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  • Other Sources  (8)
  • 1
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    Lunakhod-2 in Lemonnier crater (1975)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: A study of surface properties of the Lemonnier Crater by Lunakhod 2 is summarized. Special efforts were made to determine the variations of physical-chemical properties of the lunar surface as a function of the selenological-morphological structure in the transition zone of a mare region to the highlands. Studies were also made of the local magnetic situation, physical-mechanical properties of the soil, and the optical properties of the surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Mod. Achievements of Cosmonautics (NASA-TT-F-16221); p 5-19
    Format: text
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  • 2
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    Understanding the Role of Particles in Oblique Heliospheric Shock Oscillations (2019)
    In:  Other Sources
    Details
    Publication Date: 2019-05-25
    Description: Recent observations by DSCOVR provide high temporal resolution (50 samples per second) magnetic vector field data that allows investigating the details of oblique heliospheric shock oscillations. It was found that some of these shocks exhibit magnetic oscillations, both downstream and upstream of the shock front. The DSCOVR/MAG magnetic field data are supplemented by an extensive database of low Mach number (M 〈 3) low (〈1) shock data observed by Wind albeit with lower temporal resolution. Motivated by the observations, we use the 2.5D hybrid model of the oblique shocks with particles in addition to kinetic protons and electron fluid. We model the properties of the oblique shocks for a number of typical parameters found in observations and study the effects of the shock parameters and the relative particle abundances on the properties of the shock magnetic field, density, and velocity oscillations. We find the particles surf on the shock front and produce a wake of density oscillations. We examine the details of the phase space of the ions as well as the ion velocity distribution functions in various parts of the shock and study their nonthermal properties. We determine the effects of the particle kinetic properties and abundances on the structure and dynamics of the shock downstream oscillations for a range of parameters relevant to low Mach number low heliospheric shocks.
    Keywords: Solar Physics
    Type: GSFC-E-DAA-TN68517 , JGR Space Physics (ISSN 2169-9402) (e-ISSN 2169-9380); 124; 4; 2393-2405
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  • 3
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    Shocklets, SLAMS, and Field-Aligned Ion Beams in the Terrestrial Foreshock (2012)
    In:  CASI
    Details
    Publication Date: 2019-07-12
    Description: We present Wind spacecraft observations of ion distributions showing field- aligned beams (FABs) and large-amplitude magnetic fluctuations composed of a series of shocklets and short large-amplitude magnetic structures (SLAMS). The FABs are found to have T(sub k) approx 80-850 eV, V(sub b)/V(sub sw) approx 1.3-2.4, T(sub perpendicular,b)/T(sub paralell,b) approx 1-8, and n(sub b)/n(sub o) approx 0.2-11%. Saturation amplitudes for ion/ion resonant and non-resonant instabilities are too small to explain the observed SLAMS amplitudes. We show two examples where groups of SLAMS can act like a local quasi-perpendicular shock reflecting ions to produce the FABs, a scenario distinct from the more-common production at the quasi-perpendicular bow shock. The SLAMS exhibit a foot-like magnetic enhancement with a leading magnetosonic whistler train, consistent with previous observations. Strong ion and electron heating are observed within the series of shocklets and SLAMS with temperatures increasing by factors approx 〉 5 and approx 〉3, respectively. Both the core and halo electron components show strong perpendicular heating inside the feature.
    Keywords: Geophysics
    Type: GSFC-E-DAA-TN6704
    Format: application/pdf
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  • 4
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    Interplanetary Magnetic Field Power Spectrum Variations in the Inner Heliosphere: A Wind and MESSENGER Study (2011)
    In:  CASI
    Details
    Publication Date: 2019-07-19
    Description: The newly reprocessed high time resolution (11/22 vectors/sec) Wind mission interplanetary magnetic field data and the similar observations made by the MESSENGER spacecraft in the inner heliosphere affords an opportunity to compare magnetic field power spectral density variations as a function of radial distance from the Sun under different solar wind conditions. In the reprocessed Wind Magnetic Field Investigation (MFI) data, the spin tone and its harmonics are greatly reduced that allows the meaningful fitting of power spectra to the approx.2 Hz limit above which digitization noise becomes apparent. The powe'r spectral density is computed and the spectral index is fitted for the MHD and ion inertial regime separately along with the break point between the two for various solar wind conditions. Wind and MESSENGER magnetic fluctuations are compared for times when the two spacecraft are close to radial and Parker field alignment. The functional dependence of the ion inertial spectral index and break point on solar wind plasma and magnetic field conditions will be discussed.
    Keywords: Space Sciences (General)
    Type: GSFC.ABS.5528.2011
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  • 5
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    Interplanetary Magnetic Field Power Spectrum Variations: A VHO Enabled Study (2010)
    In:  CASI
    Details
    Publication Date: 2019-07-19
    Description: The newly reprocessed high time resolution (11/22 vectors/sec) Wind mission interplanetary magnetic field data and the solar wind key parameter search capability of the Virtual Heliospheric Observatory (VHO) affords an opportunity to study magnetic field power spectral density variations as a function of solar wind conditions. In the reprocessed Wind Magnetic Field Investigation (MFI) data, the spin tone and its harmonics are greatly reduced that allows the meaningful fitting of power spectra to the approx.2 Hz limit above which digitization noise becomes apparent. The power spectral density is computed and the spectral index is fitted for the MHD and ion inertial regime separately along with the break point between the two for various solar wind conditions . The time periods of fixed solar wind conditions are obtained from VHO searches that greatly simplify the process. The functional dependence of the ion inertial spectral index and break point on solar wind plasma and magnetic field conditions will be discussed
    Keywords: Solar Physics
    Type: 2010 AGU (American Geophysical Union) Fall Meeting; Dec 13, 2010 - Dec 17, 2010; San Francisco, CA; United States
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  • 6
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    Interplanetary Magnetic Field Power Spectrum Variations: A VHO Enabled Study (2011)
    In:  CASI
    Details
    Publication Date: 2019-07-19
    Description: The newly reprocessed high time resolution (11/22 vectors/sec) Wind mission interplanetary magnetic field data and the solar wind key parameter search capability of the Virtual Heliospheric Observatory (VHO) affords an opportunity to study magnetic field power spectral density variations as a function of solar wind conditions. In the reprocessed Wind Magnetic Field Investigation (MFI) data, the spin tone and its harmonics are greatly reduced that allows the meaningful fitting of power spectra to the ~2 Hz limit above which digitization noise becomes apparent. The power spectral density is computed and the spectral index is fitted for the MHD and ion inertial regime separately along with the break point between the two for various solar wind conditions. The time periods of fixed solar wind conditions are obtained from VHO searches that greatly simplify the process. The functional dependence of the ion inertial spectral index and break point on solar wind plasma and magnetic field conditions will be discussed
    Keywords: Space Sciences (General)
    Type: 4th Solar Orbiter Workshop; Mar 27, 2011 - Mar 31, 2011; telluride, CO; United States
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  • 7
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    Relationship of Interplanetary Shock Micro and Macro Characteristics: A Wind Study (2008)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: The non-linear least squared MHD fitting technique of Szabo 11 9941 has been recently further refined to provide realistic confidence regions for interplanetary shock normal directions and speeds. Analyzing Wind observed interplanetary shocks from 1995 to 200 1, macro characteristics such as shock strength, Theta Bn and Mach numbers can be compared to the details of shock micro or kinetic structures. The now commonly available very high time resolution (1 1 or 22 vectors/sec) Wind magnetic field data allows the precise characterization of shock kinetic structures, such as the size of the foot, ramp, overshoot and the duration of damped oscillations on either side of the shock. Detailed comparison of the shock micro and macro characteristics will be given. This enables the elucidation of shock kinetic features, relevant for particle energization processes, for observations where high time resolution data is not available. Moreover, establishing a quantitative relationship between the shock micro and macro structures will improve the confidence level of shock fitting techniques during disturbed solar wind conditions.
    Keywords: Meteorology and Climatology
    Type: WING SWG and 3008 Fall (AGU) Meeting; Dec 11, 2008 - Dec 21, 2008; San Francisco, CA; United States
    Format: text
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  • 8
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    Observations of Electromagnetic Whistler Precursors at Supercritical Interplanetary Shocks (2012)
    In:  CASI
    Details
    Publication Date: 2019-07-12
    Description: We present observations of electromagnetic precursor waves, identified as whistler mode waves, at supercritical interplanetary shocks using the Wind search coil magnetometer. The precursors propagate obliquely with respect to the local magnetic field, shock normal vector, solar wind velocity, and they are not phase standing structures. All are right-hand polarized with respect to the magnetic field (spacecraft frame), and all but one are right-hand polarized with respect to the shock normal vector in the normal incidence frame. They have rest frame frequencies f(sub ci) 〈 f much 〈 f(sub ce) and wave numbers 0.02 approx 〈 k rho (sub ce) approx 〈. 5.0. Particle distributions show signatures of specularly reflected gyrating ions, which may be a source of free energy for the observed modes. In one event, we simultaneously observe perpendicular ion heating and parallel electron acceleration, consistent with wave heating/acceleration due to these waves. Al though the precursors can have delta B/B(sub o) as large as 2, fluxgate magnetometer measurements show relatively laminar shock transitions in three of the four events.
    Keywords: Geophysics
    Type: GSFC.JA.01075.2012
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