Forward modelling to determine the observational signatures of white-light imaging and interplanetary scintillation for the propagation of an interplanetary shock in the ecliptic plane - Astrophysics > Solar and Stellar AstrophysReportar como inadecuado




Forward modelling to determine the observational signatures of white-light imaging and interplanetary scintillation for the propagation of an interplanetary shock in the ecliptic plane - Astrophysics > Solar and Stellar Astrophys - Descarga este documento en PDF. Documentación en PDF para descargar gratis. Disponible también para leer online.

Abstract: Recent coordinated observations of interplanetary scintillation IPS andstereoscopic heliospheric imagers HIs are significant to continuously trackthe propagation and evolution of solar eruptions throughout interplanetaryspace. In order to obtain a better understanding of the observationalsignatures in these two remote-sensing techniques, the magnetohydrodynamics ofthe macro-scale interplanetary disturbance and the radio-wave scattering of themicro-scale electron-density fluctuation are coupled and investigated using anewly-constructed multi-scale numerical model. This model is then applied to acase of an interplanetary shock propagation within the ecliptic plane. Theshock could be nearly invisible to an HI, once entering the Thomson-scatteringsphere of the HI. The asymmetry in the optical images between the western andeastern HIs suggests the shock propagation off the Sun-Earth line. Meanwhile,an IPS signal, strongly dependent on the local electron density, is insensitiveto the density cavity far downstream of the shock front. When this cavity orthe shock nose is cut through by an IPS ray-path, a single speed component atthe flank or the nose of the shock can be recorded; when an IPS ray-pathpenetrates the sheath between the shock nose and this cavity, two speedcomponents at the sheath and flank can be detected. Moreover, once a shockfront touches an IPS ray-path, the derived position and speed at theirregularity source of this IPS signal, together with an assumption of a radialand constant propagation of the shock, can be used to estimate the laterappearance of the shock front in the elongation of the HI field of view. Theresults of synthetic measurements from forward modelling are helpful ininferring the in-situ properties of coronal mass ejection from realobservational data via an inverse approach.



Autor: Ming Xiong 1, A. R. Breen 1, M. M. Bisi 1, M. J. Owens 2, R. A. Fallows 1, G. D. Dorrian 3, J. A. Davies 4, P. Thomasson 5 1 Aber

Fuente: https://arxiv.org/







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