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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 (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) 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:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
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 --- <e> Eccentricity <e2>1/2 (1) 26- 31 F6.2 deg omega Longitude of periastron ω 33- 38 F6.3 deg <i> 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)
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.
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 20-Nov-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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