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During 3 seasons of PAIPS (Pulsating Aurora Imaging System) photometers at Verkhnetulomsky observatory (VTL, CGM coordinates: 65.49 N, 110.06 E) operation a number of events which represent a series of short bright bursts in a 300–400 nm wavelength range (UV-microbursts) was measured. It is a most transient form of auroral emission which can be caused by high energy electrons microbursts precipitation. UV-microbursts series duration ranges from 10 s to \(\sim \) 1 h. Time interval between pulses is not constant and varies in a range between 100 ms and 5 s. To clarify the origin of UV-microbursts analyses of geomagnetic conditions, including K \(_\textrm{P}\) -index, interplanetary magnetic field, global structure of field-aligned currents and ionospheric equivalent currents, was done. It was shown that in most cases UV-microbursts are observed during weakly disturbed geomagnetic conditions (average K \(_\textrm{P}\) index is 1 \(^+\) for the first observation season and 3 \(^{-}\) for the second season) at the evening sector of MLT. These events are associated with the weak geomagnetic storm recovery phase (SYM-H index about 100 nT). Based on these analyses a classification of the UV-microbursts observational conditions is suggested and discussed in the manuscript.

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Geomagnetic Conditions During UV-Microbursts Detected by PAIPS Photometer in the Auroral Zone

  • 会议论文

  • 发表日期：

    2026年

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  • Pavel Klimov,
  • Andrey Kotikov,
  • Vera Nikolaeva,
  • Konstantin Shchelkanov

摘要

During 3 seasons of PAIPS (Pulsating Aurora Imaging System) photometers at Verkhnetulomsky observatory (VTL, CGM coordinates: 65.49 N, 110.06 E) operation a number of events which represent a series of short bright bursts in a 300–400 nm wavelength range (UV-microbursts) was measured. It is a most transient form of auroral emission which can be caused by high energy electrons microbursts precipitation. UV-microbursts series duration ranges from 10 s to \(\sim \) 1 h. Time interval between pulses is not constant and varies in a range between 100 ms and 5 s. To clarify the origin of UV-microbursts analyses of geomagnetic conditions, including K \(_\textrm{P}\) -index, interplanetary magnetic field, global structure of field-aligned currents and ionospheric equivalent currents, was done. It was shown that in most cases UV-microbursts are observed during weakly disturbed geomagnetic conditions (average K \(_\textrm{P}\) index is 1 \(^+\) for the first observation season and 3 \(^{-}\) for the second season) at the evening sector of MLT. These events are associated with the weak geomagnetic storm recovery phase (SYM-H index about 100 nT). Based on these analyses a classification of the UV-microbursts observational conditions is suggested and discussed in the manuscript.