Giant Planet Occurrence in the Stellar Mass-Metallicity Plane
Open accessAbstract
Correlations between stellar properties and the occurrence rate of exoplanets can be used to inform the target selection of future planet-search efforts and provide valuable clues about the planet-formation process. We analyze a sample of 1266 stars drawn from the California Planet Survey targets to determine the empirical functional form describing the likelihood of a star harboring a giant planet as a function of its mass and metallicity. Our stellar sample ranges from M dwarfs with masses as low as 0.2 M ⊙ to intermediate-mass subgiants with masses as high as 1.9 M ⊙ . In agreement with previous studies, our sample exhibits a planet-metallicity correlation at all stellar masses; the fraction of stars that harbor giant planets scales as f ∝ 10 1.2[Fe/H] . We can rule out a flat metallicity relationship among our evolved stars (at 98% confidence), which argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." Our data also rule out a constant planet occurrence rate for [Fe/H] < 0, indicating that giant planets continue to become rarer at sub-Solar metallicities. We also find that planet occurrence increases with stellar mass ( f ∝ M ⋆ ), characterized by a rise from 3% around M dwarfs (0.5 M ⊙ ) to 14% around A stars (2 M ⊙ ), at Solar metallicity. We argue that the correlation between stellar properties and giant planet occurrence is strong supporting evidence of the core-accretion model of planet formation.
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Only 1% of Sun-like stars host a hot Jupiter, and the occurrence rate falls off around M dwarfs.
“Only 1% of Sun-like stars host one, and the occurrence rate falls off around the most numerous stars, the M dwarfs (Johnson et al. 2010).”
From Origins of Hot Jupiters (2018) · cites this paper as Johnson et al. 2010
The Introduction says M dwarfs are more numerous than Sun-like stars and are less likely to host Jupiter-mass planets. But the paper measures giant-planet occurrence using planets with semimajor axes under 2.5 AU (section 2.2); it does not establish that 1% of Sun-like stars host a hot Jupiter or that the hot-Jupiter rate specifically falls around M dwarfs. Page numbers are unavailable in our copy. (LLM, conf=0.88)
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Research works printed but not linked: 8
- Artigau, É., Biller, B. A., Wahhaj, Z., Hartung, M., Hayward, T. L., Close, L. M., Chun, M. R., Liu, M. C., et al. 2008, Proc. SPIE, 7014, 70141Z.
- Bean, J. L., Seifahrt, A., Hartman, H., Nilsson, H., Wiedemann, G., Reiners, A., Dreizler, S., & Henry, T. J. 2009, preprint (ArXiv:0911.3148) · arXiv
- Claudi, R. U., Turatto, M., Antichi, J., Gratton, R., Scuderi, S., Cascone, E., Mesa, D., Desidera, S., et al. 2006, Proc. SPIE, 6269, 62692Y
- Gould, A., Dong, S., Gaudi, B. S., Udalski, A., Bond, I. A., Greenhill, J., Street, R. A., Dominik, M., et al. 2010, ArXiv e-prints Gray, D. F., & Nagar, P. 1985, ApJ, 298, 756
- Haghighipour, N., Vogt, S. S., Butler, R. P., Rivera, E. J., Laughlin, G., Meschiari, S., & Henry, G. W. 2010, ArXiv e-prints Hatzes, A. P., Cochran, W. D., Endl, M., McArthur, B., Paulson, D. B., Walker, G. A. H., Campbell, B., & Yang, S. 2003, ApJ, 599, 1383
- Howard, A. W., Johnson, J. A., Marcy, G. W., Fischer, D. A., Wright, J. T., Bernat, D., Henry, G. W., Peek, K. M. G., et al. 2010a, ArXiv e-prints ---. 2010b, ArXiv e-prints 914 JOHNSON ET AL. 2010 PASP, 122:905-915
- Meru, F., & Bate, M. R. 2010, ArXiv e-prints Mordasini, C., Alibert, Y., Benz, W., & Naef, D. 2009, A&A, 501, 1161
- Nielsen, E. L., & Close, L. M. 2009, preprint (ArXiv:0909.4531) · arXiv
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Dawson, R. I., & Johnson, J. A. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051853 · Cited by 622 · see citing works
Self-citationTHE FREQUENCY OF HOT JUPITERS ORBITING NEARBY SOLAR-TYPE STARS
Wright, J. T., Marcy, G. W., Howard, A. W., Johnson, J. A., Morton, T. D., & Fischer, D. A. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/753/2/160 · Cited by 371 · see citing works
Self-citationExoplanet Biosignatures: A Framework for Their Assessment
Catling, D. C., Krissansen-Totton, J., Kiang, N. Y., Crisp, D., Robinson, T. D., DasSarma, S., Rushby, A. J., Del Genio, A., Bains, W., & Domagal-Goldman, S. (2018) · Astrobiology · doi:10.1089/ast.2017.1737 · Cited by 225 · see citing works
Statistical properties of brown dwarf companions: implications for different formation mechanisms
Ma, B., & Ge, J. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu134 · Cited by 153 · see citing works
- Authors
- Johnson, J. A., Aller, K. M., Howard, A. W., & Crepp, J. R.
- Affiliations
- University of Hawaiʻi at Mānoa (US)
- Space Sciences Laboratory (US)
- California Institute of Technology (US)
- Venue
- Publications of the Astronomical Society of the Pacific
- Publisher
- IOP Publishing
- Published
- 2010-08
- Volume
- 122
- Issue
- 894
- Pages
- 905-915
- ISSN
- 0004-6280 (ISSN-L)
- 1538-3873
- OpenAlex
- W2126624130
- Cited by
- 782
- References
- 0
- Citations by year
- 2026: 25 · 2025: 58 · 2024: 53 · 2023: 51 · 2022: 43 · 2021: 59 · 2020: 48 · 2019: 55 · 2018: 48 · 2017: 47 · 2016: 60 · 2015: 48 · 2014: 44 · 2013: 44 · 2012: 55
- FWCI
- 25.38
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Publications of the Astronomical Society of the Pacific (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- metallicity, stellar mass, M dwarfs, subgiants, planet-metallicity correlation, core accretion, planet formation, stellar evolution
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