THE EXTREME COMPRESSION OF THE MAGNETOSPHERE ON MAY 4, 1998, AS OBSERVED BY THE POLAR SPACECRAFT

 

C. T. Russell1,2, G. Le1, P. Chi1, X.-W. Zhou1,2, J.-H. Shue3, S. M. Petrinec4, P. Song5, F. R. Fenrich6 and J. G. Luhmann6

 

1Institute of Geophysics and Planetary Physics, University of California,Los Angeles, CA, USA

2Department of Earth and Space Sciences, University of California, Los Angeles, CA, USA

3STELAB, University of Nagoya, Japan

4Lockheed Martin, Palo Alto, CA, USA

5Space Research Laboratory, University of Michigan, USA

6Space Sciences Laboratory, University of California, Berkeley, CA, USA

Originally published in Adv. Space Res., 25(7/8), 1369-1375, 2000.

ABSTRACT

On May 4, 1998 the velocity and density of the solar wind were high and the interplanetary magnetic field was strong and southward. The POLAR spacecraft crossed the dayside magnetopause well inside geosynchronous orbit, at 5.3 RE and a solar zenith angle of 19o. After this crossing, POLAR spent most of the rest of its outbound orbit in the magnetosheath and for brief periods crossed into the solar wind at distances from 7.3 RE and a solar zenith angle of 32o to a distance of only 8.5 RE and a solar zenith angle of 45o. This corresponds to subsolar distances of only 6.8 to 7.5 RE for the shock. During this very disturbed period of time, predictions of the locations of the magnetopause by both Shue and co-workers and by Petrinec and co-workers indicate extremem distortions of the magnetopause location. Because of the importance of such events to the understanding of space weather, we recommend that this event be pursued as a special IACG 2 campaign.

 

INTRODUCTION

The increasing use of space for commercial purposes has resulted in an escalating number of spacecraft at all altitudes in the magnetosphere. In particular there are satellites now being placed between geosynchronous orbit and low Earth orbit where none had been placed before. We know very little about this region of space. Much of our understanding of the magnetosphere under extreme conditions of the solar wind and interplanetary magnetic field comes from geosynchronous orbit. From these measurements we know that the magnetopause lies inside of synchronous orbit at the nose of the magnetosphere about 0.3% of the time (Russell, 1976; Shue et al., 1988); however, these data do not constrain well the distance to which the magnetopause is eroded or compressed under such conditions because the geosynchronous spacecraft see the boundary only as it passes by and not while it is at an equilibrium position.

Many models of the location of the magnetopause have been published but only two make a reasonable case for treating these extreme conditions (Shue et al., 1997; Petrinec and Russell, 1995). It is important that such claims be verified with extreme solar wind data that compress the magnetopause well inside synchronous orbit. Moreover, it is important to obtain data away from the equatorial plane. May 4, 1998 provides us with such an opportunity.

 

SOLAR WIND CONDITIONS AND PREDICTIONS

Initially on May 4, 1998 the solar wind was flowing at about 500 km/s. At 0230 this velocity increased to 700 km/s and then to over 800 km/s at 0300. Simultaneously with the velocity jump at 0230 the magnetic field increased to 40 nT and was largely southward with a Bz component of -30 nT. Figures 1a and b show the interplanetary magnetic field and the solar-wind time series as measured by WIND 240 RE upstream. The expected time delay after the velocity increase from WIND to the magnetosphere was approximately 25 min. We note that the magnetic field strength, the dynamic pressure and the non-radial components of solar wind were all unusually high. The east, west, north and south oscillations in the solar-wind direction may also affect the crossing time of the magnetopause and shock for spacecraft near and beyond the terminators.

Figure 1.Solar wind and interplanetary magnetic field conditions on May 4, 1998 from 0000 to 1600 UT. Left. WIND observations of the interplanetary field in GSM coordinates. Right. WIND observations of the solar wind velocity, dynamic pressure and thermal velocity.

To anticipate what POLAR observed on this day, Figure 2 shows the predicted position of the magnetopause at the subsolar point and along the flanks according to the Shue et al. (1998) model. The magnetopause crosses synchronous orbit repeatedly, getting as close as 5 Re in the subsolar region. Above the terminators the magnetopause reaches a distance of about 8 Re.

 

OBSERVATIONS BY THE POLAR SPACECRAFT

When the disturbed solar wind reached the Earth, the POLAR spacecraft was at perigee. Figure 3 shows the projection of the POLAR orbit in the noon-midnight trajectory as expressed in solar magnetospheric coordinates. The plane of the orbit is close to this plane, being centered roughly on the 11 AM meridian at this time. We recall that the solar magnetospheric coordinate system (GSM) differs from the solar magnetic coordinate system (SM) by the tilt of the dipole axis. The GSM system is most useful for examining boundary locations that are ordered more by the direction of the solar wind flow than by the Earth's field. The SM coordinate system is most useful for examining the boundaries well within the magnetosphere where magnetic stresses dominate over solar-wind-induced stresses.

Figure 2. Predicted size of the magnetosphere at the nose and the terminator (bottom panels) according to the southward IMF and solar-wind dynamic pressure shown in the top two panels.These panels do not account for the propogation time to the Earth from WIND Figure 3. The projection of the POLAR orbit in the noon-midnight meridian in GSM coordinates.

When the interplanetary magnetic field (IMF) is northward, the magnetopause location is essentially determined by the dynamic pressure scaled by the sixth root of the dynamic pressure. One way to illustrate the effect of the solar wind is to scale the location of the satellite by this factor and keep the boundary fixed. This is done in Figure 4 that shows the distance to POLAR as a function of solar zenith angle. Whenever the scaled orbit is beyond the magnetopause, POLAR is predicted to be in the magnetosheath by the solar-wind pressure alone. Figure 4 shows that this occurs during the majority of the time from approximately 0600 UT onward to 1230 UT. POLAR approaches but does not cross the bow shock according to these predictions.

Figure 4. The POLAR orbit in GSM coordinates expressed as distance from the Earth as a function of solar zenith angle. The irregular curve is an expansion of the distance of the spacecraft from the Earth by the sixth root of the dynamic pressure. The average magnetopause and bow shock location for a dynamic pressure of 2nPa are shown. Figure 5. The magnetic field measured at POLAR across the 0541 UT magnetopause crossing in GSM coordinates.

Figure 5 shows the magnetic field observed by POLAR (Russell et al., 1995) on May 4, 1998 from 0540 to 0546 UT. At this time the IMF as convected to Earth should be still strongly southward but near the end of its long southward orientation period. The magnetopause crossing at 0541:22 is clearly seen and is most impressive. Prior to the crossing, the magnetic field is over 200 nT northward; it then switches to over 200 nT southward. There is a small dip in the magnitude of the field as the crossing is made but no overall change in field magnitude; thus, the discontinuity is principally a rotational discontinuity indicating strong reconnection at this point. The spacecraft returns briefly to the magnetosphere at 0544:30. At the two crossings of the magnetopause the magnetic field now decreases greatly from the magnetosphere to the magnetosheath.

Figure 6. The magnetic field measured at POLAR at 6 sec resolution in GSM coordinates for the entire period from 0530 UT to 1530 UT.

Figure 6 shows the POLAR magnetic field for the entire period from 0530 to 1530 UT on May 4, 1998 in GSM coordinates. On this plot the magnetopause crossing at 0541 UT, discussed above, can most readily be recognized in the Bz reversal. Later the magnetic field turns northward while still depressed in magnitude. This is probably associated with a northward turning of the IMF. At about 0615 UT the field becomes quieter and lies more in the expected direction of the magnetoshperic field. This probably signals the reentry into the magnetosphere. At 0648 UT the field rotates and the magnitude drops signaling a reentry into the magnetosheath. After this point the field is disturbed almost continually until about 1205 UT. It is difficult to rule out any magnetospheric reentry without further analysis of the field and plasma data but it is reasonable to assume that POLAR is predominantly in the magnetosheath during this interval. Finally, there is a period of disturbed and depressed magnetic field from 1336 to 1359 UT, which appears to be a final entry into the magnetosheath.

There are three surprising events during the interval, two of which are shown in Figure 7. These are crossings of the bow shock and entry into the solar wind. The first pair of crossings is at 0735:45 and 0738:10 when the spacecraft was at (6.17, -1.24, 3.74) RE in GSM coordinates. This corresponds to a subsolar shock distance of about 6.8 RE close to synchronous orbit and a magnetopause distance of about 5.3 RE. A second pair of shock crossings is at 0919:30 and 0920:40. The third pair of shock crossings occur at 0944 and 0950 UT. POLAR was at 8.5 RE at this time at a solar zenith angle of 45o. This corresponds roughly to a subsolar shock location of 7.5 Re.

Figure 7. The magnetic field measured at POLAR at 120 ms resolution in GSM coordinates for two periods of entry into the solar wind. Left. 0735-0739 UT Right. 0940 to 0952 UT.

 

CORRESPONDENCE WITH PREDICTIONS

In order to test if we can accurately predict the location of the magnetopause under these extreme conditions, we have calculated POLAR's distance from the magnetopause according to the Shue et al. (1998) and Petrinec and Russell (1995) models. These predictions are shown in Figure 8. The first entry into the magnetosheath at 0541 is correctly predicted by the both models. They also predict an extended entry of the magnetosheath from 0845 to 1200 UT. However, it is difficult to verify when POLAR precisely left the magnetosphere near 0845 UT from the magnetic field observations alone. Neither model predicts the period of magnetosheath entry from 1335 to 1400 UT but the Petrinec and Russell (1995) model predicts closer approach to the boundary than the Shue et al. (1998) model. This failure to predict a magnetosheath entry may be due to the non-cylindrical symmetry of the magnetopause.

Figure 8. The predicted distance of the POLAR spacecraft from the magnetopause according to two models of the dependence of the magnetopause location on IMF conditions. (Top) The Shue et al. (1998) model. (Bottom) The Petrinec and Russell (1995) model. This figure does take into account the time delay from WIND to the Earth.

Petrinec (1998) has produced a movie of the predicted magnetopause (Petrinec and Russell, 1995; 1996) and shock locations (Farris et al., 1991; Farris and Russell, 1994) during the May 4 period. Figure 9 shows one frame of that movie at a very compressed epoch near 0500 UT. The nose of the bow shock here is predicted to reach synchronous orbit. The movie documents the rapid dynamic changes experienced by the magnetosphere on this day. It is clear that many spacecraft at geosynchronous orbit left the magnetosphere for a time on this day. Another type of prediction for this event regards the buildup of the ring current as measured by Dst. Figure 10 shows the solar-wind conditions measured by ACE and the predicted Dst index from these data according to the Fenrich and Luhmann (1998) model that modified the formula of Burton et al. (1975). The prediction very nicely agrees with the preliminary Dst shown in the bottom panel of Figure 10. The maximum Dst value is close to -250 nT. In short this interval is valuable not only as it illustrates the extreme size distortions under which the magnetosphere can undergo but it also provides a good case study of the development of a larger storm.

Figure 9. A snapshot of the distortion of the magnetosphere and bow shock on May 4, 1998 from a movie of the interaction. The top panels show the IMF Bz and solar wind dynamic pressure. The bottom panel shows the ecliptic plane cross sections of the magnetopause and bow shock. The dashed circle is synchronous orbit.

Figure 10. The solar wind conditions observed by ACE on May 4, 1998 and the predicted and observed Dst indices. Top panel shows the solar wind density; the second panel the solar wind to speed; the third panel the IMF Bz; the fourth panel the predicted Dst index and the bottom panel the preliminary Dst index.

 

SUMMARY AND CONCLUSIONS

The solar wind conditions on May 4, 1998 were extremely disturbed and led to a very large geomagnetic storm. These disturbances greatly compressed the magnetosphere and that compression was documented by the POLAR spacecraft. Some of the existing models do very well at predicting the compression of the magnetosphere and the ensuing buildup of the ring current; nevertheless, improvements in these models can be made and May 4 should be very useful in determining what adjustments need to be made in these models. We nominate this interval for study by the IACG Boundary Layer Campaign.

 

ACKNOWLEDGMENTS

We are grateful to A.J. Lazarus, K.W. Ogilvie and J.T. Steinberg for providing the WIND ion data and R.P. Lepping for providing the WIND magnetic field measurements. This work was supported by the National Aeronautics and Space Administration under research grant NAG 5-3171.

 

REFERENCES

Burton, R. K., R. L. McPherron and C. T. Russell, An Empirical Relationship Between Interplanetary Conditions and Dst, J. Geophys. Res., 80, 4204-4214, (1975).

Farris, M.H., S.M. Petrinec, and C.T. Russell, The thickness of the magnetosheath: Constraints on the polytropic index, Geophys. Res. Lett., 18, 1821-1824, 1991.

Farris, M.H. and C.T. Russell, Determining the standoff distance of the bowshock: Mach number dependence and use of models, J. Geophys. Res, 99, 17681-17689, (1994).

Fenrich, F. R. and J. G. Luhmann, Geomagnetic Response to Magnetic Clouds of Different Polarity, Geophys. Res. Lett., in press, (1998).

Petrinec, S. M., Movie of Magnetopause and bow shock location during the May 4, 1998 compression and erosion events, http://www-ssc.igpp.ucla.edu/personnel/russell/papers/Extreme_comp/, (1998).

Petrinec, S. M. and C. T. Russell, Comments on "Magnetopause Shape as a Bivariate Function of Interplanetary Magnetic Field Bz and Solar Wind Dynamic Pressure" by E. C. Roelof and D. G. Sibeck, J. Geophys. Res., 100, 1899-1901, (1995).

Petrinec, S. M. and C. T. Russell, Near-Earth magnetotail shape and size as determined from the magnetopause flaring angle, J. Geophys. Res., 101, 137-152, (1996).

Russell, C. T., On the Occurrence of Magnetopause Crossings at 6.6 RE, Geophys. Res. Lett., 3, 593-595, (1976).

Russell, C. T., R. C. Snare, J. D. Means, D. Pierce, D. Dearborn, M. Larson, G. Barr and G. Le, "The GGS Polar Magnetic Fields Investigation" in The Global Geospace Mission, 563-582, Kluwer Academic Publishers, Dordrecht, The Netherlands, (1995).

Shue, J-H., J. K. Chao, H. C. Fu, C. T. Russell, P. Song, K. K. Khurana and H. J. Singer, A New Functional Form to Study the Solar Wind Control of the Magnetopause Size and Shape, J. Geophys. Res., 102, 9497-9511, (1997).

Shue, J-H., P. Song, C. T. Russell, J. T. Steinberg, J. K. Chao, G. Zastenker, O. L. Vaisberg, S. Kokubun, H. J. Singer, T. R. Detman and H. Kawano, Magnetopause Location Under Extreme Solar Wind Conditions, J. Geophys. Res, 103, 17691, (1998).


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