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Peer-reviewedCC BY 4.0The Astronomical Journal

The Discovery of K2-232c: Divergent Formation Histories for Hot and Warm Jupiters Based on Outer Companion Eccentricity

  • Jessica A. Ranshaw1
  • Xian-Yu Wang1
  • Jennifer A. Burt2
  • Juan I. Espinoza-Retamal3,4,5
  • Brandon T. Radzom1,6
  • R. Paul Butler7
  • Bradford P. Holden8
  • Steven S. Vogt8
  • Songhu Wang1
8 affiliations
  1. 1Indiana University
  2. 2California Institute of Technology
  3. 3Princeton University
  4. 4Pontificia Universidad Católica de Chile
  5. 5Millennium Institute for Astrophysics
  6. 6Caltech/IPAC-NASA Exoplanet Science Institute
  7. 7Carnegie Science
  8. 8University of California
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Abstract

Ever since their discovery, hot Jupiters have been one of the most studied types of exoplanets to exist thanks to their significant size, their proximity to their host star, and their significant departure from anything present in our solar system. Yet, the details of their formation and evolution remain unclear, including their connection, if any, to the wider-orbiting warm-Jupiter population. In this work, we present the discovery of K2-232c, an eccentric cold Jupiter ( P = 195 0 − 120 + 140 days, e = 0.35 2 − 0.076 + 0.095 , M sin i = 5.3 1 − 0.45 + 0.48 M J ) companion in a known warm Jupiter ( P = 11.1684377 ± 0.0000010 days, e = 0.24 5 − 0.024 + 0.023 , M = 0.42 7 − 0.036 + 0.039 M J ) system. Placing this system in context with the literature, we find that cold-Jupiter eccentricities are generally higher in hot-Jupiter systems as compared to warm-Jupiter systems, suggesting the formation of hot Jupiters is more dynamically violent than warm Jupiters. This adds further evidence to the claim that these two populations are independent from one another with cold Jupiters appearing to play a crucial role in shaping the formation of both.

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Cite

BibTeXRIS
BibTeX
@article{ranshaw2026discovery,
  title = {{The Discovery of K2-232c: Divergent Formation Histories for Hot and Warm Jupiters Based on Outer Companion Eccentricity}},
  author = {Jessica A. Ranshaw and Xian-Yu Wang and Jennifer A. Burt and Juan I. Espinoza-Retamal and Brandon T. Radzom and R. Paul Butler and Bradford P. Holden and Steven S. Vogt and Songhu Wang},
  journal = {The Astronomical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-3881/ae9ff1},
  url = {https://iopscience.iop.org/article/10.3847/1538-3881/ae9ff1},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - The Discovery of K2-232c: Divergent Formation Histories for Hot and Warm Jupiters Based on Outer Companion Eccentricity
AU  - Jessica A. Ranshaw
AU  - Xian-Yu Wang
AU  - Jennifer A. Burt
AU  - Juan I. Espinoza-Retamal
AU  - Brandon T. Radzom
AU  - R. Paul Butler
AU  - Bradford P. Holden
AU  - Steven S. Vogt
AU  - Songhu Wang
PY  - 2026
DA  - 2026/10/08
JO  - The Astronomical Journal
DO  - 10.3847/1538-3881/ae9ff1
UR  - https://iopscience.iop.org/article/10.3847/1538-3881/ae9ff1
AB  - Ever since their discovery, hot Jupiters have been one of the most studied types of exoplanets to exist thanks to their significant size, their proximity to their host star, and their significant departure from anything present in our solar system. Yet, the details of their formation and evolution remain unclear, including their connection, if any, to the wider-orbiting warm-Jupiter population. In this work, we present the discovery of K2-232c, an eccentric cold Jupiter ( P = 195 0 − 120 + 140 days, e = 0.35 2 − 0.076 + 0.095 , M sin i = 5.3 1 − 0.45 + 0.48 M J ) companion in a known warm Jupiter ( P = 11.1684377 ± 0.0000010 days, e = 0.24 5 − 0.024 + 0.023 , M = 0.42 7 − 0.036 + 0.039 M J ) system. Placing this system in context with the literature, we find that cold-Jupiter eccentricities are generally higher in hot-Jupiter systems as compared to warm-Jupiter systems, suggesting the formation of hot Jupiters is more dynamically violent than warm Jupiters. This adds further evidence to the claim that these two populations are independent from one another with cold Jupiters appearing to play a crucial role in shaping the formation of both.
SN  - 0004-6256
SN  - 1538-3881
ER  -