Observations and Models of the Interaction of a Large Red Oval with the Great Red Spot in June-July 2008

Details Observations and Models of the Interaction of a Large Red Oval with the Great Red Spot in June-July 2008 Observations and Models of the Interaction of a Large Red Oval with the Great Red Spot in June-July 2008

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5001s&link_type=abstract

American Astronomical Society, DPS meeting #40, #50.01; Bulletin of the American Astronomical Society, Vol. 40, p.487

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Interactions of large-scale features with the GRS gives us insight of its still poorly known dynamical structure and vortex nature. Typically, the GRS interacts directly with small anticyclones at 20ºS and curved dark disturbances (known as STrD) between latitudes 20ºS and 28ºS. The interaction of large oval anticyclones with the GRS (about half length its size) at latitude 24ºS is rare. Previously we reported such an interaction in the Eastward side of the GRS that lead to a partial absorption and expulsion of the destroyed vortex clouds by the GRS (A. Sánchez Lavega et al., Icarus, 136, 14 - 26 (1998)). Here we report the uncommon interaction of a similar size-vortex with the Westward side of the GRS that occurred in June-July 2008. This vortex attracted some attention due to its marked red colour that compares with the GRS itself and nearby in latitude BA anticyclone. We followed the interaction using images in the visible range coming from the International Outer Planets Watch (IOPW) - PVOL data set (http://www.pvol.ehu.es/). The vortex, which was nearly stationary in System-III, was reached by the GRS West side at the end of June, entering the GRS periphery moving rapidly alongside its southern edge, accelerating and reaching a peak velocity of 120 m/s. The oval became elongated due to hydro-dynamical compression when moving along the narrow channel left between the GRS and BA which were close in longitude. The debris reached the Eastern side of the GRS with part of them being probably entrained by the GRS and with other residuals moving eastward GRS. We present a set of numerical simulations of the interaction using the EPIC code and their results are discussed in terms of the vortices properties.
This work made use of computing facilities at CESCA in Barcelona with the help of MEC.

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