11 RE and that once initiated, the perturbation propagates both toward the Earth and toward the distant tail. Comparisons of the measurements with recently published 2D full particle simulations of the reconnection process by Oka et al. (2008) indicate a good agreement between data and simulated magnetic lobe signatures. This suggests that the lobe magnetic changes are the signature of a tailward retreating neutral line, with its associated current disruption/reduction.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 4
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    Star formation and environmental quenching of GEEC2 group galaxies at z ~ 1 (2014)
    Oxford University Press
    Details
    Publication Date: 2014-02-20
    Description: We present new analysis from the Group Environment Evolution Collaboration 2 (GEEC2) spectroscopic survey of galaxy groups at 0.8 〈  z  〈 1. Our previous work revealed an intermediate population between the star-forming and quiescent sequences and a strong environmental dependence in the fraction of quiescent galaxies. Only ~5 per cent of star-forming galaxies in both the group and field sample show a significant enhancement in star formation, which suggests that quenching is the primary process in the transition from the star-forming to the quiescent state. To model the environmental quenching scenario, we have tested the use of different exponential quenching time-scales and delays between satellite accretion and the onset of quenching. We find that with no delay, the quenching time-scale needs to be long in order to match the observed quiescent fraction, but then this model produces too many intermediate galaxies. Fixing a delay time of 3 Gyr, as suggested from the local Universe, produces too few quiescent galaxies. The observed fractions are best matched with a model that includes a delay that is proportional to the dynamical time and a rapid quenching time-scale (~0.25 Gyr), but this model also predicts intermediate galaxies H strength higher than that observed. Using stellar synthesis models, we have tested other scenarios, such as the rejuvenation of star formation in early-type galaxies and a portion of quenched galaxies possessing residual star formation. If environment quenching plays a role in the GEEC2 sample, then our work suggests that only a fraction of intermediate galaxies may be undergoing this transition and that quenching occurs quite rapidly in satellite galaxies (0.25 Gyr).
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 5
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    The sun and heliosphere at solar maximum (2003)
    American Association for the Advancement of Science (AAAS)
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    Publication Date: 2003-11-15
    Description: Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitude sources reach all latitudes, including the polar caps. The very fast high-latitude wind and polar coronal holes disappear and reappear together. Solar wind speed continues to be inversely correlated with coronal temperature. The cosmic ray flux is reduced symmetrically at all latitudes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, E J -- Marsden, R G -- Balogh, A -- Gloeckler, G -- Geiss, J -- McComas, D J -- McKibben, R B -- MacDowall, R J -- Lanzerotti, L J -- Krupp, N -- Krueger, H -- Landgraf, M -- New York, N.Y. -- Science. 2003 Nov 14;302(5648):1165-9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/14615526" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    Energetic Charged-Particle Phenomena in the Jovian Magnetosphere: First Results from the Ulysses COSPIN Collaboration (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-09-11
    Description: The Ulysses spacecraft made the first exploration of the region of Jupiter's magnetosphere at high Jovigraphic latitudes ( approximately 37 degrees south) on the dusk side and reached higher magnetic latitudes ( approximately 49 degrees north) on the day side than any previous mission to Jupiter. The cosmic and solar particle investigations (COSPIN) instrumentation achieved a remarkably well integrated set of observations of energetic charged particles in the energy ranges of approximately 1 to 170 megaelectron volts for electrons and 0.3 to 20 megaelectron volts for protons and heavier nuclei. The new findings include (i) an apparent polar cap region in the northern hemisphere in which energetic charged particles following Jovian magnetic field lines may have direct access to the interplanetary medium, (ii) high-energy electron bursts (rise times 〈/= 1 minute and energies extending to 〉 approximately 17 megaelectron volts) on the dusk side that are apparently associated with field-aligned currents and radio burst emissions, (iii) persistence of the global 10-hour relativistic electron "clock" phenomenon throughout Jupiter's magnetosphere, (iv) on the basis of charged-particle measurements, apparent dragging of magnetic field lines at large radii in the dusk sector toward the tail, and (v) consistent outflow of megaelectron volt electrons and large-scale departures from corotation for nucleons.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Simpson, J A -- Anglin, J D -- Balogh, A -- Burrows, J R -- Cowley, S W -- Ferrando, P -- Heber, B -- Hynds, R J -- Kunow, H -- Marsden, R G -- McKibben, R B -- Muller-Mellin, R -- Page, D E -- Raviart, A -- Sanderson, T R -- Staines, K -- Wenzel, K P -- Wilson, M D -- Zhang, M -- New York, N.Y. -- Science. 1992 Sep 11;257(5076):1543-50.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17776166" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 7
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    Cassini magnetometer observations during Saturn orbit insertion (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-02-26
    Description: Cassini's successful orbit insertion has provided the first examination of Saturn's magnetosphere in 23 years, revealing a dynamic plasma and magnetic environment on short and long time scales. There has been no noticeable change in the internal magnetic field, either in its strength or its near-alignment with the rotation axis. However, the external magnetic field is different compared with past spacecraft observations. The current sheet within the magnetosphere is thinner and more extended, and we observed small diamagnetic cavities and ion cyclotron waves of types that were not reported before.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Dougherty, M K -- Achilleos, N -- Andre, N -- Arridge, C S -- Balogh, A -- Bertucci, C -- Burton, M E -- Cowley, S W H -- Erdos, G -- Giampieri, G -- Glassmeier, K-H -- Khurana, K K -- Leisner, J -- Neubauer, F M -- Russell, C T -- Smith, E J -- Southwood, D J -- Tsurutani, B T -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1266-70.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Blackett Laboratory, Imperial College London, SW7 2AZ, UK. m.dougherty@imperial.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731444" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    The heliospheric magnetic field over the South polar region of the sun (1995)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1995-05-19
    Description: Magnetic field measurements from the Ulysses space mission overthe south polar regions of the sun showed that the structure and properties of the three-dimensional heliosphere were determined by the fast solar wind flow and magnetic fields from the large coronal holes in the polar regions of the sun. This conclusion applies at the current, minimum phase of the 11-year solar activity cycle. Unexpectedly, the radial component of the magnetic field was independent of latitude. The high-latitude magnetic field deviated significantly from the expected Parker geometry, probably because of large amplitude transverse fluctuations. Low-frequency fluctuations had a high level of variance. The rate of occurrence of discontinuities also increased significantly at high latitudes.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Balogh, A -- Southwood, D J -- Forsyth, R J -- Horbury, T S -- Smith, E J -- Tsurutani, B T -- New York, N.Y. -- Science. 1995 May 19;268(5213):1007-10.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17774226" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 9
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    Magnetic field observations during the ulysses flyby of jupiter (1992)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1992-09-11
    Description: The Jovian flyby of the Ulysses spacecraft presented the opportunity to confirm and complement the findings of the four previous missions that investigated the structure and dynamics of the Jovian magnetosphere and magnetic field, as well as to explore for the first time the high-latitude dusk side of the magnetosphere and its boundary regions. In addition to confirming the general structure of the dayside magnetosphere, the Ulysses magnetic field measurements also showed that the importance of the current sheet dynamics extends well into the middle and outer magnetosphere. On the dusk side, the magnetic field is swept back significantly toward the magnetotail. The importance of current systems, both azimuthal and field-aligned, in determining the configuration of the field has been strongly highlighted by the Ulysses data. No significant changes have been found in the internal planetary field; however, the need to modify the external current densities with respect to previous observations on the inbound pass shows that Jovian magnetic and magnetospheric models are highly sensitive to both the intensity and the structure assumed for the current sheet and to any time dependence that may be assigned to these. The observations show that all boundaries and boundary layers in the magnetosphere have a very complex microstructure. Waves and wave-like structures were observed throughout the magnetosphere; these included the longest lasting mirror-mode wave trains observed in space.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Balogh, A -- Dougherty, M K -- Forsyth, R J -- Southwood, D J -- Smith, E J -- Tsurutani, B T -- Murphy, N -- Burton, M E -- New York, N.Y. -- Science. 1992 Sep 11;257(5076):1515-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17776160" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
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    Efficient satellite quenching at z~1 from the GEEC2 spectroscopic survey of galaxy groups (2013)
    Oxford University Press
    Details
    Publication Date: 2013-04-13
    Description: We present deep Gemini Multi-Object Spectrograph-South spectroscopy for 11 galaxy groups at 0.8 〈 z  〈 1.0, for galaxies with r AB  〈 24.75. Our sample is highly complete (〉66 per cent) for eight of the 11 groups. Using an optical–near-infrared colour–colour diagram, the galaxies in the sample were separated with a dust insensitive method into three categories: passive (red), star-forming (blue) and intermediate (green). The strongest environmental dependence is observed in the fraction of passive galaxies, which make up only ~20 per cent of the field in the mass range 10 10.3  〈 M star /M  〈 10 11.0 , but are the dominant component of groups. If we assume that the properties of the field are similar to those of the ‘pre-accreted’ population, the environment quenching efficiency ( ) is defined as the fraction of field galaxies required to be quenched in order to match the observed red fraction inside groups. The efficiency obtained is ~0.4, similar to its value in intermediate-density environments locally. While green (intermediate) galaxies represent ~20 per cent of the star-forming population in both the group and field, at all stellar masses, the average specific star formation rate of the group population is lower by a factor of ~3. The green population does not show strong H absorption that is characteristic of starburst galaxies. Finally, the high fraction of passive galaxies in groups, when combined with satellite accretion models, require that most accreted galaxies have been affected by their environment. Thus, any delay between accretion and the onset of truncation of star formation () must be 2 Gyr, shorter than the 3–7 Gyr required to fit data at z  = 0. The relatively small fraction of intermediate galaxies require that the actual quenching process occurs quickly, with an exponential decay time-scale of q 1 Gyr.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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