Abstract

Introduction How does Venus lose the heat? The rates of resurfacing on Venus is lower than the catastrophic event happened 500 My ago which covered 80% of the surface. The low level of ongoing volcanism and tectonism does not explain Venus ́ heat loss [1]. Hot spots contribute less than 5% of Venus ́ heat budget [2].Data from the Magellan mission showed no evidence of global systems of active plate tectonics and the thin lithosphere predicted by these models appears to be inconsistent [3].Recent studies have shown that subduction could possibly occur around large structures called coronas, speci cally around large corona such as Quetzalpetlatl and Artemis [4] Results The study area is located south-east of the tectonic structure called Parga. Venus Express images show high levels of radiation south of Parga, in Themis region [5]. There are also geomorphological and tectonic features denoting high volcanic activity and relatively young age [6]. The high levels in emissivity are interpreted as regions with volcanism type hot spots. Parga is a structure of large dimensions and is characterized by having a high number of coronas [7]. For this work, we measure the emissivity of Parga and Themis region using Venus Express data. We proposed high values of emissivity in new volcanic structure with activity not previously reported. These structures are found around Atete corona, the largest corona in Parga. Conclusions A geological model is proposed that explains the possible relevance of the volcanic activity around these coronas, providing more information and evidence before the possible subduction and liberation of energy on this planet through this mechanism. One of the main dif culties in seeking indirect evidence of subduction and volcanic activity is the lack of satellite image information. Against this scenario, the Atete corona is considered a good candidate to look for signs of volcanic activity and evidence of subduction, because it images of this region are available. Reference [1] Shalygin, E., et al (2015). Geophysical Research Letters, p 4762–4769. [2] Turcotte,D. (1995). Journal of Geophysical Research, 100: 16,931-16,940. [3] Smrekar, S., et al (1997). SCIENCE, 277:1289-1293. [4] Davaille, A., et al (2017). Nature Geoscience, 10(5), 349. [5] Smrekar, S. E., et al (2010). Science, 328(5978):605–608. [6] Airey, M. W., et al (2017). Geophys. Res. Planets, 122, 1626–1649. [7]Martin, P. et al (2007). Journal of Geophysical Research: Planets, 112(E4)