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THE FREQUENCY OF HOT JUPITERS ORBITING NEARBY SOLAR-TYPE STARS
Open accessAbstract
We determine the fraction of F, G, and K dwarfs in the solar neighborhood hosting hot Jupiters as measured by the California Planet Survey from the Lick and Keck planet searches. We find the rate to be 1.2% ± 0.38%, which is consistent with the rate reported by Mayor et al. from the HARPS and CORALIE radial velocity (RV) surveys. These numbers are more than double the rate reported by Howard et al. for Kepler stars and the rate of Gould et al. from the OGLE-III transit search; however, due to small number statistics these differences are of only marginal statistical significance. We explore some of the difficulties in estimating this rate from the existing RV data sets and comparing RV rates to rates from other techniques.
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“Discovery and characterization of thousands of hot Jupiters in exoplanetary systems via the transit method ( Wright et al. 2012 ) .”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Wright et al. 2012
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Cites
A Jupiter-mass companion to a solar-type star
Mayor, M., & Queloz, D. (1995) · Nature · doi:10.1038/378355a0 · Cited by 4,111
The Planet‐Metallicity Correlation
Fischer, D. A., & Valenti, J. A. (2005) · The Astrophysical Journal · doi:10.1086/428383 · Cited by 1,641
Self-citationDetection of Planetary Transits Across a Sun-like Star
Charbonneau, D., Brown, T. M., Latham, D. W., & Mayor, M. (2000) · The Astrophysical Journal · doi:10.1086/312457 · Cited by 1,415
A Transiting “51 Peg–like” Planet
Henry, G. W., Marcy, G. W., Butler, R. P., & Vogt, S. S. (2000) · The Astrophysical Journal · doi:10.1086/312458 · Cited by 964
Self-citationButler, R. P., Wright, J. T., Marcy, G. W., Fischer, D. A., Vogt, S. S., Tinney, C. G., Jones, H. R. A., Carter, B. D., Johnson, J. A., McCarthy, C., et al. (2006) · The Astrophysical Journal · doi:10.1086/504701 · Cited by 914
Self-citationCumming, A., Butler, R. P., Marcy, G. W., Vogt, S. S., Wright, J. T., & Fischer, D. A. (2008) · Publications of the Astronomical Society of the Pacific · doi:10.1086/588487 · Cited by 892
Self-citationKEPLERINPUT CATALOG: PHOTOMETRIC CALIBRATION AND STELLAR CLASSIFICATION
Brown, T. M., Latham, D. W., Everett, M. E., & Esquerdo, G. A. (2011) · The Astronomical Journal · doi:10.1088/0004-6256/142/4/112 · Cited by 868
Giant Planet Occurrence in the Stellar Mass-Metallicity Plane
Johnson, J. A., Aller, K. M., Howard, A. W., & Crepp, J. R. (2010) · Publications of the Astronomical Society of the Pacific · doi:10.1086/655775 · Cited by 782
Self-citationThe metal-rich nature of stars with planets
Santos, N. C., Israelian, G., & Mayor, M. (2001) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20010648 · Cited by 502
ELODIE metallicity-biased search for transiting Hot Jupiters
Bouchy, F., Udry, S., Mayor, M., Moutou, C., Pont, F. J., Iribarne, N., da Silva, R., Ilovaisky, S. A., Queloz, D. P., Santos, N. C., et al. (2005) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200500201 · Cited by 495
Research works printed but not linked: 7
- Bonfils, 2011, A&A
- Borucki, 2010, BAAS, 41, 215
- Gould, 2006, Acta Astron., 56, 1
- Howard, 2011, ApJ
- Malmquist, 1920, Medd. Lund. Astron. Obs., 22, 1
- Mayor, 2011, A&A
- Perryman, 1997, The HIPPARCOS and TYCHO Catalogues, Astrometric and Photometric Star Catalogues Derived from the ESA HIPPARCOS Space Astrometry Mission
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Tran, Q. H., Bowler, B. P., Cochran, W. D., Endl, M., Stefánsson, G., Mahadevan, S., Ninan, J. P., Bender, C. F., Halverson, S., Roy, A., et al. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/abe041 · Cited by 20
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BackgroundInfluentialSelf-citationA SOPHIE RV search for giant planets around young nearby stars (YNS)
Grandjean, A., Lagrange, A. ‐., Meunier, N., Rubini, P., Desidera, S., Galland, F., Borgniet, S., Zicher, N., Messina, S., Chauvin, G., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039672 · Cited by 18
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BackgroundInfluentialQuantifying the Influence of Jupiter on the Earth’s Orbital Cycles
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A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Gan, T., Cadieux, C., Jahandar, F., Vazan, A., Wang, S. X., Mao, S., Alvarado-Montes, J. A., Lin, D. N. C., Artigau, É., Cook, N. J., et al. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acf56d · Cited by 22
TOI-1670 c, a 40 day Orbital Period Warm Jupiter in a Compact System, Is Well Aligned
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Self-citationHow Complete Are Surveys for Nearby Transiting Hot Jupiters?
Yee, S. W., Winn, J. N., & Hartman, J. D. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac2958 · Cited by 20
Scholz, A., Mužić, K., Jayawardhana, R., Quinlan, L., & Wurster, J. (2022) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ac9431 · Cited by 16
Survivability of moon systems around ejected gas giants
Rabago, I., & Steffen, J. H. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2552 · Cited by 15
“If a significant fraction of hot Jupiter systems are formed by planet-planet scattering (hot Jupiters exist around roughly 1% of stars (Wright et al. 2012)), then the number of potential life-harboring rogue planets could be hundreds of millions or billions across the galaxy.”
BackgroundFormation of giant planets around intermediate-mass stars
Johnston, H. F., Panić, O., & Liu, B. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3254 · Cited by 19
Planet Occurrence: Doppler and Transit Surveys
Winn, J. N. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_195 · Cited by 18
Populations of Planets in Multiple Star Systems
Martin, D. V. (2018) · Springer eBooks · doi:10.1007/978-3-319-30648-3_156-1 · Cited by 15
An, Q., Brandt, T. D., Brandt, G. M., & Venner, A. (2025) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/adfa99 · Cited by 15
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Zandt, J. V., Petigura, E. A., Lubin, J., Weiss, L. M., Turtelboom, E. V., Fetherolf, T., Murphy, J. M. A., Crossfield, I. J. M., Gilbert, G. J., Močnik, T., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/adbbed · Cited by 14
Self-citationForming different planetary systems
Zhou, J., Xie, J., Liu, H.-G., Zhang, H., & Sun, Y. (2012) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/12/8/010 · Cited by 15
“However, with the increase of RV precision and the number of detected exoplanets, HJs are found to be in fact rare objects (e.g., Cumming et al. 2008; Wright et al. 2012).”
BackgroundMethodInfluentialScaling K2. III. Comparable Planet Occurrence in the FGK Samples of Campaign 5 and Kepler
Zink, J. K., Hardegree-Ullman, K., Christiansen, J., Petigura, E., Dressing, C., Schlieder, J., Ciardi, D., & Crossfield, I. (2020) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 14
Orphaned exomoons: Tidal detachment and evaporation following an exoplanet–star collision
Martinez, M. A. S., Stone, N. C., & Metzger, B. D. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2464 · Cited by 14
“While the fraction of Solar type stars hosting Hot Jupiters is only ∼ 1% (Wright et al. 2012), the exoplanet fraction as a whole is higher around more massive stars (Johnson et al. 2010).”
BackgroundA sensitivity analysis of the WFCAM Transit Survey for short-period giant planets around M dwarfs
Kovács, G., Hodgkin, S. T., Sipőcz, B., Pinfield, D. J., Barrado, D., Birkby, J., Cappetta, M., Cruz, P., Koppenhoefer, J., Martín, E. L., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt571 · Cited by 14
“RV studies determined a rate of 0.9–1.5 per cent (Marcy et al. 2005; Cumming et al. 2008; Mayor et al. 2011; Wright et al. 2012), while transit studies have a systematically lower rate (roughly half of this value) at 0.3–0.5 per cent (Gould et al. 2006; Howard et al. 2012, H12 hereafter).”
BackgroundInfluentialHot Jupiter engulfment by an early red giant in 3D hydrodynamics
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Ikoma, M., & Kobayashi, H. (2025) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-052722-094843 · Cited by 22
MASS CONSTRAINTS OF THE WASP-47 PLANETARY SYSTEM FROM RADIAL VELOCITIES
Sinukoff, E., Howard, A. W., Petigura, E. A., Fulton, B. J., Isaacson, H. T., Weiss, L. M., Brewer, J. M., Hansen, B. M. S., Hirsch, L. A., Christiansen, J. L., et al. (2017) · University of Southern Queensland ePrints (University of Southern Queensland) · Cited by 13
Self-citationGaidos, E. J., Anderson, D. R., Lépine, S., Colón, K. D., Maravelias, G., Narita, N., Chang, E., Beyer, J., Fukui, A., Armstrong, J. D., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2078 · Cited by 13
“Our determination of an order-of-magnitude lower relative occurrence of hot Neptunes around Kepler stars echoes the findings of Wright et al. (2012), who found a deficit of hot Jupiters around these stars.”
ResultJohns, D., Reed, P. A., Rodriguez, J. E., Pepper, J. A., Stassun, K. G., Penev, K., Gaudi, B. S., Labadie-Bartz, J. M., Fulton, B. J., Quinn, S. N., et al. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab24c7 · Cited by 13
HAT-P-55b: A Hot Jupiter Transiting a Sun-Like Star1
Juncher, D., Buchhave, L. A., Hartman, J. D., Bakos, G. Á., Bieryla, A., Kovács, T., Boisse, I., Latham, D. W., Kovács, G., Bhatti, W., et al. (2015) · Publications of the Astronomical Society of the Pacific · doi:10.1086/682725 · Cited by 13
“The occurrence rate of hot Jupiters in the Solar neighborhood is around 1% (Udry & Santos 2007; Wright et al. 2012).”
BackgroundK2-HERMES II. Planet-candidate properties from K2 Campaigns 1-13
Wittenmyer, R. A., Clark, J., Sharma, S., Stello, D., Horner, J., Kane, S. R., Stevens, C. P., Wright, D. J., Spina, L., Čotar, K., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1528 · Cited by 12
“…planets orbiting perilously close to their host stars (e.g. Mayor & Queloz 1995; Masset & Papaloizou 2003; Bouchy et al. 2005; Hellier et al. 2011; Wright et al. 2012; Albrecht et al. 2012), and discovered others with planets moving on highly elongated, eccentric orbits, similar to those of…”
ResultResidual Gas and Dust around Transition Objects and Weak T Tauri Stars*
Doppmann, G. W., Najita, J. R., & Carr, J. S. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa5c3c · Cited by 12
“Hot Jupiters (P<10 days; >M i Msin 0.1 J) are present in ∼1% of Sunlike stars (Wright et al. 2012), whereas TOs represent 10%– 15% of the disk-bearing population of young stars (Muzerolle et al. 2010; Espaillat et al. 2014).”
BackgroundInfluentialKPS-1b: The First Transiting Exoplanet Discovered Using an Amateur Astronomer's Wide-field CCD Data
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“Despite their rarity in the Milky Way (∼1% occurrence rate, e.g., Wright et al. 2012), hot Jupiters (i.e., planets with minimum mass M sin i>0.5MJup and orbital period P 10 days) are particularly favorable targets for non-space surveys.”
BackgroundThe exomoon corridor for multiple moon systems
Teachey, A. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1840 · Cited by 12
TESSgiants transiting giants V – two hot Jupiters orbiting red giant hosts
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Self-citationSpinning up a Daze: TESS Uncovers a Hot Jupiter Orbiting the Rapid Rotator TOI-778
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“This brackets the rate found by radial velocity surveys of 1.2 ± 0.38% (Wright et al. 2012), with the caveat that our estimates would be lowered by tidal disruptions (Guillochon et al. 2011) and hot Jupiters migrating into the host star through tidal dissipation in the central body (Beaugé &…”
BackgroundInfluentialLack of close-in, massive planets of main-sequence A-type stars from Kepler
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KPS-1b: The First Transiting Exoplanet Discovered Using an Amateur Astronomer's Wide-field CCD Data
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The Demographics of Wide-Separation Planets
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“From RV surveys, it is known that hot Jupiters are relatively rare compared to the population of Jupiters with longer periods [167].”
BackgroundTransit Photometry as an Exoplanet Discovery Method
Deeg, H. J., & Alonso, R. (2018) · Springer eBooks · doi:10.1007/978-3-319-30648-3_117-1 · Cited by 10
Tracking Advanced Planetary Systems (TAPAS) with HARPS-N
Niedzielski, A., Villaver, E., Nowak, G., Adamów, M., Kowalik, K., Wolszczan, A., Deka-Szymankiewicz, B., Adamczyk, M., & Maciejewski, G. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527869 · Cited by 12
“Currently, we know that about 0.5% of stars hosts these kind of objects (Wright et al. 2012) and the class is limited to gas planets within 0.1 AU or, roughly, with orbital periods of up to ten days.”
BackgroundInfluentialExoplanet Geology: What Can We Learn from Current and Future Observations?
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“Work on exoplanet population statistics has now shown that hot Jupiters are not common, with frequencies of ∼ 1 % (e.g. Wright et al. 2012; Dawson & Johnson 2018; Zhu & Dong 2021).”
BackgroundSearching for GEMS: The Occurrence of Giant Planets Orbiting M Dwarfs within 100 pc
Glusman, R., Cañas, C., Kanodia, S., Han, T., Fernandes, R., Stefánsson, G., Ford, E. B., Maney, M., Monson, A., Hotnisky, A., et al. (2025) · Astronomical Journal · doi:10.3847/1538-3881/ae2fbb · Cited by 9
Self-citationData calibration for the MASCARA and bRing instruments
Talens, G. J., Deul, E. R., Stuik, R., Burggraaff, O., Lesage, A.-L., Spronck, J. F. P., Mellon, S. N., Bailey, J. I., Mamajek, E. E., Kenworthy, M. A., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834070 · Cited by 9
“From radial velocity (RV) surveys the occurrence rate of hot Jupiters around FGK-stars is estimated to to be ∼1% (e.g. Mayor et al. 2011; Wright et al. 2012), while transit surveys such as Kepler suggest a lower occurrence rate of ∼0.4% (e.g. Howard et al. 2012; Fressin et al. 2013).”
BackgroundResultInfluentialMULTIPLEXING PRECISION RVs: SEARCHING FOR CLOSE-IN GAS GIANTS IN OPEN CLUSTERS
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“…are needed to find the comparatively rare cases with detectable velocity amplitudes: only 1.2 ± 0.4% of all FGK stars in the solar neighborhood harbor hot gas giants (Wright et al. 2012) and cluster occurrence rates appear similar (Meibom et al. 2013) so hundreds of targets must be monitored.”
BackgroundInfluentialRadial-velocity search and statistical studies for short-period planets in the Pleiades open cluster
拓也, 宝., Takarada, T., 文衛, 佐., Bun'ei, S., 正士, 大., Masashi, O., 安範, 堀., Yasunori, H., & Fujii, M. S. (2019) · Institutional Repositories DataBase (IRDB) · Cited by 9
Harada, C., Dressing, C., Turtelboom, E., Kane, S., Blunt, S., Dietrich, J., Hinkel, N., Li, Z.-X., Mamajek, E. E., Rice, M., et al. (2024) · Astronomical Journal · doi:10.3847/1538-3881/ae0b62 · Cited by 9
Data calibration for the MASCARA and bRing instruments
Talens, G. J., Deul, E., Stuik, R., Burggraaff, O., Lesage, A.-L., Spronck, J. F. P., Mellon, S. N., Bailey, J. I., Mamajek, E. E., Kenworthy, M. A., et al. (2018) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201834070/pdf · Cited by 8
Populations of Extrasolar Giant Planets from Transit and Radial Velocity Surveys
Santerne, A. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_154 · Cited by 8
“The occurrence rate estimates were first published in Marcy et al. (2005), and subsequently in Cumming et al. (2008), Howard et al. (2010), and Wright et al. (2012).”
BackgroundParametric study of polar configurations around binaries
Giuppone, C. A., & Cuello, N. (2019) · Journal of Physics Conference Series · doi:10.1088/1742-6596/1365/1/012023 · Cited by 8
The highly inflated giant planet WASP-174b
Mancini, L., Sarkis, P., Henning, T. K., Bakos, G. Á., Bayliss, D., Bento, J., Bhatti, W., Brahm, R., Csubry, Z., Espinoza, N., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936532 · Cited by 8
“Given that hot giant planets are known to be relatively rare from both RV surveys (Mayor et al. 2011; Wright et al. 2012) and transit surveys (Fressin et al. 2013; Fulton & Petigura 2018), in order to discover such planets it Article published by EDP Sciences A30, page 1 of 12 is necessary to scan…”
BackgroundNiedzielski, A., Villaver, E., Nowak, G., Adamów, M., Maciejewski, G., Kowalik, K., Wolszczan, A., Deka-Szymankiewicz, B., & Adamczyk, M. (2016) · LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) · Cited by 8
Making hot Jupiters in stellar clusters: The importance of binary exchange
Li, D., Mustill, A. J., Davies, M. B., & Gong, Y. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3387 · Cited by 14
The origin of the occurrence rate profile of gas giants inside 100 d
Ali-Dib, M., Johansen, A., & Huang, C. X. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1272 · Cited by 7
“They found a HJ occurrence rate about half of what is found by the radial velocity surveys (Marcy et al. 2005; Wright et al. 2012), and confirmed a similar deficit of planets outside the period valley starting at 10 days orbits.”
Mass-Radius Relations of Giant Planets: The Radius Anomaly and Interior Models
Laughlin, G. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_1 · Cited by 9
Characterizing Exoplanet Habitability
Kopparapu, R. (2005) · University of Arizona Press eBooks · doi:10.2458/azu_uapress_9780816540068-ch017 · Cited by 8
MASCARA-4 b/bRing-1 b: A retrograde hot Jupiter around a bright A-type star
Dorval, P., Talens, G. J., Otten, G. P. P. L., Brahm, R., Jordán, A., Torres, P., Vanzi, L., Zapata, A., Henry, T. J., Paredes, L. A., et al. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935611/pdf · Cited by 7
A search for transiting planets around hot subdwarfs
Thuillier, A., Grootel, V. V., Dévora-Pajares, M., Pozuelos, F. J., Charpinet, S., & Siess, L. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243554 · Cited by 7
Relative Occurrence Rate between Hot and Cold Jupiters as an Indicator to Probe Planet Migration
Gan, T., Guo, K., Liu, B., Wang, S. X., Mao, S., Büchner, J., & Fulton, B. J. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad3deb · Cited by 8
Dynamical instabilities in post-disc evolution: hot Jupiters left isolated
He, Y., Wu, D.-H., & Jin, S. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1076 · Cited by 9
Zandt, J. V., & Petigura, E. A. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad8c3b · Cited by 7
CoRoT: The First Space-Based Transit Survey to Explore the Close-in Planet Population
Deleuil, M., & Fridlund, M. C. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_79 · Cited by 7
“For hot-Jupiters, this result is in agreement with the occurrence rates estimated for this planet population from radial velocity surveys (Wright et al. 2012; Mayor et al. 2011) but not with those from Kepler data (Howard et al.”
ResultAnanyeva, V. I., Ivanova, A., Venkstern, A. A., Shashkova, I. A., Yudaev, A., Tavrov, A. V., Korablev, O., & Bertaux, J. (2020) · Icarus · doi:10.1016/j.icarus.2020.113773 · Cited by 7
Microlensed radio emission from exoplanets
Shiohira, Y., Terada, Y., Mukuno, D., Fujii, Y., & Takahashi, K. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1294 · Cited by 7
“The occurrence of a hot Jupiter around FGK stars has been estimated to be PHJ ∼ 1% (Mayor et al. 2011; Wright et al. 2012; Fressin et al. 2013).”
BackgroundOrbital Decay of the Ultra-hot Jupiter TOI-2109b: Tidal Constraints and Transit-timing Analysis
Alvarado-Montes, J. A., Sucerquia, M., Zuluaga, J. I., & Schwab, C. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ade057 · Cited by 6
The New Generation Planetary Population Synthesis (NGPPS)
Emsenhuber, A., Mordasini, C., Mayor, M., Marmier, M., Udry, S., Burn, R., Schlecker, M., Mishra, L., Alibert, Y., Benz, W., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452485 · Cited by 6
Making hot Jupiters in stellar clusters – II. Efficient formation in binary systems
Li, D., Mustill, A. J., Davies, M. B., & Gong, Y. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3207 · Cited by 9
Combining Transit and Radial Velocity: A Synthesized Population Model
Kunimoto, M., & Bryson, S. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/abd2c1 · Cited by 6
“This paper has not yet been accepted, though it has been cited in several previous occurrence-rate studies (e.g., Wright et al. 2012; Santerne et al. 2016; Fernandes et al. 2019).”
ResultNGTS-21b: an inflated Super-Jupiter orbiting a metal-poor K dwarf
Alves, D. R., Jenkins, J. S., Vines, J. I., Nielsen, L. D., Gill, S., Acton, J. S., Anderson, D. R., Bayliss, D., Bouchy, F., Breytenbach, H. B., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2884 · Cited by 6
Peluso, D. O., Dalba, P. A., Wright, D. J., Esposito, T. M., Sgro, L. A., Weaver, I. C., Marchis, F., Dragomir, D., Villanueva, S., Fulton, B. J., et al. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad2772 · Cited by 6
Bagheri, F., López, R., & Shahmoradi, A. (2024) · Frontiers in Astronomy and Space Sciences · doi:10.3389/fspas.2024.1400032 · Cited by 6
“A multitude of exoplanet detection techniques rely on indirect optical/infrared wavelength observations (Mandel and Agol, 2002; Seager and Hui, 2002; Guyon et al., 2005; Traub and Oppenheimer, 2010; Gaudi, 2012; Wright et al., 2012; Knutson et al., 2014; Bagheri et al., 2019).”
Bagheri, F., Lopez, R., & Pham, K. H. (2024) · Frontiers in Astronomy and Space Sciences · doi:10.3389/fspas.2024.1398379 · Cited by 6
Planet Occurrence: Doppler and Transit Surveys
Winn, J. N. (2018) · Springer eBooks · doi:10.1007/978-3-319-30648-3_195-1 · Cited by 8
“There is a 3 σ discrepancy between the rate of 0.8–1.2% measured in Doppler surveys (Wright et al. 2012; Mayor et al. 2011) and 0.6% measured using Kepler data (Howard et al. 2012; Petigura et al. 2018).”
MethodInfluentialThe Demographics of Close-In Planets
Biazzo, K., Bozza, V., Mancini, L., & Sozzetti, A. (2022) · Astrophysics and space science library · doi:10.1007/978-3-030-88124-5_3 · Cited by 7
TOI-1135 b: A young hot Saturn-size planet orbiting a solar-type star
Mallorquín, M., Lodieu, N., Béjar, V. J. S., Osorio, M. R. Z., Sanz‐Forcada, J., Alarcón, M. R., Tabernero, H. M., Nagel, E., Collins, K. A., Ciardi, D. R., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202349016 · Cited by 6
Generation of an optimal target list for the Exoplanet Characterisation Observatory (EChO)
Varley, R., Waldmann, I. P., Pascale, E., Tessenyi, M., Hollis, M. D. J., Morales, J., Tinetti, G., Swinyard, B. M., Deroo, P., Ollivier, M., et al. (2015) · UCL Discovery (University College London) · Cited by 5
A Search for Transiting Planets in the Globular Cluster M4 with K2: Candidates and Occurrence Limits
Wallace, J. J., Hartman, J. D., & Bakos, G. Á. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab66b4 · Cited by 5
Winter, A. J., Clarke, C. J., Rosotti, G. P., & Giersz, M. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1863 · Cited by 6
The rate of planet–star coalescences due to tides and stellar evolution
Popkov, A. V., & Попов, С. Б. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2783 · Cited by 6
“If in our numerical calculations we select only mergers of main sequence stars with hot jupiters (using the criterion from Wright et al. 2012), we obtain for the same Q′? the rate 3× 10−3 yr−1 (for direct impacts, tidal disruptions and stable accretion events altogether).”
BackgroundInfluentialMost Hot Jupiters Were Cool Giant Planets for More Than 1 Gyr
Schmidt, S. P., & Schlaufman, K. C. (2026) · The Astronomical Journal · doi:10.3847/1538-3881/ae3c11 · Cited by 11
Kovács, G., Hodgkin, S. T., Sipőcz, B., Pinfield, D. J., Barrado, D., Birkby, J., Cappetta, M., Cruz, P., Koppenhoefer, J., Martín, E. L., et al. (2013) · EPJ Web of Conferences · doi:10.1051/epjconf/20134701002 · Cited by 4
SEEJ: SmallSat Exosphere Explorer of Hot Jupiters
Wolk, S. J., Hong, J. E., Romaine, S. E., Poppenhaeger, K., Kenter, A. T., Moorhead, A. V., Gallagher, D. L., Moore, C. S., Elvis, M. E., Kraft, R., et al. (2019) · UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy · doi:10.1117/12.2529380 · Cited by 4
“Statistically, it is estimated that about 1% of stars host a hot Jupiter [19].”
BackgroundMorgan, M., Bowler, B. P., & Tran, Q. H. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/ae0e16 · Cited by 7
MANGOS – II. Five new giant planets orbiting low-mass stars
Dransfield, G., Timmermans, M., Sebastian, D., Rackham, B. V., Burgasser, A. J., Barkaoui, K., Triaud, A. H. M. J., Gillon, M., Almenara, J. M., Casewell, S. L., et al. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag448 · Cited by 5
Li, J., & Zhu, W. (2026) · The Astronomical Journal · doi:10.3847/1538-3881/ae5e52 · Cited by 3
Elemental Abundances of Kepler Objects of Interest in APOGEE DR17
Behmard, A., Ness, M., Cunningham, E. C., & Bedell, M. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acc32a · Cited by 3
The evolution of lithium in FGK dwarf stars
de Andrés, F. L., Reza, R. D. L., Cruz, P., Cuenda-Muñoz, D., Alfaro, E. J., Chavero, C., & Cifuentes, C. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202346744 · Cited by 3
Constraining planetary formation models using conditional occurrences of various planet types
Gajendran, S., Jiang, I., Yeh, L., & Sariya, D. P. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae501 · Cited by 3
TOI-2458 b: A mini-Neptune consistent with in situ hot Jupiter formation
Šubjak, J., Gandolfi, D., Goffo, E., Rapetti, D., Jankowski, D., Mizuki, T., Dai, F., Serrano, L. M., Wilson, T. G., Goździewski, K., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451057 · Cited by 3
The Case for Edge-on Binaries: An Avenue Toward Comparative Exoplanet Demographics
Hand, J. E., Gerbig, K., & Rice, M. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/adce04 · Cited by 3
Tran, Q. H., Bowler, B. P., Cochran, W. D., Bender, C. F., Halverson, S., Mahadevan, S., Ninan, J. P., Robertson, P. M., Roy, A., Stefánsson, G., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/ade230 · Cited by 3
Pinotti, R., Boechat-Roberty, H. M., & de Mello, G. F. P. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2592 · Cited by 3
“Studies indicate that they are expected to be present in 1.2% of the F, G and K dwarfs in the solar neighborhood (Wright et al. 2012), an estimate which is still not well established (Wang et al. 2015).”
BackgroundInfluentialNew photometric analysis of hot Jupiter: WASP-135b
Öztürk, O., & Erdem, A. (2020) · New Astronomy · doi:10.1016/j.newast.2020.101454 · Cited by 3
Winter, A. J., Rosotti, G. P., Clarke, C. J., & Giersz, M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3272 · Cited by 3
Metadata
- Authors
- Wright, J. T., Marcy, G. W., Howard, A. W., Johnson, J. A., Morton, T. D., & Fischer, D. A.
- Affiliations
- Pennsylvania State University (US)
- University of California, Berkeley (US)
- California Institute of Technology (US)
- Yale University (US)
- Corresponding author
- Wright, J. T.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2012-06-25
- Volume
- 753
- Issue
- 2
- Pages
- 160
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2158240367
- Cited by
- 371
- References
- 40
- Citations by year
- 2026: 15 · 2025: 21 · 2024: 24 · 2023: 16 · 2022: 20 · 2021: 22 · 2020: 27 · 2019: 32 · 2018: 41 · 2017: 34 · 2016: 35 · 2015: 28 · 2014: 25 · 2013: 18 · 2012: 10
- FWCI
- 14.18
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (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 › Instrumentation › Astronomy and Astrophysical Research
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Keywords
- hot Jupiters, solar-type stars, planet occurrence rate, radial velocity surveys, transit surveys, Kepler, OGLE-III, Lick Observatory, Keck Observatory, nearby stars
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