ULF waves: the main periodicities and their relationships with solar wind structures and magnetospheric electron flux

Tuesday, 15 December 2015
Poster Hall (Moscone South)
Tommaso Alberti1, Mirko Piersanti2, Fabio Lepreti1, Antonio Vecchio1, Umberto Villante2 and Vincenzo Carbone3, (1)University of Calabria - Ponte P. Bucci, Rende, Italy, (2)University of L'Aquila, L'Aquila, Italy, (3)Università della Calabria, Dept di Fisica, Arcavacata di Rende, Italy
We use high latitude ULF wave power in the range 2-7 mHz (Pc5 geomagnetic micropulsations), solar wind speed and dynamic pressure, and relativistic magnetospheric electron flux (E > 0.6 MeV),
in the period January - September 2008, in order to detect typical periodicities and physical mechanisms involved into the solar wind-magnetosphere coupling
during the declining phase of the 23th solar cycle. Using the Empirical Mode Decomposition (EMD) and applying a statistical test and cross-correlation analysis,
we investigate the timescales and the physical mechanisms involved into the solar wind-magnetosphere coupling.
Summarizing, we obtain the following results:
1. We note the existence of two different timescales into the four datasets which are related to the short-term dynamics, with a characteristic timescale τ<3 days, and to the longer timescale dynamics, with a timescale between 7 and 80 days. The short-term variations could be related to the fluctuations around a characteristic mean value, while longer timescales dynamics can be associated with solar rotational periodicity and mechanisms regarding the occurrence of high-speed streams and corotating interaction regions but also with stream-stream interactions and synodic solar rotation.
2. The cross-correlation analysis highlights the relevant role of the dynamical coupling between solar wind and magnetosphere via pressure balance and direct transfer of compressional waves into the magnetosphere. Moreover, it shows that the Kelvin-Helmholtz instability is not the primary source of geomagnetic ultra-low frequency wave activity. These results are in agreement with previous works [Engebretson et al, 1998].
3. The cross-correlation coefficient between Pc5 wave power and relativistic electron flux longscale reconstructions shows that Pc5 wave activity leads enhancements in magnetospheric electron flux to relativistic energy with a characteristic time delay of about 54 hours, which is in agreement with the lag of about 2 days found by [Mann et al., 2004].