J/A+A/605/A72 Planetary systems AMD-stability (Laskar+, 2017)
AMD-stability and the classification of planetary systems.
Laskar J., Petit A.
<Astron. Astrophys. 605, A72 (2017)>
=2017A&A...605A..72L 2017A&A...605A..72L (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Stars, double and multiple ; Planets
Keywords: chaos - celestial mechanics -
planets and satellites: dynamical evolution and stability -
planets and satellites: formation - planets and satellites: general
Abstract:
We present here in full detail the evolution of the angular momentum
deficit (AMD) during collisions as it was described in (Laskar 2000,
Physical Review Letters, 84, 3240). Since then, the AMD has been
revealed to be a key parameter for the understanding of the outcome of
planetary formation models. We define here the AMD-stability criterion
that can be easily verified on a newly discovered planetary system. We
show how AMD-stability can be used to establish a classification of
the multiplanet systems in order to exhibit the planetary systems that
are long-term stable because they are AMD-stable, and those that are
AMD- unstable which then require some additional dynamical studies to
conclude on their stability. The AMD-stability classification is
applied to the 131 multiplanet systems from The Extrasolar Planet
Encyclopaedia database (exoplanet.eu) for which the orbital elements
are sufficiently well known.
Description:
We give here the values of the AMD-stability coefficients β
computed in the paper as well as the orbital elements used for this
computation. Most of the orbital elements are issued from the
Extrasolar Planet Encyclopaedia (exoplanet.eu). For some systems, we
chose to use the values of the Exoplanets Orbit Database
(exoplanets.org) or of the original articles. Details on the
computation of the coefficients can be found in the paper.
The systems are sorted alphabetically, planets are sorted by period.
Periods are in days and masses in Earth mass (using the recommended
nominal value from Prsa et al. (2016AJ....152...41P 2016AJ....152...41P)). For the
extrasolar systems, in order to take into account the uncertainties
provided in the catalogs, we used as an effective eccentricity the
quantity noted here sqrt<e2>. It corresponds to the mean of the
eccentricity distribution computed from the assumed Gaussian
distributions for ecosω and esinω. The coefficients β
correspond to the AMD-stability of the inner pair. For the first
planet, it corresponds to the AMD-stability associated to the first
planet and the star. The orbital elements of the Solar System are the
initial conditions at J2000 from Laskar et al. (2004A&A...428..261L 2004A&A...428..261L),
expressed in the invariant reference frame of Laskar et al.
(2004A&A...428..261L 2004A&A...428..261L). For the Solar System, we used the real AMD of
the system instead of assuming the equipartition between the
eccentricity and inclinations contributions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 58 313 AMD-stability coefficients of extrasolar systems
tablea2.dat 65 8 AMD-stability coefficients of the Solar System
tablea3.dat 34 27 AMD-stability coefficients of the hierarchical
systems
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- System System name
16 A1 --- Planet Planet designation
18- 28 F11.4 d Per Period
30- 37 F8.2 Mgeo Mass Mass ((GM)NEp)
39- 43 F5.3 --- Ecc Eccentricity
45- 49 F5.3 --- <Ecc> Mean eccentricity, sqrt(<e2>)
51- 58 F8.3 --- beta beta AMD-stability coefficient
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Planet Planet designation
9- 20 F12.6 d Per Period
22- 32 F11.7 Mgeo Mass Mass ((GM)NEp)
34- 43 F10.8 --- Ecc Eccentricity
45- 52 F8.6 deg Inc Inclination
55- 65 F11.7 --- beta beta AMD-stability coefficient
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- System System name
20- 26 A7 --- Planet Planet designation
28- 34 F7.5 --- beta beta AMD-stability coefficient
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Acknowledgements:
Jacques Laskar, laskar(at)imcce.fr
(End) Patricia Vannier [CDS] 14-Jun-2017