bluuebunny/crossref_metadata_2025 huggingface dataset:
MAPPS as a multi-mission and multi-body Science Planning and Simulation Tool for ESA solar system missions
Authors: Muñiz Solaz Carlos , Cardesin-Moinelo Alejandro , Nespoli Federico , Martin Patrick , Marin-Yaseli de la Parra Julia , Merrit Donald , Sierra Mar , Esquej Pilar ,   ESA Planetary Science Operations Centres
Published: September 2022

The Mission Analysis and Payload Planning System (MAPPS) is a multi-mission software system developed during the last 20 years to support the science operations planning for the ESA solar system missions at the European Space Astronomy Centre (ESAC) near Madrid.

Developed initially only to visualise the coverage of MEX experiments onto the Martian surface. The tool has been evolved progressively to satisfy planning requirements for the different missions that have been launched in the last two decades: SMART-1, Venus Express, Rosetta, Mars Express, Exomars TGO, Bepi Colombo, Solar Orbiter, Juice and EnVision.

The planning requirements sometimes are specific to a mission and on other occasions they are contradicting. As an example, consider the power and thermal requirements of a mission like Bepi Colombo, very close to the sun, in contrast to those same requirements for a mission like Juice, very far away. The complexity of these requirement implies that the software needs to be very configurable and continuously adapting to the needs of each mission.

In recent years, there has been the need to extend even further the tool to support multi-body and constellation coordination capabilities.

In the case of Juice, the spacecraft will spend many months orbiting Jupiter and three of its Jovian moons. This has required a big effort to modify the existing features and observations in MAPPS that were initially developed for a central body to be able to cope with several bodies.

In the case of Mars, the arrival of new spacecrafts and rovers has broadened what can be done scientifically as well as opening the international collaboration among agencies. MAPPS has been extended to facilitate the collaboration with other Mars missions, in particular the new  radio-science experiment between MEX-TGO [1], various communication tests between ESA and NASA orbiters, and the regular data relays in support of all surface assets, including the new Chinese Zhurong mission.

Here we present how MAPPS has contributed and supports the Science Ground Segment teams in ESA to achieve their goal of planning scientific operations in an efficient and optimised way, together with the new features implemented for the ever more demanding needs of the new scientific missions.

[1] Cardesin Moinelo, A. et al: First year of coordinated science observations by Mars Express and ExoMars 2016 Trace Gas Orbiter, ICARUS 353, 2021

 
Spins and shapes of V-type asteroids outside the dynamical Vesta family
Authors: Oszkiewicz Dagmara , Troianskyi Volodymyr , Wilawer Emil , Galad Adrian , Marciniak Anna , Skiff Brian , Fohring Dora , Polakis Tom , Geier Stefan , Kwiatkowski Tomasz , Kolenczuk Paweł , Moskovitz Nicholas , Benishek Vladimir , Pray Donald , Shevchenko Vasilij , Kankiewicz Paweł , Hasegawa Sunao ,   SONATA-13
Published: September 2022

Vast majority of known V-type asteroids belong to the dynamical Vesta family. A small number of V-types in the mid and outer parts of the Main Asteroid Belt is considered unrelated to the fossil planetesimal (4) Vesta. These objects have low probability of dynamically evolving from the Vesta family and show spectral properties distinct from typical Vestoids [1-7]. Whether there are V-types unrelated to Vesta (non-Vestoids) in the inner part of the Main Asteroid Belt is still an open question. 

To answer it, we performed a large and long-lasting observing campaign of V-types in the inner Main Belt outside the dynamical Vesta family [8,9]. We determine their rotational properties and compare them with the numerical simulations made by Nesvorny et al. 2008. According to that study 81% of objects evolving from the Vesta family to so-called Cell I (defined by orbital elements 2.2 au<a<2.3 au, 0.05<e<0.2, 0 deg <i<10 deg) and 40% to Cell II (2.32 au <a<2.48 au, 0.05<e<0.2, 2 deg<i< 6 deg) should have retrograde rotations. 

We observed a total of 23 asteroids larger than 5 km in diameter in both of those Cells over multiple apparitions. We determined spins and shapes for 13 of them so far. In Cell I we found only retrograde objects and in Cell II 6 prograde and 2 retrograde objects. With the complete sample we plan to put constraints on the distribution of possible non-Vestoids in the inner Main Belt.

[1] Lazzaro, D. et al., 2000, Science 288, 2033–2035.

[2] Hardersen et al., 2004, 167, Icarus 170–177

[3] Michtchenko et al., 2002, Icarus 158, 343–359.

[4] Fulvio, D. et al, 2018, Planetary and Space Science 164, 37–43.

[5] Ieva, et al. 2016, Monthly Notices of the Royal Astronomical Society 455, 2871–2888.

[6] Ieva, S.et al., 2018, Monthly Notices of the Royal Astronomical Society 479, 2607–2614.

[7] Roig, F. et al. 2008, Icarus 194, 125–136.

[8] Oszkiewicz, D., et al., 2020, Astronomy & Astrophysics 643, A117

[9] Oszkiewicz, D. et al., 2021, Icarus 357, 114158.

[10] Nesvorný, D., et al., 2008, Icarus 193, 85–95.
The D/H ratio in Titan's acetylene from high spectral resolution IRTF/Texes observations
Authors: Bézard Bruno , Vinatier Sandrine , Greathouse Tommy , Giles Rohini , Nixon Conor , Lombardo Nicolas , Jolly Antoine , Despan Daniela
Published: September 2022

In July 2017, we used the Texes high-resolution spectrometer at the NASA Infrared Telescope Facility to observe Titan in the 19.3-µm (519 cm-1) region where the ν4 band of deuterated acetylene (C2HD) is located. Six individual lines were clearly detected with a S/N ratio up to 10. Spectral intervals around 8.0 (745 cm-1) and 13.4 µm (1247 cm-1) were observed during the same run to constrain the disk-averaged temperature profile and acetylene (C2H2) abundance profile respectively. Telluric correction and flux calibration were obtained from observations of asteroid Hygiea. Constraints from Cassini/CIRS observations in 2017 around the sub-Earth latitude were also used to constrain the atmospheric model and check the flux calibration. The D/H ratio is derived from the C2HD/C2H2 abundance ratio. Preliminary results of this analysis indicate a D/H ratio in acetylene around 1.7×10-5 with an uncertainty of about 10%, in agreement with the previous, less precise, determination from Cassini/CIRS measurements. This ratio is slightly larger than that in methane (approximately 1.3×10-5), which suggests some fractionation at work in the photochemical production of acetylene from methane.
Updated Ganymede Mosaic from Juno Perijove 34 Images
Authors: Kersten Elke , Zubarev Anatoly E. , Nadezhdina Irina E. , Roatsch Thomas , Matz Klaus-Dieter , Szczech Claudia Camila
Published: September 2022

1. Introduction

In preparation of the JUICE mission with the primary target Ganymede [1] we generated a new controlled version of the global Ganymede image mosaic from Voyager 1 and 2 and Galileo images [2] based on a new 3D control point network from Zubarev et al., 2016 [3]. In 2021, the Juno mission acquired new Ganymede images with its onboard wide-angle camera JunoCam [4]. We used the best available images from Perijove 34 to integrate them into the global Ganymede mosaic.

2. Image data

On June 7th, 2021, near the end of Juno’s prime mission, the spacecraft flew by Ganymede to obtain four close-ups of the leading side of the moon from an altitude of about 1046 km. The derived image data has been integrated into the control point network of Ganymede to find a global solution for all three datasets. The new control point network consists of 4968 points.

3. Mosaicking

After aligning the Juno images photogrammetrically to fit onto the global Ganymede mosaic from Voyager and Galileo images brightness and contrast corrections have been applied to the Juno images manually to create a consistent look within the global mosaic. The small crater Anat is defining the longitude system at 232° East and the radius is set to 2631.2 km. The updated version of the global Ganymede mosaic will become available at https://janus.dlr.de/ and will be archived at PSA’s GSF.

4. Outlook

With this work we hope to support the JUICE team during pre-arrival investigations and the observation planning of Ganymede.

References

[1] Grasset et al., 2013, Planetary and Space Science, 78, 1-21, DOI: 10.1016/S0032063312003777. [2] Kersten et al., 2021, Planetary and Space Science 206, DOI: 10.1016/j.pss.2021.105310. [3] Zubarev et al., 2016, Solar System Research, 50, 5, 352-360, DOI: 10.1134/S0038094616050087. [4] Hansen et al., 2017, Space Science Reviews, 213, pages 475-506.
A Search for Long-Period Transiting Exoplanets with TESS and CHEOPS
Authors: Tuson Amy ,   CHEOPS Consortium
Published: September 2022

Detecting exoplanets via the transit method is inherently biased towards short-period planets. Due to the nature of its observing strategy, the Transiting Exoplanet Survey Satellite (TESS) is particularly susceptible to this detection bias; only 12% of planets confirmed by TESS have orbital periods longer than 20 days. It’s crucial that we expand this sample of long-period planets to gain a more complete view of the exoplanet population. One way to do this is using duotransits - planet candidates with two observed transits separated by a large gap, typically two years. The true period of the duotransit is unknown, instead they have a discrete set of possible period aliases. We use these aliases to perform targeted follow-up of the duotransit with the CHaracterising ExOPlanets Satellite (CHEOPS), to recover the true period and ultimately confirm the planet. This allows us to find longer-period planets than are typically found by the TESS mission alone. To select the optimal targets for our CHEOPS follow-up we have developed a specialised pipeline that searches for duotransits in the TESS data. We will present this duotransit pipeline and the results from our CHEOPS follow-up program so far. We have discovered 10 long-period exoplanets, including two planets in the TOI-2076 system, all of which have P > 21 days, RP < 5 REarth and Gaia magnitude < 12. Previously there were only 8 exoplanets discovered by TESS in this exciting parameter space, so our work has more than doubled the sample. These small, long-period transiting exoplanets are amenable to radial velocity follow-up and future atmospheric characterisation with the recently launched James Webb Space Telescope (JWST).
Eyes on Mars - Increasing Awareness of UK based Mars Exploration
Authors: Regan Catherine , Patel Priya
Published: September 2022

The UK is currently playing a key role in the development of Mars Exploration, with scientists and engineers working on many current and upcoming missions such as the European Space Agency’s Mars Express satellite (2003 – present) and the upcoming Rosalind Franklin Rover (launch TBD). The camera onboard the Rosalind Franklin Rover was designed, built and tested at the Mullard Space Science Laboratory, part of University College London, in Surrey, England. The rover was also assembled at Airbus in Stevenage. These facts are not well known to the public in the UK, and our public engagement project, Eyes on Mars, aims to increase awareness of UK’s involvement in progressing Mars science and with this, promote STEM education in UK. We received funding from the Science and Technology Facilities Council’s Public Engagement Sparks Award and the Royal Astronomical Society education and outreach grant.

To accomplish this, Eyes on Mars has two main foci – a social media campaign and providing resources to be used in classrooms, youth groups and at home. The social media campaign will showcase short and informal snippets of information that highlights Mars facts and various space careers. It will also include interviews of diverse individuals from across Europe that are in the space sector, specifically, highlighting their paths into STEM careers.

Furthermore, Eyes on Mars has put together a selection of free resources that are available to download or given to participating schools to carry out science curriculum activities in class. We have provided various education videos, worksheets and activity plans, including making your own filter wheel similar to the filter wheel onboard the Rosalind Franklin Rover. All materials for this craft activity are provided by the Eyes on Mars team, and are sent out to schools or groups across the UK. 

Having both come from state-schools in the UK, and not being in the ‘top-set’ for science at school, Catherine Regan and Priya Patel are now PhD students in planetary physics, researching Mars. Both have been told at some point during their education that they weren’t “clever enough” for a career in science, and are now both working on space missions with NASA and the European Space Agency. We want to use Eyes on Mars to be role models for those that may not think they can succeed in science, and to highlight the different possibilities there are for a career in space, especially in the UK.
The Trans-Neptunian Object (19521) Chaos as seen from stellar occultations and photometry observations
Authors: Ortiz Jose L. , Morales Nicolas , Vara-Lubiano Monica , Kretlow Mike , Sicardy Bruno , Santos-Sanz Pablo , Fernandez-Valenzuela Estela , Braga-Ribas Felipe , Desmars Josselin , Duffard Rene , Camargo Julio , Souami Damya , Kilic Yucel , Rommel Flavia , Vieira-Martins Roberto , Assafin Marcelo , Álvarez-Candal Álvaro , Morgado Bruno , Benedetti-Rossi Guga , Gomes-Junior Altair ,   Chaos occultation team
Published: September 2022

Trans-Neptunian Objects (TNOs) are important solar system bodies that carry valuable information on the first stages of our solar system and its evolution. The TNO named (19521) Chaos (formerly known as 1998 WH24) is a large object, presumably in the 600-km size range judging by its approximate absolute magnitude and assuming a typical geometric albedo for a TNO. This is a comparable size to that of the three largest asteroids in the main asteroid belt. Therefore, it is an important body to study and characterize through stellar occultations and through other techniques. On October 20th, 2020, a three-chord stellar occultation was recorded by our team (Vara-Lubiano et al. 2021) within the context of the Lucky Star international collaboration* on stellar occultations by TNOs and other outer solar system bodies, and recently, on January 14th, 2022, another stellar occultation by Chaos has been recorded, whose main preliminary results will be presented. In this case 24 sites participated in the campaign. There were 8 positive detections and 3 near misses. The analysis of this occultation combined with the previous one and with photometry data obtained along 17 years (within our own TNO observing program) will be presented. We expect to derive an accurate size and shape as well as an accurate geometric albedo, which can be compared with radiometric measurements. We also expect to provide constraints on the spin axis orientation. The fact that no satellite around Chaos has been discovered so far means that we do not know the system mass so we cannot infer a bulk density for the body to compare with hydrostatic equilibrium computations, but we can derive other useful constraints.

*Lucky Star (LS) is an EU-funded research activity to obtain physical properties of distant Solar System objects using stellar occultations. LS collaboration agglomerates the efforts of the Paris, Granada, and Rio teams. https://lesia.obspm.fr/lucky-star/ 
Investigating the Global Dust Storm in Mars Year 28 with Mars Express
Authors: Regan Catherine , Coates Andrew , Wellbrock Anne , Haythornthwaite Richard , Jones Geraint , Sánchez-Cano Beatriz , Holmström Mats , Frahm Rudy , Garnier Philippe
Published: September 2022

Global dust storms at Mars engulf the entire planet in a dusty haze, causing increases in temperature and ion escape as dust is lifted up to 80 km in altitude. The two most recent storms occurred in 2007 (Mars Year (MY) 28) and 2018 (MY34), and have been observed by spacecrafts such as Mars Express (MEx). MEx has been operating at Mars since 2004, and has produced a long time-base of plasma measurements from as low as 250 km. Using MEx, we investigate whether the 2007 dust storm has influenced the magnetosphere of Mars by looking at the position of the bow shock and induced magnetospheric boundary, compared to the expected position provided by 3D magnetohydrodynamical models. To identify boundary positions, we use data from the ASPERA-3 instrument (Analyser of Space Plasma and EneRgetic Atoms) onboard MEx, which contains an electron spectrometer (ELS), ion mass analyser (IMA), neutral particle imager (NPI) and neutral particle detector (NPD). For this study, we use data from ELS and IMA. We consider a number of influences on the boundary position, including the solar wind conditions and the crustal fields. Our study period includes time before, during, and after the MY28 global storm, and we expected the bow shock and induced magnetospheric boundary to increase in altitude due to the storm. Out results show that the system is more complex, and multiple influences need to be distinguished to leave any change due to the dust storm itself.
An update on the SPECULOOS project and new results
Authors: Delrez Laetitia ,   SPECULOOS team
Published: September 2022

In the age of JWST, temperate terrestrial exoplanets transiting nearby late-type M dwarfs provide unique opportunities for characterizing their atmospheres, as well as searching for biosignature gases. In this context, the benchmark TRAPPIST-1 planetary system has garnered the interest of a broad scientific community.

The SPECULOOS (Search for habitable Planets EClipsing ULtra-cOOl Stars) project, an exoplanet transit survey targeting a volume-limited (40 pc) sample of about 1700 late-type (M6 and later) dwarfs using a network of 1m-class robotic telescopes, began its scientific operations three years ago. In this talk, I will present an update on the current status of the survey and an overview of recent results.

In particular, I will describe how an efficient synergy with the TESS mission and other ground-based facilities led to the exciting new discovery of two temperate super-Earths transiting a nearby M6 dwarf, with the outer one orbiting in the habitable zone. In terms of potential for atmospheric characterization, we estimate that this planet is the second-most favorable habitable-zone terrestrial planet found so far after the TRAPPIST-1 planets. The discovery of this remarkable system offers another rare opportunity to study temperate terrestrial planets around our smallest and coolest neighbours.
BepiColombo First Mercury Fly-by: first taste of the mission results on investigation of the environment around the planet
Authors: Milillo Anna ,   BERM, MAG-MGF, MPPE, PWI, SERENA and SIXS teams
Published: September 2022

The ESA-JAXA BepiColombo satellite suite has passed by its target planet Mercury for the first time on 1st October 2021. The flyby trajectory was passing Mercury in the southern hemisphere from nightside dusk toward dayside dawn, thus crossing the magnetosheath, the magnetotail, nightside plasma sheet and exiting in dayside dawnward magnetopause and bow shock. It explored, for the first time, regions never observed by other spacecraft in the past. All the instruments able to perform science observations in cruise configurations have been operated providing the first observations of Mercury’s inner southern magnetosphere and surrounding regions. These observations include magnetic fields, solar wind and magnetospheric ions and electrons in different energy ranges, plasma waves, energetic particles and exosphere. During the pass, BepiColombo encountered a low interplanetary magnetic field and low energy solar wind. Unexpected interesting signals have been observed in the solar wind before the magnetospheric bow shock, at the magnetopause inbound as well as in the outbound solar wind. This paper will present a general overview of the observations, just as a first taste of the great results expected from this mission.
Martian Meteoric Mg+: an intercomparison of MAVEN/IUVS observations with simulations using the LMD Mars GCM
Authors: Marsh Daniel , Feng Wuhu , Plane John , Carrillo-Sánchez Juan Diego , Janches Diego , Crismani Matteo , Chaufray Jean-Yves , Forget François , González-Galindo Francisco , Schneider Nicholas
Published: September 2022

The Imaging Ultraviolet Spectrograph (IUVS) on the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission has been used to observe the Mg+ in the upper atmosphere of Mars since 2015. These observations reveal significant diurnal, seasonal and latitudinal variations. For example, a factor of two change in Mg+ occurs during the day at the equator and Mg+ above 100 km decreases across the globe during the Southern Hemisphere summertime.  Possible causes include the influence of photo-chemistry, atmospheric dynamics and the injection rate of meteoric material. To delineate these sources of variability, a 3-dimensional model of the Martian Mg has been developed. The model is based on the Laboratoire de Météorologie Dynamique (LMD) Mars global circulation model (GCM), which is capable of simulating the seasonal cycles in the Martian atmosphere arising from changes in heating rates from orbital geometry and the distribution of dust in the lower atmosphere. The model solves for the dynamics and primary constituents of the atmosphere from the surface to the thermosphere. For this study, the chemistry has been augmented with neutral and ion chemistry for meteoric metals within a CO2 atmosphere, incorporating 7 neutral and 8 ionized Mg-containing species and an additional 42 neutral and ion-molecule reactions. The atmospheric input of meteoric material is specified from seasonal and latitudinal fits to new estimates of the deposition of the ablated metals in the atmosphere. Here we present the first detailed intercomparison of the MAVEN IUV Mg+ observations with simulated Mg+ from the LMD Mars GCM. Model variability is consistent with observations and indicates tropical variability is caused by a combination of photochemistry and vertical transport by atmospheric tides. Comparisons of simulations performed with variable and fixed meteoric input show that the high latitude variations are caused by both seasonal variation in ablation rates and the residual circulation. Finally, we show how Mg+ varies in relation to neutral Mg and the remaining Mg-containing species to determine how Mg+ may be used as a proxy for total Mg variability.
Water-group pickup ions from Europa-genic neutrals orbiting Jupiter 
Authors: Szalay Jamey , Smith Todd , Zirnstein Eric , McComas David , Begley Luke , Bagenal Fran , Delamere Peter , Wilson Robert , Valek Phil , Poppe Andrew , Nenon Quentin , Allegrini Frederic , Ebert Robert , Bolton Scott
Published: September 2022

Water-group gas continuously escapes from Jupiter’s icy moons to form co-orbiting populations of particles, or neutral toroidal clouds. We report the first observations of H2+ pickup ions in Jupiter’s magnetosphere from 13-18 Jovian radii, confirming the presence of a neutral H2 toroidal cloud. Pickup ion densities are consistent with an advecting Europa-genic cloud source. As the observed H2+ ions are originally produced from H2 lost from Europa, the abundance of detected ions allows us to determine that ~1 kg/s of neutral H2 is lost from Europa. Hence, these observations presented here for the first time directly measure ions from a neutral H2 toroidal cloud at Jupiter, prove the cloud provides an additional plasma source in Jupiter’s magnetosphere, and provide the most direct constraints on Europa’s loss of neutral H2 via observations of the neutral toroidal cloud’s primary loss process – pickup ions.
Field line resonances in Ganymede’s magnetosphere observed by Juno
Authors: Martos Yasmina M , Romanelli Norberto , Espley Jared , Connerney Jack , Kotsiaros Stavros
Published: September 2022

On June 7, 2021 Juno performed a close flyby of Ganymede. Here we study the high-resolution magnetic field spectrum which indicates that Juno travelled within Ganymede’s closed magnetic field line region for around 3 minutes during the closest approach. This result is supported by two main facts. 1) The harmonic structure in the spectrum of the high-resolution magnetometer data agrees very well with the frequencies predicted for resonances of a dipole field. 2) The inferred plasma density near the equator at 1.7 RG (L-shell of the closest approach) is approximately 25 amu/cm3, which is much lower than the local density of the plasma sheet near Ganymede (~100 amu/cm3). We also discuss our results together with those obtained by other Juno instruments and theoretical models.
Dune, Waterworld, and Everything in-between: Creating a Titan-like Climate on an Earth-like Planet
Authors: McKinney Matthew , Mitchell Jonathan
Published: September 2022

We recreate a Titan-like climate using an Earth-like global climate model (GCM) by varying a small set of planetary parameters. Understanding the range of possible climate states for Earth-like planets is important for interpreting exoplanet observations and Earth’s own climate history. We find that simply reducing the available water at the surface does not fully reproduce Titan-like conditions. This may indicate that there are many possible “in-between” states an Earth-like planet can have that span the gap between the Earth and Titan climate archetypes. We use three observationally motivated criteria to determine Titan-like conditions: 1) the peak in surface specific humidity is not at the equator, despite it having the warmest annual-mean temperatures (Ádámkovics et al. 2016); 2) the vertical profile of specific humidity in the equatorial column is nearly constant through the lower troposphere (Niemann et al. 2005); and 3) the relative humidity near the surface at the equator is significantly lower than saturation (lower than 60%; Niemann et al. 2005; Tokano et al. 2006). We first limit the available water by placing a continental land strip centered on the equator and varying its width. This mimics Titan’s dry tropics and wet poles, and could be similar to past continental arrangements in Earth’s history. Land strips alone allow some experiments to meet two Titan-like criteria, but none show the near-constant vertical profile of specific humidity. We take three of these land strip widths and vary the rotation period, starting with Earth’s rotation and moving towards Titan’s (16 Earth days). Slowing the rotation results in fewer experiments meeting any of the Titan-like criteria due to increased access to oceanic moisture from the widened Hadley Circulation. For the same three land strip widths and using Earth rotation, we vary the volatility of the condensable via a constant multiplied to the saturation vapor pressure. Titan’s condensable, methane, is more volatile under Titan’s surface conditions than water is on Earth, resulting in high specific humidities. By artificially increasing the saturation vapor pressure, we can approximate this effect without changing the properties of the condensable. Experiments with a volatility constant of 2.5 (the maximum used in this work) meet all three Titan-like criteria, demonstrating that an Earth-like planet can display Titan-like climatology by changing only a few physical parameters.
A CHEOPS-enhanced view of the HD3167 system
Authors: Bourrier Vincent , Deline Adrien ,   CHEOPS and HARPS-N consortia
Published: September 2022

Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d/c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor 3. Internal structure and atmospheric simulations draw a contrasting
picture between HD3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD3167d/c. Dynamical simulations indeed show that the outer planetary system d/c/e was tilted as a whole early in the system history, when HD3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD3167 system, which remains a target of choice for follow-up observations and simulations.
Northern hemispheric atmospheric ethane trends in the upper troposphere and lower stratosphere (2006–2016) with reference to methane and propane
Authors: Li Mengze , Pozzer Andrea , Lelieveld Jos , Williams Jonathan
Published: September 2022

Abstract. Methane, ethane, and propane are among the most abundant
hydrocarbons in the atmosphere. These compounds have many emission sources
in common and are all primarily removed through OH oxidation. Their mixing
ratios and long-term trends in the upper troposphere and stratosphere are
rarely reported due to the paucity of measurements. In this study, we
present long-term (2006–2016) northern hemispheric ethane, propane, and
methane data from airborne observation in the upper troposphere-lower
stratosphere (UTLS) region from the IAGOS-CARIBIC project. The methane and
propane observations provide additional information for understanding
northern hemispheric ethane trends, which is the major focus of this study.
The linear trends, moving averages, nonlinear trends and monthly variations
of ethane, methane and propane in 2006–2016 are presented for the upper
troposphere and lower stratosphere over 5 regions (whole Northern
Hemisphere, Europe, North America, Asia and the rest of the world). The growth
rates of ethane, methane, and propane in the upper troposphere are −2.24 % yr−1,
0.33 % yr−1, and −0.78 % yr−1, respectively, and in the lower stratosphere they
are −3.27 % yr−1, 0.26 % yr−1, and −4.91 % yr−1, respectively, in 2006–2016. This dataset
is of value to future global ethane budget estimates and the optimization of
current ethane inventories. The data are publicly accessible at https://doi.org/10.5281/zenodo.6536109 (Li et al., 2022a).
Uncertainty and sensitivity analysis for probabilistic weather and climate-risk modelling: an implementation in CLIMADA v.3.1.0
Authors: Kropf Chahan M. , Ciullo Alessio , Otth Laura , Meiler Simona , Rana Arun , Schmid Emanuel , McCaughey Jamie W. , Bresch David N.
Published: September 2022

Abstract. Modelling the risk of natural hazards for society, ecosystems, and the economy is subject to strong uncertainties, even more so in the context of a changing climate, evolving societies, growing economies, and declining ecosystems. Here, we present a new feature of the climate-risk modelling platform CLIMADA (CLIMate ADAptation), which allows us to carry out global uncertainty and sensitivity analysis. CLIMADA underpins the Economics of Climate Adaptation (ECA) methodology which provides decision-makers with a fact base to understand the impact of weather and climate on their economies, communities, and ecosystems, including the appraisal of bespoke adaptation options today and in future. We apply the new feature to an ECA analysis of risk from tropical cyclone storm surge to people in Vietnam to showcase the comprehensive treatment of uncertainty and sensitivity of the model outputs, such as the spatial distribution of risk exceedance probabilities or the benefits of different adaptation options. We argue that broader application of uncertainty and sensitivity analysis will enhance transparency and intercomparison of studies among climate-risk modellers and help focus future research. For decision-makers and other users of climate-risk modelling, uncertainty and sensitivity analysis has the potential to lead to better-informed decisions on climate adaptation. Beyond provision of uncertainty quantification, the presented approach does contextualize risk assessment and options appraisal, and might be used to inform the development of storylines and climate adaptation narratives.
A joint assimilation of satellite soil moisture and flood extent maps to improve a flood hazard modelling.
Authors: Hostache Renaud , Matgen Patrick , van Leuuwen Peter-Jan , Nichols Nancy , Chini Marco , Pelich Ramona , Delenne Carole
Published: September 2022

The main objective of this study is to investigate how innovative satellite Earth observation techniques that allow for the estimation of soil moisture and the mapping of flood extents can help in reducing errors and uncertainties in hydro-meteorological modelling especially in ungauged areas where potentially no or limited runoff records are available. A conceptual hydrological model is loosely coupled with a shallow water model allowing for the simulation of soil moisture and flood extent. Using as forcing of this model rainfall and air temperature time series provided in the globally and freely available ERA5 database it is then possible to carry out long-term simulations of soil moisture, discharge and flood extent. Next, time series of soil moisture and flood extent observations derived from freely available satellite image databases are jointly assimilated into the hydrological model in order to retrieve optimal parameter sets. For this assimilation experiment, we take benefit of recently introduced Particle Filters with tempering that circumvent some of the usual particle filter limitations such as degeneracy and sample impoverishment. As a proof of concept, we set up an identical twin experiment based on synthetically generated observations and we evaluate the performance of the calibrated model.
From piezometers to water actors and back again. A grounded sociohydrology towards the sharing of hydrological knowledge (Senegal River delta).
Authors: Riaux Jeanne , Mohamed Ahmed Salem , Leduc Christian , Ba Cheikh A.A.M. , Lam Mamadou
Published: September 2022

The Senegal River delta is characterised by two distinct features. First is the rich historical link between people and water. In this area shaped by the river flow, inhabitants developed multiple water-related activities over history and adapted to hydrological fluctuations. Fresh, salt and brackish water, from the surface and underground, are used in the daily life of riverside people, through fishing, market gardening, fluvial trade, biodiversity conservation, etc. Second is the hydraulic history of this river, commanded by periods of flood and recession. Since the 1980s, massive hydraulic development profoundly modified the river dynamics with dikes, dams and large irrigation schemes. These changes affected the functioning of the lower delta, and especially the distribution of flood waters. People adapted their practices to these changes. One of the driving forces behind these adaptations is the comprehension of the hydrological changes and their impacts on the hydrological regime, in space and time. To do this, all water actors involved in the delta (inhabitants, managers and scientists) develop a dynamic and composite body of knowledge, enabling each of them to build up a specific understanding of the river, in line with their needs for action.

Our research uses grounded sociohydrology to analyse the ways in which this knowledge is constructed. It highlights the variety of information that water actors mobilise in order to build their hydrological knowledge. Each individual produces his own indicators, data and observations. The typical distinction operated between scientific and local knowledge does not resist to this analysis. Knowledge is distinguished by the underlying logic of action and not by the kind of expertise it mobilises. For example, groundwater levels and their variations are of equal interest to hydrogeologists and farmers. Only the observation tools, wells or piezometers, may differ.

This work identifies the ways water actors share information in order to build answers to pending questions about the hydrological dynamics of the Senegal River delta. In a highly anthropised semi-arid context this information sharing enhances the level of knowledge of all groups of actors.
Scale influence in water resources management for heterogeneous oak-savanna distinctive microclimates.
Authors: Andreu Ana , Carpintero Elisabet , Muñoz-Gomez Maria J. , Blazquez-Carrasco Angel , González-Dugo Maria P.
Published: September 2022

Dehesas are savanna-type ecosystems subject to regular water deficits; they have a complex structure with multiple vegetation layers that differ in phenology, physiology, and function, and each one contributes differently to turbulent exchanges and the radiative transfer budget. The combined differential functioning and characteristics of the vegetation components affect water dynamics, resulting in high spatio-temporal variability that creates distinct intra-ecosystem microclimates. This structure influences ecological processes, such as plant growth, and plays an important role in Dehesa resilience, making the system an efficient convector of sensible heat and keeping the canopy surface temperature within the survival range. Dehesas are productive landscapes, and one of their multiple uses, extensive livestock farming, requires an environment that is comfortable for animals and produces sufficient biomass yields. Thus, microclimate regulation and stability are key to maintaining the ecosystem’s profitability. We need to better understand the interactions between vegetation structure and dynamics, and microclimate delineation and regulation, at scales relevant to both farming management and the dominant mesoscale hydrologic regime. 

We evaluated the water use patterns estimated by different modeling approaches (FAO56, ALEXI - DisAlexi with STARFM, and SEBS) with different spatial resolutions (5 km to 10 m) of the herbaceous stratum and other typical vegetation patches (scrubs, humid areas, creek shore), which shape the distinctive dehesa microclimates. From a farm management viewpoint, we demonstrated the need for sufficient spatial and temporal resolution when evaluating water consumption. Higher spatial-temporal scales were crucial to determining the pasture drying cycle and can benefit the assessment of the nutritional quality for livestock feeding. In humid or denser areas that provide essential ecosystem services (e.g. shelter, soils with increased water retention) transpiration rates were higher throughout the year and often underestimated when using coarse data. Over mixed patches (grass and trees with low coverage fraction) products with coarse resolution (1 km to 5 km) reflected well the water use pattern. From a hydrological viewpoint, the 30 m resolution ET product may be useful to identify and delineate areas with different water storage capacities and runoff processes within the basin. Nevertheless, coarse resolutions are enough for regional managing purposes.
Assessment of climate change impact on hydrology of isser river basin, algeria
Authors: Tadlaoui Sarra , Belarbi Halima , Derbal Radia , Boukhateb Assia
Published: September 2022

This research assessed the impact of climate change on hydrology over Isser River basin in Algeria using the data of 4 hydrometric stations:  Sidi-Abdelli, Chouly, Maghnia, Sidi-Bel-Abbes (North-West Algeria). Using climate projection from the Global Circulation Model (GCM) CanESM2, the Statistical DownScaling Model (SDSM) was used to downscale the GCM data from RCP2.6, RCP4.5 and RCP8.5 emissions scenarios for future climate predictions. The outputs generated from the statistical downscaled model (precipitation and temperature) were used to derive a hydrological model GR2M. GR2M was calibrated and used to assess the hydrological response over the Isser River basin due to climate change. GR2M hydrological model simulation was run for the baseline and three future scenarios (2030s, 2060s, and 2090s) to understand climate change impacts on river runoff. The average water balance components of the RCP2.6, RCP4.5 and RCP8.5 scenarios for the three periods were compared with the baseline hydrological simulation. Results demonstrates that the hydrology of the basin is very sensitive to climate change. The projected minimum and maximum temperatures increase in three scenarios are within the range projected by IPCC which reported average temperature will increase in future for the North Africa. The increase in temperature will be accompanied with decrease in the total annual precipitation for the three scenarios RCP2.6, RCP4.5, RCP8.5 at the four stations indicating that the watershed will be hotter and drier in the future.
Citizens AND HYdrology (CANDHY): on the application of a transdisciplinary framework for assessing citizen science projects addressing hydrological challenges
Authors: Nardi Fernando , Cudennec Christophe , Abrate Tommaso , Annis Antonio , Assumpção Thaine H. , Aubert Alice H. , Berod Dominique , Braccini Alessio Maria , Buytaert Wouter , Dasgupta Antara , Hannah David M. , Mazzoleni Maurizio , Polo Maria J. , Sæbø Øystein , Seibert Jan , Tauro Flavia , Teutonico Rita , Uhlenbrook Stefan , Wahrmann Vargas Cristina , Grimaldi Salvatore
Published: September 2022

Earth and water monitoring and observation systems provide open geo data to scientists and professionals supporting distributed knowledge of major hydromet dynamics and extremes. Mobile technologies, at the same time, are empowering citizens who are nowadays informed and involved in volunteering actions designed and implemented to make our communities more safe and sustainable. Citizen science, as a consequence, is gaining momentum empowering the general public, from the “pleasure of doing science” to complementing observations, increasing scientific literacy, and supporting collaborative behaviour to solve specific water-related challenges. This work illustrates a conceptual transdisciplinary assessment model that was designed with the goal of standardizing the use of citizen science for advancing hydrology. This work was promoted by the Citizens AND HYdrology (CANDHY) Working Group established by the International Association of Hydrological Sciences (IAHS), and that is composed by a diverse group of hydrological, computer and social science experts. A community paper (Nardi et al., in press) presented the conceptualization of this transdisciplinary framework by identifying the shared constituents, interfaces and interlinkages between hydrological sciences and other academic and non-academic disciplines. Particular emphasis was given to the integration of human sensing and behavioural mechanisms into citizen science programs addressing hydrological problems. The proposed CANDHY transdisciplinary framework is here further tested and applied to assess some selected citizen science programs to understand the knowledge gaps and opportunities arising from ongoing citizen science programs. This comparative assessment shows some interesting preliminary results demonstrating the capacity of the proposed framework in homogenizing and accumulating knowledge from the collaboration of diverse participatory programs addressing similar or complementary hydrological challenges.

 

Nardi F. et al., in press. Citizens AND HYdrology (CANDHY): conceptualizing a transdisciplinary framework for citizen science addressing hydrological challenges. Hydrological Sciences Journal, https://doi.org/10.1080/02626667.2020.1849707
Le château d’eau de l’Afrique de l’Ouest est-il hydrologiquement résilient ?
Authors: Descroix Luc , Manga Sylvie Paméla , Dièye Arame , Diedhiou Ange Bouramanding , Diallo Kadiatou , Sakho Yaya , Fall Ababacar , Andrieu Julien , Ogilvie Andrew , Marega Oumar , Diouf Ousmane , Faty Bakary
Published: September 2022

Le Fouta Djallon est considéré comme le « château d’eau » de l’Afrique de l’Ouest. La plupart des grands cours d’eau d’Afrique de l’Ouest y prennent leur source. Les eaux provenant de ce massif constituent l’essentiel du débit des grands cours d’eau apportant de l’eau douce à la bande sahélo-soudanienne, en particulier, d’ouest en est, la Gambie, le Sénégal et le Niger.

Ce massif est caractérisé par une forte hydraulicité. Ceci est lié avant tout à une forte pluviométrie, à des pentes appréciables et à une lithologie peu perméable. Les roches sont en effet peu poreuses, ce qui s’oppose grandement à la nation de « château d’eau ». de fait, les réserves sont faibles, et essentiellement liées à la présence de 8000 petites zones humides qui stockent des volumes d’eau permettant de garantir des écoulements faibles en fin de saison sèche, mais pérennes sur de nombreux cours d’eau.

La couverture végétale du Fouta Djalon n’est pas très dense, du fait d’une lithologie peu propice. Mais elle ne montre pas, ni sur le court ni sur le long terme de signes de dégradation pouvant menacer sa résilience.

Après la période hyper humide 1950-1967 et la longue sécheresse de 1968 à 1993, la pluviométrie annuelle est en croissance au point de dépasser, dans de nombreuses régions d’Afrique de l’Ouest, la moyenne de long terme. Mais les débits mettent du temps à rejoindre ceux de la période antérieure à la phase hyper humide, du fait de la reconstitution des stocks d’eau suite à leur vidange progressive durant la phase sèche où elles ont longtemps soutenu les étiages.

Cette recherche vise à déterminer les conditions de la résilience hydrologique du massif du Fouta Djalon, source majeure d’alimentation en eau douce de la bande sahélo-soudanienne.
The Water-Food-Health Nexus; Exploring the Water Foundations of Family to Community to Global Health.
Authors: Geere Jo-Anne , Lankford Bruce
Published: September 2022

Many people in low-income countries and fragile states struggle to access the foundations of family and community health which we see as a three-way nexus of; access to safe water and sanitation, a sufficient and balanced diet and effective health services. These factors interact with each other to affect personal and community health in different ways mediated by environmental and social factors specific to local and national contexts. Our paper conceptually explores the hydrological foundations of safe water, food and health interactions that underpin individual, community and global health. In doing so we recognise the recursive dynamics of water and sanitation and health (WASH), food and diet systems, climate change, emergent diseases, conflict and freshwater ecosystems degradation, loss of biodiversity and migration.  Outbreaks of Ebola and the COVID-19 pandemic have demonstrated that localised community health problems, and the local freshwater needed to combat them, can emerge and quickly escalate to have global health, economic, social, and political consequences. Therefore, a focus on improving the foundations of health (improved water access, food and nutrition security and health services) in low-income communities (LIC) and fragile or conflict affected states (FCS) not only targets populations in greatest need and most likely to benefit but creates opportunities to strengthen and protect global health.