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Topic: Magnetopause

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	UCLA - IGPP Space Physics SSC Tutorial - The Magnetopause
		The magnetopause is the interface between the shocked solar wind in the magnetosheath and the geomagnetic field and plasma in the magnetosphere.
		Velocity and thickness of the magnetopause (Berchem and Russell, 1982a).
		Another behavior of the magnetopause that seems to be dependent on the beta of the plasma is the rotation of the magnetic field in the plane of the magnetopause.
	www-ssc.igpp.ucla.edu /ssc/tutorial/magnetopause.html (5591 words)

	Research paper for physics 5422 (Site not responding. Last check: 2007-10-22)
		It is an interactive summary of the paper "The Structure of the Magnetopause" by C.
		Nonetheless, Russell continues to use the word "magnetopause" throughout the paper as if we've successfully defined it, because the authors of the various papers seemed to have settled on their own definitions.
		Russell claims that diffusion is not a dominant process in determining the thickness of the magnetopause, because the medium's resistivity in estimates is too low to have a significant effect on thickening.
	ham.spa.umn.edu /barbara/russell.html (1995 words)

	Magnetopause [Oulu] (Site not responding. Last check: 2007-10-22)
		Magnetopause is a direct consequence of solar wind interaction with magnetized planets.
		In the first approximation, magnetopause is formed at a distance where the solar wind dynamic pressure equals the magnetic pressure of Earth's field.
		Luhmann, J. G., The magnetopause counterpart at the weakly magnetized planets: The ionopause, in Physics of the Magnetopause, Geophysical Monograph 90, American Geophysical Union, 71-79, 1995.
	www.oulu.fi /~spaceweb/textbook/magnetopause.html (555 words)

	The Effect of the Foreshock on the Motion of the Dayside Magnetopause
		The role of the foreshock in causing motions of the magnetopause is studied using both the number of crossings of the magnetopause found as ISEE passed through the expected region of the magnetopause on each orbit and by determining the minimum and maximum distances to the magnetopause on each pass.
		This data set provides two measures of the motion of the magnetopause: the number of crossings of the magnetopause observed on each pass through the magnetopause region and the amplitude of the motion of the magnetopause measured as the minimal and maximal radial distance of the magnetopause seen on each pass.
		This suggests that at noon magnetopause motions are associated with the intrinsic pressure oscillations of the solar wind.
	ssc.igpp.ucla.edu /personnel/russell/papers/Effect (2257 words)

	Magnetosphere [Oulu] (Site not responding. Last check: 2007-10-22)
		In front of the dayside magnetopause another boundary called the bow shock is formed because the solar wind is supersonic.
		The region between the bow shock and the magnetopause is called the magnetosheath.
		Regions closest to the magnetopause are called boundary layers (of which the cusp is shown in the figure).
	www.oulu.fi /~spaceweb/textbook/magnetosphere.html (373 words)

	The Magnetopause
		The magnetopause is the thin boundary separating the shocked solar wind plasma from the plasma of the magnetosphere.
		Interior to the magnetopause, in the magnetosphere, the plasma's motion is dominated by Earth's magnetic field.
		Consistent with Figures 14.2 and 14.3 the magnetopause current is primarily westward near the equator at the front and mid-tail regions of the magnetopause, before turning above/below the magnetic equator (more properly, the tail's current sheet) and closing on the eastward side of the magnetopause.
	www.physics.usyd.edu.au /~cairns/teaching/lecture14/node3.html (1527 words)

	Jorvik MIST abstracts (Site not responding. Last check: 2007-10-22)
		Four-point coverage of the Earth's magnetopause began on the 9th and 10th November 2000 when all spacecraft first exited the dusk-side magnetosphere at about 1900 LT, providing extensive coverage of the near, flank magnetosheath and magnetopause boundary layer on re- entry to the magnetosphere.
		The magnetopause traversal on this occasion was caused by the arrival of an intense solar storm at the Earth, which produced a large compression of the magnetopause and high magnetic activity.
		The radar observations show evidence for two distinct high-latitude merging regions on the dayside magnetopause that is in favour of the anti-parallel merging hypothesis and contradicts the subsolar merging hypothesis.
	www.nerc-bas.ac.uk /public/uasd/mist/mistsa01.html (11907 words)

	ON THE SELF-CONSISTENT DETERMINATION OF DAYSIDE MAGNETOPAUSE SHAPE AND POSITION (Site not responding. Last check: 2007-10-22)
		Pressure distributions on the magnetopause, obtained in some of considered numerical implementations are presented in Figure 8.
		In all of the implemented numerical examples the shape and the position of the bow shock and those of the tangential discontinuity simulating dayside magnetopause, are obtained in terms of discontinuity-fitting approach.
		The character dimple on the magnetopause arises almost at the same position, while the subsonic ``pocked'' with Mach number smaller than 1 in the self- consistent case is moved slightly downstream.
	geospace4.imbm.bas.bg /pubnew/public_html/magnetopause.html (2849 words)

	* Magnetopause - (Astronomy): Definition (Site not responding. Last check: 2007-10-22)
		A magnetopause is the boundary between the area in which a planet's magnetic field dominates and the magnetic field of the rest of the Solar System dominates.
		Magnetosphere - The outermost part of the atmosphere of a planet, within which a very thin plasma is dominated by the planet's magnetic field...
		The first pictures from Nasa's Imager for Magnetopause to Aurora Global Exploration (Image) spacecraft are showing for the first time the global ebb and flow of hot, electrified gas (plasma) around the Earth as it is wafted by the solar wind.
	www.mimihu.com /astronomy/magnetopause.html (240 words)

	Concerning the Shape of the Magnetopause
		[1991] assumed that the magnetopause was an ellipse with a focus fixed at Earth whose dimensions varied self-similarly with respect to the solar wind dynamic pressure.
		In addition, their results indicated that the effects of the IMF upon the location of the subsolar magnetopause are greater during periods of high solar wind dynamic pressure than during periods of low solar wind dynamic pressure, in contrast to expectations based on Equation 3 above and the results obtained by Roelof and Sibeck [1993].
		We forced the locations of the solid curves for the dayside and nightside magnetopause to match at the terminator by renormalizing the shape of the dayside magnetopause to a solar wind dynamic pressure of 2.04 nPa, rather than the value of 2.5 nPa used by Petrinec and Russell [1995].
	www.agu.org /revgeophys/sibeck01/node3.html (1904 words)

	Direct Observation Of 3D Magnetic Reconnection
		Magnetic reconnection on the Earth's magnetopause is considered to be the most efficient mechanism for solar material to penetrate the Earth's magnetic shield.
		In the direction of the Sun, the magnetopause "nose" is located at about 10 RE from the Earth's center (1 RE = 6378 km - the Earth's equatorial radius), which is about 1/6th of the distance to the moon.
		On 30 June 2001, the Cluster spacecraft were straddling the magnetopause in the dawn sector, under quiet solar wind conditions and a slightly northward IMF.
	www.spacedaily.com /news/earth-magnetic-05c.html (2564 words)

	Dayside Magnetopause Models (ResearchIndex)
		Abstract: A review of empirical data-based models of the magnetopause and a comparative analysis are given with special attention to the dynamics of the dayside boundary.
		Recently different research groups have presented new magnetopause models as an alternative to the model of Roelof and Sibeck (1993).
		All models have a greater parametric extent than the model of Roelof and Sibeck and allow prediction of the magnetopause location during extreme solar wind and IMF conditions.
	citeseer.ist.psu.edu /340920.html (415 words)

	INITIAL ISEE MAGNETOMETER RESULTS: MAGNETOPAUSE OBSERVATIONS
		If the magnetopause were stationary during this crossing, it would have a thickness of 2200 km, the distance travelled by the spacecraft along the normal from 16:59 to 17:15.
		Thus, this magnetopause is evidently the thickest traversed on this pass, being at least ~960 km thick.
		As indicated on Figure 9 the boundary layer is detached from the magnetopause on this orbit.
	ssc.igpp.ucla.edu /personnel/russell/papers/151 (10533 words)

	The Magnetopause
		For instance, when the boundary is hit by a fast flow from a coronal mass ejection, the "nose" is pushed in, occasionally (a few times a year, usually) even past the synchronous orbit at 6.6 RE.
		About 2 RE ahead of the magnetopause is a standing shock front, like the one formed ahead of a supersonic bullet or airplane.
		The absence of a strong field to hold off the solar wind means that these are "weak spots" on the magnetopause, and solar wind plasma penetrates there to fill two funnel-shaped regions.
	www.geophys.washington.edu /Space/ESS205/Education/wmpause.html (1055 words)

	ESA Science & Technology: Direct observation of 3D magnetic reconnection
		Variations observed in the solar wind are manifested as "waves" along the bow shock and the magnetopause.
		The magnetopause was found to be located between the SC3 satellite in the magnetosphere and the three other Cluster spacecraft in the magnetosheath (SC1, SC2 and SC4).
		All quantities are displayed in the boundary normal (L, M, N) frame, with N normal to the magnetopause or MP (pointing towards the magnetosheath), L in the plane containing N and the average magnetospheric field, M completing the system.
	sci.esa.int /science-e/www/object/index.cfm?fobjectid=36447 (3033 words)

	Solar Storms and You: Classroom Activities
		The location of the magnetopause at any given time depends on the balance between the pressure exerted by the solar wind on the magnetosphere pushing in and the pressure of the particles within the magnetosphere pushing out.
		Determining the location of the magnetopause is important to scientists (and people in general!), because knowing where the magnetopause is and how its location responds to changes in solar wind activity will help us understand the connection between what happens on the sun and the consequences for us here on Earth.
		For example, if the general direction to the magnetopause is between O' and 180', the x- component antenna registers a.29 microvolt induced voltage, the y-component antenna registers a.50 microvolt induced voltage and the voltages are in phase, then the signal is reflecting from a direction of 120 degrees.
	image.gsfc.nasa.gov /poetry/workbook/pine2.html (2642 words)

	EMPIRICAL MODEL OF THE DAYSIDE MAGNETOPAUSE (Site not responding. Last check: 2007-10-22)
		Dayside magnetopause model is presented alternative to well- known Roelof and Sibeck model.
		The first is due to geosynchronous satellite magnetopause crossings added to the basic data on high-apogee crossing.
		There were found from geosynchronous data analysis an asymmetric dayside magnetopause shape during disturbed solar wind condition and the pressure balance change manner during strong negative Bz.
	www.sinp.msu.su /eng/scienceinc/publicat/abstracts/96-37-444.html (113 words)

	Modelling signatures of pulsed magnetopause reconnection in cusp ion dispersion signatures seen at middle altitudes
		It is shown that the open magnetosphere model can reproduce both the down-going and the up-going magnetosheath ions seen in the cusp and mantle regions by the Polar satellite at middle altitudes.
		The pass studied shows a series of discontinuities in the ion dispersion, most of which are shown to arise from pulses of magnetopause reconnection rate.
		A total of 9 pulses are detected in an interval estimated to be about 30 min long, giving a mean repetition period of about 3 min: they vary in length between 0.5 min and 3.5 min and are separated by periods of much slower reconnection of duration 1–3 min.
	dx.doi.org /10.1029/98GL00185 (255 words)

	AGU Web Site: A Beginner's Guide to the Earth's Magnetosphere
		In Figure 1a, the interplanetary magnetic field is compressed against the magnetopause and draped over it by the flow, but ultimately the field lines slip around the "sides" of the magnetosphere, frozen into the magnetosheath plasma.
		When the frozen-in condition is relaxed, the field will diffuse relative to the plasma in the magnetopause, allowing the interplanetary and terrestrial field lines to connect through the boundary, as shown in Figure 1b.
		However, it is the breakdown of this picture at the 10–20% level due to reconnection at the magnetopause that is critical to the Earth's magnetospheric dynamics.
	www.agu.org /sci_soc/cowley.html (3002 words)

	IRFU, Magnetopause (Site not responding. Last check: 2007-10-22)
		The idea of the session is to look at the magnetopause from small scales (electron gyroradius and electron inertial length) up to mesoscales (ion gyroradius and ion inertial length).
		The topics of interest could be the structure of the electron (if found) and ion diffusion regions, small scale current sheets, different waves (e.g.
		Magnetopause splinter session from Cluster Workshop I. Data plots
	www.cluster.irfu.se /magnetopause (408 words)

	Close-Up of Colliding Magnetic Fields
		In a narrow region at the center of the magnetopause, high-pressure electrons should also diffuse and eject upwards and downwards, propelled by a combination of like-charge (Coulomb) repulsion and the energy acquired from the reconnection process.
		The magnetopause's particle flows generate complex electric and magnetic fields, but until recently, even space-based studies could not resolve the central region well, says Forrest Mozer of the University of California at Berkeley.
		That's where the surprise came in: some of the electrons were moving toward the central magnetopause where they were expected to form a jet aimed away from it.
	focus.aps.org /story/v9/st30 (497 words)

	The Magnetopause
		For instance, when the boundary is hit by a fast flow from a coronal mass ejection, the "nose" is pushed in, occasionally (a few times a year, usually) even past the synchronous orbit at 6.6 R
		It follows that near the magnetopause, field lines located equatorward of the cusp are slanted northward and point away from the Sun, while lines tailward of the cusp slant southward and point towards the Sun.
		The magnetopause is usually further away, but at times of high solar wind pressure, "Polar" has found itself in the cusp region and even outside the magnetopause.
	www-spof.gsfc.nasa.gov /Education/wmpause.html (1267 words)

	solarwindglossary (Site not responding. Last check: 2007-10-22)
		Magnetosheath--the region between the magnetopause and the bow shock, containing solar wind which has been slowed down by passage through the bow shock.
		As the magnetosheath plasma streams away from the bow shock, it gradually regains its former velocity.
		Magnetosphere--The region around Earth, bounded by the magnetopause, whose processes are dominated by the Earth´s magnetic field.
	edmall.gsfc.nasa.gov /99invest.Site/SUN-EARTH1/slrwnd/solarwindglossary.html (482 words)

	Artificial Neural Network Model of the Dayside Magnetopause: Physical Consequences. (ResearchIndex) (Site not responding. Last check: 2007-10-22)
		Empirical model of the dayside magnetopause developed by means of Artificial Neural Network (ANN) package `NeuroShell 2` is discussed.
		ANN model describes 3D shape of the magnetopause as a function of four external parameters: solar wind velocity, density, B y and B z components of interplanetary magnetic field.
		The model shows that the magnetopause shape has the dawn-dusk asymmetry under any solar wind conditions independently on the B y direction.
	citeseer.ist.psu.edu /262452.html (282 words)

	Occurrence probability, width and number of steps of cusp precipitation for fully pulsed reconnection at the dayside ...
		We discuss the characteristics of magnetosheath plasma precipitation in the ‘‘cusp’’ ionosphere for when the reconnection at the dayside magnetopause takes place only in a series of pulses.
		We use FTE observation statistics to predict, for this case of entirely pulsed reconnection, the occurrence frequency, the distribution of latitudinal widths, and the number of ion dispersion steps of the cusp precipitation for a variety of locations of the reconnection site and a range of values of the local de-Hoffman Teller velocity.
		We show that the best test of the relative frequency of these three types of reconnection is to survey the distribution of steps in the cusp ion dispersion characteristics.
	dx.doi.org /10.1029/94JA02197 (346 words)

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