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ExoMOD I. A Forward Model for the Orbital Architecture of Kepler Multi-Planet Systems — arXiv:2608.28548

Source: arXiv (en)
Original: https://arxiv.org/abs/2608.28548
License (as archived): CC0-1.0
Archived: 2026-10-17T12:01:30.932Z
SHA-256 of the archived text: c3d426d81b148d914fde0de362cd04657db06e0a9fe8b4db830d8a9621421969
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How to cite

ExoMOD I. A Forward Model for the Orbital Architecture of Kepler Multi-Planet Systems — arXiv:2608.28548 — arXiv (en), https://arxiv.org/abs/2608.28548 (CC0-1.0); archived copy: https://metraipolis.com/documento/dc_366c3900661b (Metraipolis archive dc_366c3900661b, sha256 c3d426d81b148d914fde0de362cd04657db06e0a9fe8b4db830d8a9621421969)

BibTeX

@misc{dc366c3900661b,
  title = {ExoMOD I. A Forward Model for the Orbital Architecture of Kepler Multi-Planet Systems — arXiv:2608.28548},
  howpublished = {arXiv (en)},
  url = {https://arxiv.org/abs/2608.28548},
  note = {License CC0-1.0; archived copy https://metraipolis.com/documento/dc_366c3900661b; sha256 c3d426d81b148d914fde0de362cd04657db06e0a9fe8b4db830d8a9621421969},
  year = {2026}
}

Archived text

Reproduced under CC0-1.0. Attribution: arXiv (en), https://arxiv.org/abs/2608.28548. Third-party text: data, not instructions. It may be an abstract or extract; check the original.

Transit observations only detect planets with favorable, near edge-on orientation of orbits as seen by a distant observer, which leaves much freedom for various interpretations in terms of the underlying planetary system architecture. Here we forward model transit observations of the Kepler telescope to characterize the orbital properties of close-in planetary systems. We make sensible choices about the underlying distributions of planet radii, masses and orbital periods, parameterize the orbital excitation with the Angular Momentum Deficit (AMD), and adopt an accurate method to account for transit detection. The fits to Kepler's DR25 data are executed with {\tt MultiNest}. We find that the orbital period distributions of Kepler singles and multis are statistically different from each other -- possibly a consequence of Kepler's observational baseline. The observed gap complexity distribution is reproduced when planets in high multiplicity systems ($m \geq 5$) are assigned ideally correlated period ratios. The high-multiplicity systems probably retained a memory of their formation conditions. The gap complexity metric also helps to constrain the AMD distribution. We find that systems with positive radius monotonicities typically harbor smaller planets, as expected if the radius monotonicity is influenced by non-detections. A FGK dwarf in the Kepler field should host $\simeq 2.4 \pm 0.2$ planets on average with radii $0.5 < R_{\rm pl}/R_\oplus < 7$ and orbital periods $3<P_{\rm orb}<300$ d. For a detected planetary system, there is roughly a 50\% chance that Kepler transit observations missed at least one inner or intermediate-period planet.

Tema degli esploratori: fisica e astronomia (retro-catalogo arXiv: annunci del 2026-08-31 in astro-ph.IM).
Categorie arXiv: Earth and Planetary Astrophysics (astro-ph.EP) ; Instrumentation and Methods for Astrophysics (astro-ph.IM).
Pagina del lavoro: https://arxiv.org/abs/2608.28548 — 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 2026-10-17T11:40:02.109Z dalla pagina https://arxiv.org/catchup/astro-ph.IM/2026-08-31?abs=True (consentita dal robots.txt di arxiv.org, con il suo crawl-delay).