A Model Scenario for Kieserite-Dominated Evaporites in Juventae Chasma, Mars

Abstract

Introduction: Juventae Chasma, located north of Valles Marineris, stretches for approximately 150 km east-west and 250 km north-south. The basin floor lies ~ 5 km and more below the surrounding surface and shows a smooth topography. A large dune field covers the bottom of the basin. Juventae Chasma contains several interior layered deposits (ILD). The four most distinctive deposits have been named from south to north mound A-D by [1, 2]. Several articles have been published discussing the origin and history of monoand polyhydrated sulphate deposits within Juventae Chasma [1-7] based on studies of OMEGA and CRISM data. Formation theories range from a volcanic origin as a result of sub-ice volcanic eruptions [1], lake deposits, delta-deposits [4] and spring deposits [5], to mention a few. The composition of these sulphate bearing mounds has attracted the attention of many scientists because it still hides the information about a paleo-hydrogeological history. Based on the spectral observations of [7] our study presents an additional contribution to the ongoing discussion about the origin of the sulphate deposits within Juventae Chasma with kieserite (MgSO