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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

The slower rotation of planet-hosting stars revisited

  • Avraham Binnenfeld1
  • Amitay Sussholz2
  • Simchon Faigler2
  • Tsevi Mazeh2,3
  1. 1Institute of Physics, École Polytechnique Fédérale de Lausanne (EPFL) , Observatoire de Sauverny, Chemin Pegasi 51b, 1290 Versoix ,
  2. 2School of Physics and Astronomy, Tel Aviv University , Tel Aviv 6997801 ,
  3. 3Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg ,
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Abstract

Previous studies combined rotation periods derived from Kepler photometry, stellar parameters from previous Gaia Data Releases, and planet hosts from the NASA Exoplanet Archive to conclude that statistically planet-hosting stars rotate slower than stars without detected planets. Here, we revisit these studies by using similar Kepler rotational period sample, but with an updated Gaia DR3-based stellar parameter catalogue and an updated exoplanet catalogue. We apply minimal sample cuts in evolutionary state, metallicity, and distance, and then model the stellar rotation period as a function of effective temperature alone. For each star, we derive the ratio of its observed period to the temperature-expected period, and compare the ratio distributions for the planet-host and non-host stars. For periods shorter than 20 d, the planet-host distribution of this ratio is shifted towards longer periods; the period-ratio median is ∼15% larger for hosts than for non-hosts (pKS = 2.4 × 10−4). We also examine the recently published TESS All-Sky Rotation Survey (TARS) and find a similar trend. However, the strongly structured period distribution precludes a robust comparison between the host and the non-host stars. Therefore, the updated analysis, using more robust stellar and planetary parameters, recovers the previously reported association, strengthening the case for a genuine connection between stellar rotation and planet occurrence.

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Cite

BibTeXRIS
BibTeX
@article{binnenfeld2026slower,
  title = {{The slower rotation of planet-hosting stars revisited}},
  author = {Avraham Binnenfeld and Amitay Sussholz and Simchon Faigler and Tsevi Mazeh},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = nov,
  doi = {10.1093/mnras/stag2119},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2119/9013661},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - The slower rotation of planet-hosting stars revisited
AU  - Avraham Binnenfeld
AU  - Amitay Sussholz
AU  - Simchon Faigler
AU  - Tsevi Mazeh
PY  - 2026
DA  - 2026/11/05
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2119
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2119/9013661
AB  - Previous studies combined rotation periods derived from Kepler photometry, stellar parameters from previous Gaia Data Releases, and planet hosts from the NASA Exoplanet Archive to conclude that statistically planet-hosting stars rotate slower than stars without detected planets. Here, we revisit these studies by using similar Kepler rotational period sample, but with an updated Gaia DR3-based stellar parameter catalogue and an updated exoplanet catalogue. We apply minimal sample cuts in evolutionary state, metallicity, and distance, and then model the stellar rotation period as a function of effective temperature alone. For each star, we derive the ratio of its observed period to the temperature-expected period, and compare the ratio distributions for the planet-host and non-host stars. For periods shorter than 20 d, the planet-host distribution of this ratio is shifted towards longer periods; the period-ratio median is ∼15% larger for hosts than for non-hosts (pKS = 2.4 × 10−4). We also examine the recently published TESS All-Sky Rotation Survey (TARS) and find a similar trend. However, the strongly structured period distribution precludes a robust comparison between the host and the non-host stars. Therefore, the updated analysis, using more robust stellar and planetary parameters, recovers the previously reported association, strengthening the case for a genuine connection between stellar rotation and planet occurrence.
SN  - 0035-8711
SN  - 1365-2966
ER  -