Titan After Cassini-Huygens

1st Edition - January 20, 2025
Editors: Rosaly M.C. Lopes, Charles Elachi, Ingo Mueller-Wodarg, Anezina Solomonidou
Language: English
Paperback ISBN:
9 7 8 - 0 - 3 2 3 - 9 9 1 6 1 - 2
eBook ISBN:
9 7 8 - 0 - 3 2 3 - 9 9 1 6 2 - 9

Titan After Cassini-Huygens is the most up-to-date and comprehensive coverage of our knowledge on Titan, including results and insights from the joint NASA/European Space Agency/It… Read more

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Titan After Cassini-Huygens is the most up-to-date and comprehensive coverage of our knowledge on Titan, including results and insights from the joint NASA/European Space Agency/Italian Space Agency mission Cassini-Huygens and the conclusions drawn by experts following detailed analysis of the mission data. Our knowledge of Titan has increased substantially due to observations from the Cassini-Huygens mission, which ended in 2017. Since then, observations from Earth, as well as laboratory and theoretical studies, have continued to add to our knowledge. These conclusions, combined with the latest ground-based and theoretical research, provide the most recent understanding of the science of Titan, covering the origin and evolution of Titan, its magnetic and plasma environment, surface, interior structure, geology, atmosphere, and the astrobiological potential for the oceans on the moon.
The first book of the new COSPAR book series, Titan After Cassini-Huygens, is an integral reference for scientists, researchers, and academics working on Titan or ocean worlds.

Part of the COSPAR Book Series
Edited by Jean-Louis Fellous, former Executive Director of COSPAR (Committee on Space Research; 2008–2019)

Titan After Cassini-Huygens
Cover image
Title page
Table of Contents
Copyright
Contributors
Chapter 1 Introduction: Titan, the Earth of the outer solar system
Abstract
Keywords
Acknowledgments
1 Introduction
2 Book structure
3 Titan's bulk properties
4 Titan's regions and nomenclature
Chapter 2 History of Titan exploration
Abstract
Keywords
Acknowledgments
1 Prologue
2 The initial steps
3 Joint ESA-NASA study
4 Mission overview
5 Launch
6 Cruise
7 Saturn orbit insertion (SOI)
8 Beginning the tour: Cassini's Prime Mission
9 Huygens probe mission
10 Titan and satellite tour
11 Viewing Saturn's rings edge-on: Equinox Mission (EM)
12 Summer in the northern hemisphere: SM
13 Satisfying planetary protection requirements: Grand finale orbits
14 Epilogue
Appendix
References
Chapter 3 The origin and evolution of Titan
Abstract
Keywords
Acknowledgments
1 Introduction: Key issues in the origin and evolution of Titan
2 Cassini-Huygens and other data sets relevant to origin and evolution
2.1 Atmospheric composition: Molecular and isotopic
2.2 Surface properties
3 Models of the growth of satellites around Saturn
3.1 Context: Growth of Saturn
3.2 Titan's accretion in the Saturn environment
4 Earliest evolution of Titan
4.1 Evolution of a primitive ammonia-water “magma” ocean and crust formation
4.2 Interior differentiation and water-organics-rock interactions
4.3 Conversion of NH3 to N2 by various mechanisms
5 Coupled evolution of the interior and atmosphere of Titan up to the last billion years
5.1 Evolution of Titan's internal ocean and link with its orbit
5.2 Isotopic constraints on the atmosphere evolution
6 The last billion years
6.1 Evidence for and against a standing global methane-ethane ocean in the past
6.2 The resupply of methane over the last billion years: Steady state or episodic?
7 What we seek to learn from Dragonfly and future missions about the origin and evolution of Titan
References
Chapter 4 Titan orbital and rotational dynamics
Abstract
Keywords
Acknowledgments
1 Introduction
2 Observations and dynamical characteristics
3 Short-term evolution
3.1 The orbital motion
3.2 Titan's rotation
4 Long-term evolution
4.1 Evolution and origin of the Titan-Hyperion resonance
4.2 Past resonance crossings with Iapetus
4.3 Migration of Titan and the evolution of Saturn's obliquity
5 Conclusion
References
Chapter 5 Titan's magnetic and plasma environment
Abstract
Keywords
Acknowledgments
1 Introduction
2 Titan internal field and upper atmosphere/exosphere/ionosphere
2.1 Internal magnetic field
2.2 Titan's atmosphere, ionosphere, and exosphere
3 Upstream from Titan
4 Induced magnetosphere through specific cases
5 General trends
6 Ion pickup and escape
7 Numerical simulations
8 Conclusions and outstanding questions
References
Chapter 6 Titan's upper neutral atmosphere and ionosphere
Abstract
Keywords
Acknowledgments
1 Introduction
2 Observations
2.1 The vertical distribution of neutral gases
2.2 Trends and horizontal distribution of neutral gases
2.3 Thermal structure
2.4 Electron and ion densities
3 Global structure and variability
3.1 Observed structure and variability
3.2 Waves
3.3 Magnetosphere forcing
4 Escape
5 Dynamics
6 Concluding thoughts and future exploration
References
Chapter 7 Titan's atmospheric structure, composition, haze, and dynamics
Abstract
Keywords
Acknowledgments
1 Introduction
2 Main vertical structure
3 Atmospheric composition
3.1 Major constituents and inert gases
3.2 Minor constituents
3.3 Isotopes
4 Gas phase atmospheric chemistry
5 Haze and ice clouds
5.1 Photochemical haze
5.2 Stratospheric ice clouds
6 Middle atmosphere dynamics
6.1 Zonal winds
6.2 Meridional circulation
6.3 Polar vortices
6.4 Haze spatial distribution
7 Conclusions: The future of Titan's atmosphere exploration
References
Chapter 8 Titan's weather, climate, and paleoclimate
Abstract
Keywords
Acknowledgments
1 Introduction
2 Two seasons of weather from Cassini–Huygens
2.1 Observed environment of the lower atmosphere
2.2 Observations of clouds and rain
2.3 Mechanisms of cloud formation
3 Titan's climate and its variability
3.1 Influence of the surface
3.2 Influence on the surface
4 Paleoclimate and climate evolution
5 Conclusion
References
Chapter 9 Global geology of Titan
Abstract
Keywords
Acknowledgments
1 Introduction
2 Major Titan terrain types
2.1 Plains
2.2 Dunes
2.3 Mountains/hummocky terrains
2.4 Labyrinths
2.5 Lakes
2.6 Craters
3 Global map of Titan
4 Icy material processes
4.1 Impact craters
4.2 Mountains
4.3 Cryovolcanism
4.4 Xanadu
4.5 Water ice materials evolution summary
5 Organic material cycling
5.1 Labyrinth terrains
5.2 Dunes
5.3 Plains
5.4 Summary of the organic cycle
6 The liquid hydrocarbon cycle
6.1 Channels
6.2 Lakes and mare
6.3 Summary of liquid hydrocarbon cycle
7 The ground truth: Huygens landing site on Titan
8 Summary of Titan landscape and material evolution
9 Future exploration
References
Chapter 10 Titan's fluvial and lacustrine landscapes
Abstract
Keywords
Acknowledgments
1 Introduction
2 Titan's fluvial landscapes
2.1 Liquid-filled polar valley networks
2.2 Equatorial and mid-latitude valley networks
2.3 Fluvial deposits
3 Titan's lacustrine landscapes
3.1 Liquid-filled north polar seas and large lakes
3.2 Ontario lacus and southern Paleoseas
3.3 Filled and empty lakes
3.4 Low-latitude lacustrine features
4 Outstanding open questions post-Cassini
4.1 How does bedrock break down on Titan's hillslopes?
4.2 How much of Titan's topography have rivers exhumed?
4.3 What surface processes help regulate Titan's long-term climate?
4.4 How important is chemical erosion on Titan relative to mechanical erosion?
4.5 What can Titan's rivers reveal about its materials and climate?
4.6 Do Titan's ternary fluids produce new dynamics not encountered on Earth?
4.7 What can Titan's coastlines reveal about climate variations and long-term methane inventories?
4.8 How do Titan's SEDs form?
5 Summary
References
Chapter 11 Titan's surface composition
Abstract
Keywords
1 The importance of unveiling the surface composition to understand Titan
1.1 Surface composition as an imprint of Titan's origin and evolution
1.2 Surface composition as a clue for Titan's habitability
1.3 Seeing the surface through the opaque veil of Titan's atmosphere
2 Pre-Cassini speculations and observations
2.1 Pre-Voyager
2.2 Voyager on surface conditions
2.3 Speculations about the surface and the interior composition
2.4 Ground-based and space telescope observations
2.5 Outstanding questions on Titan's surface composition before Cassini
3 Huygens and Cassini observations
3.1 Huygens in situ measurements
3.2 Cassini remote measurements
3.3 Knowledge of the composition of Titan's main geological units after Cassini-Huygens
3.4 Open questions after Cassini
4 Ongoing and future investigation
4.1 Laboratory analogs for Titan's composition
4.2 James Webb space telescope observations
4.3 Future Dragonfly in situ measurements
4.4 Mission concepts and composition
References
Chapter 12 Titan's interior
Abstract
Keywords
Acknowledgments
1 Introduction
2 Cassini and other relevant data sets
3 Interior models
4 The ice crust
5 Titan's deep water ocean
6 High-pressure ice layer
7 Core of refractory material
8 Conclusions
References
Chapter 13 Exchange processes between surface, atmosphere, and interior
Abstract
Keywords
Acknowledgments
1 Introduction
2 Cassini and other data sets relevant to mass and chemical exchange processes
2.1 Atmosphere composition, structure, and interactions with the surface
2.2 Impacts
2.3 Cryovolcanoes
3 Possible transport of surface materials into the ocean
4 Tectonism and implications for solid-state convection
5 The complex role of organic materials in Titan's exchange processes
5.1 Stability of seafloor ices, hydrates, and clathrates
6 Conclusion
References
Chapter 14 Astrobiology of Titan's subglacial, high pressure ocean: A review and introduction of a relevant experimental system
Abstract
Keywords
Acknowledgments
1 Introductory remarks: How does astrobiology apply to Titan?
2 Astrobiology on Titan and icy ocean worlds
2.1 Titan's icy crust and ice/ocean interface as a potential habitat
2.2 Titan's ocean and core/ice/ocean interfaces as potential habitats
2.3 Upcoming missions that will focus on Titan's astrobiology
2.4 Biomolecules to biosignatures
3 Life at high pressure and cold temperature (and high salinity)
3.1 Life has been found in high-pressure environments: Earth's piezophiles
3.2 Life has been found in cold environments: Earth's psychrophiles
3.3 Examples of Earth extremophiles that have relevance to Titan
4 High-pressure culturing and experimentation and what has been revealed about potential life on Titan
4.1 Experimental approaches
4.2 Genomic, transcriptomic, proteomic, and phenotypic responses of organisms grown under pressure
4.3 Membrane adaptations to high pressure
5 A novel high-pressure, high-culture volume experimental culturing system for Titan astrobiology research
5.1 Description of the high-pressure system and culturing vessels
5.2 Adaptations that allow ease of experimentation with live cultures
5.3 Applications and proof of concept
6 Closing remarks
References
Chapter 15 Open questions and future directions in Titan science
Abstract
Keywords
Acknowledgments
1 Introduction: Current sources of knowledge
2 Open questions
2.1 Questions about Titan's formation (1–3)
2.2 Questions about Titan's interior (4–6)
2.3 Questions about Titan's surface (8–13)
2.4 Questions about Titan's atmosphere (14–20)
3 Future directions
3.1 Telescopes
3.2 Laboratory work
3.3 Modeling
3.4 Missions
3.5 Terrestrial field analog studies
References
Index

Rosaly M.C. Lopes

Rosaly Lopes is a Senior Research Scientist at the Jet Propulsion Laboratory, where she is also Manager of the Planetary Science Section. An expert on planetary volcanism, she worked on the Galileo mission to Jupiter and is currently on the science team of the Cassini mission to Saturn. Her research expertise is on volcanoes in the Solar System, particularly the active volcanoes of Jupiter's moon Io and the ice volcanoes of Saturn's icy moons. She is a Fellow of the American Association for the Advancement of Science and the Geological Society of America, and the winner of the American Astronomical Society’s 2005 Carl Sagan Medal. She has published seven books and over one hundred and twenty peer-reviewed publications

Affiliations and expertise

Senior Research Scientist, Jet Propulsion Laboratory, CA, USA

Charles Elachi

Dr. Charles Elachi is Professor (Emeritus) of Electrical Engineering and Planetary Science at the California Institute of Technology. From 2001 to 2016 he was the Director of the Jet Propulsion Laboratory and Vice President of California Institute of Technology. During his tenure, he oversaw the development and operations of over 45 flight missions and instruments, and was principal investigator on a number of NASA-sponsored studies and projects including the Shuttle Imaging Radar series the Magellan Imaging Radar, the Cassini Titan Radar and the Europa Sounding Radar. He was the Team Leader for the Titan Imaging Radar on the Cassini mission and has been honored with numerous awards, including the von Karman award from the International Academy of Astronautics and three NASA Outstanding Leadership Medals. In 1989, Asteroid 1982 SU was renamed 4116 Elachi in recognition of his contribution to planetary exploration and, in 2016 the JPL/NASA Mission Control Center was renamed “The Charles Elachi Mission Control Center”. He has authored over 230 publications and holds several patents in his fields.

Affiliations and expertise

Professor (Emeritus), Department Electrical Engineering and Planetary Science, California Institute of Technology, USA

Ingo Mueller-Wodarg

Dr Ingo Mueller-Wodarg is Professor in Physics at Imperial College London and an expert in the study of atmospheres of planets, moons and smaller objects in our Solar System. He developed the only published global circulation model of Titan’s upper atmosphere and similar models for other solar system atmospheres. He has authored or co-authored more than 100 peer-reviewed scientific papers, including 30 on Titan, and was lead editor of the 2014 Cambridge University Press book "Titan: Interior, Surface, Atmosphere and Space Environment". In 2002 he was awarded a Royal Society University Research Fellowship. He was Science Team Member of the Cassini Ion Neutral Mass Spectrometer and Team Leader for the Venus Express Atmospheric Drag Experiment and is currently Co-Principal Investigator of the Radio and Plasma Wave Instrument on ESA’s forthcoming Jupiter Icy Moon Explorer (JUICE).

Affiliations and expertise

Professor in Physics, Imperial College London, UK

Anezina Solomonidou

Dr. Anezina Solomonidou is a planetary scientist specializing in planetary geology and investigating the potentially habitable worlds of our solar system. She is the Scientific Officer of the Greek Space Agency for Space Sciences and Exploration. She has obtained her doctoral title on astronomy and astrophysics from the Paris Observatory in France. She has worked for many years at NASA's Jet Propulsion Laboratory (JPL) and Caltech in Los Angeles, California, on the Cassini-Huygens and the Europa Clipper missions, as well as the European Space Agency (ESA) in Madrid for the preparation of ESA’s new space mission, JUICE. She has authored a plethora of articles in peer-reviewed scientific journals and chapters in books. Dr. Solomonidou has proposed a series of planetary experiments and has contributed to the design of future missions. She is the President of the Division for Planetary Sciences (PS) for the European Geosciences Union (EGU) and serves as a review panelist for international boards and NASA panels, where she evaluates scientific proposals for planetary research.

Affiliations and expertise

Planetary Scientist, Hellenic Space Center, Greece

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Titan After Cassini-Huygens

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Innovate. Sustain. Transform.

Institutional subscription on ScienceDirect

Rosaly M.C. Lopes

Charles Elachi

Ingo Mueller-Wodarg

Anezina Solomonidou