III. Ecosmos: A Revolutionary Fertile, Habitable, Solar-Bioplanet, Incubator Lifescape

H. Stellar Planetary Systems: A Stochastic Profusion of Galaxies, Solar Orrerys, and Habitable Zones

Tamayo, Daniel, et al. A Criterion for the Onset of Chaos in Compact, Eccentric Multiplanet Systems. arXiv:2106.14863. We cite this June entry by Princeton University and University of Toronto astrophysicists including Scott Tremaine and Joshua Winn as another frontier instance whereof whole host star and orbital arrays are being treated as a unified assembly.

We derive a semi-analytic criterion for the presence of chaos in compact, eccentric multiplanet systems. We show that the onset of chaos is due to the overlap of two-body mean motion resonances (MMRs), like it is in two-planet systems and the secular evolution causes the MMR widths to expand and contract. For closely spaced two-planet systems, a near-symmetry suppresses this secular modulation. We make routines for evaluating the chaotic boundary available to the community through the open-source SPOCK package. (Abstract excerpt)

Tinetti, Giovanna. Galactic Planetary Science. Proceedings of the Royal Society A. 372/20130077, 2014. The University College London astrophysicist introduces this grand 2010s vista unto explorations of a novel animate universe which populates itself with myriad orbital worlds in starry arrangements. Since our own solar system is realized to be especially orderly and stable, one might suggest such studies might be seen as a “Galactic Positioning System” as we Earthlings come to realize our special situation and import.

The University College London astrophysicist introduces this grand 2010s vista unto explorations of a novel animate universe which populates itself with myriad orbital worlds in starry arrangements. Since our own solar system is realized to be especially orderly and stable, one might suggest such studies might be seen as a “Galactic Positioning System” as we Earthlings come to realize our special situation and import.

Tinetti, Giovanna, et al. The EChO Science Case. arXiv:1502.05747. With some 350 authors and 50 pages, this is a manifesto for an Exoplanet Classification Observatory project over the next decade as a scientific survey of a grand new genesis universe that fills itself with stars and planets so that an intelligent species can achieve its own self-comprehension. A sample of diverse subjects might be: exoplanet core to atmospheric composition, how many large gaseous planets, what is the range of planetary spin, orbit shape, dynamic movement, and can planets around low mass stars keep their atmospheres. And akin to the views of Elke Pilat-Lohinger above, a significant finding is just being realized. Our own solar system which contains a bioplanet able to do this is not typical at all, and especially conducive due to its long term stability. Whatever to make of this?

EChO has been conceived to address the following fundamental questions:• Why are exoplanets as they are? • What are the causes for the observed diversity? • Can their formation and evolution in history be traced back from their current composition? EChO would provide spectroscopic information on the atmospheres of a large, select sample of exoplanets allowing the composition, temperature, size and variability to be determined at a level never previously attempted. This information can be used to address a wide range of key scientific questions relative to exoplanets: • What are they made of? • Do they have an atmosphere? • What is the energy budget? • How were they formed? • How do they evolve? • How do weather conditions vary with time? And of course: • Do any of the planets observed have habitable conditions?

Conclusion: Our knowledge of planets other than the eight “classical” Solar System bodies is in its infancy. We have discovered over a thousand planets orbiting stars other than our own, and yet we know little or nothing about their chemistry, formation and evolution. Planetary science therefore stands at the threshold of a revolution in our knowledge and understanding of our place in the Universe: just how special are the Earth and our Solar System? It is only by undertaking a comprehensive chemical survey of the exoplanet zoo that we will answer this critical question.

Tosi, Nicola, et al. The Habitability of a Stagnant-Lid Earth. Astronomy & Astrophysics. Online July, 2017. A ten person exoplanetologist team from Technische Universitat Berlin, and the German Aerospace Center, note that mobile crustal land masses are a minority case, with stationary mantles more prevalent. While Earth’s continental movements may be more conducive for evolutionary life, a “stagnant-lid” world could yet have living systems.

Plate tectonics is a fundamental component for the habitability of the Earth. Yet whether it is a recurrent feature of terrestrial bodies orbiting other stars or unique to the Earth is unknown. The stagnant lid may rather be the most common tectonic expression on such bodies. To understand whether a stagnant-lid planet can be habitable, i.e. host liquid water at its surface, we model the thermal evolution of the mantle, volcanic outgassing of H2O and CO2, and resulting climate of an Earth-like planet lacking plate tectonics. We used a 1D model of parameterized convection to simulate the evolution of melt generation and the build-up of an atmosphere of H2O and CO2 over 4.5 Gyr. Our results suggest that stagnant-lid planets can be habitable over geological timescales and that joint modelling of interior evolution, volcanic outgassing, and accompanying climate is necessary to robustly characterize planetary habitability. (Abstract excerpts)

Tremaine, Scott. The Statistical Mechanics of Planet Orbits. arXiv:1504.01160. It is noteworthy in this post-Kepler era of myriad solar systems that scientists such as this Institute for Advanced Study, Princeton University, astrophysicist and leading expositor of galactic dynamics, can consider a common physical theory by which planetary bodies arrange themselves. On this e-print site and across the astro- journals, articles like Spacing of Kepler Planets: Sculpting by Dynamical Instability (1502.05449) and Consolidating and Crushing Exoplanet (1502.06558) now treat solar system formations as a valid subject amenable to theoretical explanations.

The final "giant-impact" phase of terrestrial planet formation is believed to begin with a large number of planetary "embryos" on nearly circular, coplanar orbits. Mutual gravitational interactions gradually excite their eccentricities until their orbits cross and they collide and merge; through this process the number of surviving bodies declines until the system contains a small number of planets on well-separated, stable orbits. In this paper we explore a simple statistical model for the orbit distribution of planets formed by this process, based on the sheared-sheet approximation and the ansatz that the planets explore uniformly all of the stable region of phase space. The model provides analytic predictions for the distribution of eccentricities and semimajor axis differences, correlations between orbital elements of nearby planets, and the complete N-planet distribution function, in terms of a single parameter that is determined by the planetary masses. The predicted properties are generally consistent with both N-body simulations and the Kepler catalog of extrasolar planets. A similar model may apply to the orbits of giant planets if these orbits are determined mainly by dynamical evolution after the planets have formed and the gas disk has disappeared. (Abstract)

Turbet, Martin, et al. CO2 Condensation is a Serious Limit to the Deglaciation of Earth-like Planets. arXiv:1703.04624. Sorbonne, Bordeaux, and Nantes University astroresearchers, including Francois Forget, identify another critically poised exoplanetary feature vital for life and evolution. Intricate, geochemical dynamics produce and interact with carbon dioxide levels in exoatmospheres, which then affects the degree of colder or warmer conditions. Another window of viability thus seems to be balanced between a frigid frozen or hot gaseous world. Search here for Haqq-Misra, Jacob, et al for another angle on this.

It is widely believed that the carbonate-silicate cycle is the main agent to trigger deglaciations by CO2 greenhouse warming on Earth and on Earth-like planets when they get in frozen state. Here we use a 3D Global Climate Model to simulate the ability of frozen planets to escape from glaciation by accumulating enough gaseous CO2. We find that Earth-like planets orbiting a Sun-like star may never be able to escape from glaciation if their orbital distance is greater than ∼ 1.27 AU (Flux < 847 W m−2), because CO2 would condense at the poles forming permanent CO2 ice caps. This limits the amount of CO2 in the atmosphere and thus its greenhouse effect. Our results may have implications for the search for life-suitable extrasolar planets orbiting in the Habitable Zone of Sun-like stars.
(Abstract excerpts)

Valencia, Diana. Composition and Internal Dynamics of Super-Earths. Karato, Shun-ichiro, ed.. Physics and Chemistry of the Deep Earth. Chichester, UK: Wiley-Blackwell, 2013. Into this 21st century, it is worth notice that the composite collaboration of a sentient, linguistic, technological species now of global cast and import, can proceed to so explore, name, quantify, and describe these depths of these myriad orbiting worlds. We cite this chapter by a Sagan NASA postdoctoral fellow (mellow) at MIT, to illustrate how our novel collective abilities can span the planet-filled galactic reaches.

Though the deep interior of the Earth (and other terrestrial planets) is inaccessible to humans, we are able to combine observational, experimental and computational (theoretical) studies to begin to understand the role of the deep Earth in the dynamics and evolution of the planet. This book brings together a series of reviews of key areas in this important and vibrant field of studies. A range of material properties, including phase transformations and rheological properties, influences the way in which material is circulated within the planet. This circulation re-distributes key materials such as volatiles that affect the pattern of materials circulation. The understanding of deep Earth structure and dynamics is a key to the understanding of evolution and dynamics of terrestrial planets, including planets orbiting other stars. This book contains chapters on deep Earth materials, compositional models, and geophysical studies of material circulation which together provide an invaluable synthesis of deep Earth research. (Publisher)

My research comprises the characterisation of the low-mass planets: super-Earths and mini-Neptunes. The former are planets that are mostly solid, either rocky or icy in composition, while the latter posses also a volatile envelope. My goal is to determine if planets with masses between 1-15 Earth-masses are scaled up versions of Earth, or scaled-down versions of Neptune in terms of their composition, evolution and physical properties. To date, out of the ~600 discovered exoplanets, and 1000+ planet candidates reported by space mission Kepler, there are a handful of low-mass planets with measured masses and radii. This number will continue to increase as new data from Kepler arrives, and new discoveries are reported from other missions such as ground-based MEarth, or space mission CoRoT, as well as follow-up work to radial velocity planets. (DV website)

Valencia, Diana, et al. Radius and Structure of the First Super-Earth Planet. Astrophysical Journal. 656/545, 2007. Improved viewing and survey methods allow a new domain of terrestrial, rocky planets to be detected. Dubbed “super-earths” for their affinity to our home stone, they are somewhat larger in mass but by orders of magnitude as previous gas giants.

Vannah, Sara, et al.. An Information Theory Approach to Identifying Signs of Life on Transiting Planets.. Monthly Notices of the Royal Astronomical Society: Letters. October, 2023. SV and Marcelo Gleiser, Dartmouth College and Lisa Kaltenegger, Cornell University astrobiologists propose a novel way to detect advanced bioworld habitation by an evidential notice of a semblance of various communicative content.

Here we apply information theory to a range of simulated exoplanet transmission spectra as a diagnostic tool to search for potential signatures of life on Earth-analog planets. We test the algorithms on three epochs of evolution for Earth-like planets orbiting a range of host stars. The James Webb Space Telescope and upcoming ground- and space-based mironinssions promise to achieve sufficient high-resolution data that information theory can be applied to assess habitability. (Abstract)

This approach provides a framework and a tool for observers to assess exoplanet spectra. Just as we analysed simulated transmission spectra of Earth-like planets at different ages and around host stars in this paper, observed exoplanet spectra could be compared to modern Earth. Additionally, this approach is not limited to Earth-like planets or to identifying signs of life. This framework can similarly be used to compare an exoplanet spectrum to any Solar System object, or any specifically selected exoplanet to look for similarities.(6)

Vazquez, Manuel, et al, eds. The Earth as a Distant Planet: A Rosetta Stone for the Search of Earth-like Worlds. New York: Springer, 2010. As this 21st century project goes forward, little noticed by the general public, a comprehensive survey from the Instituto de Astrofisica de Canarias, Tenerife, explores how evidences from our own home, the one iconic world we can know, might guide this grand cosmic quest.

Vedantham, H. K., et al. Coherent Radio Emission from a Quiescent Red Dwarf Indicative of Star-Planet Interaction. arXiv:2002.08727. We cite this entry by fourteen astronomers from the Netherlands, France, the USA, Scotland, Germany, and Ireland to record how a sunny star and its orbital worlds altogether compose a dynamic system as if, to take license, as a solar incubator.

Veras, Dimitri. The Fates of Solar System Analogues with One Additional Distant Planet. arXiv:1608.07580. As the list of uniquely favorable features of our home planet and solar system for regnant life and humanity continues to grow, a University of Warwick astrophysicist theorizes that this eight world orrery – Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, sans dwarf Pluto – would become unstable if a further ninth planet was present. See also by DV the papers Relating Binary-Star Planetary Systems to Central Configurations (1607.08606), and Post-Main Sequence Planetary System Evolution (1601.05419.

The potential existence of a distant planet ("Planet Nine") in the Solar system has prompted a re-think about the evolution of planetary systems. As the Sun transitions from a main sequence star into a white dwarf, Jupiter, Saturn, Uranus and Neptune are currently assumed to survive in expanded but otherwise unchanged orbits. However, a sufficiently-distant and sufficiently-massive extra planet would alter this quiescent end scenario through the combined effects of Solar giant branch mass loss and Galactic tides. Here, I estimate bounds for the mass and orbit of a distant extra planet that would incite future instability in systems with a Sun-like star and giant planets with masses and orbits equivalent to those of Jupiter, Saturn, Uranus and Neptune. I find that this boundary is diffuse and strongly dependent on each of the distant planet's orbital parameters. Nevertheless, I claim that instability occurs more often than not when the planet is as massive as Jupiter and harbours a semimajor axis exceeding about 300 au, or has a mass of a super-Earth and a semimajor axis exceeding about 3000 au. This instability scenario might represent a common occurrence, as potentially evidenced by the ubiquity of metal pollution in white dwarf atmospheres throughout the Galaxy. (Abstract)

The consequences for other planetary systems are profound. Multiple planets beyond about 5 au (such as analogues of Jupiter, Saturn, Uranus and Neptune) may be common, but are so far unfortunately effectively hidden from detection by Doppler radial velocity and transit photometry techniques, the two most successful planet-finding techniques. If more distant, trans-Neptunian-like planets are also common, then the ingredients may exist to regularly generate instability and a frequently-changing dynamical environment during white dwarf phases of evolution. (14)

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