A solar-wind-driven empirical model of Pc3 wave activity at a mid-latitude location

Lotz, S.; Heilig, B.; Sutcliffe, P.

doi:https://doi.org/10.5194/angeo-33-225-2015

Articles | Volume 33, issue 2

https://doi.org/10.5194/angeo-33-225-2015

© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.

https://doi.org/10.5194/angeo-33-225-2015

© Author(s) 2015. This work is distributed under
the Creative Commons Attribution 3.0 License.

Articles | Volume 33, issue 2

Regular paper

|

26 Feb 2015

Regular paper |

| 26 Feb 2015

A solar-wind-driven empirical model of Pc3 wave activity at a mid-latitude location

S. Lotz, B. Heilig, and P. Sutcliffe

Related authors

Spectral structure of Pc3–4 pulsations: possible signatures of cavity modes

P. R. Sutcliffe, B. Heilig, and S. Lotz

Ann. Geophys., 31, 725–743, https://doi.org/10.5194/angeo-31-725-2013,https://doi.org/10.5194/angeo-31-725-2013, 2013

Short summary

This paper describes the development of empirical models that are capable of predicting Pc3 pulsation intensity from solar wind parameters (e.g. plasma flow speed, proton density, and interplanetary magnetic field (IMF) orientation). We also calculate the typical timescales at which different solar wind parameters influence the excitation of these waves: solar wind speed influences pulsation intensity at much longer timescales (about 2 days) than IMF orientation (about 1 hour).