Effects of Secular Interactions in Extrasolar Planetary Systems

Fred C. Adams; Gregory Laughlin

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Effects of Secular Interactions in Extrasolar Planetary Systems

Fred C. Adams, Gregory Laughlin

Astrophysics · Submitted 14 Jun 2006

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim For the case of hot Jupiters, we discuss how the absence of observed eccentricity implies the absence of companion planets.

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What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.27 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.96 · compares with prior results 0.09 · mentions code or data availability 0.02.

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arXiv listing abstract v1. Results and the main claim are underlined; show every role.

This paper studies the effects of dynamical interactions among the planets in observed extrasolar planetary systems, including hypothetical additional bodies, with a focus on secular perturbations. These interactions cause the eccentricities of the planets to explore a distribution of values over time scales that are long compared to observational time baselines, but short compared to the age of the systems. The same formalism determines the eccentricity forcing of hypothetical test bodies (terrestrial planets) in these systems and we find which systems allow for potentially habitable planets. Such planets would be driven to nonzero orbital eccentricity and we derive the distribution of stellar flux experienced by the planets over the course of their orbits. The general relativistic corrections to secular interaction theory are included in the analysis and such effects are important in systems with close planets ($\sim$4 day orbits). Some extrasolar planetary systems (e.g., Upsilon Andromedae) can be used as a test of general relativity, whereas in other systems, general relativity can be used to constrain the system parameters (e.g., $\sin i \gta 0.93$ for HD160691). For the case of hot Jupiters, we discuss how the absence of observed eccentricity implies the absence of companion planets.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	This paper studies the effects of dynamical interactions among the planets in observed extrasolar planetary systems, including hypothetical additional bodies, with a focus on secular perturbations.	contribution 0.99	0.89	0.06	asserted 0.94
s1	These interactions cause the eccentricities of the planets to explore a distribution of values over time scales that are long compared to observational time baselines, but short compared to the age of the systems.	result 0.75	0.35	0.13	asserted 1.00
s2	The same formalism determines the eccentricity forcing of hypothetical test bodies (terrestrial planets) in these systems and we find which systems allow for potentially habitable planets.	contribution 0.74	0.94	0.15	asserted 1.00
s3	Such planets would be driven to nonzero orbital eccentricity and we derive the distribution of stellar flux experienced by the planets over the course of their orbits.	contribution 0.46	0.92	0.09	asserted 0.88
s4	The general relativistic corrections to secular interaction theory are included in the analysis and such effects are important in systems with close planets ($\sim$4 day orbits).	method 0.64	0.80	0.06	asserted 0.99
s5	Some extrasolar planetary systems (e.g., Upsilon Andromedae) can be used as a test of general relativity, whereas in other systems, general relativity can be used to constrain the system parameters (e.g., $\sin i \gta 0.93$ for HD160691).	result 0.71	0.71	0.07	asserted 0.59
s6	For the case of hot Jupiters, we discuss how the absence of observed eccentricity implies the absence of companion planets.	interpretation 0.77	0.68	0.16	asserted 0.79

What kind of paper the classifier reports this is: theoretical result 0.78 · evidence from proof or derivation 0.75.

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The paper

Original abstract

This paper studies the effects of dynamical interactions among the planets in observed extrasolar planetary systems, including hypothetical additional bodies, with a focus on secular perturbations. These interactions cause the eccentricities of the planets to explore a distribution of values over time scales that are long compared to observational time baselines, but short compared to the age of the systems. The same formalism determines the eccentricity forcing of hypothetical test bodies (terrestrial planets) in these systems and we find which systems allow for potentially habitable planets. Such planets would be driven to nonzero orbital eccentricity and we derive the distribution of stellar flux experienced by the planets over the course of their orbits. The general relativistic corrections to secular interaction theory are included in the analysis and such effects are important in systems with close planets ($\sim$4 day orbits). Some extrasolar planetary systems (e.g., Upsilon Andromedae) can be used as a test of general relativity, whereas in other systems, general relativity can be used to constrain the system parameters (e.g., $\sin i \gta 0.93$ for HD160691). For the case of hot Jupiters, we discuss how the absence of observed eccentricity implies the absence of companion planets.

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References

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2 arXiv papers cite this in 2 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it

Uses its method or tool 1 paper

To determine the habitable zone for each of our stars, we compute the flux using Equation 1 from [ref] [ref] : [equation] where $L_⋆$ is stellar luminosity, $a_p$ is semi-major axis of the planet's orbit, and $e_p$ is the planetary eccentricity.

Assessing Planetary Stability and Long-Term Habitability in Nearby Stellar Binaries: 70 Oph, 36 Oph, $\gamma$ Leo · Habitable Zone Calculation · 0.94

Cites it as background 1 paper

In the first scenario, planets are perturbed to an eccentric orbit by the gravitational influence of an outer body (such as another planet or a stellar companion, known as Kozai-Lidov oscillations), secular interactions or planet-planet scattering [ref] .

The TASSIE Program. II: Three Close-In Companions Orbiting Sun-Like Stars · Introduction · 0.97

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