Volume 581, September 2015
|Number of page(s)||8|
|Section||Planets and planetary systems|
|Published online||28 August 2015|
The Solar Twin Planet Search
II. A Jupiter twin around a solar twin⋆
1 Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave, Chicago, IL 60637, USA
2 Departamento de Astronomia do IAG/USP, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900 São Paulo, SP, Brazil
3 McDonald Observatory and Department of Astronomy, University of Texas at Austin, USA
4 Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston, ACT 2611, Australia
5 Instituto de Fisica, Universidade Federal do Rio Grande do Sul, Av. Bento Goncalves 9500, Porto Alegre, RS, Brazil
6 Institut für Astrophysik, University of Göttingen, Germany
Received: 26 January 2015
Accepted: 27 June 2015
Context. With high-precision radial velocity surveys reaching a sufficiently long time baseline, the domain of long-period planet detections has recently opened up. The search for Jupiter-like planets is especially important if we wish to investigate the prevalence of solar system analogs, but their detection is complicated by the existence of stellar activity cycles on similar timescales. Radial velocity data with sufficiently long-term instrumental precision and robust methods of diagnosing activity are crucial to the detection of extrasolar Jupiters.
Aims. Through our HARPS survey for planets around solar twin stars, we have identified a promising Jupiter twin candidate around the star HIP11915. We characterize this Keplerian signal and investigate its potential origins in stellar activity.
Methods. We carry out a Markov chain Monte Carlo (MCMC) analysis of the radial velocity data. To examine the signal’s origin, we employ a variety of statistical tests using activity diagnostics such as the Ca II H and K lines and line asymmetry tracers.
Results. Our analysis indicates that HIP11915 hosts a Jupiter-mass planet with a 3800-day orbital period and low eccentricity. Although we cannot definitively rule out an activity cycle interpretation, we find that a planet interpretation is more likely based on a joint analysis of radial velocity and activity index data.
Conclusions. The challenges of long-period radial velocity signals addressed in this paper are critical for the ongoing discovery of Jupiter-like exoplanets. If planetary in nature, the signal investigated here represents a very close analog to the solar system in terms of both Sun-like host star and Jupiter-like planet.
Key words: planets and satellites: detection / techniques: radial velocities / stars: activity
Table 3 and Fig. 5 are available in electronic form at http://www.aanda.org
© ESO, 2015
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