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\begin{document}

\title{The geologically recent areas as one key target for identifying active
volcanism on Venus.}



\author[1]{Piero D'Incecco}%
\author[2]{Justin Filiberto}%
\author[3]{Ivan Lopez Ruiz-Labranderas}%
\author[4]{Gabriel L. Eggers}%
\author[5]{Gaetano Di Achille}%
\author[6]{Goro Komatsu}%
\author[7]{Dmitry Gorinov}%
\author[8]{Carmelo Monaco}%
\author[9]{Simone Aveni}%
\author[10]{Nicola Mari}%
\author[11]{Matthew Blackett}%
\author[12]{Marco Mastrogiuseppe}%
\author[1]{Marco Cardinale}%
\author[13]{Mayssa El Yazidi}%
\affil[1]{National Institute for Astrophysics (INAF) - Astronomical Observatory of Abruzzo, Teramo, Italy}%
\affil[2]{NASA JSC}%
\affil[3]{Rey Juan Carlos University}%
\affil[4]{4Lunar and Planetary Institute, USRA, 3600 Bay Area Boulevard, Houston, TX 77058, USA}%
\affil[5]{Istituto Nazionale di Astrofisica}%
\affil[6]{International Research School of Planetary Sciences}%
\affil[7]{Space Research Institute of the Russian Academy of Sciences (IKI)}%
\affil[8]{University of Catania}%
\affil[9]{Centre for Agroecology, Water and Resilience (CAWR), Coventry University, UK}%
\affil[10]{University of Pavia}%
\affil[11]{School of Energy, Construction and Environment, Coventry University}%
\affil[12]{La Sapienza Università di Roma}%
\affil[13]{Center for Studies and Activities for Space}%


\vspace{-1em}



  
  \date{May 22, 2024}


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\selectlanguage{english}
\begin{abstract}
The recently selected NASA VERITAS and DAVINCI missions, the ESA
EnVision, the Roscosmos Venera-D will open a new era in the exploration
of Venus. One of the key targets of the future orbiting and in-situ
investigations of Venus is the identification of volcanically active
areas on the planet. The study of the areas characterized by recent or
ongoing volcano-tectonic activity can inform us on how volcanism and
tectonism are currently evolving on Venus. Following this key target,
the manuscript by Brossier et al. (2022)
(https://doi.org/10.1029/2022GL099765) extends the successful approach
and methodology used by previous works to Ganis Chasma in Atla Regio. We
comment here on the main results of the manuscript published by Brossier
et al. (2022) (https://doi.org/10.1029/2022GL099765) and discuss the
important implications of their work for the future orbiting and in-situ
investigation of Venus. Their results add further lines of evidence
indicating possibly recent volcanism on Venus.%
\end{abstract}%



\sloppy


\textbf{The geologically recent areas as one key target for identifying
active volcanism on Venus.}

P. D'Incecco\textsuperscript{1}, J. Filiberto\textsuperscript{2}, I.
L\selectlanguage{ngerman}ópez\textsuperscript{3}, G. L. Eggers\textsuperscript{4}, G. Di
Achille\textsuperscript{1}, G. Komatsu\textsuperscript{5}, D. A.
Gorinov\textsuperscript{6}, C. Monaco\textsuperscript{7,8}, S.
Aveni\textsuperscript{9}, N. Mari\textsuperscript{10}, M.
Blackett\textsuperscript{9}, M. Mastrogiuseppe\textsuperscript{11}, M.
Cardinale\textsuperscript{1}, M. El Yazidi\textsuperscript{12}.

\emph{\textsuperscript{1}National Institute for Astrophysics (INAF) -
Astronomical Observatory of Abruzzo, Teramo, Italy
(piero.dincecco@inaf.it); \textsuperscript{2}Astromaterials Research and
Exploration Science (ARES) Division, X13, NASA Johnson Space Center,
Houston, TX, 77058, USA; \textsuperscript{3}Departamento de Biología,
Geología, Física y Química Inorgánica. Universidad Rey Juan Carlos,
Madrid, Spain; \textsuperscript{4}Lunar and Planetary Institute, USRA,
3600 Bay Area Boulevard, Houston, TX 77058,
USA;\textsuperscript{5}International Research School of Planetary
Sciences, Università G. d'Annunzio, Pescara, Italy;
\textsuperscript{6}Space Research Institute of the Russian Academy of
Sciences, Moscow, Russia;\textsuperscript{7}Dipartimento di Scienze
Biologiche Geologiche e Ambientali, Università di Catania, Italy;
\textsuperscript{8}Istituto Nazionale di Geofisica e Vulcanologia,
Osservatorio Etneo---Sezione di Catania, Italy;
\textsuperscript{9}Centre for Agroecology, Water and Resilience (CAWR),
Coventry University, UK;\textsuperscript{10}Department of Earth and
Environmental Sciences, University of Pavia, 27100 Pavia, Italy;
\textsuperscript{11}``La Sapienza'' University of Rome, Rome, Italy;
\textsuperscript{12}Center for Studies and Activities for Space ''G.
Colombo''- CISAS, University of Padova, Italy.}

Keywords: Solar System, Venus, Volcanism, Geology, Spectroscopy

\textbf{Abstract}

The recently selected NASA VERITAS and DAVINCI missions, the ESA
EnVision, the Roscosmos Venera-D will open a new era in the exploration
of Venus. One of the key targets of the future orbiting and in-situ
investigations of Venus is the identification of volcanically active
areas on the planet. The study of the areas characterized by recent or
ongoing volcano-tectonic activity can inform us on how volcanism and
tectonism are currently evolving on Venus. Following this key target,
the manuscript by Brossier et al. (2022)
(\emph{https://doi.org/10.1029/2022GL099765} ) extends the successful
approach and methodology used by previous works to Ganis Chasma in Atla
Regio. We comment here on the main results of the manuscript published
by Brossier et al. (2022) (\emph{https://doi.org/10.1029/2022GL099765})
and discuss the important implications of their work for the future
orbiting and in-situ investigation of Venus. Their results add further
lines of evidence indicating possibly recent volcanism on Venus.

\textbf{The importance of identifying volcanically active areas in the
future exploration of Venus}

The exploration of Venus will go through a new golden era thanks to the
recently selected NASA Venus Emissivity, Radio Science, InSAR,
Topography, and Spectroscopy (VERITAS) (Smrekar et al., 2020) and Deep
Atmosphere Venus Investigation of Noble gases, Chemistry, and Imaging
(DAVINCI) (Garvin et al., 2022) missions, the ESA EnVision mission
(Ghail et al., 2020), and the Roscosmos Venera-D mission (Zasova et al.,
2019). Moreover, other two missions are currently being evaluated for
selection: the ISRO Shukrayaan-1 mission (i.e., Haider et al., 2018;
Sundararajan, 2021) and the Chinese VOICE mission (e.g., Wang et al.
2022). These missions will focus on the analysis of the chemical
composition of the atmosphere and the geologic features of Venus.

One of the main targets of the future missions to Venus will be the
identification of potentially volcanically active areas on Venus.
Identifying the locations of possibly active volcanism with its related
composition is crucial to estimate energy and volatile budget on Venus,
that is of great importance to understand the geodynamic evolution of
Venus and the terrestrial planets. Evidence of ongoing volcanism can
give us clues in the debate between catastrophic (i.e., Schaber et al.,
1992; Basilevsky and Head, 1998; Romeo and Turcotte, 2010) and
equilibrium resurfacing (i.e., Phillips et al., 1992; Guest and Stofan,
1999; O'Rourke et al., 2014), indicating how volcanic and tectonic
activity is currently evolving on Venus (e.g., Weller and Kiefer 2020).
The analysis of recently erupted (chemically unweathered) lava flows
will also provide useful information about the volatile content of the
mantle of Venus (e.g., Filiberto 2014). We comment here the results of
the work by Brossier et al. (2022)
(\emph{https://doi.org/10.1029/2022GL099765}) and the related
implications for the future orbiting and in-situ investigations of
Venus.

As observed by previous studies (e.g., Pettengill et al., 1992), the
presence of high dielectric (ferroelectric) minerals can increase the
radar reflectivity and lower the radar emissivity on Venus. It is
observed that some minerals (e.g., perovskite, chloroapatite) can lower
the emissivity even at anomalously low altitudes. Theoretical studies
indicate that the high dielectric minerals can be formed over the time
by the interactions between the surface and lower atmosphere, also known
as chemical weathering (e.g., Zolotov 2019). In this way, dielectric
measurements on Venus can be used as a potential chronometer to
constrain the age of surface materials.

Brossier et al. (2022) (\emph{https://doi.org/10.1029/2022GL099765})
analyze the radar emissivity excursions of seven different sites at
Ganis Chasma, four of which already studied by Shalygin et al. (2015)
using Venus Monitoring Camera (VMC) data of the Venus Express, while
other three sites were selected separately for comparison (Fig. 1).
Their results show that for a given (range of) altitude and temperature,
the emissivity excursions do not occur uniformly over all the analyzed
surface materials (Fig.2). This implies that, in the study area, the
observed emissivity excursions are mainly controlled by the presence (or
absence) of distinct ferroelectric minerals with high dieletric
constant. Based on the magnitude of the observed radar emissivity
excursions of the seven different sites, the authors conclude that sites
1, 3, and 4 may be characterized by unweathered and thus extremely young
surface materials where high dielectric minerals have not yet been
formed.

Similarly, using a holistic approach, other recent studies have combined
laboratory results, geologic interpretation, and Venus Express VIRTIS 1
micron surface emissivity data to provide additional lines of evidence
for recently or possibly ongoing volcano-tectonic activity at Idunn
Mons, the major volcanic structure of Imdr Regio on Venus (D'Incecco et
al., 2017, 2021a,b,c; Filiberto et al., 2020., 2021; Cutler et al.,
2020; López et al., 2022). Combining this new work with previous studies
by Brossier et al., (2020) and Brossier and Gilmore (2021), this
demonstrates that the Magellan dataset is able to provide important
clues about the materials on the surface, which can be used as a
potential chronometer for the surface age of Venus. The results of this
manuscript are extremely relevant to our understanding of how volcanic
processes are currently acting on Venus. Further, these models can be
tested with the upcoming fleet of missions expected to arrive at Venus
in the next decade.\selectlanguage{english}
\begin{figure}[H]
\begin{center}
\includegraphics[width=0.70\columnwidth]{figures/image1/image1}

\end{center}
\end{figure}

Figure 1: Ganis Chasma (192\selectlanguage{ngerman}°E, 18°N) showing Magellan Synthetic Aperture
Radar image (gray scale) and the main morphologic features. The seven
sites of interest are outlined in red. Morphologic features are mapped
after Ivanov and Head (2011): Ganis Chasma (rift zone), Sitwell crater
(with its parabola), Bashkirtseff crater, Yolkai-Estsan Mons, and
surrounding tesserae. Maps have a simple cylindrical projection and
north is up. \emph{From Brossier et al., 2022} .\selectlanguage{english}
\begin{figure}[H]
\begin{center}
\includegraphics[width=0.70\columnwidth]{figures/image2/image2}

\end{center}
\end{figure}

Figure 2: (a) Elevation versus emissivity plots obtained for the studied
sites. Dashed lines in plots are mean global values of emissivity at
0.85 (vertical, black), and planetary radius at 6,051.8 km (horizontal,
gray). (b) Magnitude of emissivity excursions (percent change from
global average value of 0.85) detected in each site versus corresponding
altitude and temperature. Temperatures are given by the Vega 2 lander
data (Brossier et al., 2020; Lorenz et al., 2018; Seiff,
1987).\emph{From Brossier et al., 2022} .

The wealth of data to be provided by the future missions will tell us
more about ongoing volcanic activity on Venus. For this reason, it is
crucial to select a number of relevant volcanically and tectonically
active areas on Earth as suitable Venus's analogues. To this regard,
Project ``Analogues for VENus's GEologically Recent Surfaces'' aims to
create a list of suitable analogue volcanic sites on Earth, which can
help us to: i) collect spectral signatures from lava flow samples on
Earth, whose chemical composition is known, to compare with the spectra
to be provided by the future investigations of Venus; ii) analyze radar
backscattering over volcanically active areas on Earth to check how to
evaluate changes in the areal extent of the lava flows in short amounts
of time due to the effect of possibly ongoing eruptions; and iii) use
easily accessible volcanic sites on Earth as test areas for drilling
operations and in-situ elemental analyses. As a first analogue site for
Project AVENGERS, preliminary studies are currently being conducted on
Mount Etna, one of the most active and well monitored volcanoes on
Earth. Building off this, studying active and recently active volcanism
on the Earth is vital to test models for Venus exploration, such as
Brossier et al. (2022) in order to be able to constrain potentially
active volcanism and tectonism on Venus with the future missions due to
arrive and make repeated measurements over the same surface previously
measured by Magellan.

\textbf{Data Availability Statement}

For this commentary article, no new data were used. The data we
commented in this article come from the previously published research by
Brossier et al. (2022), on this journal.

\textbf{Acknowledgements}

This work was supported by the ASI/INAF agreement 2022-15-HH.0.

D.G. was supported by the program \#\selectlanguage{russian}АААА-А18-118052890092-7 of the
Ministry of High Education and Science of Russian Federation.

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