J/MNRAS/448/1044 Simulation data for 50 planetary model systems (Hansen+, 2015)
Secular effects of tidal damping in compact planetary systems.
Hansen B.M.S., Murray N.
<Mon. Not. R. Astron. Soc., 448, 1044-1059 (2015)>
=2015MNRAS.448.1044H 2015MNRAS.448.1044H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Models, evolutionary
Keywords: planets and satellites: dynamical evolution and stability -
planet-star interactions
Abstract:
We describe the long-term evolution of compact systems of terrestrial
planets, using a set of simulations that match the statistical
properties of the observed exoplanet distribution. The evolution is
driven by tidal dissipation in the planetary interiors, but the
systems evolve as a whole due to secular gravitational interactions.
We find that, for Earth-like dissipation levels, planetary orbits can
be circularized out to periods ∼100 d, an order of magnitude larger
than is possible for single planets. The resulting distribution of
eccentricities is a qualitative match to that inferred from transit
timing variations, with a minority of non-zero eccentricities
maintained by particular secular configurations. The coupling of the
tidal and secular processes enhance the inward migration of the
innermost planets in these systems, and can drive them to short
orbital periods. Resonant interactions of both the mean motion and
secular variety are observed, although the interactions are not strong
enough to drive systemic instability in most cases. However, we
demonstrate that these systems can easily be driven unstable if
coupled to giant planets on longer period orbits.
Description:
We have used the results (after 10 Myr of evolution) of 50 model
realizations of the 20 M⊕ rocky planet systems from
Hansen & Murray (2013ApJ...775...53H 2013ApJ...775...53H) to define the initial state of
our systems, given in Table A1. We assume all the planets are of
terrestrial class, in the sense that they obey the tidal dissipation,
and evolve them for 10 Gyr according to our model for tidal+secular
evolution. The final configurations are given in Table A2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 60 294 Initial Conditions for each of the 50 model
systems
tablea2.dat 60 245 Final conditions of model systems shown in
Table A1, after 1010 yr of evolution with
Q'p=10
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See also:
J/AJ/116/1998 : Outer planetary systems (Levison+, 1998)
J/AJ/151/59 : Catalog of Earth-Like Exoplanet Survey Targets
(Chandler+, 2016)
Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Model [1/50] Model system number
4- 5 I2 --- Num [1/10] Condition number
7- 11 F5.3 AU a Semi-major axis, in AU
13- 18 F6.3 Mgeo M Planet mass, in earth mass
20- 24 F5.3 --- Eccentricity <e2>1/2 (1)
26- 31 F6.2 deg omega Longitude of periastron ω
33- 38 F6.3 deg Inclination <i2>1/2 (1)
40- 45 F6.2 deg Omega Longitude of ascending node Ω
47- 60 A14 --- emode Indicates to which eccentricity oscillation
mode(s) each planet is strongly coupled (2)
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Note (1): The eccentricities and inclinations are shown as the average of each
planet over the secular oscillations given the initial configuration.
Note (2): Modes are numbered by frequency, with one being the highest frequency
mode. In most cases, this is the frequency of the mode dominated by
the innermost planet, although this is sometimes superseded if there
is a near-commensurability in the system.
The numerical labels indicate which planets (counting from inside out)
are strongly coupled in the sense defined in Section 2.1.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 20-Nov-2017