ALBERT

All Library Books, journals and Electronic Records Telegrafenberg

X
feed icon rss

Your email was sent successfully. Check your inbox.

An error occurred while sending the email. Please try again.

Proceed reservation?

Export
  • 1
    facet.materialart.
    Unknown
    Pitch angle distributions of energetic electrons at Saturn (2011)
    Wiley
    Details
    Publication Date: 2011-01-29
    Description: Pitch angle distributions of energetic electrons (110–365 keV) at Saturn are statistically analyzed for 2005–2009. Using a nondipolar model magnetic field, pitch angle distributions are mapped to the magnetospheric equator and sorted by equatorial crossing distance. The results are quantified using a standard function for the pitch angle distribution, f(α) = AsinKα (where α is the pitch angle and K is the power). Inside of ∼10 RS, the distributions are mostly peaked at 90° (K 〈 0), signifying a trapping distribution. Outside of this distance, the distributions are mostly field aligned (K 〉 0) with maxima near 0° and 180°. The 10 RS boundary maps to Saturn's ionosphere at latitudes equatorward of the aurora. Very few “flat” distributions are observed (K ≈ 0). The pitch angle distributions are not as well organized in local time as they are in radial distance, but over the 5 year survey between 10 and 20 RS field-aligned distributions appear most often near midnight, while trapping distributions are found elsewhere.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 2
    facet.materialart.
    Unknown
    Mediation of the solar wind termination shock by non-thermal ions (2008)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2008-07-04
    Description: Broad regions on both sides of the solar wind termination shock are populated by high intensities of non-thermal ions and electrons. The pre-shock particles in the solar wind have been measured by the spacecraft Voyager 1 (refs 1-5) and Voyager 2 (refs 3, 6). The post-shock particles in the heliosheath have also been measured by Voyager 1 (refs 3-5). It was not clear, however, what effect these particles might have on the physics of the shock transition until Voyager 2 crossed the shock on 31 August-1 September 2007 (refs 7-9). Unlike Voyager 1, Voyager 2 is making plasma measurements. Data from the plasma and magnetic field instruments on Voyager 2 indicate that non-thermal ion distributions probably have key roles in mediating dynamical processes at the termination shock and in the heliosheath. Here we report that intensities of low-energy ions measured by Voyager 2 produce non-thermal partial ion pressures in the heliosheath that are comparable to (or exceed) both the thermal plasma pressures and the scalar magnetic field pressures. We conclude that these ions are the 〉0.028 MeV portion of the non-thermal ion distribution that determines the termination shock structure and the acceleration of which extracts a large fraction of bulk-flow kinetic energy from the incident solar wind.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Decker, R B -- Krimigis, S M -- Roelof, E C -- Hill, M E -- Armstrong, T P -- Gloeckler, G -- Hamilton, D C -- Lanzerotti, L J -- England -- Nature. 2008 Jul 3;454(7200):67-70. doi: 10.1038/nature07030.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland 20723, USA. robert.decker@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18596801" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 3
    facet.materialart.
    Unknown
    Energetic particles at venus: galileo results (1991)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1991-09-27
    Description: At Venus the Energetic Particles Detector (EPD) on the Galileo spacecraft measured the differential energy spectra and angular distributions of ions 〉22 kiloelectron volts (keV) and electrons 〉 15 keV in energy. The only time particles were observed by EPD was in a series of episodic events [0546 to 0638 universal time (UT)] near closest approach (0559:03 UT). Angular distributions were highly anisotropic, ordered by the magnetic field, and showed ions arriving from the hemisphere containing Venus and its bow shock. The spectra showed a power law form with intensities observed into the 120- to 280-keV range. Comparisons with model bow shock calculations show that these energetic ions are associated with the venusian foreshock-bow shock region. Shock-drift acceleration in the venusian bow shock seems the most likely process responsible for the observed ions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Williams, D J -- McEntire, R W -- Krimigis, S M -- Roelof, E C -- Jaskulek, S -- Tossman, B -- Wilken, B -- Studemann, W -- Armstrong, T P -- Fritz, T A -- Lanzerotti, L J -- Roederer, J G -- New York, N.Y. -- Science. 1991 Sep 27;253(5027):1525-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17784094" 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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 4
    facet.materialart.
    Unknown
    Energetic particles in the jovian magnetotail (2007)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2007-10-13
    Description: When the solar wind hits Jupiter's magnetic field, it creates a long magnetotail trailing behind the planet that channels material out of the Jupiter system. The New Horizons spacecraft traversed the length of the jovian magnetotail to 〉2500 jovian radii (RJ; 1 RJ identical with 71,400 kilometers), observing a high-temperature, multispecies population of energetic particles. Velocity dispersions, anisotropies, and compositional variation seen in the deep-tail (greater, similar 500 RJ) with a approximately 3-day periodicity are similar to variations seen closer to Jupiter in Galileo data. The signatures suggest plasma streaming away from the planet and injection sites in the near-tail region (approximately 200 to 400 RJ) that could be related to magnetic reconnection events. The tail structure remains coherent at least until it reaches the magnetosheath at 1655 RJ.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McNutt, R L Jr -- Haggerty, D K -- Hill, M E -- Krimigis, S M -- Livi, S -- Ho, G C -- Gurnee, R S -- Mauk, B H -- Mitchell, D G -- Roelof, E C -- McComas, D J -- Bagenal, F -- Elliott, H A -- Brown, L E -- Kusterer, M -- Vandegriff, J -- Stern, S A -- Weaver, H A -- Spencer, J R -- Moore, J M -- New York, N.Y. -- Science. 2007 Oct 12;318(5848):220-2.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. ralph.mcnutt@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17932283" target="_blank"〉PubMed〈/a〉
    Keywords: Electrons ; Extraterrestrial Environment ; Ions ; *Jupiter ; Oxygen ; Protons ; Spacecraft ; Sulfur ; Temperature
    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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 5
    facet.materialart.
    Unknown
    Structures and spectral variations of the outer heliosphere in IBEX energetic neutral atom maps (2009)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2009-10-17
    Description: The Interstellar Boundary Explorer (IBEX) has obtained all-sky images of energetic neutral atoms emitted from the heliosheath, located between the solar wind termination shock and the local interstellar medium (LISM). These flux maps reveal distinct nonthermal (0.2 to 6 kilo-electron volts) heliosheath proton populations with spectral signatures ordered predominantly by ecliptic latitude. The maps show a globally distributed population of termination-shock-heated protons and a superimposed ribbonlike feature that forms a circular arc in the sky centered on ecliptic coordinate (longitude lambda, latitude beta) = (221 degrees, 39 degrees), probably near the direction of the LISM magnetic field. Over the IBEX energy range, the ribbon's nonthermal ion pressure multiplied by its radial thickness is in the range of 70 to 100 picodynes per square centimeter AU (AU, astronomical unit), which is significantly larger than the 30 to 60 picodynes per square centimeter AU of the globally distributed population.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Funsten, H O -- Allegrini, F -- Crew, G B -- DeMajistre, R -- Frisch, P C -- Fuselier, S A -- Gruntman, M -- Janzen, P -- McComas, D J -- Mobius, E -- Randol, B -- Reisenfeld, D B -- Roelof, E C -- Schwadron, N A -- New York, N.Y. -- Science. 2009 Nov 13;326(5955):964-6. doi: 10.1126/science.1180927. Epub 2009 Oct 15.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Los Alamos National Laboratory, Los Alamos, NM 87545, USA. hfunsten@lanl.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19833918" 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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 6
    facet.materialart.
    Unknown
    Energetic neutral atom emissions from Titan interaction with Saturn's magnetosphere (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-05-14
    Description: The Cassini Magnetospheric Imaging Instrument (MIMI) observed the interaction of Saturn's largest moon, Titan, with Saturn's magnetosphere during two close flybys of Titan on 26 October and 13 December 2004. The MIMI Ion and Neutral Camera (INCA) continuously imaged the energetic neutral atoms (ENAs) generated by charge exchange reactions between the energetic, singly ionized trapped magnetospheric ions and the outer atmosphere, or exosphere, of Titan. The images reveal a halo of variable ENA emission about Titan's nearly collisionless outer atmosphere that fades at larger distances as the exospheric density decays exponentially. The altitude of the emissions varies, and they are not symmetrical about the moon, reflecting the complexity of the interactions between Titan's upper atmosphere and Saturn's space environment.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mitchell, D G -- Brandt, P C -- Roelof, E C -- Dandouras, J -- Krimigis, S M -- Mauk, B H -- New York, N.Y. -- Science. 2005 May 13;308(5724):989-92.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 21042, USA. don.mitchell@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15890874" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; Ions ; Magnetics ; *Saturn ; Spacecraft
    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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 7
    facet.materialart.
    Unknown
    Dynamics of Saturn's magnetosphere from MIMI during Cassini's orbital insertion (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-02-26
    Description: The Magnetospheric Imaging Instrument (MIMI) onboard the Cassini spacecraft observed the saturnian magnetosphere from January 2004 until Saturn orbit insertion (SOI) on 1 July 2004. The MIMI sensors observed frequent energetic particle activity in interplanetary space for several months before SOI. When the imaging sensor was switched to its energetic neutral atom (ENA) operating mode on 20 February 2004, at approximately 10(3) times Saturn's radius RS (0.43 astronomical units), a weak but persistent signal was observed from the magnetosphere. About 10 days before SOI, the magnetosphere exhibited a day-night asymmetry that varied with an approximately 11-hour periodicity. Once Cassini entered the magnetosphere, in situ measurements showed high concentrations of H+, H2+, O+, OH+, and H2O+ and low concentrations of N+. The radial dependence of ion intensity profiles implies neutral gas densities sufficient to produce high loss rates of trapped ions from the middle and inner magnetosphere. ENA imaging has revealed a radiation belt that resides inward of the D ring and is probably the result of double charge exchange between the main radiation belt and the upper layers of Saturn's exosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krimigis, S M -- Mitchell, D G -- Hamilton, D C -- Krupp, N -- Livi, S -- Roelof, E C -- Dandouras, J -- Armstrong, T P -- Mauk, B H -- Paranicas, C -- Brandt, P C -- Bolton, S -- Cheng, A F -- Choo, T -- Gloeckler, G -- Hayes, J -- Hsieh, K C -- Ip, W-H -- Jaskulek, S -- Keath, E P -- Kirsch, E -- Kusterer, M -- Lagg, A -- Lanzerotti, L J -- Lavallee, D -- Manweiler, J -- McEntire, R W -- Rasmuss, W -- Saur, J -- Turner, F S -- Williams, D J -- Woch, J -- New York, N.Y. -- Science. 2005 Feb 25;307(5713):1270-3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. tom.krimigis@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15731445" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; *Gases ; Hydrogen ; *Ions ; *Magnetics ; Nitrogen ; Oxygen ; *Saturn ; Spacecraft ; Spectrum Analysis ; *Water
    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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 8
    facet.materialart.
    Unknown
    Voyager 1 in the foreshock, termination shock, and heliosheath (2005)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2005-09-24
    Description: Voyager 1 (V1) began measuring precursor energetic ions and electrons from the heliospheric termination shock (TS) in July 2002. During the ensuing 2.5 years, average particle intensities rose as V1 penetrated deeper into the energetic particle foreshock of the TS. Throughout 2004, V1 observed even larger, fluctuating intensities of ions from 40 kiloelectron volts (keV) to 〉/=50 megaelectron volts per nucleon and of electrons from 〉26 keV to 〉/=350 keV. On day 350 of 2004 (2004/350), V1 observed an intensity spike of ions and electrons that was followed by a sustained factor of 10 increase at the lowest energies and lesser increases at higher energies, larger than any intensities since V1 was at 15 astronomical units in 1982. The estimated solar wind radial flow speed was positive (outward) at approximately +100 kilometers per second (km s(-1)) from 2004/352 until 2005/018, when the radial flows became predominantly negative (sunward) and fluctuated between approximately -50 and 0 km s(-1) until about 2005/110; they then became more positive, with recent values (2005/179) of approximately +50 km s(-1). The energetic proton spectrum averaged over the postshock period is apparently dominated by strongly heated interstellar pickup ions. We interpret these observations as evidence that V1 was crossed by the TS on 2004/351 (during a tracking gap) at 94.0 astronomical units, evidently as the shock was moving radially inward in response to decreasing solar wind ram pressure, and that V1 has remained in the heliosheath until at least mid-2005.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Decker, R B -- Krimigis, S M -- Roelof, E C -- Hill, M E -- Armstrong, T P -- Gloeckler, G -- Hamilton, D C -- Lanzerotti, L J -- New York, N.Y. -- Science. 2005 Sep 23;309(5743):2020-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA. robert.decker@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16179469" 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)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 9
    facet.materialart.
    Unknown
    No meridional plasma flow in the heliosheath transition region (2012)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2012-09-08
    Description: Over a two-year period, Voyager 1 observed a gradual slowing-down of radial plasma flow in the heliosheath to near-zero velocity after April 2010 at a distance of 113.5 astronomical units from the Sun (1 astronomical unit equals 1.5 x 10(8) kilometres). Voyager 1 was then about 20 astronomical units beyond the shock that terminates the free expansion of the solar wind and was immersed in the heated non-thermal plasma region called the heliosheath. The expectation from contemporary simulations was that the heliosheath plasma would be deflected from radial flow to meridional flow (in solar heliospheric coordinates), which at Voyager 1 would lie mainly on the (locally spherical) surface called the heliopause. This surface is supposed to separate the heliosheath plasma, which is of solar origin, from the interstellar plasma, which is of local Galactic origin. In 2011, the Voyager project began occasional temporary re-orientations of the spacecraft (totalling about 10-25 hours every 2 months) to re-align the Low-Energy Charged Particle instrument on board Voyager 1 so that it could measure meridional flow. Here we report that, contrary to expectations, these observations yielded a meridional flow velocity of +3 +/- 11 km s(-1), that is, one consistent with zero within statistical uncertainties.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Decker, Robert B -- Krimigis, Stamatios M -- Roelof, Edmond C -- Hill, Matthew E -- England -- Nature. 2012 Sep 6;489(7414):124-7. doi: 10.1038/nature11441.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, The Johns Hopkins University, Laurel, Maryland 20723, USA. robert.decker@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22955623" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
  • 10
    facet.materialart.
    Unknown
    Zero outward flow velocity for plasma in a heliosheath transition layer (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-06-17
    Description: Voyager 1 has been in the reservoir of energetic ions and electrons that constitutes the heliosheath since it crossed the solar wind termination shock on 16 December 2004 at a distance from the Sun of 94 astronomical units (1 AU = 1.5 x 10(8) km). It is now approximately 22 AU past the termination shock crossing. The bulk velocity of the plasma in the radial-transverse plane has been determined using measurements of the anisotropy of the convected energetic ion distribution. Here we report that the radial component of the velocity has been decreasing almost linearly over the past three years, from approximately 70 km s(-1) to approximately 0 km s(-1), where it has remained for the past eight months. It now seems that Voyager 1 has entered a finite transition layer of zero-radial-velocity plasma flow, indicating that the spacecraft may be close to the heliopause, the border between the heliosheath and the interstellar plasma. The existence of a flow transition layer in the heliosheath contradicts current predictions--generally assumed by conceptual models--of a sharp discontinuity at the heliopause.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Krimigis, Stamatios M -- Roelof, Edmond C -- Decker, Robert B -- Hill, Matthew E -- England -- Nature. 2011 Jun 15;474(7351):359-61. doi: 10.1038/nature10115.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Applied Physics Laboratory, The Johns Hopkins University, Laurel, Maryland 20723, USA. tom.krimigis@jhuapl.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21677754" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
    Location Call Number Expected Availability
    BibTip Others were also interested in ...
    PAPER CURRENT
Close ⊗
This website uses cookies and the analysis tool Matomo. More information can be found here...