Polar observations and model predictions during May 4, 1998, magnetopause, magnetosheath, and bow shock crossings

Song, P.; Kozyra, J. U.; Chandler, M. O.; Russell, C. T.; Peterson, W. K.; Trattner, K. J.; Friedel, R. H. W.; Shue, J.‐H.; Moore, T. E.; Ogilvie, K. W.; Lepping, R. P.; McComas, D. J.

doi:10.1029/2000ja900126

Cited by 6 publications

(4 citation statements)

References 19 publications

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“…On a case‐by‐case basis we find for most of our events a very good correlation between the Dst variation and the data from the monitor located at L1. This is in good agreement with the study of the interplanetary and magnetosheath conditions by Song et al [2001]. The efficiency and objectivity of the proposed method will be demonstrated in the next sections.…”

Section: Data Treatmentsupporting

confidence: 86%

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Necessary conditions for geosynchronous magnetopause crossings

et al. 2005

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[1] The International Solar Terrestrial Physics database of the magnetic measurements on GOES and plasma measurements on Los Alamos National Laboratory (LANL) geosynchronous satellites is used for selection of 169 case events containing 638 geosynchronous magnetopause crossings (GMCs) in 1995 to 2001. The GMCs and magnetosheath intervals associated with them are identified using advanced methods that take into account (1) strong deviation of the magnetic field measured by GOES from the magnetospheric field, (2) high correlation between the GOES magnetic field and interplanetary magnetic field (IMF), and (3) substantial increase of the midenergy ion and electron fluxes measured by LANL. Accurate determination of the upstream solar wind conditions for the GMCs is performed using correlation of geomagnetic activity (Dst (SYM-H) index) with the upstream solar wind pressure. The location of the GMCs and associated upstream solar wind conditions are ordered in an aberrated GSM coordinate system (aGSM) with X-axis directed along the solar wind flow. In the selected data set of GMCs the solar wind total pressure Psw varies up to 100 nPa and the southward IMF Bz reaches 60 nT. We study the conditions necessary for geosynchronous magnetopause crossings using scatterplots of the GMCs in the coordinate space of Psw versus Bz. In such a representation the upstream solar wind conditions show a sharp envelope boundary beyond which no GMCs are observed. The boundary has two straight horizontal branches where Bz does not influence the magnetopause location. The first branch is located in the range of Psw = 21 nPa for large positive Bz and is associated with a regime of pressure balance. The second branch asymptotically approaches the range of Psw = 4.8 nPa under strong negative Bz, and it is associated with a regime in which the Bz influence saturates. The intermediate region of the boundary ranges from moderate negative to moderate positive IMF Bz and can be well approximated by a hyperbolic tangent function. We interpret the envelope boundary as a range of necessary upstream solar wind conditions required for the magnetopause to reach geosynchronous orbit at its closest approach to the Earth (its ''perigee'' location).

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Section: Data Treatmentsupporting

confidence: 86%

“…The problem of determining the best choice of upstream monitor for better forecasting the near‐Earth environment was formulated by Song et al [2001]. We propose here a good way to solve this problem for any particular case event in the magnetosphere.…”

Section: Data Treatmentmentioning

confidence: 99%

Necessary conditions for geosynchronous magnetopause crossings

et al. 2005

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“…The prediction of the field direction made by the GDCF model correlates very well with the magnetosheath observations. More documented cases and the comparison between the vacuum dipole magnetopause model and the Shue et al [1998] model can be found in Song et al [1999bSong et al [ , 2000. In addition to making space weather forecasts, the GDCF model has been used as a research tool.…”

Section: Calibration Factorsmentioning

confidence: 99%

Model Predictions of Magnetosheath Conditions

Song

2013

Geophysical Monograph Series

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The magnetosheath and its two boundaries-the bow shock and the magnetopause-interface the magnetosphere with the solar wind. This interface specifies the upstream conditions for magnetospheric models. Major progress has been made in the last few years in specifying the magnetosheath conditions. The classical Spreiter magnetosheath model is modified to include more physical processes. The modified model has been tested under various upstream conditions. Magnetohydrodynamic models have been developed. The spatial and temporal resolutions of these models are limited by the computer capability and costs for running. The performance of these models remains to be tested. The modified Spreiter model provides fast and inexpensive specification of the magnetosheath conditions. The direction of the magnetic field in the magnetosheath, which is most important for space weather magnetospheric models, is the best-predicted quantity. This paper summarizes the model approximations, procedures and validations.

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“…[3] Under extreme solar wind conditions the geosynchronous spacecraft can be excluded from the protection of the geomagnetic field by the inward motion of the magnetopause [Russell et al, 2000;Song et al, 2001;Shue et al, 2001]. It has been established that the location of the magnetopause is controlled by the balance between the solar wind dynamic pressure and the geomagnetic pressure.…”

Section: Introductionmentioning

confidence: 99%

Magnetopause response to variations in the solar wind: Conjunction observations between Cluster, TC-1, and SuperDARN

Zhang¹,

Shen²,

Liu³

et al. 2011

J. Geophys. Res.

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[1] How the solar wind affects the location of the magnetopause has been widely studied and excellent models of the magnetopause based on in situ observations in the solar wind and at the magnetopause have been established, while the careful insight into the responses of the magnetopause to the variations in the solar wind can still provide us some new information about the processes in space plasmas. The short distance from Cluster to TC-1 on 9 March 2004, between 06:10 and 08:10 UT, gives us a good opportunity to precisely monitor the responses of the magnetopause to the variations in the solar wind. On the basis of the combined observations between Cluster, TC-1, and SuperDARN we analyze the magnetopause crossings associated with magnetopause motion or magnetic reconnection when the solar wind conditions have a series of variations. New results about the time delays for the propagation from the solar wind monitor to the magnetopause of the interplanetary magnetic fields (IMF) and of the solar wind dynamic pressure, respectively, and the intrinsic time for reconnection onset at the magnetopause are obtained. The most important feature of the event is that the dynamic pressure and the IMF in the solar wind do not arrive at the magnetopause at the same time, which will direct us to find out how the variation in the solar wind dynamic pressure is transported from the bow shock to the magnetopause. Another significant feature is that this event presents a shorter intrinsic time, ∼2 min, for reconnection onset at the dayside magnetopause than that given by the previous work of Le et al. (1993) and Russell et al. (1997).

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Polar observations and model predictions during May 4, 1998, magnetopause, magnetosheath, and bow shock crossings

Cited by 6 publications

References 19 publications

Necessary conditions for geosynchronous magnetopause crossings

Necessary conditions for geosynchronous magnetopause crossings

Model Predictions of Magnetosheath Conditions

Magnetopause response to variations in the solar wind: Conjunction observations between Cluster, TC-1, and SuperDARN

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