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Are Near Resonant Multiple-planet Systems from Kepler Young? — arXiv:2608.12786

Source: arXiv (en)
Original: https://arxiv.org/abs/2608.12786
License (as archived): CC0-1.0
Archived: 2026-10-19T05:08:38.101Z
SHA-256 of the archived text: 8d6a8b93c4f985be7ecd2c230bca2f8e0ccf345cc64d0bd2494d4bfb4c900d2b
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How to cite

Are Near Resonant Multiple-planet Systems from Kepler Young? — arXiv:2608.12786 — arXiv (en), https://arxiv.org/abs/2608.12786 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_77ff45cfa2df (Metraipolis archive dc_77ff45cfa2df, sha256 8d6a8b93c4f985be7ecd2c230bca2f8e0ccf345cc64d0bd2494d4bfb4c900d2b)

BibTeX

@misc{dc77ff45cfa2df,
  title = {Are Near Resonant Multiple-planet Systems from Kepler Young? — arXiv:2608.12786},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2608.12786},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_77ff45cfa2df; sha256 8d6a8b93c4f985be7ecd2c230bca2f8e0ccf345cc64d0bd2494d4bfb4c900d2b},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2608.12786. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Recent studies have claimed that Kepler multi-planet systems hosting near-resonant planet pairs---particularly those near second-order mean-motion resonances (MMRs)---exhibit smaller stellar velocity dispersions than the general population of Kepler planet hosts. Interpreting velocity dispersion as an age indicator, these works concluded that near-resonant systems are systematically younger. We revisit this claim, but we explicitly account for contamination by thick disk stars, which are kinematically hotter and follow a different age-velocity dispersion relation (AVR) than thin disk stars. Using the kinematic criterion to separate thin and thick disk stars, we show that systems classified as having plausible second-order resonant pairs are preferentially hosted by brighter, closer stars and are therefore less contaminated by thick disk stars than the overall sample. After applying a cut to remove probable thick disk contaminants (${\rm TD/D}<0.1$), the vertical velocity dispersion of near-resonant systems becomes statistically indistinguishable from that of the overall Kepler multi-planet sample. We conclude that the apparent kinematic youth of near-resonant systems in Kepler may not be due to a genuine age difference, but rather arises from observational selection effects linked to host star properties and planet detectability. We also comment on the kinematic ages of ultra-short-period planets (USPs).

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-08-14 in astro-ph.EP).
Categorie arXiv: Earth and Planetary Astrophysics (astro-ph.EP) ; Astrophysics of Galaxies (astro-ph.GA).
Pagina del lavoro: https://arxiv.org/abs/2608.12786 — autori e testo completo sono lì (qui omessi i nomi: nessun dato personale nel deposito).
Licenza: titolo e abstract sono metadati arXiv distribuiti in CC0 1.0; il testo completo ha la licenza scelta dagli autori, indicata sulla pagina.
Letto il 2026-10-19T05:00:24.497Z dalla pagina https://arxiv.org/catchup/astro-ph.EP/2026-08-14?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).