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<ul> <li>Introduction</li> </ul> <p>The characterization of the complex magnetic susceptibility (real and imaginary parts) of rocks is an unexplored tool to constrain the composition, structure and geological history of rocks in surface planetary exploration. We propose the NEWTON susceptometer for the determination of the complex magnetic susceptibility, to provide valuable information about the regolith and surface rocks in rocky bodies of the solar system, to be used as a selection criterion of rocks for sample return missions or for the in-situ scientific studies of the magnetic properties during planetary missions [1]. The instrument is based on AC - inductive methods, and its dynamic range of the real susceptibility covers magnetic susceptibility values for rocks from the Earth, Moon and Mars [2, 3, 4]. The sensor is suitable to be placed on board rovers, or to be used as a portable device during field campaigns and by astronauts in manned space missions. This sensor provides a great advantage compared to available commercial susceptometers due to its robustness, compatibility with the planetary environments and that it does not require sample preparation, but only minimum sample dimensions (<strong>~</strong>50 x 20 x 20 mm). </p> <p>The aim of this work is to test the capability of the instrument in two different scenarios with distinct types of samples representative of a wide susceptibility range: 1) the in-situ real magnetic susceptibility determination in Cerro Gordo volcano, considered as a terrestrial analogue [5]; and 2) the characterization of meteorites from the collection of the Museo Geominero (Madrid, Spain).</p> <p>The first study case consists of an intraplate volcano, with potential similar composition and structure of volcanoes from Mars. The second study case comprises various meteorite samples of different origins. </p> <p>2.1 Terrestrial analogue: Cerro Gordo volcano</p> <p>Cerro Gordo volcano was proposed as a Martian analogue due to its structural similarities with Martian volcanoes. It lies to the SW of Almagro (38°49’13”N/3°44’37”W), within the Campo de Calatrava volcanic region in Spain [6], and is emplaced among Paleozoic host rocks where the Armorican quartzite yields the topographic heights.</p> <p>Cerro Gordo is part of a volcanic lineation, all of olivinic nefelinite composition and thought to have erupted coevally (1.5 ± 0.3 Ma [7]), that follows a NNE-SSW fracture [8]. Its eruptive style varied with time from phreatomagmatic to strombolian and phreatomagmatic again to end with an effusive phase [9]. For this reason the deposits found in the field (pyroclastic surge deposits, lahar facies, scoria and pyroclastic deposits, a lava flow, tuffs, breccias and spatter deposits) are varied in composition and structure, and therefore comprise a large range of magnetic susceptibility values,  making Cerro Gordo an excellent scenario for a demonstration campaign of the susceptometer prototype.</p> <p>2.2 Meteorites</p> <p>A total of 16 meteorites of different compositions, and therefore varied susceptibility ranges, have been measured for this work, 10 aerolites and 6 siderites. The criteria followed was that their volume accomplished the minimum size stated in the introduction. The samples were divided into faces and measured twice in each of them. In the case of the siderites showing a flat polished face with Widmanstätten structures, the polished face was measured in two orthogonal directions to test the possible influence of the internal structural ordering.</p> <ul> <li>Conclusions</li> </ul> <p>Previous results from Cerro Gordo showed the capability of the magnetic susceptibility results to distinguish between different rock deposits. The ongoing work on the collected samples analysis and geological description of the study location is intended to relate the magnetic susceptibility values with the mineral composition of the rocks, enhancing the comprehension of the susceptibility measurements and the structure of the volcano. The measurements on meteorites are currently under analysis, and aim to classify the measured samples as a function of their magnetic susceptibility [10].</p> <p>Acknowledgements:</p> <p>This work has been funded by the Spanish Programme for Research, Development and Innovation under the grants of references ESP2017-88930-R and PID2020-119208RB-I00: MagAres and MINOTAUR, respectively, as well as the European Union Project NEWTON, of grant agreement 730041. JSO is funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement SIGMA no 893304.</p> <p> </p> <p>References:</p> <p>[1] Díaz Michelena et al. 2017, Sensor Actuat A-Phys, vol. 263, pp. 471-479</p> <p>[2] Rochette et al. 2005, Meteoritic and Planetary Science, 40 (4): 529–540</p> <p>[3] Rochette 2010, Earth Planet. Sci. Lett., 292: 383–391.</p> <p>[4] Hunt et al. 2013, Wiley. Online Library. DOI: 10.1029/RF003p0189.</p> <p>[5] Monasterio et al. 2021, Terrestrial Analogs Conference (LPI Contrib. No. 2595)</p> <p>[6] Becerra-Ramírez et al. 2020, Geosciences, 10, 441.</p> <p>[7] Ancoechea & Huertas 2021, J. Iberian Geology (47): 209-223.</p> <p>[8] Ancoechea 1999, Enseñanza de las Ciencias de la Tierra (73): 237-243.</p> <p>[9] González et al. 2010, Aportaciones Recientes en Volcanología 2005-2008: 57-65.</p> <p>[10] Rochette et al. 2003, Meteoritics & Planet. Sci., 38: 251-268.</p>

<p>The main objective of this contribution is to present the evolution of NEWTON novel magnetic susceptometer for planetary exploration, a state of the art sensor for the measurement of the complex magnetic susceptibility developed in the frame of an EU H2020 funded project [1].</p><p>The magnetic susceptibility is a complex parameter dependent on the external magnetic field amplitude, direction and frequency. NEWTON susceptometer has been developed to determine the magnetic susceptibility of rocks and soils, with the capability to determine not only the real part but also the imaginary part of the susceptibility.</p><p>The calibration and validation process for the susceptometer prototype casted very good results in comparison with other commercial and high resolution laboratory devices, reaching a resolution in the order of χ = 10<sup>−4</sup> (I.S. Vol. Susceptibility), representative of Earth, Moon and Mars rocks. The critical parts of the prototype have been subjected to different tests, i.e. vibration and TVT, to verify the capability to withstand the hard environmental conditions of interplanetary missions.</p><p>In this work we discuss the potential contribution of NEWTON instrument on the technical and scientific objectives achievement in future investigations on the Moon, either as payload during in-situ exploration with rovers or in sample return missions, providing a useful tool for fast in place sample analysis.</p><p>There are still open questions regarding Moon’s magnetic field and geological characteristics of the satellite. Most hypotheses to explain the magnetic characteristics and anomalies on the lunar surface invoke a thermally driven core dynamo during its Pre-Nectarian and Nectarian history [2]. However, this theory is problematical given the small size of the core and the required strong magnetic field strength of an ancient dynamo. Further investigations on the lunar samples from missions [3] indicate ancient magnetic fields with intensities of <1 to 120 μT for the period between 4.2 to 4.0 Ga. This huge range of intensities may indicate that the Moon’s magnetic field experienced extreme high temporal variations [2]. Even if considering large uncertainties, dynamo models should consider paleointensities of at least ~35 μT for this high-field period.</p><p>The use of scientific instruments like NEWTON susceptometer in rover exploration missions could shed some light on the ancient dynamo magnetic field, the magnetic and mineral composition of the lunar crust and other unanswered questions from the Moon.</p><p>Acknowledgements:</p><p>This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement No 730041 and the Spanish Programme of Research, Development and Innovation oriented to the challenges of the society under grant ESP2017-88930-R.</p><p> </p><p><strong>References:</strong></p><p>[1] M.Diaz Michelena, J.L Mesa Uña, M. Perez Jimenez, M. Maicas Ramos, P. Cobos Arribas, C. Aroca Hernandez-Ros, Sensors and Actuators, A: Physical, volume 263, pages 471-479 (2017)</p><p>[2] Tikoo, S.M., Weiss, B.P., Cassata, W.S., Shuser, D.L., Gattacceca, J., Lima, E.A., Suavet, C., Nimmo, F. & Fuller, M.D. Earth Planet. Sci. Lett., 404: 89-97 (2014)</p><p>[3] Tsunakawa, H., Takahashi, F., Shimizu, H., Shibuya, H., & Matsushima, M. Icarus 228: 35-53 (2014).</p><p>[3] Fuller, M. (1974). Reviews of Geophysics, 12 – 1, 101-103 (1974)</p>

Volcanoes are typical features of the solar system that offer a window into the interior of planets. Thus, their study can improve the understanding of the interiors and evolution of planets. On Earth, volcanoes are monitored by multiple sensors during their dormant and active phases. Presently, this is not feasible for other planets’ volcanoes. However, robotic vehicles and the recent technological demonstration of Ingenuity on Mars open up the possibility of using the powerful and non-destructive geophysical tool of magnetic surveys at different heights, for the investigation of surfaces and subsurfaces. We propose a methodology with a view to extract information from planetary volcanoes in the short and medium term, which comprises an analysis of the morphology using images, magnetic field surveys at different heights, in situ measurements of magnetic susceptibility, and simplified models for the interpretation of geological structures. This methodology is applied successfully to the study of different examples of the main volcanic zones of the Iberian Peninsula, representative of the Martian intraplate volcanism and similar to Venus domes, as a preparatory action prior to the exploration of the rocky planets’ surfaces.