The Wave Properties of Coronal Bright Fronts Observed Using SDO/AIA

Coronal bright fronts (CBFs) are large scale wavefronts that propagate though the solar corona at hundreds of kilometers per second. While their kinematics have been studied in detail, many questions remain regarding the temporal evolution of their amplitude and pulse width. Here, contemporaneous high cadence, multi-thermal observations of the solar corona from the Solar Dynamic Observatory (SDO) and Solar TErrestrial RElations Observatory (STEREO) spacecraft are used to determine the kinematics and expansion rate of a CBF wavefront observed on 2010 August 14. The CBF was found to have a lower initial velocity with weaker deceleration in STEREO observations compared to SDO (∼340 km s−1 and −72 m s−2 as opposed to ∼410 km s−1 and −279 m s−2). The CBF kinematics from SDO were found to be highly passband-dependent, with an initial velocity ranging from 379±12 km s−1 to 460±28 km s−1 and acceleration ranging from −128±28 m s−2 to −431±86 m s−2 in the 335 Å and 304 Å passbands respectively. These kinematics were used to estimate a quiet coronal magnetic field strength range of ∼1–2 G. Significant pulse broadening was also observed, with expansion rates of ∼130 km s−1 (STEREO) and ∼220 km s−1 (SDO). By treating the CBF as a linear superposition of sinusoidal waves within a Gaussian envelope, the resulting dispersion rate of the pulse was found to be ∼8–13 Mm s−1. These results are indicative of a fast-mode magnetoacoustic wave pulse propagating through an inhomogeneous medium. Subject headings: Sun: Corona—Sun: magnetic topology—waves Astrophysics Research Group, School of Physics, Trinity College Dublin, Dublin 2, Ireland ar X iv :1 10 9. 58 97 v1 [ as tr oph .S R ] 2 7 Se p 20 11