Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1001.4774)
· On-line Data
· References in the article
· Citations to the Article (93) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (9)
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The HARPS search for southern extra-solar planets. XIX. Characterization and dynamics of the GJ 876 planetary system
Authors:
Correia, A. C. M.; Couetdic, J.; Laskar, J.; Bonfils, X.; Mayor, M.; Bertaux, J.-L.; Bouchy, F.; Delfosse, X.; Forveille, T.; Lovis, C.; Pepe, F.; Perrier, C.; Queloz, D.; Udry, S.
Affiliation:
AA(Departamento de Física, Universidade de Aveiro, Campus de Santiago, 3810-193 Aveiro, Portugal ; IMCCE, CNRS-UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France ), AB(IMCCE, CNRS-UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France), AC(IMCCE, CNRS-UMR8028, Observatoire de Paris, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France), AD(Laboratoire d'Astrophysique, Observatoire de Grenoble, Université J. Fourier, CNRS-UMR5571, BP 53, 38041 Grenoble, France), AE(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland), AF(Service d'Aéronomie du CNRS/IPSL, Université de Versailles Saint-Quentin, BP 3, 91371 Verrières-le-Buisson, France), AG(Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie, 98 bis Bd Arago, 75014 Paris, France), AH(Laboratoire d'Astrophysique, Observatoire de Grenoble, Université J. Fourier, CNRS-UMR5571, BP 53, 38041 Grenoble, France), AI(Laboratoire d'Astrophysique, Observatoire de Grenoble, Université J. Fourier, CNRS-UMR5571, BP 53, 38041 Grenoble, France), AJ(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland), AK(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland), AL(Laboratoire d'Astrophysique, Observatoire de Grenoble, Université J. Fourier, CNRS-UMR5571, BP 53, 38041 Grenoble, France), AM(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland), AN(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland)
Publication:
Astronomy and Astrophysics, Volume 511, id.A21, 10 pp. (A&A Homepage)
Publication Date:
02/2010
Origin:
EDP Sciences
Astronomy Keywords:
stars: individual: GJ 876, planetary systems, techniques: radial velocities, methods: observational, methods: numerical, celestial mechanics
DOI:
10.1051/0004-6361/200912700
Bibliographic Code:
2010A&A...511A..21C

Abstract

Precise radial-velocity measurements for data acquired with the HARPS spectrograph infer that three planets orbit the M 4 dwarf star GJ 876. In particular, we confirm the existence of planet d, which orbits every 1.93785 days. We find that its orbit may have significant eccentricity (e = 0.14), and deduce a more accurate estimate of its minimum mass of 6.3~M_⊕. Dynamical modeling of the HARPS measurements combined with literature velocities from the Keck Observatory strongly constrain the orbital inclinations of the b and c planets. We find that ib = 48.9° ± 1.0° and ic = 48.1° ± 2.1°, which infers the true planet masses of Mb = 2.64~± 0.04~M_Jup and Mc = 0.83 ± 0.03~M_Jup, respectively. Radial velocities alone, in this favorable case, can therefore fully determine the orbital architecture of a multi-planet system, without the input from astrometry or transits. The orbits of the two giant planets are nearly coplanar, and their 2:1 mean motion resonance ensures stability over at least 5 Gyr. The libration amplitude is smaller than 2°, suggesting that it was damped by some dissipative process during planet formation. The system has space for a stable fourth planet in a 4:1 mean motion resonance with planet b, with a period around 15 days. The radial velocity measurements constrain the mass of this possible additional planet to be at most that of the Earth.

Based on observations made with the HARPS instrument on the ESO 3.6 m telescope at La Silla Observatory under the GTO programme ID 072.C-0488; and on observations obtained at the Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology.The Table with the HARPS radial velocities is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/511/A21


Associated Articles

Part  1     Part  2     Part  3     Part  4     Part  6     Part  5     Part  7     Part  8     Part 11     Part  9     Part 10     Part 12     Part 13     Part 14     Part 15     Part 17     Part 18     Catalog Description     Part 19     Part 20     Part 21     Part 22     Part 23     Part 24     Part 25     Part 26     Part 27     Part 28     Part 29     Part 30     Part 31     Part 32     Part 33     Part 34     Part 35    


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints