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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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Citations
Cites
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Cited by
Sorted by citations
LSST: From Science Drivers to Reference Design and Anticipated Data Products
Ivezić, Ž., Kahn, S. M., Tyson, J. A., Abel, B., Acosta, E., Allsman, R., Alonso, D., AlSayyad, Y., Anderson, S. F., Andrew, J., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab042c · Cited by 4,357
“• Discovery and characterization of thousands of hot Jupiters in exoplanetary systems via the transit method (Wright et al. 2012).”
MethodThe Occurrence and Architecture of Exoplanetary Systems
Winn, J. N., & Fabrycky, D. C. (2015) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082214-122246 · Cited by 926
“The discrepancy might be attributable to differences in metallicity or the frequency of multiple-star systems between the two samples (Gould et al. 2006, Bayliss & Sackett 2011, Wright et al. 2012).”
BackgroundThe NASA Exoplanet Archive: Data and Tools for Exoplanet Research
Akeson, R., Chen, X., Ciardi, D. R., Crane, M. K., Good, J., Harbut, M., Jackson, E. S., Kane, S. R., Laity, A. C., Leifer, S. D., et al. (2013) · Publications of the Astronomical Society of the Pacific · doi:10.1086/672273 · Cited by 906
“This includes high-resolution spectra from the N2K Consortium (Fischer et al. 2007), the M2K program (Fischer et al. 2012), and the California Planet search team (Wright et al. 2012).”
MethodDawson, R. I., & Johnson, J. A. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051853 · Cited by 622
Self-citationImaging Extrasolar Giant Planets
Bowler, B. P. (2016) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/128/968/102001 · Cited by 450
“…stellar host mass, the overall giant planet occurrence rate for the full sample of 384 stars is 0.6+0.7 −0.5%, which happens to be comparable to the frequency of hot Jupiters around FGK stars in the field (1.2 ± 0.4%; Wright et al. 2012) and in the Kepler sample (0.5 ± 0.1%; Howard et al. 2012).”
BackgroundInfluentialThe California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets
Petigura, E. A., Marcy, G. W., Winn, J. N., Weiss, L. M., Fulton, B. J., Howard, A. W., Sinukoff, E., Isaacson, H., Morton, T. D., & Johnson, J. A. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaa54c · Cited by 399
“Wright et al. (2012) reported 10 hot Jupiters from a sample of 836 stars or a rate of 1.2± 0.4%, twice the rate presented here.”
BackgroundMethodInfluentialSelf-citationTERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE
Burke, C. J., Christiansen, J. L., Mullally, F. R., Seader, S., Huber, D., Rowe, J. F., Coughlin, J. L., Thompson, S. E., Catanzarite, J., Clarke, B. D., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/809/1/8 · Cited by 356
“…Field, CA 94035, USA 2005; Naef et al. 2005; Gould et al. 2006; Sahu et al. 2006; Cumming et al. 2008; Bowler et al. 2010; Howard et al. 2010; Bayliss & Sackett 2011; Mayor et al. 2011; van Saders & Gaudi 2011; Wright et al. 2012; Bonfils et al. 2013; Meibom et al. 2013; Clanton & Gaudi 2014).”
Self-citationParmentier, V., Line, M. R., Bean, J. L., Mansfield, M., Kreidberg, L., Lupu, R., Visscher, C., Désert, J.-M., Fortney, J. J., Deleuil, M., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833059 · Cited by 340
“Ultra hot Jupiters are actually a rare outcome of planet formation (Wright et al. 2012), yet fortunately many are known mainly due to the excellent sky coverage of groundbased transit surveys like WASP (Pollacco et al. 2006), HATNet and HATSouth (Bakos 2018), KELT (Pepper et al. 2007), and MASCARA…”
BackgroundMAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND
Lee, E. J., Chiang, E., & Ormel, C. W. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/797/2/95 · Cited by 307
“The prevalence of super-Earths is consonant with the rarity of Jupiters at these distances (e.g., Jones et al. 2003; Udry et al. 2003; Wright et al. 2012; Fressin et al. 2013; Dawson & Murray-Clay 2013).”
BackgroundInfluentialSiverd, R. J., Beatty, T. G., Pepper, J. A., Eastman, J. D., Collins, K. A., Bieryla, A., Latham, D. W., Buchhave, L. A., Jensen, E. L. N., Crepp, J. R., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/761/2/123 · Cited by 277
“8) FGK dwarfs in the sky have been monitored using precision radial velocity surveys for many years, and as a result most of the giant planets with periods of less than a few years orbiting these stars have already been discovered (e.g., Wright et al. 2012).”
MethodON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES
Naoz, S., Farr, W. M., & Rasio, F. A. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/754/2/l36 · Cited by 293
“Taking fb ≃ 0.3, estimated from the tail of the distribution in Duquennoy & Mayor (1991), and fp ≃ 0.07, consistent with the studies from Wright et al. (2012) and Marcy et al. (2005), we find f ≃ 0.0032.”
MethodInfluentialA spin-down clock for cool stars from observations of a 2.5-billion-year-old cluster
Meibom, S., Barnes, S. A., Platais, I., Gilliland, R. L., Latham, D. W., & Mathieu, R. D. (2014) · Nature · doi:10.1038/nature14118 · Cited by 283
SOPHIE velocimetry of Kepler transit candidates
Santerne, A., Moutou, C., Tsantaki, M., Bouchy, F., Hébrard, G., Adibekyan, V., Almenara, J. M., Amard, L., Barros, S. C. C., Boisse, I., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527329 · Cited by 277
“However, this value seems to be systematically different with the values measured independently by RV in the California Planet Survey (Wright et al. 2012) and the Swiss-led planet survey (Mayor et al. subm.).”
ResultAN EFFICIENT AUTOMATED VALIDATION PROCEDURE FOR EXOPLANET TRANSIT CANDIDATES
Morton, T. D. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/761/1/6 · Cited by 270
“For KOI 552.01 I calculate FPP=0.90 (assuming a specific occurrence of 1%, appropriate for Jupiter-sized planets (Wright et al. 2012))—in other words, this procedure clearly identifies this signal as a very likely false positive using only the photometry, and no follow-up information at all.”
BackgroundInfluentialSelf-citationThe California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets
Petigura, E. A., Marcy, G. W., Winn, J. N., Weiss, L. M., Fulton, B. J., Howard, A. W., Sinukoff, E., Isaacson, H. T., Morton, T. D., & Johnson, J. A. (2018) · eScholarship (California Digital Library) · Cited by 249
Self-citationGIANT PLANETS ORBITING METAL-RICH STARS SHOW SIGNATURES OF PLANET-PLANET INTERACTIONS
Dawson, R. I., & Murray-Clay, R. A. (2013) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/767/2/l24 · Cited by 244
“Approximately 1% of stars host hot Jupiters, ousted from their birthplaces to short-period orbits (Wright et al. 2012) via mechanisms that remain debated.”
BackgroundResultInfluentialExoplanet Statistics and Theoretical Implications
Zhu, W., & Dong, S. (2021) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-112420-020055 · Cited by 276
Lissauer, J. J., Marcy, G. W., Bryson, S., Rowe, J. F., Jontof‐Hutter, D., Agol, E., Borucki, W. J., Carter, J. A., Ford, E. B., Gilliland, R. L., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/784/1/44 · Cited by 225
“It may be that very close-in planets truly lack nearby planetary neighbors, as is the case for hot jupiters (Steffen et al. 2012, Wright et al. 2012), and/or that very close-in planets tend to have substantial orbital inclinations relative to more distant planets in their systems.”
BackgroundSelf-citationSTEADY-STATE PLANET MIGRATION BY THE KOZAI-LIDOV MECHANISM IN STELLAR BINARIES
Petrovich, C. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/1/27 · Cited by 205
“The difference in the estimated rates from RV and TR surveys might be due to a difference in metallicity in both samples (Wright et al. 2012; Dawson & Murray-Clay 2013).”
BackgroundInfluentialHOT JUPITERS FROM COPLANAR HIGH-ECCENTRICITY MIGRATION
Petrovich, C. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/805/1/75 · Cited by 213
“At least ∼10%–15% of Sun-like stars harbor a Jovianmassplanet, while only ∼0.5%–1% harbor a so-called hot Jupiter (HJ) with semi-major axis <0.1 AU (Marcy et al. 2005; Gould et al. 2006; Mayor et al. 2011; Howard et al. 2012; Wright et al. 2012).”
BackgroundInfluentialWolfgang, A., & Lopez, E. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/183 · Cited by 198
“…Dressing & Charbonneau 2013; Morton & Swift 2013; Petigura et al. 2013), the consistency between RV and transit surveys (Wolfgang & Laughlin 2012; Wright et al. 2012; Figueira et al. 2012), the Kepler eccentricity distribution (Moorhead et al. 2011; Kane et al. 2012; Wu & Lithwick 2013), and the…”
BackgroundThe Super Earth–Cold Jupiter Relations
Zhu, W., & Wu, Y. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aad22a · Cited by 190
“With P (HJ) ≈ 1% (Wright et al. 2012), this gives P (HJ|CJ) ≈ 5% and therefore sets an upper limit of P (SE|CJ) .”
BackgroundWARM JUPITERS ARE LESS LONELY THAN HOT JUPITERS: CLOSE NEIGHBORS
Huang, C., Wu, Y., & Triaud, A. H. M. J. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/825/2/98 · Cited by 207
“We note that this rate is quite uncertain, (Mayor et al. 2011) report the multiplicity rate for small planets are ∼ 70% with an unclear statistic significance.”
BackgroundInfluentialObserved Properties of Extrasolar Planets
Howard, A. (2013) · Science · doi:10.1126/science.1233545 · Cited by 144
Self-citationSOPHIE velocimetry ofKeplertransit candidates
Santerne, A., Díaz, R. F., Moutou, C., Bouchy, F., Hébrard, G., Almenara, J. M., Bonomo, A. S., Deleuil, M., & Santos, N. C. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201219608 · Cited by 170
“The occurrence rate of hot Jupiters around GK dwarfs when considering candidates from their measured transit depth appears to agree better with radial velocity surveys (see Wright et al. 2012, and reference therein) than selecting them according to their estimated radius.”
BackgroundAnderson, K. R., Storch, N. I., & Lai, D. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2906 · Cited by 172
THE RADIUS DISTRIBUTION OF PLANETS AROUND COOL STARS
Morton, T. D., & Swift, J. J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/791/1/10 · Cited by 179
“But not unlike many areas of astronomy, the first discoveries are not representative samples; rather, close-in giant planets are relatively rare (Wright et al. 2012; Howard et al. 2010) in comparison to the new populations of exoplanets now being revealed by the Kepler Mission (Borucki et al. 2011;…”
BackgroundSelf-citationTWO “b”s IN THE BEEHIVE: THE DISCOVERY OF THE FIRST HOT JUPITERS IN AN OPEN CLUSTER
Quinn, S. N., White, R. J., Latham, D. W., Buchhave, L. A., Cantrell, J. R., Dahm, S. E., Fűrész, G., Szentgyorgyi, A. H., Geary, J. C., Torres, G., et al. (2012) · The Astrophysical Journal · doi:10.1088/2041-8205/756/2/l33 · Cited by 170
Hellier, C., Anderson, D. R., Cameron, A. C., Doyle, A. P., Fumel, A., Gillon, M., Jehin, E., Lendl, M., Maxted, P. F. L., Pepe, F. A., et al. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21780.x · Cited by 166
“In the following we discuss the relative period distribution of hot Jupiters, but do not consider their absolute occurrence rate (for which see e.g. Wright et al. 2012).”
BackgroundThe CARMENES search for exoplanets around M dwarfs
Sabotta, S., Schlecker, M., Chaturvedi, P., Guenther, E. W., Rodríguez, I. M., Muñoz-Sánchez, J. C., Caballero, J. A., Shan, Y., Reffert, S., Ribas, I., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202140968 · Cited by 160
Characterizing Transiting Planet Atmospheres through 2025
Cowan, N. B., Greene, T. P., Angerhausen, D., Batalha, N. E., Clampin, M., Colón, K. D., Crossfield, I. J. M., Fortney, J. J., Gaudi, B. S., Harrington, J., et al. (2015) · Publications of the Astronomical Society of the Pacific · doi:10.1086/680855 · Cited by 157
“In short, these planets are expected to be less extreme than hot Jupiters in terms of radiative forcing, but probably more interesting in terms of chemistry.”
BackgroundInfluentialTHE IN SITU FORMATION OF GIANT PLANETS AT SHORT ORBITAL PERIODS
Boley, A. C., Contreras, A. P. G., & Gladman, B. (2016) · The Astrophysical Journal Letters · doi:10.3847/2041-8205/817/2/l17 · Cited by 167
“Finally, the differences between the solar neighborhood and Kepler HJ frequencies, assuming both samples are representative, might be resolved by metallicity (Wright et al. 2012).”
BackgroundInfluentialMoe, M., & Kratter, K. M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2328 · Cited by 173
Hot super-Earths and giant planet cores from different migration histories
Cossou, C., Raymond, S. N., Hersant, F., & Pierens, A. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424157 · Cited by 154
“Only 0.5-1% of stars host a hot Jupiter (Cumming et al. 2008; Howard et al. 2010, 2012; Mayor et al. 2011; Wright et al. 2012).”
BackgroundInfluentialThe New Generation Planetary Population Synthesis (NGPPS)
Emsenhuber, A., Mordasini, C., Burn, R., Alibert, Y., Benz, W., & Asphaug, E. I. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038863 · Cited by 171
A hot Jupiter orbiting a 2-million-year-old solar-mass T Tauri star
Donati, J. F., Moutou, C., Malo, L., Baruteau, C., Yu, L., Hébrard, E., Hussain, G., Alencar, S., Ménard, F., Bouvier, J., et al. (2016) · Nature · doi:10.1038/nature18305 · Cited by 147
Wittenmyer, R. A., Wang, S., Horner, J., Butler, R. P., Tinney, C. G., Carter, B., Wright, D. J., Jones, H. R. A., Bailey, J., O'Toole, S. J., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3436 · Cited by 154
“From the warm and hot Jupiters and pulsar planets that marked our entry to the era (e.g. Wolszczan, & Frail 1992; Mayor & Queloz 1995; Wright et al. 2012), to the highly eccentric worlds found by radial velocity surveys (e.g. Jones et al. 2006; Wittenmyer et al. 2007; Tamuz et al. 2008; Wittenmyer…”
BackgroundTHE METALLICITIES OF STARS WITH AND WITHOUT TRANSITING PLANETS
Buchhave, L. A., & Latham, D. W. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/808/2/187 · Cited by 143
“The hot-Jupiter type exoplanets with periods shorter than about 10 days dominated the initial discoveries, but we now know these types of planets to be rare (found around ∼ 1% of Sun-like stars; Wright et al. 2012).”
BackgroundMass inventory of the giant-planet formation zone in a solar nebula analogue
Zhang, K., Bergin, E. A., Blake, G. A., Cleeves, L. I., & Schwarz, K. R. (2017) · Nature Astronomy · doi:10.1038/s41550-017-0130 · Cited by 142
Wang, J., Fischer, D. A., Xie, J.-W., & Ciardi, D. R. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/791/2/111 · Cited by 141
“However, this direct method is prone to flux contamination of stellar companions, which affects measurement precision (Wright et al. 2012).”
BackgroundSelf-citationNEAR-IR DIRECT DETECTION OF WATER VAPOR IN TAU BOÖTIS b
Lockwood, A., Johnson, J. A., Bender, C. F., Carr, J. S., Barman, T., Richert, A. J. W., & Blake, G. A. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/783/2/l29 · Cited by 127
“Since the first detection of an exoplanet around a mainsequence star (Mayor & Queloz 1995), astronomers have discovered hundreds of exoplanets using the radial velocity (RV) technique (Wright et al. 2012).”
MethodSelf-citationHot super-Earths and giant planet cores from different migration histories
Cossou, C., Raymond, S. N., Hersant, F., & Pierens, A. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201424157/pdf · Cited by 154
EVIDENCE FOR THE TIDAL DESTRUCTION OF HOT JUPITERS BY SUBGIANT STARS
Schlaufman, K. C., & Winn, J. N. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/772/2/143 · Cited by 126
Instrumentation for the detection and characterization of exoplanets
Pepe, F. A., Ehrenreich, D., & Meyer, M. R. (2014) · Nature · doi:10.1038/nature13784 · Cited by 122
Zhou, G., Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, D. W., Quinn, S. N., Collins, K. A., Winn, J. N., Wong, I., Kovács, G., et al. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab36b5 · Cited by 121
Super-Earth masses sculpted by pebble isolation around stars of different masses
Liu, B., Lambrechts, M., Johansen, A., & Liu, F. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936309 · Cited by 119
“Observations imply that the occurrence rate of cold gas giants is a factor of 5−10 higher than the hot-Jupiters (Cumming et al. 2008; Wright et al. 2012).”
BackgroundHot Jupiters Are Destroyed by Tides While Their Host Stars Are on the Main Sequence
Hamer, J. H., & Schlaufman, K. C. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab3c56 · Cited by 123
GAS GIANT PLANETS AS DYNAMICAL BARRIERS TO INWARD-MIGRATING SUPER-EARTHS
Izidoro, A., Raymond, S. N., Morbidelli, A., Hersant, F., & Pierens, A. (2015) · The Astrophysical Journal · doi:10.1088/2041-8205/800/2/l22 · Cited by 114
“Only about 0.5–1% of Sun-like stars host hot-Jupiters (Cumming et al. 2008; Howard et al. 2010, 2012; Wright et al. 2012).”
BackgroundInfluentialDoppler spectroscopy as a path to the detection of Earth-like planets
Mayor, M., Lovis, C., & Santos, N. C. (2014) · Nature · doi:10.1038/nature13780 · Cited by 118
An Updated Study of Potential Targets for Ariel
Edwards, B., Mugnai, L. V., Tinetti, G., Pascale, E., & Sarkar, S. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab1cb9 · Cited by 114
Chauvin, G., Vigan, A., Bonnefoy, M., Desidera, S., Bonavita, M., Mesa, D., Boccaletti, A., Buenzli, E., Carson, J., Delorme, P., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423564 · Cited by 84
“C-0252A) different stellar hosts (Howard et al. 2010; Mayor et al. 2011; Wright et al. 2012; Bonfils et al. 2013).”
A CANDIDATE YOUNG MASSIVE PLANET IN ORBIT AROUND THE CLASSICAL T TAURI STAR CI TAU*
Johns‐Krull, C. M., McLane, J. N., Prato, L. A., Crockett, C., Jaffe, D. T., Hartigan, P. M., Beichman, C., Mahmud, N. I., Chen, W., Skiff, B. A., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/2/206 · Cited by 112
“An excess in the young hot Jupiter population may indicate the prevalence of destructive mechanisms which result in the relative paucity of massive, short-period planets around main-sequence stars, ∼1% (e.g., Wright et al. 2012).”
BackgroundAdvances in exoplanet science from Kepler
Lissauer, J. J., Dawson, R. I., & Tremaine, S. D. (2014) · Nature · doi:10.1038/nature13781 · Cited by 113
“10 days for R p. 4R and below 2 { 3 days for giant planets. The occurrence rate of giant { 9 { planets on small orbits is a factor of three lower than in radial-velocity surveys (Howard et al. 2012; Wright et al. 2012; Fressin et al. 2013), perhaps because a signicant fraction of giant planets are injected into small…”
BackgroundON THE OCCURRENCE RATE OF HOT JUPITERS IN DIFFERENT STELLAR ENVIRONMENTS
Wang, J., Fischer, D. A., Horch, E. P., & Huang, C. X. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/2/229 · Cited by 115
“Emulating the Howard et al. sample, but using the California Planet Survey (CPS) sample, Wright et al. (2012) found that the occurrence rate of HJs for the Doppler sample is 1.20±0.38%.”
BackgroundMethodInfluentialSelf-citationOccurrence and core-envelope structure of 1–4× Earth-size planets around Sun-like stars
Marcy, G. W., Weiss, L. M., Petigura, E. A., Isaacson, H. T., Howard, A. W., & Buchhave, L. A. (2014) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.1304197111 · Cited by 102
“Intriguingly, the occurrence rate of close-in Jupiter-size planets found around stars in the Kepler field of view seems to be about half that found around nearby stars, a difference not understood (18).”
BackgroundSelf-citationHD 285507b: AN ECCENTRIC HOT JUPITER IN THE HYADES OPEN CLUSTER
Quinn, S. N., White, R. J., Latham, D. W., Buchhave, L. A., Torres, G., Stefanik, R. P., Berlind, P., Bieryla, A., Calkins, M. C., Esquerdo, G. A., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/787/1/27 · Cited by 121
“One such grouping of planets is the hot Jupiters, gas giant planets in short period orbits (defined herein as MP > 0.3 MJup and P < 10 days), which occur at rates of ∼1.2% around Sun-like field stars (see Wright et al. 2012; Mayor et al. 2011).”
BackgroundInfluentialClarke, C. J., Tazzari, M., Juhász, A., Rosotti, G. P., Booth, R. A., Facchini, S., Ilee, J. D., Johns-Krull, C. M., Kama, M., Meru, F., et al. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aae36b · Cited by 101
“Since the 1995 discovery of the first hot Jupiter (Mayor & Queloz 1995), it is now established that such gas giant planets orbiting at radii < 0.1 au from their parent stars are found in around 1% of main sequence solar type stars (Wright et al. 2012).”
BackgroundInfluentialKELT-20b: A Giant Planet with a Period of P ∼ 3.5 days Transiting the V ∼ 7.6 Early A Star HD 185603
Lund, M. B., Rodriguez, J. E., Zhou, G., Gaudi, B. S., Stassun, K. G., Johnson, M. C., Bieryla, A., Oelkers, R. J., Stevens, D. J., Collins, K. A., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa8f95 · Cited by 108
“It is the prototypical “hot Jupiter,” a class of planets that are now known to orbit 0.5% 1%~ – of stars (Gould et al. 2006; Howard et al. 2012; Wright et al. 2012), but whose origins and characteristics remain important topics of study.”
BackgroundInfluentialSelf-citationThree planetary companions around M 67 stars
Brucalassi, A., Pasquini, L., Saglia, R. P., Ruíz, M. T., Bonifacio, P., Bedin, L. R., Biazzo, K., Melo, C., Lovis, C., & Randich, S. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322584 · Cited by 97
“…planets for RV surveys around FGK stars we find an exoplanet host-rate higher than 10% for planets with a period of up to a few years and 1.20± .38% at solar metallicity, for very close-in hot-Jupiters with a period shorter than ten days (Cumming et al. 2008; Mayor et al. 2011; Wright et al. 2012).”
BackgroundInfluentialZhou, G., Huang, C. X., Bakos, G. Á., Hartman, J. D., Latham, D. W., Quinn, S. N., Collins, K. A., Winn, J. N., Wong, I., Kovács, G., et al. (2019) · University of Southern Queensland ePrints (University of Southern Queensland) · doi:10.48550/arxiv.1906.00462 · Cited by 96
The Hyades open cluster is chemically inhomogeneous
Liu, F., Yong, D., Asplund, M., Ramírez, I., & Meléndez, J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw247 · Cited by 96
“…and they suggested a hot Jupiter frequency of 1.97+0.92 −1.07% in the Hyades open cluster, which is consistent with the hot Jupiter frequency in the field stars (1.2± 0.38%, Wright et al. 2012), while no hot Jupiters were discovered around our selected Hyades stars (Paulson, Cochran & Hatzes 2004).”
ResultInfluentialA hot Jupiter around the very active weak-line T Tauri star TAP 26
Yu, L., Donati, J.-F., Hébrard, E. M., Moutou, C., Malo, L., Grankin, K. N., Hussain, G. A. J., Cameron, A. C., Vidotto, A. A., Baruteau, C., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx009 · Cited by 93
“…around young stars (van Eyken et al. 2012; Donati et al. 2016, 2017; Mann et al. 2016; Johns-Krull et al. 2016; David et al. 2016), our result may suggest a surprisingly high frequency of hJs around young solar-type stars, with respect to that around more evolved stars ('1%, Wright et al. 2012).”
BackgroundWASP-77 Ab: A Transiting Hot Jupiter Planet in a Wide Binary System1
Maxted, P. F. L., Anderson, D. R., Cameron, A. C., Doyle, A. P., Fumel, A., Gillon, M., Hellier, C., Jehin, E., Lendl, M., Pepe, F. A., et al. (2012) · Publications of the Astronomical Society of the Pacific · doi:10.1086/669231 · Cited by 93
“The occurrence rate for hot Jupiters around solar-type stars is known to be about 1% from radial velocity surveys of bright stars (Wright et al. 2012).”
BackgroundStrong biases in retrieved atmospheric composition caused by day–night chemical heterogeneities
Pluriel, W., Zingales, T., Leconte, J., & Parmentier, V. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202037678 · Cited by 88
“Currently only a few UHJs have been discovered and studied using both transit and eclipse spectroscopy (Wright et al. 2012; Haynes et al. 2015; Sheppard et al. 2017; Evans et al. 2017; Kreidberg et al. 2018).”
BackgroundMiniature Exoplanet Radial Velocity Array I: design, commissioning, and early photometric results
Swift, J. J., Bottom, M., Johnson, J. A., Wright, J. T., McCrady, N., Wittenmeyer, R., Plavchan, P. P., Riddle, R. L., Muirhead, P. S., Herzig, E., et al. (2015) · Journal of Astronomical Telescopes Instruments and Systems · doi:10.1117/1.jatis.1.2.027002 · Cited by 93
Self-citationWang, J., Fischer, D. A., Xie, J.-W., & Ciardi, D. R. (2014) · University of Southern Queensland ePrints (University of Southern Queensland) · Cited by 87
Self-citationA COMPREHENSIVE STATISTICAL ASSESSMENT OF STAR-PLANET INTERACTION
Miller, B. P., Gallo, E., Wright, J. T., & Pearson, E. G. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/799/2/163 · Cited by 86
“While it is now clear that such systems are exceptional rather than the norm (e.g., Wright et al. 2012), and likely result from planet-disk or planet-planet migration, these extreme cases permit investigation of planetary events that are irrelevant or observationally inaccessible for longer-period…”
BackgroundSelf-citationUltra-short-period Planets from Secular Chaos
Petrovich, C., Deibert, E., & Wu, Y. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab0e0a · Cited by 86
Skaf, N., Bieger, M. F., Edwards, B., Changeat, Q., Morvan, M., Kiefer, F., Blain, D., Zingales, T., Poveda, M., Al-Refaie, A. F., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab94a3 · Cited by 84
“Although many planets have been detected and it is thought that they are common in our Galaxy (Cassan et al. 2012; Wright et al. 2012; Batalha et al. 2013; Dressing & Charbonneau 2013; Howard 2013), our current knowledge of their atmospheric characteristics is still very limited.”
BackgroundGan, T., Wang, S. X., Wang, S., Mao, S., Huang, C. X., Collins, K. A., Stassun, K. G., Shporer, A., Zhu, W., Ricker, G. R., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac9b12 · Cited by 100
Hirsch, L. A., Rosenthal, L. J., Fulton, B. J., Howard, A. W., Ciardi, D. R., Marcy, G. W., Nielsen, E. L., Petigura, E. A., Rosa, R. J. D., Isaacson, H., et al. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/abd639 · Cited by 84
“…RV time series surpassing the survey minimum requirement, due to their inclusion in the California Planet Survey (e.g., Marcy et al. 2008, 2014; Howard et al. 2012, 2014; Wright et al. 2012), which was carried out at Lick and Keck Observatories starting in the late 1980s and continues today.”
BackgroundSelf-citationVick, M., Lai, D., & Anderson, K. R. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz354 · Cited by 92
“…et al. 2010; Ngo et al. 2015), Fp ∼ 10% (as in ASL16), and FHJ ∼ 4% from our population synthesis calculation, we obtain an estimate of RHJ ∼ 0.2%, which is nearly an order of magnitude smaller than the observed occurrence rate of 1% (Marcy et al. 2005; Wright et al. 2012; Fressin et al. 2013).”
BackgroundInfluentialGaidos, E. J., & Mann, A. W. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/762/1/41 · Cited by 78
“Wright et al. (2012) report that the occurrence of “hot Jupiters” (P < 10 days) in the Kepler catalog is only half that seen in Doppler surveys, and adjustment for a high false-positive rate would worsen this discrepancy.”
BackgroundGas Giant Planets as Dynamical Barriers to Inward-Migrating Super-Earths
Morbidelli, A., Izidoro, A., & Raymond, S. N. (2015) · HAL · Cited by 84
WHY IS THERE A DEARTH OF CLOSE-IN PLANETS AROUND FAST-ROTATING STARS?
Teitler, S., & Königl, A. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/786/2/139 · Cited by 80
“This value is consistent (within a factor of ∼ 2) with the average mass ofMp ≥ M⊕ planets with Porb ≤ 10 days around planet-bearing stars that is inferred from radial-velocity surveys (e.g., Mayor et al. 2011; Wright et al. 2012), which suggests that most of the mass associated with close-in planets is accounted for i…”
BackgroundLow-eccentricity migration of ultra-short-period planets in multiplanet systems
Pu, B., & Lai, D. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1817 · Cited by 78
“…2009); since then, about a hundred USPs have been found by various transit surveys (Sanchis-Ojeda et al. 2014), and the overall occurence rate of USPs sits at ∼ 1%, a figure that is similar to the census of hot Jupiters, i.e. giant planets with P ≤ 10 days (Cumming et al. 2008; Wright et al. 2012).”
ResultCONSTRAINTS ON PLANET OCCURRENCE AROUND NEARBY MID-TO-LATE M DWARFS FROM THE MEarth PROJECT
Berta, Z. K., Irwin, J., & Charbonneau, D. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/775/2/91 · Cited by 47
“Our non-detection of any 300K Jupiters translates to < 0.44 planets/star for such planets at 95% confidence, again showing contradiction neither with M dwarf radial velocity surveys (Endl et al. 2003; Johnson et al. 2010; Bonfils et al. 2013) nor with microlensing surveys (Sumi et al. 2010; Gould et al. 2010).”
BackgroundInfluentialKELT-3b: A HOT JUPITER TRANSITING AV= 9.8 LATE-F STAR
Pepper, J. A., Siverd, R. J., Beatty, T. G., Gaudi, B. S., Stassun, K. G., Eastman, J. D., Collins, K. A., Latham, D. W., Bieryla, A., Buchhave, L. A., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/773/1/64 · Cited by 74
“On the other hand, RV surveys start to become incomplete for stars fainter thanV ∼ 8 (Wright et al. 2012).”
BackgroundExoplanet spectroscopy and photometry with the Twinkle space telescope
Edwards, B., Rice, M., Zingales, T., Tessenyi, M., Waldmann, I. P., Tinetti, G., Pascale, E., Savini, G., & Sarkar, S. (2018) · Experimental Astronomy · doi:10.1007/s10686-018-9611-4 · Cited by 74
“[6, 12, 18, 29, 73]), our current knowledge of their atmospheric, thermal and compositional characteristics is still very limited.”
BackgroundTayar, J., Ceillier, T., García-Hernández, D. A., Nicholas, T., Mathur, S., García, R. A., Zamora, O., Johnson, J. A., Pinsonneault, M. H., Mészáros, S., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/1/82 · Cited by 84
“Detection of significant numbers of close-in giant planets at rates between 3/1000 stars (Gould et al. 2006) and 12/1000 stars (Wright et al. 2012) leads to the logical conclusion that at minimum 1% of stars should accrete mass from planetary size companions as their radii expand on the giant…”
BackgroundSelf-citationDawson, R. I., Murray-Clay, R. A., & Johnson, J. A. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/798/2/66 · Cited by 106
“Roughly 1% of Sun-like stars host hot Jupiters, giant planets with small semi-major axes (Mayor et al. 2011; Howard et al. 2012; Wright et al. 2012).”
BackgroundResultSelf-citationTHE CURIOUS CASE OF ELEMENTAL ABUNDANCE DIFFERENCES IN THE DUAL HOT JUPITER HOSTS WASP-94A AND B*
Teske, J. K., Khanal, S., & Ramírez, I. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/819/1/19 · Cited by 73
“WASP-94 is of particular interest because hot Jupiter planets (roughly defined as MP sini > 0.1MJ and P<10 days) are rare, found around .1% of FGK dwarfs (Wright et al. 2012, Table 2).”
BackgroundPROBABILITY OF CME IMPACT ON EXOPLANETS ORBITING M DWARFS AND SOLAR-LIKE STARS
Kay, C., Opher, M., & Kornbleuth, M. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/2/195 · Cited by 74
“While hot Jupiters may account for approximately 20% of discovered exoplanets, Wright et al. (2012) suggest that only 1% of F-, G-, and K-type stars host a hot Jupiter.”
BackgroundTransiting exoplanets from the CoRoT space mission
Csizmadia, S., Hatzes, A. P., Gandolfi, D., Deleuil, M., Bouchy, F., Fridlund, M. C., Szabados, L., Parviainen, H., Cabrera, J., Aigrain, S., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526763 · Cited by 70
“FGK dwarf stars for periodsP < 10 days (Wright et al. 2012).”
BackgroundA tale of planet formation: from dust to planets
Liu, B., & Ji, J. (2020) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/20/10/164 · Cited by 82
Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b
Helling, C., Iro, N., Corrales, L., Samra, D., Ohno, K., Alam, M. K., Steinrueck, M. E., Lew, B. W. P., Molaverdikhani, K., MacDonald, R. J., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935771 · Cited by 70
Fulton, B. J., Collins, K. A., Gaudi, B. S., Stassun, K. G., Pepper, J. A., Beatty, T. G., Siverd, R. J., Penev, K., Howard, A. W., Baranec, C. J., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/810/1/30 · Cited by 67
“These planets are some of the easiest to detect and characterize but also some of the most intrinsically rare, occurring around only 0.3 to 1.5% of Sun-like stars (Gould et al. 2006; Cumming et al. 2008; Bayliss & Sackett 2011; Wright et al. 2012; Howard et al. 2012).”
BackgroundInfluentialSelf-citationWang, J., Fischer, D. A., Horch, E. P., & Xie, J. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/248 · Cited by 67
“Unfortunately, for ground based surveys, the detection efficiency of planets in MSS is affected by flux contamination from the additional stellar components (Wright et al. 2012).”
BackgroundSelf-citationStrong biases in retrieved atmospheric composition caused by day–night chemical heterogeneities
Pluriel, W., Zingales, T., Leconte, J., & Parmentier, V. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202037678/pdf · Cited by 66
Search for giant planets in M67
Brucalassi, A., Pasquini, L., Saglia, R. P., Ruíz, M. T., Bonifacio, P., Leão, I. C., Martins, B. L. C., Medeiros, J. R. D., Bedin, L. R., Biazzo, K., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527561 · Cited by 64
“Our values are higher than those derived from the RV surveys around FGK stars (1.2%± 0.38 of HJs Wright et al. 2012).”
BackgroundResultInfluentialThe hot Jupiter of the magnetically active weak-line T Tauri star V830 Tau
Donati, J.-F., Yu, L., Moutou, C., Cameron, A. C., Malo, L., Grankin, K. N., Hébrard, E., Hussain, G. A. J., Vidotto, A. A., Alencar, S. H. P., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2904 · Cited by 64
“…of young close-in giants around TTSs (e.g., van Eyken et al. 2012; Mann et al. 2016; Johns-Krull et al. 2016; David et al. 2016; Yu et al. 2016), our result suggests that newborn hJs may be frequent, possibly more so than their mature equivalents around Sun-like stars (Wright et al. 2012).”
BackgroundConnecting planet formation and astrochemistry
Cridland, A. J., van Dishoeck, E. F., Alessi, M., & Pudritz, R. E. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038767 · Cited by 67
THE SOLAR SYSTEM AS AN EXOPLANETARY SYSTEM
Martin, R. G., & Livio, M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/810/2/105 · Cited by 64
“However, we now know that they are quite rare and orbit only about one percent of solar type stars (e.g. Wright et al. 2012).”
BackgroundStephan, A. P., Naoz, S., & Gaudi, B. S. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aad6e5 · Cited by 63
FRIENDS OF HOT JUPITERS. III. AN INFRARED SPECTROSCOPIC SEARCH FOR LOW-MASS STELLAR COMPANIONS
Piskorz, D., Knutson, H. A., Ngo, H., Muirhead, P. S., Batygin, K., Crepp, J. R., Hinkley, S., & Morton, T. D. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/814/2/148 · Cited by 63
“In Section 4 we compare our results to those of the adaptive optics and radial velocity portions of the Friends of Hot Jupiters survey.”
BackgroundInfluentialSelf-citationAn infrared transient from a star engulfing a planet
De, K., MacLeod, M., Karambelkar, V., Jencson, J. E., Chakrabarty, D., Conroy, C., Dekany, R., Eilers, A., Graham, M. J., Hillenbrand, L. A., et al. (2023) · Nature · doi:10.1038/s41586-023-05842-x · Cited by 62
The formation efficiency of close-in planets via Lidov–Kozai migration: analytic calculations
Muñoz, D. J., Lai, D., & Liu, B. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw983 · Cited by 72
“5 days – is estimated to be around 1% for FGK stars (Marcy et al. 2005; Wright et al. 2012; Howard et al. 2012; Fressin et al. 2013; Petigura, Howard & Marcy 2013).”
BackgroundWASP-94 A and B planets: hot-Jupiter cousins in a twin-star system
Neveu-VanMalle, M., Queloz, D. P., Anderson, D. R., Charbonnel, C., Cameron, A. C., Delrez, L., Gillon, M., Hellier, C., Jehin, E., Lendl, M., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424744 · Cited by 64
“Although many hot Jupiters are known, they rarely occur around solar-type stars with rates from 0.3 to 1.5% (Wright et al. 2012) depending on the metallicity ([Fe/H]) of the stellar sample studied.”
BackgroundInfluentialZanazzi, J. J., & Lai, D. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1075 · Cited by 62
“1% (e.g. Marcy et al. 2005; Gould et al. 2006; Cumming et al. 2008; Howard et al. 2010, 2012; Bayliss & Sackett 2011; Wright et al. 2012), the occurrence rates of Jovian-mass planets orbiting interior to ∼ few au is ∼ 5 − 10% (e.g. Cumming et al. 2008; Clanton & Gaudi 2016), and potentially as high…”
BackgroundCluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602
Bouma, L. G., Hartman, J. D., Brahm, R., Evans, P., Collins, K. A., Zhou, G., Sarkis, P., Quinn, S. N., de Leon, J., Livingston, J., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/abb9ab · Cited by 67
“The modern 0.5- 1% occurrence rate suggests that these early transit surveys would have needed a greater data volume at higher precision TOI 837 IN IC 2602 3 for detection to be possible (Mayor et al. 2011; Wright et al. 2012; Howard et al. 2012; Petigura et al. 2018).”
BackgroundInfluential
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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