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  • 1
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    The 1983 tail-era data series. Volume 2: ISEE 3 magnetic field (1990)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: ISEE 3 spacecraft measurements within and near the Earth's magnetic tail is presented. Plots are shown of ISEE 3 magnetic field data. The plots in this volume showing observations from the ISEE 3 vector helium magnetometer experiment were produced from a tape of merged plasma/magnetic field data. The magnetometer produced six vector measurements/sec that were subsequently averaged over one minute intervals before merging with plasma data. Merging was accomplished by associating the nearest 1 minute field average with each plasma sample.
    Keywords: ASTROPHYSICS
    Type: NASA-TM-105049 , NSSDC/WDC-A-R/S-90-12-VOL-2 , NAS 1.15:105049
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 2
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    The 1983 tail-era series. Volume 1: ISEE 3 plasma (1991)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Observations from the ISEE 3 electron analyzer are presented in plots. Electrons were measured in 15 continuous energy levels between 8.5 and 1140 eV during individual 3-sec spacecraft spins. Times associated with each data point are the beginning time of the 3 sec data collection interval. Moments calculated from the measured distribution function are shown as density, temperature, velocity, and velocity azimuthal angle. Spacecraft ephemeris is shown at the bottom in GSE and GSM coordinates in units of Earth radii, with vertical ticks on the time axis corresponding to the printed positions.
    Keywords: ASTROPHYSICS
    Type: NASA-TM-105048-VOL-1 , NAS 1.15:105048-VOL-1 , NSSDC/WDC-A-R/S-90-11-VOL-1
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 3
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    Three spacecraft measurements of an unusual disturbance in the solar wind - Further evidence for a cometary encounter (1985)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: It is noted that, while the Pioneer Venus orbiter detected an unusual IMF and solar wind plasma disturbance on Feb. 11, 1982, the Venera 13 and 14 spacecraft were conducting IMF measurements 6 million miles away which exhibit very weak disturbances several hours after the peak of the Pioneer Venus event. It is speculated that, if the event had been a solar-initiated disturbance, it should have been detected in virtually unaltered form by Venera 13 and 14; whose data therefore furnish further evidence for the cometary nature of this event.
    Keywords: ASTROPHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 12; 476-478
    Format: text
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  • 4
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    A possible observation of a cometary bow shock (1984)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: In February, 1982, an unusual enhancement of the IMF was observed by the Pioneer Venus orbiter at 0.72 AU. The three discontinuities within this large disturbance, previously suggested to be due to the possible passage of a comet, are examined in view of the alternative possibility of their representing the first observation to date of a cometary shock. It is noted that number density, temperature, and velocity changes, as well as the magnetic structure of the discontinuities, are consistent with this hypothesis.
    Keywords: ASTROPHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 11; 1022-102
    Format: text
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  • 5
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    Interplanetary magnetic flux - Measurement and balance (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: A new method for determining the approximate amount of magnetic flux in various solar wind structures in the ecliptic (and solar rotation) plane is developed using single-spacecraft measurements in interplanetary space and making certain simplifying assumptions. The method removes the effect of solar wind velocity variations and can be applied to specific, limited-extent solar wind structures as well as to long-term variations. Over the 18-month interval studied, the ecliptic plane flux of coronal mass ejections was determined to be about 4 times greater than that of HFDs.
    Keywords: ASTROPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 97; 171-177
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  • 6
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    Near-tail reconnection as the cause of cometary tail disconnections (1986)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: In a cometary tail disconnection event the plasma tail appears to separate from the coma and to accelerate away from it. As this occurs a new tail begins to form. It is proposed that these disconnections arise in a manner analogous to geomagnetic substorms, i.e., by the formation of a strongly reconnecting region in the near tail that forms a magnetic island in the coma and ejects the plasma tail by strengthening the magnetic 'slingshot' within the tail. This reconnection process may be triggered by several different processes, such as interplanetary shocks or variations in the Alfven Mach number.
    Keywords: ASTROPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 91; 1417-142
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  • 7
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    Characteristics of cometary picked-up ions in a global model of Giacobini-Zinner (1987)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Energetic ions observed during the International Cometary Explorer (ICE) spacecraft flyby of comet Giacobini-Zinner provide information about both the constitution of comets and the plasma physical processes associated with their interaction with the solar wind. In this investigation the details of ion 'pickup,' in the limit where small-scale fluctuations in the plasma and magnetic field are neglected, are modeled by following the motion of a large number of initially cold, heavy (mass 18) ions in a global magnetohydrodynamic model of the local plasma and magnetic field. The results indicate how the background or macroscopic velocity and magnetic field structure of the comet can affect the average spatial and spectral characteristics of the observed cometary ions. These effects, which occur by virtue of forces associated with the compression and the curvature of the magnetic field in the presence of the stagnating plasma flow, can explain the double maxima in the time series of the energetic ion flux observed along the ICE trajectory.
    Keywords: ASTROPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 92; 8536-854
    Format: text
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  • 8
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    Magnetic field draping in the Comet Halley coma - Comparison of Vega observations with computer simulations (1987)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: During the Vega-1 encounter with Comet Halley, the magnetometer observed draping and compression of the interplanetary magnetic field. These are reproduced well by a three-dimensional MHD simulation of the cometary interaction. Rotations in the magnetic field similar to those at closest approach are also observed 2.75 hours earlier. It is suggested that both rotations correspond to the same IMF interval and that the spacecraft had overtaken the plasma and encountered 'older' magnetic field as it penetrated the coma. Analysis of the MHD model indicates that it should take about 3 to 5 hours for a solar wind parcel to pass from the unperturbed solar wind to Vega-1 at closest approach. A simulated magnetic field profile composed of nested sections for different IMF orientations closely resembles the observations. This result supports the hypothesis of layered magnetic orientations in the coma.
    Keywords: ASTROPHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 14; 640-643
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  • 9
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    Interplanetary flux enhancements - Comparison with cometary models and observations (1986)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: Interplanetary field enhancements (IFE's) are unusual nearly symmetric increases in the strength of the interplanetary magnetic field lasting tens of minutes to hours. Examples of interplanetary field enhancements are compared with MHD models and with the data obtained by the ICE spacecraft at Giacobini-Zinner. These comparisons suggest that the varying properties of IFE's are due to the fact that some events are due to passages in front of the nucleus, others in the near tail and yet others in the distant tail.
    Keywords: ASTROPHYSICS
    Type: Advances in Space Research (ISSN 0273-1177); 6; 1 19
    Format: text
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