Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published August 20, 2014 | Submitted + Published
Journal Article Open

Influence of Stellar Multiplicity on Planet Formation. II. Planets are Less Common in Multiple-star Systems with Separations Smaller than 1500 AU

Abstract

Almost half of the stellar systems in the solar neighborhood are made up of multiple stars. In multiple-star systems, planet formation is under the dynamical influence of stellar companions, and the planet occurrence rate is expected to be different from that of single stars. There have been numerous studies on the planet occurrence rate of single star systems. However, to fully understand planet formation, the planet occurrence rate in multiple-star systems needs to be addressed. In this work, we infer the planet occurrence rate in multiple-star systems by measuring the stellar multiplicity rate for planet host stars. For a subsample of 56 Kepler planet host stars, we use adaptive optics (AO) imaging and the radial velocity (RV) technique to search for stellar companions. The combination of these two techniques results in high search completeness for stellar companions. We detect 59 visual stellar companions to 25 planet host stars with AO data. Three stellar companions are within 2'' and 27 within 6''. We also detect two possible stellar companions (KOI 5 and KOI 69) showing long-term RV acceleration. After correcting for a bias against planet detection in multiple-star systems due to flux contamination, we find that planet formation is suppressed in multiple-star systems with separations smaller than 1500 AU. Specifically, we find that compared to single star systems, planets in multiple-star systems occur 4.5 ± 3.2, 2.6 ± 1.0, and 1.7 ± 0.5 times less frequently when a stellar companion is present at a distance of 10, 100, and 1000 AU, respectively. This conclusion applies only to circumstellar planets; the planet occurrence rate for circumbinary planets requires further investigation.

Additional Information

© 2014 American Astronomical Society. Received 2014 May 15; accepted 2014 July 11; published 2014 August 4. The authors thank Howard Isaacson and Matt Giguere for helpful comments and proofreading the paper. The research is made possible by the data from the Kepler Community Follow up Observing Program (CFOP). The authors acknowledge all the CFOP users who uploaded the AO and RV data used in the paper. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Jiwei Xie is supported by a Foundation for the Author of National Excellent Doctoral Dissertation (FANEDD) of PR China.

Attached Files

Published - 0004-637X_791_2_111.pdf

Submitted - 1407.3344v1.pdf

Files

0004-637X_791_2_111.pdf
Files (1.6 MB)
Name Size Download all
md5:6da7755c0a2121736e0e3d723bfb0f15
894.7 kB Preview Download
md5:9701ef39508891c80b499416f9421d88
716.4 kB Preview Download

Additional details

Created:
August 22, 2023
Modified:
October 17, 2023