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1998 Incoherent Scatter Coordinated Observation Days

In the following table, column 2 gives the start and end date of the experiment, column 3 gives the day of the week of the start of the experiment, column 4 is the length of the experiment, column 5 shows dates when IMP 8 is in the solar wind and column 6 shows the date of the new moon.

Incoherent Scatter Coordinated Observation Days start at 1600UT on the first day indicated and end at 1600UT on the last day indicated. However, radars are encouraged to start earlier on the first day where operational considerations allow.

Month Dates Day Length IMP8 NewMoon Notes
January 20-21 Tue 1 15-22 28 1
February


23-01 26
March 23-27 Mon 4 20-26 28 2
April 27-29
(06-10)
(13-17)
(20-24)		 Mon 2 26-02
01-07
13-20		 26 3
May 26-28 Tue 2 21-28 25 4
June 23-24 Tue 1
24 1
July


21-29 23
August 18-19 Tue 1 16-23 22 1
September 21-25 Mon 4 22-29 20 2
October 19-21
(05-09)
(12-16)
(26-30)		 Mon 2 17-23
04-11
 20 3
November 16-19 Mon 3 11-17 19 4
December 08-09 Tue 1 06-12 18 1
Total

21


Notes

  1. DATABASE. The emphasis should be on broad latitudinal coverage of the F region.

    A. van Eyken - tony@eiscat.no

  2. MLTCS/CADITS. Combined local E and F region measurements, including vector velocities, with 15 minute time resolution. Latitudinal coverage may be sacrificed to meet this goal.

    C. Fesen - fesen@tides.dartmouth.edu
    R. Johnson - rjohnson@dexter.sprl.umich.edu

  3. WLS. Wide-Latitude Substorm Dynamics These are 'floating' days, the exact operation dates to be selected about one month before based on available predictions. Radars which cannot accommodate this flexibility should run on the dates specified on the firts line of the entry. Modes with temporal resolutions better than 5 minutes should be used. The WLS campaigns differ from GISMOS in that they concentration on the extent and dynamics of the auroral oval using the longitudinally spaced ISRs available in the late 1990s.

    J. Foster - jcf@haystack.mit.edu

  4. POLITE aims to advance our understanding of topside light ion morphology and dynamics through a combination of modeling efforts and coordinated observations by the ISR chain and by DMSP satellite overflights. The use of the full latitudinal and longitudinal extent of the ISR chain is critical to the campaign, as one key objective is the study of the latitudinal and longitudinal variations of hydrogen, oxygen, and helium ions. Simultaneous measurements of neutral oxygen, hydrogen, and helium are also important, in order to explore the coupling between ionic and neutral species in the lower topside. Observations at the solstices are of particular interest. The helium ion layer descends in altitude and increases in strength during the wintertime, making observation easier for the ISR chain. Significant asymmetries in field-aligned flows are also at their maximums during summer and winter solstices. IMF support is not very important, but new moon periods are critical since optical support is required for simultaneous neutral species measurements.

    P. Erickson - pje@haystack.mit.edu

Updated 24 January 1998.