scholarly journals Habitable Zones in Binary Star Systems: A Zoology

Galaxies ◽  
2020 ◽  
Vol 8 (3) ◽  
pp. 65
Author(s):  
Siegfried Eggl ◽  
Nikolaos Georgakarakos ◽  
Elke Pilat-Lohinger
Keyword(s):  
Orbital Motion ◽  
Binary Star ◽  
Full Scale ◽  
Terrestrial Planets ◽  
Gravitational Perturbations ◽  
Habitable Zones ◽  
Planetary Orbits ◽  
Self Consistent ◽  
Habitable Planet

Several concepts have been brought forward to determine where terrestrial planets are likely to remain habitable in multi-stellar environments. Isophote-based habitable zones, for instance, rely on insolation geometry to predict habitability, whereas radiative habitable zones take the orbital motion of a potentially habitable planet into account. Dynamically informed habitable zones include gravitational perturbations on planetary orbits, and full scale, self consistent simulations promise detailed insights into the evolution of select terrestrial worlds. All of the above approaches agree that stellar multiplicity does not preclude habitability. Predictions on where to look for habitable worlds in such environments can differ between concepts. The aim of this article is to provide an overview of current approaches and present simple analytic estimates for the various types of habitable zones in binary star systems.

Formation, Frequency and Spacing of Habitable Planets

1997 ◽  
Vol 161 ◽  
pp. 289-297
Author(s):  
Jack J. Lissauer
Keyword(s):  
Planet Formation ◽  
Orbital Stability ◽  
Young Stars ◽  
Giant Planets ◽  
Terrestrial Planets ◽  
Habitable Zone ◽  
Habitable Planets ◽  
Habitable Zones ◽  
Planetary Orbits ◽  
Rocky Planets

AbstractModels of planet formation and of the orbital stability of planetary systems are described and used to discuss estimates of the abundance of habitable planets which may orbit stars within our galaxy. Modern theories of star and planet formation, which are based upon observations of the Solar System and of young stars and their environments, predict that most single stars should have rocky planets in orbit about them. Terrestrial planets are believed to grow via pairwise accretion until the spacing of planetary orbits becomes large enough that the configuration is stable for the age of the system. Giant planets orbiting within or near the habitable zone could either prevent terrestrial planets from forming, destroy such planets or remove them from habitable zones. The implications of the giant planets found in recent radial velocity searches for the abundances of habitable planets are discussed.

scholarly journals AN ANALYTIC METHOD TO DETERMINE HABITABLE ZONES FOR S-TYPE PLANETARY ORBITS IN BINARY STAR SYSTEMS

2012 ◽  
Vol 752 (1) ◽  
pp. 74 ◽  
Author(s):  
Siegfried Eggl ◽  
Elke Pilat-Lohinger ◽  
Nikolaos Georgakarakos ◽  
Markus Gyergyovits ◽  
Barbara Funk
Keyword(s):  
Binary Star ◽  
Analytic Method ◽  
Habitable Zones ◽  
Planetary Orbits

scholarly journals Binary Gravitational Perturbations and Their Influence on the Habitability of Circumstellar Planets

2021 ◽  
Vol 8 ◽  
Author(s):  
Elke Pilat-Lohinger ◽  
Ákos Bazsó
Keyword(s):  
Binary Stars ◽  
Binary Star ◽  
Giant Planet ◽  
Planetary Motion ◽  
Atmospheric Conditions ◽  
Orbital Parameters ◽  
Gravitational Perturbations ◽  
Planetary Orbits

In order to assess the habitability of planets in binary star systems, not only astrophysical considerations regarding stellar and atmospheric conditions are needed, but orbital dynamics and the architecture of the system also play an important role. Due to the strong gravitational perturbations caused by the presence of the second star, the study of planetary orbits in double star systems requires special attention. In this context, we show the important role of the main gravitational perturbations (resonances) and review our recently developed methods which allow a quick determination of locations of secular resonances (SRs) in binary stars for circumstellar planetary motion where a giant planet has to move exterior to the habitable zone (HZ). These methods provide the basis for our online-tool ShaDoS which allows a quick check of circumstellar HZs regarding secular perturbations. It is important to know the locations of SRs since they can push a dynamically quiet HZ into a high-eccentricity state which will change the conditions for habitability significantly. Applications of SHaDoS to the wide binary star HD106515 AB and the tight system HD41004 AB reveal a quiet HZ for both systems. However, the study of these systems indicates only for the tight binary star a possible change of the HZ's dynamical state if the orbital parameters change due to new observational data.

scholarly journals On the Habitability of Terrestrial Planets in Binary Star Systems

2012 ◽  
Vol 8 (S293) ◽  
pp. 140-145
Author(s):  
Elke Pilat-Lohinger ◽  
Barbara Funk ◽  
Siegfried Eggl
Keyword(s):  
Planetary System ◽  
Binary Star ◽  
Terrestrial Planet ◽  
Dynamical Behaviour ◽  
Terrestrial Planets ◽  
Analytic Method ◽  
Habitable Zone ◽  
Secular Resonances ◽  
Mean Motion Resonances ◽  
Gravitational Perturbations

AbstractThe growing number of detected planets in binary star systems requires methods for a quick assessment of possible habitability of planets in such environments. We offer an analytic method to determine habitability of a terrestrial planet in binary star systems. In this context we give an answer to the most important question: Do the radiative and gravitational perturbations of a secondary influence the extent of the habitable zone (HZ)?After we have defined the borders of the HZ, we will show the dynamical behaviour of a terrestrial planet in the HZ when adding a Jupiter to the system. In such a system the HZ shows signs of mean motion resonances and secular resonances, depending on the architecture of the planetary system.

scholarly journals Dynamics and Habitability in Binary Star Systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 53-57
Author(s):  
Siegfried Eggl ◽  
Nikolaos Georgakarakos ◽  
Elke Pilat-Lohinger
Keyword(s):  
Main Sequence ◽  
Binary Star ◽  
Atmospheric Models ◽  
Main Sequence Stars ◽  
Habitable Zones ◽  
Planetary Orbits ◽  
Consistent Manner ◽  
Earth Like Planets ◽  
Complex Matter ◽  
Planetary Habitability

AbstractDetermining planetary habitability is a complex matter, as the interplay between a planet's physical and atmospheric properties with stellar insolation has to be studied in a self consistent manner. Standardized atmospheric models for Earth-like planets exist and are commonly accepted as a reference for estimates of Habitable Zones. In order to define Habitable Zone boundaries, circular orbital configurations around main sequence stars are generally assumed. In gravitationally interacting multibody systems, such as double stars, however, planetary orbits are forcibly becoming non circular with time. Especially in binary star systems even relatively small changes in a planet's orbit can have a large impact on habitability. Hence, we argue that a minimum model for calculating Habitable Zones in binary star systems has to include dynamical interactions.

scholarly journals Circumbinary Habitable Zones in the Presence of a Giant Planet

2021 ◽  
Vol 8 ◽  
Author(s):  
Nikolaos Georgakarakos ◽  
Siegfried Eggl ◽  
Ian Dobbs-Dixon
Keyword(s):  
Binary Systems ◽  
Binary Star ◽  
Giant Planet ◽  
Giant Planets ◽  
Habitable Zone ◽  
Complex Environments ◽  
The Past ◽  
Habitable Zones ◽  
Planetary Orbits

Determining habitable zones in binary star systems can be a challenging task due to the combination of perturbed planetary orbits and varying stellar irradiation conditions. The concept of “dynamically informed habitable zones” allows us, nevertheless, to make predictions on where to look for habitable worlds in such complex environments. Dynamically informed habitable zones have been used in the past to investigate the habitability of circumstellar planets in binary systems and Earth-like analogs in systems with giant planets. Here, we extend the concept to potentially habitable worlds on circumbinary orbits. We show that habitable zone borders can be found analytically even when another giant planet is present in the system. By applying this methodology to Kepler-16, Kepler-34, Kepler-35, Kepler-38, Kepler-64, Kepler-413, Kepler-453, Kepler-1647, and Kepler-1661 we demonstrate that the presence of the known giant planets in the majority of those systems does not preclude the existence of potentially habitable worlds. Among the investigated systems Kepler-35, Kepler-38, and Kepler-64 currently seem to offer the most benign environment. In contrast, Kepler-16 and Kepler-1647 are unlikely to host habitable worlds.

Habitable Planet Formation in Binary Star Systems

Icarus ◽  
1998 ◽  
Vol 132 (1) ◽  
pp. 196-203 ◽  
Author(s):  
Daniel P Whitmire ◽  
John J Matese ◽  
Lee Criswell ◽  
Seppo Mikkola
Keyword(s):  
Planet Formation ◽  
Binary Star ◽  
Habitable Planet

scholarly journals Resilient habitability of nearby exoplanet systems

2019 ◽  
Vol 492 (1) ◽  
pp. 352-368 ◽  
Author(s):  
Giorgi Kokaia ◽  
Melvyn B Davies ◽  
Alexander J Mustill
Keyword(s):  
Giant Planet ◽  
Planetary Systems ◽  
Observational Constraints ◽  
Habitable Zone ◽  
Habitable Zones ◽  
Test Particles ◽  
Planetary Orbits ◽  
Two Systems ◽  
Earth Like Planets ◽  
Exoplanet Systems

ABSTRACT We investigate the possibility of finding Earth-like planets in the habitable zone of 34 nearby FGK-dwarfs, each known to host one giant planet exterior to their habitable zone detected by RV. First we simulate the dynamics of the planetary systems in their present day configurations and determine the fraction of stable planetary orbits within their habitable zones. Then, we postulate that the eccentricity of the giant planet is a result of an instability in their past during which one or more other planets were ejected from the system. We simulate these scenarios and investigate whether planets orbiting in the habitable zone survive the instability. Explicitly we determine the fraction of test particles, originally found in the habitable zone, which remain in the habitable zone today. We label this fraction the resilient habitability of a system. We find that for most systems the probability of planets existing [or surviving] on stable orbits in the habitable zone becomes significantly smaller when we include a phase of instability in their history. We present a list of candidate systems with high resilient habitability for future observations. These are: HD 95872, HD 154345, HD 102843, HD 25015, GJ 328, HD 6718, and HD 150706. The known planets in the last two systems have large observational uncertainties on their eccentricities, which propagate into large uncertainties on their resilient habitability. Further observational constraints of these two eccentricities will allow us to better constrain the survivability of Earth-like planets in these systems.

Stability of inclined orbits of terrestrial planets in habitable zones

2009 ◽  
Vol 57 (4) ◽  
pp. 434-440 ◽  
Author(s):  
Barbara Funk ◽  
Richard Schwarz ◽  
Elke Pilat-Lohinger ◽  
Áron Süli ◽  
Rudolf Dvorak
Keyword(s):  
Terrestrial Planets ◽  
Habitable Zones
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