Precise radial velocities of giant stars

XIII. A second Jupiter orbiting in 4:3 resonance in the 7 CMa system

R. Luque*, T. Trifonov, S. Reffert, A. Quirrenbach, M. H. Lee, S. Albrecht, M. Fredslund Andersen, V. Antoci, F. Grundahl, C. Schwab, Wolthoff

*Corresponding author for this work

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

We report the discovery of a second planet orbiting the K giant star 7 CMa based on 166 high-precision radial velocities obtained with Lick, HARPS, UCLES, and SONG. The periodogram analysis reveals two periodic signals of approximately 745 and 980 d, associated with planetary companions. A double-Keplerian orbital fit of the data reveals two Jupiter-like planets with minimum masses mb sini ∼ 1.9 MJ and mc sini ∼ 0.9 MJ, orbiting at semimajor axes of ab ∼ 1.75 au and ac ∼ 2.15 au, respectively. Given the small orbital separation and the large minimum masses of the planets, close encounters may occur within the time baseline of the observations; thus, a more accurate N-body dynamical modeling of the available data is performed. The dynamical best-fit solution leads to collision of the planets and we explore the long-term stable configuration of the system in a Bayesian framework, confirming that 13% of the posterior samples are stable for at least 10 Myr. The result from the stability analysis indicates that the two planets are trapped in a low-eccentricity 4:3 mean motion resonance. This is only the third discovered system to be inside a 4:3 resonance, making this discovery very valuable for planet formation and orbital evolution models.

Original languageEnglish
Article numberA136
Pages (from-to)1-8
Number of pages8
JournalAstronomy and Astrophysics
Volume631
DOIs
Publication statusPublished - 6 Nov 2019

Keywords

  • techniques: radial velocities
  • planetary systems
  • planets and satellites: dynamical evolution and stability
  • planets and satellites: detection

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