Position of the source of daylight high-latitude magnetic pulses in the magnetosphere according to DMSP satellite data

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Daytime high-latitude geophysical phenomena provide a ground-based observer with information about processes at the daytime magnetopause and/or in adjacent magnetospheric domains. It is assumed that these phenomena are initiated by changes in the parameters of the interplanetary medium and therefore can be used as a tool for studying the ways in which solar wind energy penetrates through the magnetopause. Such phenomena include magnetic impulses, which are an isolated train of damped oscillations of 2–3 bursts with a repetition period of 8–12 minutes. Using data from the Scandinavian network of magnetometers IMAGE, eight magnetic impulse events were studied for which DMSP satellites flew over the observation area during, shortly before and immediately after the pulse, crossing the boundaries of several domains. Based on ground-based and satellite data, it has been shown that the downward field-aligned current associated with the impulses is located away from the magnetopause. This means that the impulse cannot be considered as an ionospheric trace of a reconnected magnetic flux tube (flux transfer event, FTE) and/or as a traveling convection vortex (TCV). Using more statistics, it has been established that the pulse is preceded by noticeable changes in the By and Bz components of the IMF, while the contribution to the generation of the impulse from the pressure jump and solar wind speed, as well as the Bx component of the IMF, is not obvious. A possible scenario for the initiation of a magnetic pulse by IMF variations is discussed.

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V. Safargaleev

Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS, St. Petersburg Department

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Email: Vladimir.safargaleev@pgia.ru
俄罗斯联邦, St. Petersburg

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2. Fig. 1. (a) − Magnetic pulse on a chain of IMAGE stations (highlighted in gray). The moment of the F16 satellite's flight is shown by an arrow. (b) is the 1D distribution of the equivalent ionospheric current, showing the dynamics of the eastern (+) and western (-) magnetic pulse currents at the meridian of 22° E. (c) is the vortex nature of the equivalent current distribution. The current direction is indicated by arrows.

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3. Fig. 2. (a) − The pattern of precipitation along the satellite's trajectory, indicating the magnetospheric domains three minutes after the start of the pulse. (b) is a fragment of the trajectory F16. The position of the cps/bps boundaries is shown by crosses. The area of bps eruptions is shaded in gray. The dashed line is the geomagnetic latitude (domain boundaries outside the trajectory). The square is the center of the vortex on the meridian 22°E, along which the 1D distribution of the equivalent current was calculated in Fig. 1b.

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4. 3. (a) − The antiphase character of the magnetic field change. The arrow shows the moment when the F17 satellite flew over the IMAGE network. (b) is the dynamics of the eastern (+) and western (-) magnetic pulse currents at the meridian of 22° E. The thin vertical line is the time point for which the equivalent current map was calculated. (c) is a vortex–shaped structure with several centers on the map of the equivalent magnetic pulse current. The current direction is indicated by arrows. (d) is the pattern of precipitation over the observation area according to DMSP F17 data. (e) is a fragment of the F17 trajectory. Crosses are reference points for building a trajectory. The squares are the position of the center of the vortex.

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5. Fig. 4. Variations in the parameters of the interplanetary medium at the frontal point of the shock wave over a period of time, including the observation interval of the magnetic pulse (highlighted in gray, see also Fig. 3a). From top to bottom: the speed and pressure of the solar wind, the three components of the MMP. The lower panel shows a step–by-step magnification of the X-components of the geomagnetic field at the AAE equatorial station.

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6. Fig. 5. Three examples of magnetic pulses (the intervals are highlighted in gray) in the context of changes in the parameters of the interplanetary medium at the frontal point of the shock wave front. From top to bottom: variations in solar wind pressure and velocity, variations in MMP, magnetograms of IMAGE network stations demonstrating the antiphase nature of the magnetic pulse, variations in the geomagnetic field at equatorial stations.

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