A new predictive model for determining solar wind‐terrestrial planet interactions

Spreiter, J. R.; Stahara, S. S.

doi:10.1029/ja085ia12p06769

Cited by 260 publications

(141 citation statements)

References 26 publications

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“…First, we use this rare occasion to verify the sheath model that has been developed recently [Spreiter and Stahara, 1980;Song et al, 1999a, b]. Second, we verify magnetopause models [Spreiter and Stahara, 1980;Shue et al, 1998] under large-amplitude variations. In particular, we examine the dependence on north-south component (Bz) of the IMF in the models.…”

Section: Introductionmentioning

confidence: 99%

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

et al. 2001

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Abstract. During the rise to the maximum phase of solar cycle 23, several periods of extreme solar wind conditions have occurred. During such an example on May 4, 1998, the solar wind monitors observed a period of strong southward interplanetary magnetic field (IMF) accompanied by a solar wind dynamic pressure that was 30 times higher than average. During this period the Polar spacecraft crossed the magnetopause and bow shock and experienced its first solar wind encounter. This case provides a rare opportunity to study the magnetopause, low-latitude boundary layer, magnetosheath, and bow shock and to test our ability to model the dynamic behavior of these boundary regions under extreme and highly variable solar wind conditions. In this study we use the gas dynamic convected field model to predict the time-dependent magnetic field and plasma properties upstream from the magnetopause and the location of the Polar spacecraft relative to the magnetopause and bow shock during the event. To test the accuracy of the prediction, model magnetic field characteristics are compared to the fields observed along the satellite track by the magnetometer on Polar. The predicted model plasma characteristics (density, velocity, and temperature) are compared to moments derived from TIDE observations, extrapolated to account for the higher energy portion of the magnetosheath distributions.

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Section: Introductionmentioning

confidence: 99%

“…We then employ the gas dynamic convected field (GDCF) model [Spreiter and Stahara, 1980] to calculate the location of the bow shock and the field and plasma parameters in the magnetosheath. We extract the model values of the magnetosheath parameters along the Polar satellite trajectory and compare them to the Polar observations.…”

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

et al. 2001

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“…Since the flow is magnetized, a simple gas dynamical approach is inadequate. A very successful treatment has been elaborated by Spreiter and co-workers [Spreiter et al, 1966;Spreiter and Alskne, 1969;Spreiter and Stahara, 1980; see also Siscoe, 2002]. Called the Convected Gas Dynamic Model (CGDM), the technique involves first a solution of the gas dynamic problem to obtain the plasma parameters and the flow field, including the position of the bow shock.…”

Section: Introductionmentioning

confidence: 99%

Magnetosheath for almost‐aligned solar wind magnetic field and flow vectors: Wind observations across the dawnside magnetosheath at X = −12 Re

et al. 2010

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[1] While there are many approximations describing the flow of the solar wind past the magnetosphere in the magnetosheath, the case of perfectly aligned (parallel or antiparallel) interplanetary magnetic field (IMF) and solar wind flow vectors can be treated exactly in a magnetohydrodynamic (MHD) approach. In this work we examine a case of nearly-opposed (to within 15°) interplanetary field and flow vectors, which occurred on October 24-25, 2001 during passage of the last interplanetary coronal mass ejection in an ejecta merger. Interplanetary data are from the ACE spacecraft. Simultaneously Wind was crossing the near-Earth (X ∼ −13 Re) geomagnetic tail and subsequently made an approximately 5-hour-long magnetosheath crossing close to the ecliptic plane (Z = −0.7 Re). Geomagnetic activity was returning steadily to quiet, "ground" conditions. We first compare the predictions of the Spreiter and Rizzi theory with the Wind magnetosheath observations and find fair agreement, in particular as regards the proportionality of the magnetic field strength and the product of the plasma density and bulk speed. We then carry out a small-perturbation analysis of the Spreiter and Rizzi solution to account for the small IMF components perpendicular to the flow vector. The resulting expression is compared to the time series of the observations and satisfactory agreement is obtained. We also present and discuss observations in the dawnside boundary layer of pulsed, high-speed (v ∼ 600 km/s) flows exceeding the solar wind flow speeds. We examine various generating mechanisms and suggest that the most likely cause is a wave of frequency 3.2 mHz excited at the inner edge of the boundary layer by the Kelvin-Helmholtz instability.

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“…The procedure for correcting for the time delays was as follows: First, we corrected for the travel time or delay between the ACE satellite and the magnetopause using the measured solar wind speed and the ACE satellite distance. The calculation of this delay was the same as we used in our previous study (for details, see Jayachandran and MacDougall, 2000] and includes two components: the delay from satellite to (calculated position) bow shock at a speed equal to the measured solar wind speed, plus a delay from bow shock to (calculated position) magnetopause at 1/8 the solar wind speed [Spreiter and Stahara, 1980]. Second, we did a cross …”

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confidence: 99%

Polar cap convection relationships with solar wind

MacDougall¹,

Jayachandran²

2001

Radio Science

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A new predictive model for determining solar wind‐terrestrial planet interactions

Cited by 260 publications

References 26 publications

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

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

Magnetosheath for almost‐aligned solar wind magnetic field and flow vectors: Wind observations across the dawnside magnetosheath at X = −12 Re

Polar cap convection relationships with solar wind

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