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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
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Items 101–200 of 370
Exploring the dependence of hot Jupiter occurrence rates on stellar mass with TESS
Beleznay, M., & Kunimoto, M. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2179 · Cited by 60
Perryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511994852.011 · Cited by 71
Hamers, A. S., Antonini, F., Lithwick, Y., Perets, H. B., & Zwart, S. P. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2370 · Cited by 62
“In contrast, the observed HJ fraction isfHJ,obs ∼ 0.01 (e.g. Wright et al. 2012), an order of magnitude larger.”
BackgroundInfluentialThe occurrence of planets and other substellar bodies around white dwarfs using K2
van Sluijs, L., & Eylen, V. V. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx3068 · Cited by 58
“…by WASP and Pan-STARRS (Faedi et al. 2011; Fulton et al. 2014), and similar or lower than the the occurrence of hot Jupiters around MS stars, which is estimated as 0.3-1.5% (e.g. Marcy et al. 2005; Gould et al. 2006; Cumming et al. 2008; Howard et al. 2010; Mayor et al. 2011; Wright et al. 2012).”
BackgroundInfluentialA SEARCH FOR PLANETARY ECLIPSES OF WHITE DWARFS IN THE Pan-STARRS1 MEDIUM-DEEP FIELDS
Fulton, B. J., Tonry, J. L., Flewelling, H., Burgett, W. S., Chambers, K. C., Hodapp, K. W., Huber, M. E., Kaiser, N., Wainscoat, R. J., & Waters, C. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/796/2/114 · Cited by 57
“This is in good agreement with the frequency of hot Jupiters around solar-type stars measured to be between 0.3% and 1.5% (Marcy et al. 2005; Gould et al. 2006; Cumming et al. 2008; Howard et al. 2011; Mayor et al. 2011; Wright et al. 2012).”
InfluentialObservational studies of stellar rotation
Bouvier, J. (2013) · EAS Publications Series · doi:10.1051/eas/1362005 · Cited by 58
Guo, X., Johnson, J. A., Mann, A. W., Kraus, A. L., Curtis, J. L., & Latham, D. W. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6004 · Cited by 56
“Giant planets with periods P < 10 days and Mp > 0.1MJupiter are dubbed as hot Jupiters (HJ)5 in Wright et al. (2012) (hereafter W12), and much effort has been devoted into the study of the HJ occurrence rates both in the Kepler field and the solar neighborhood.”
BackgroundSelf-citationThe contribution of secondary eclipses as astrophysical false positives to exoplanet transit surveys
Santerne, A., Fressin, F., Díaz, R. F., Figueira, P., Almenara, J. M., & Santos, N. C. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321475 · Cited by 62
“This discrepancy (at 3.2-σ) might be explained by the difference in the occurrence rate of planets between the Kepler survey (Howard et al. 2012; Santerne et al. 2012; Fressin et al. 2013) and the radial velocity surveys (e.g. Mayor et al. 2011; Wright et al. 2012).”
InfluentialCluster 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. H., et al. (2020) · Cited by 54
Biological invasion and biological control select for different life histories
Tayeh, A., Hufbauer, R. A., Estoup, A., Ravigné, V., Frachon, L., & Facon, B. (2015) · Nature Communications · doi:10.1038/ncomms8268 · Cited by 53
Planet formation and stability in polar circumbinary discs
Cuello, N., & Giuppone, C. A. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833976 · Cited by 53
“On the one hand, these systems are intrinsically difficult to observe through radial velocities (Eggenberger & Udry 2007; Wright et al. 2012) and transit methods (Martin & Triaud 2014).”
BackgroundTayar, J., Ceillier, T., García-Hernández, D. A., Troup, N., Mathur, S., García, R., Zamora, O., Johnson, J., Pinsonneault, M., Mészáros, S., et al. (2015) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 53
Self-citationDawson, R. I., Johnson, J. A., Morton, T. D., Crepp, J. R., Fabrycky, D. C., Murray-Clay, R. A., & Howard, A. W. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/761/2/163 · Cited by 51
“Even though they make up only a small percentage of the planet population (Howard et al. 2010; Howard et al. 2012; Youdin 2011; Mayor et al. 2011; Wright et al. 2012) we focus attention on hot Jupiters because, like meteorites discovered in Antarctica, they are known to come from somewhere else,…”
BackgroundSelf-citationTOI-257b (HD 19916b): a warm sub-saturn orbiting an evolved F-type star
Addison, B., Wright, D. J., Nicholson, B. A., Cale, B., Močnik, T., Huber, D., Plavchan, P. P., Wittenmyer, R. A., Vanderburg, A. M., Chaplin, W. J., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3960 · Cited by 52
McCormac, J., Skillen, I., Pollacco, D., Faedi, F., Ramsay, G., Dhillon, V. S., Todd, I., & Gonzalez, A. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2449 · Cited by 49
“Wright et al. (2012) summarize the situation and show that the rate differs by up to a factor of 4 depending on the source.”
BackgroundPERIODIC AND APERIODIC VARIABILITY IN THE MOLECULAR CLOUD ρ OPHIUCHUS
Parks, J. R., Plavchan, P. P., White, R. J., & Gee, A. H. (2014) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/211/1/3 · Cited by 49
“If true in this case, this would demonstrate the existance of a hot protoplanet with a period of 6 days very near the peak in the period distribution for exoplanets (Wright et al. 2012).”
BackgroundPiskorz, D., Benneke, B., Crockett, N. R., Lockwood, A., Blake, G. A., Barman, T., Bender, C. F., Bryan, M. L., Carr, J. S., Fischer, D. A., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/832/2/131 · Cited by 49
“These gas giants orbit their host stars in days, are known as hot Jupiters, and have an occurence rate of only 1% in the exoplanet population (Wright et al. 2012).”
BackgroundSelf-citationPlanets, candidates, and binaries from the CoRoT/Exoplanet programme
Deleuil, M., Aigrain, S., Moutou, C., Cabrera, J., Bouchy, F., Deeg, H. J., Almenara, J.-M., Hébrard, G., Santerne, A., Alonso, R., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731068 · Cited by 49
The Demographics of Rocky Free-floating Planets and their Detectability by WFIRST
Barclay, T., Quintana, E. V., Raymond, S. N., & Penny, M. T. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa705b · Cited by 48
“We do not include systems with hot Jupiters in this estimate because they only account for approximately 1% (Wright et al. 2012) of stars and therefore are unlikely to significantly affect the overall occurrence rate.”
BackgroundDEPENDENCE OF SMALL PLANET FREQUENCY ON STELLAR METALLICITY HIDDEN BY THEIR PREVALENCE
Zhu, W., 王吉, J. W., & Huang, C. X. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/832/2/196 · Cited by 51
“Second, the dynamical evolution of some giant planets (namely, hot Jupiters) would have significant impact on those small planets in the same system (e.g., Lin et al. 1996; Rasio & Ford 1996), but the fraction of such systems is fairly low (e.g., Mayor et al. 2011; Wright et al. 2012).”
BackgroundRonco, M. P., Guilera, O. M., & de Elía, G. C. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1746 · Cited by 46
“…percentages of Hot-Jupiter occurences than those predicted observationally, which are ∼ 1% (Marcy et al. 2005; Cumming et al. 2008; Mayor et al. 2011; Wright et al. 2012), Wang et al. (2015) concluded that the current knowledge of stellar properties and the stellar multiplicity rate is yet very…”
BackgroundA Low-mass Exoplanet Candidate Detected by K2 Transiting the Praesepe M Dwarf JS 183
Pepper, J. A., Gillen, E., Parviainen, H., Hillenbrand, L. A., Cody, A. M., Aigrain, S., Stauffer, J. R., Vrba, F. J., David, T. J., Lillo-Box, J., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa62ab · Cited by 45
“…appears that the primary reason for this is that such searches were sensitive only to hot Jupiters, which are intrinsically rare (Gould et al. 2006; Wright et al. 2012), and that most open clusters do not have enough members for high-probability detection of even one hot Jupiter (Pepper & Gaudi…”
BackgroundThe K2-HERMES Survey. I. Planet-candidate Properties from K2 Campaigns 1–3
Wittenmyer, R. A., Sharma, S., Stello, D., Buder, S., Kos, J., Asplund, M., Duong, L., Lin, J., LIND, K., Ness, M., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaa3e4 · Cited by 47
Ment, K., Fischer, D. A., Bakos, G., Howard, A. W., & Isaacson, H. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aae1f5 · Cited by 47
Self-citationThe Hot Jupiter Period–Mass Distribution as a Signature of in situ Formation
Bailey, E., & Batygin, K. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aade90 · Cited by 51
“In light of the relatively low occurrence rate of hot Jupiters (∼ 1% for Sun-like stars; Howard et al. 2010, Gould et al. 2006, Wright et al. 2012), it is not straightforward to determine which of the three aforementioned 1 The fact that the process of core-nucleated accretion is relatively…”
BackgroundHot Jupiters Have Giant Companions: Evidence for Coplanar High-eccentricity Migration
Zink, J. K., & Howard, A. W. (2023) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/acfdab · Cited by 54
Self-citationHADES RV Programme with HARPS-N at TNG
Perger, M., Garcia-Piquer, A., Ribas, I., Morales, J. C., Affer, L., Micela, G., Damasso, M., Mascareño, A. S., Hernández, J. I. G., Rebolo, R., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628985 · Cited by 46
“…2008; Bowler et al. 2010; Howard et al. 2010; Nielsen & Close 2010; Borucki et al. 2011b; Cassan et al. 2012; Howard et al. 2012; Quanz et al. 2012; Wright et al. 2012; Swift et al. 2013; Clanton & Gaudi 2014; Burke et al. 2015) including different kinds of methods, stellar environments and…”
MethodPlanetary Engulfment in the Hertzsprung–Russell Diagram
MacLeod, M., Cantiello, M., & Soares-Furtado, M. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aaa5fa · Cited by 46
“The discovery of numerous giant planets in compact orbits beginning with 51 Peg b (Mayor & Queloz 1995) was unexpected given the architecture of our own solar system (Howard et al. 2012; Wright et al. 2012).”
BackgroundTOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit
Wong, I., Shporer, A., Zhou, G., Kitzmann, D., Komacek, T. D., Tan, X., Tronsgaard, R., Buchhave, L. A., Vissapragada, S., Greklek-McKeon, M., et al. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac26bd · Cited by 46
Measuring the Galactic Distribution of Transiting Planets with WFIRST
Montet, B. T., Yee, J. C., & Penny, M. T. (2017) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aa57fb · Cited by 45
“Studies have invoked stellar metallicity ( Howard et al. 2012; Wright et al. 2012; Dawson & Murray-Clay 2013 ) , stellar age ( Schlaufman & Winn 2013 ) , and stellar multiplicity ( Wang et al. 2014, 2015b ) .”
Planet formation and stability in polar circumbinary discs
Cuello, N., & Giuppone, C. A. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201833976/pdf · Cited by 44
Gaidos, E. J., Fischer, D. A., Mann, A. W., & Howard, A. W. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/771/1/18 · Cited by 43
“Wright et al. (2012) report that the occurrence of “hot” Jupiters around the FGK stars in the California Planet Search Doppler survey is 1.2%, compared to 0.4% for Kepler (Howard et al. 2012; Fressin et al. 2013).”
BackgroundResultInfluentialSelf-citationSearch for giant planets in M 67: IV. Survey results⋆⋆⋆
Brucalassi, A., Koppenhoefer, J., Saglia, R., Pasquini, L., Ruiz, M. T., Bonifacio, P., Bedin, L. R., Libralato, M., Biazzo, K., Melo, C., et al. (2017) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201527562 · Cited by 48
“These values appear to be higher than what is observed in field stars (Wright et al. 2012; Howard et al. 2011).”
BackgroundHot Jupiters Driven by High-eccentricity Migration in Globular Clusters
Hamers, A. S., & Tremaine, S. D. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa9926 · Cited by 41
“This fraction is an order of magnitude lower than the observed HJ fraction around solar-type field stars, ~1% (e.g., Wright et al. 2012).”
BackgroundThe Demographics of Rocky Free-floating Planets and their Detectability by WFIRST
Barclay, T., Quintana, E. V., Raymond, S. N., & Penny, M. T. (2017) · Civil War Book Review · Cited by 41
Cañas, C. I., Kanodia, S., Bender, C. F., Mahadevan, S., Stefánsson, G., Cochran, W. D., Lin, A. S. J., Hwang, H.-C., Powers, L. C., Monson, A. J., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac7804 · Cited by 40
Self-citationBolmont, É., Gallet, F., Mathis, S., Charbonnel, C., Amard, L., & Alibert, Y. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201730662 · Cited by 28
“…our simulations that to have 1% of hot Jupiters observed around solar mass MS stars (as observational surveys tend to show, e.g. Marcy et al. 2005; Cumming et al. 2008; Mayor et al. 2011; Wright et al. 2012), the fraction of hot Jupiters after the protoplanetary disk dispersal should be about 1.8%.”
BackgroundInfluentialHot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)
Seidel, J. V., Lendl, M., Bourrier, V., Ehrenreich, D., Allart, R., Sousa, S. G., Cegla, H. M., Bonfils, X., Conod, U., Grandjean, A., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039058 · Cited by 44
“Despite these advances and the consensus that exoplanets are ubiquitous in our Galaxy (Cassan et al. 2012; Dressing & Charbonneau 2013; Wright et al. 2012; Howard 2013; Batalha et al. 2013), the study of atmospheric composition and structure of exoplanets is still in its early days.”
BackgroundKEPLER-424 b: A “LONELY” HOT JUPITER THAT FOUND A COMPANION
Endl, M., Caldwell, D. A., Barclay, T., Huber, D., Isaacson, H. T., Buchhave, L. A., Brugamyer, E., Robertson, P. M., Cochran, W. D., MacQueen, P. J., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/795/2/151 · Cited by 38
“Wright et al. (2012) estimate a local hot Jupiter frequency of 1.2±0.38% based on the Lick and Keck RV survey results.”
BackgroundInfluentialSelf-citationPopulations of Planets in Multiple Star Systems
Martin, D. V. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_156 · Cited by 38
“This may seem surprising given the frequency of binary stars, but there have however been historical biases and strategies against finding planets in such systems (Eggenberger & Udry 2007; Wright et al. 2012).”
ResultA HARPS RV search for planets around young nearby stars
Grandjean, A., Lagrange, A. ‐., Keppler, M., Meunier, N., Mignon, L., Borgniet, S., Chauvin, G., Desidera, S., Galland, F., Messina, S., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936038 · Cited by 40
“Our comparison of these occurrence rates to those derived for MS stars (Borgniet et al. 2019; Cumming et al. 2008; Wright et al. 2012) indicates that there is no evidence for a difference in occurrence rates of HJ between young and MS stars.”
BackgroundMethodResultInfluentialReassessment of the Null Result of the HST Search for Planets in 47 Tucanae
Masuda, K., & Winn, J. N. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa647c · Cited by 37
“To demonstrate this, we perform another round of simulations using the RV 7 sample from Wright et al. (2012) instead of Kepler stars; this time SK consists of 836 stars considered in the RV sample of Wright et al. (2012), among which 10 are associated with HJs listed in Table 2.”
BackgroundMethodResultInfluentialThe Pan-Pacific Planet Search. VII. The Most Eccentric Planet Orbiting a Giant Star
Wittenmyer, R. A., Jones, M. I., Horner, J., Kane, S. R., Marshall, J. P., Mustill, A. J., Jenkins, J. S., Rojas, P. A. P., Zhao, J., Villaver, E., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa9894 · Cited by 37
“The first of many hot-Jupiters (e.g. Gaudi et al. 2005; Wright et al. 2012; Knutson et al. 2014), 51 Pegasi b was the antithesis of our own planetary system - a giant, Jupiter-mass planet practically skimming the surface of its host star.”
BackgroundThe TESS Grand Unified Hot Jupiter Survey. II. Twenty New Giant Planets*
Yee, S. W., Winn, J. N., Hartman, J. D., Bouma, L. G., Zhou, G., Quinn, S. N., Latham, D. W., Bieryla, A., Rodriguez, J. E., Collins, K. A., et al. (2023) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aca286 · Cited by 45
Self-citationThe Fundamental Connections between the Solar System and Exoplanetary Science
Kane, S. R., Arney, G., Byrne, P. K., Dalba, P. A., Desch, S. J., Horner, J., Izenberg, N. R., Mandt, K. E., Meadows, V. S., & Quick, L. C. (2021) · Journal of Geophysical Research Planets · doi:10.1029/2020je006643 · Cited by 41
On the Detection of Exomoons Transiting Isolated Planetary-mass Objects
Limbach, M., Vos, J., Winn, J., Heller, R., Mason, J., Schneider, A., & Dai, F. (2021) · Astrophysical Journal Letters · doi:10.3847/2041-8213/ac1e2d · Cited by 22
Schlaufman, K. C., & Winn, J. N. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/825/1/62 · Cited by 40
“In addition, we assume that the long-period giant planet occurrence rate observed by Cumming et al. (2008) applies to the unobserved long-period giant planet population in the larger sample of stars analyzed by Wright et al. (2012).”
BackgroundMethodInfluentialTime-scales of close-in exoplanet radio emission variability
See, V., Jardine, M., Farès, R., Donati, J. ‐., & Moutou, C. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv896 · Cited by 35
How to make giant planets via pebble accretion
Savvidou, S., & Bitsch, B. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245793 · Cited by 35
The evolution of hot Jupiters revealed by the age distribution of their host stars
Chen, D.-C., Xie, J., Zhou, J., Dong, S., Yang, J.-Y., Zhu, W., Liu, C., Huang, Y., Xiang, M., Wang, H., et al. (2023) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.2304179120 · Cited by 39
A search for circularly polarized emission from young exoplanets
Lynch, C. R., Murphy, T., Kaplan, D. L., Ireland, M., & Bell, M. E. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx354 · Cited by 34
“It is unknown what fraction of forming stars host Hot Jupiter MNRAS 000, 1–8 (2016) systems, but for Solar-type main sequence stars about 1% host Hot Jupiter systems (Wright et al. 2012).”
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., Wittenmyer, R. A., Plavchan, P. P., Riddle, R., Muirhead, P. S., Herzig, E., et al. (2015) · doi:10.34657/8759 · Cited by 34
Self-citationA Unified Treatment of Kepler Occurrence to Trace Planet Evolution. I. Methodology
Dattilo, A., Batalha, N. M., & Bryson, S. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acebc8 · Cited by 33
Chemical fingerprints of hot Jupiter planet formation
Maldonado, J., Villaver, E., & Eiroa, C. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201732001 · Cited by 34
“…planets were considered for this work as transit targets are known to have systematically lower metallicities than radial velocity targets (Gould et al. 2006; Howard et al. 2012; Wright et al. 2012; Dawson & Murray-Clay 2013) and there is no bias that prevents RV detection at small orbital periods.”
BackgroundInfluentialDYNAMICAL CONSTRAINTS ON THE ORIGIN OF HOT AND WARM JUPITERS WITH CLOSE FRIENDS
Antonini, F., Hamers, A. S., & Lithwick, Y. (2016) · The Astronomical Journal · doi:10.3847/0004-6256/152/6/174 · Cited by 43
“The observed abundance of Jupiter-size planets orbiting interior to the ice line around their stars poses a challenge to our current understanding of planet formation (Wright et al. 2012).”
BackgroundBiases in Planet Occurrence Caused by Unresolved Binaries in Transit Surveys
Bouma, L. G., Masuda, K., & Winn, J. N. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aabfb8 · Cited by 32
MASS CONSTRAINTS OF THE WASP-47 PLANETARY SYSTEM FROM RADIAL VELOCITIES
Sinukoff, E., Howard, A. W., Petigura, E. A., Fulton, B. J., Isaacson, H., Weiss, L. M., Brewer, J. M., Hansen, B. M. S., Hirsch, L. A., Christiansen, J. L., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/153/2/70 · Cited by 27
“Approximately 1% of Sun-like stars host giant planets on short-period orbits (P < 10 days), known as hot Jupiters (HJs, Howard et al. 2012; Wright et al. 2012).”
BackgroundSelf-citationBailey, J. I., Mateo, M. L., White, R. J., Shectman, S. A., & Crane, J. D. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx3266 · Cited by 32
“We chose a total exoplanet fraction such that we would expect 1.2 per cent of stars to have hot Jupiter companions consistent with Wright et al. (2012), and we start with a binary fraction of 45 per cent consistent with DK13.”
ResultInfluentialThe Effects of Stellar Companions on the Observed Transiting Exoplanet Radius Distribution
Teske, J. K., Ciardi, D. R., Howell, S. B., Hirsch, L. A., & Johnson, R. A. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aaed2d · Cited by 31
“…larger, Saturn and Jupiter-sized planets (Howard et al. 2012; Dressing & Charbonneau 2013; Fressin et al. 2013; Petigura et al. 2013; Ciardi et al. 2015; Burke et al. 2015), which were previously the most commonly detected planets (e.g., Marcy et al. 2005; Udry et al. 2007; Wright et al. 2012).”
BackgroundFormation of hot Jupiters through disk migration and evolving stellar tides
Heller, R. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833486 · Cited by 38
“In combination with the bias-corrected observed hot Jupiter occurrence rate of 1.2 ± 0.38 % (Wright et al. 2012), this implies an initial hot Jupiter formation rate of less than between 41 % and 8 % around sun-like stars.”
BackgroundInfluentialDynamical Constraints on the Origin of Hot and Warm Jupiters with Close Friends
Antonini, F., Hamers, A. S., & Lithwick, Y. (2016) · Leiden Repository (Leiden University) · Cited by 31
Transit Photometry as an Exoplanet Discovery Method
Deeg, H. J., & Alonso, R. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_117 · Cited by 31
“For surveys of Hot Jupiters, with f ≈ 1% of main-sequence (MS) stars (Wright et al. 2012; Mayor et al. 2011), this leads to minimum samples of 2000 MS stars to expect a single transit discovery.”
BackgroundBolmont, É., Gallet, F., Mathis, S., Charbonnel, C., Amard, L., & Alibert, Y. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201730662/pdf · Cited by 30
Revised Exoplanet Radii and Habitability Using Gaia Data Release 2
Johns, D., Marti, C., Huff, M., McCann, J., Wittenmyer, R. A., Horner, J., & Wright, D. J. (2018) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aae5fb · Cited by 29
“Those first planets included the first surprise of the Exoplanet Era—the “hot Jupiters”—planets the mass of Jupiter moving on orbits with periods measured in hours, or just a few days (e.g., Mayor & Queloz 1995; Hellier et al. 2011; Wright et al. 2012).”
BackgroundMASCARA-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., Paredes, L., et al. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935611 · Cited by 29
“Hot Jupiters − gas giant planets that closely orbit their host star − are relatively rare, but over-represented in both radial velocity and transit surveys because they are the easiest to find (Wright et al. 2012; Dawson & Johnson 2018).”
BackgroundWASP-92b, WASP-93b and WASP-118b: three new transiting close-in giant planets
Hay, K. L., Cameron, A. C., Doyle, A. P., Hébrard, G., Skillen, I., Anderson, D. R., Barros, S. C. C., Brown, D. J. A., Bouchy, F., Busuttil, R., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2090 · Cited by 29
“Hot Jupiters are rare objects with an occurrence rate estimated to be ∼ 1%, depending on the stellar population surveyed (Wang et al. 2015; Howard et al. 2012; Wright et al. 2012).”
BackgroundEvidence That the Occurrence Rate of Hot Jupiters around Sun-like Stars Decreases with Stellar Age
Miyazaki, S., & Masuda, K. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acff71 · Cited by 28
A HARPS RV search for planets around young nearby stars
Grandjean, A., Lagrange, A. ‐., Keppler, M., Meunier, N., Mignon, L., Borgniet, S., Chauvin, G., Desidera, S., Galland, F., Messina, S., et al. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201936038/pdf · Cited by 32
Evidence for the Late Arrival of Hot Jupiters in Systems with High Host-star Obliquities
Hamer, J. H., & Schlaufman, K. C. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac69ef · Cited by 31
Gong, Y., & Ji, J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1300 · Cited by 28
“In the transit surveys the occurrence rate is ∼ 0.1 − 0.4%, the exact numbers slightly differ for different surveys (∼ 0.4% in Kepler mission) (Wright et al. 2012; Wang et al. 2015).”
BackgroundInfluentialSchlaufman, K. C., & Winn, J. N. (2016) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 27
Another shipment of six short-period giant planets from TESS
Rodriguez, J. E., Quinn, S. N., Vanderburg, A. M., Zhou, G., Eastman, J. D., Thygesen, E., Cale, B., Ciardi, D. R., Reed, P. A., Oelkers, R. J., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad595 · Cited by 33
Signature of Planetary Mergers on Stellar Spins
Qureshi, A., Naoz, S., & Shkolnik, E. L. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aad562 · Cited by 27
Radial velocity homogeneous analysis of M dwarfs observed with HARPS
Mignon, L., Delfosse, X., Meunier, N., Chaverot, G., Burn, R., Bonfils, X., Bouchy, F., Astudillo-Defru, N., Curto, G. L., Gaisné, G., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451142 · Cited by 26
LAMBDA BOO ABUNDANCE PATTERNS: ACCRETION FROM ORBITING SOURCES
Jura, M. (2015) · The Astronomical Journal · doi:10.1088/0004-6256/150/6/166 · Cited by 26
“For F,G and K stars, the frequency of hot Jupiters is 1.2% ± 0.38% (Wright et al. 2012).”
BackgroundInfluentialDalba, P. A., Kane, S. R., Barclay, T., Bean, J. L., Campante, T. L., Pepper, J. A., Ragozzine, D., & Turnbull, M. C. (2019) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aaf183 · Cited by 26
“The combination of transit and RV occurrence rates better constrains the true underlying exoplanet population and identifies the biases of each method (e.g., Howard et al. 2012; Wright et al. 2012; Dawson & Murray-Clay 2013; Guo et al. 2017).”
MethodTruly eccentric – II. When can two circular planets mimic a single eccentric orbit?
Wittenmyer, R. A., Bergmann, C., Horner, J., Clark, J., & Kane, S. R. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz236 · Cited by 26
“We found giant, Jupiter-mass planets orbiting perilously close to their host stars (e.g. Butler et al. 1997; Hellier et al. 2011; Wright et al. 2012), as well as planets moving on orbits so eccentric that they more closely resemble the orbits of comets than the planets in our own backyard (e.g.…”
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. (2019) · UCL Discovery (University College London) · Cited by 26
Cañas, C. I., Kanodia, S., Libby-Roberts, J. E., Lin, A. S. J., Schutte, M., Powers, L. C., Jones, S., Monson, A. J., Wang, S., Stefánsson, G., et al. (2023) · The Astronomical Journal · doi:10.3847/1538-3881/acdac7 · Cited by 33
On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples
Hamers, A. S. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx035 · Cited by 23
Formation of Polar Terrestrial Circumbinary Planets
Childs, A. C., & Martin, R. G. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ac2957 · Cited by 25
Exterior Companions to Hot Jupiters Orbiting Cool Stars Are Coplanar
Becker, J. C., Vanderburg, A., Adams, F. C., Khain, T., & Bryan, M. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa9176 · Cited by 25
“…are thought to account for only about 0.9 – 1.5% of the total population of planets (Marcy et al. 2005; Cumming et al. 2008; Mayor et al. 2011; Wright et al. 2012; Wang et al. 2015), they are over-represented in our current population of discovered exoplanets due to their large masses,…”
BackgroundInfluentialFormation of Terrestrial Planets
Izidoro, A., & Raymond, S. N. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_142 · Cited by 30
“We now know that 10-20% of Sun-like stars host gas giant planets (Mayor et al. 2011b; Howard et al. 2012b) but that hot Jupiters exist around only ∼1% (Wright et al. 2012; Howard et al. 2010b).”
BackgroundThe fundamental connections between the Solar System and exoplanetary science
Kane, S. R., Arney, G., Byrne, P. K., Dalba, P. A., Desch, S. J., Horner, J., Izenberg, N. R., Mandt, K. E., Meadows, V., & Quick, L. C. (2021) · University of Southern Queensland ePrints (University of Southern Queensland) · Cited by 26
Boley, K. M., Wang, J., Zinn, J., Collins, K. A., Collins, K. I., Gan, T., & Li, T. S. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac0e2d · Cited by 24
Modeling the High-resolution Emission Spectra of Clear and Cloudy Nontransiting Hot Jupiters
Malsky, I., Rauscher, E., Kempton, E. M.-R., Roman, M. T., Long, D. E., & Harada, C. K. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac2a2a · Cited by 24
Exoplanetary Geophysics: An Emerging Discipline
Laughlin, G., & Lissauer, J. J. (2015) · Elsevier eBooks · doi:10.1016/b978-0-444-53802-4.00186-x · Cited by 34
“Among a large sample of main-sequence host stars, they are the exception rather than the rule, with an occurrence rate among nearby Sun-like main-sequence stars of only about ∼1% (Mayor et al. 2011a; Wright et al. 2012).”
BackgroundHwang, H.-C., Hamer, J. H., Zakamska, N. L., & Schlaufman, K. C. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2124 · Cited by 24
“Briefly, hot jupiters were selected from the confirmed planets table of the NASA Exoplanet Archive using the fiducial definition from Wright et al. (2012), planets having P < 10 days and M sin i > 0.1 MJup.”
BackgroundMethodInfluentialThe SOPHIE search for northern extrasolar planets
Moutou, C., Hébrard, G., Bouchy, F., Arnold, L., Santos, N. C., Astudillo-Defru, N., Boisse, I., Bonfils, X., Borgniet, S., Delfosse, X., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322067 · Cited by 24
“…massive than 50M⊕ that have periods shorter than 11 days, Howard et al. (2010) found an occurrence of 1.2±0.2% for planets more massive than 100M⊕ with periods shorter than 12 days and Wright et al. (2012) estimated 1.2±0.38% for planets more massive than 30M⊕ with periods shorter than 10 days.”
BackgroundInfluentialTracking Advanced Planetary Systems (TAPAS) with HARPS-N
Niedzielski, A., Villaver, E., Nowak, G., Adamów, M., Maciejewski, G., Kowalik, K., Wolszczan, A., Deka-Szymankiewicz, B., & Adamczyk, M. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628417 · Cited by 23
“The origin of this rare class of objects, only known to be present around approximately 0.5–1% of FGK stars (Wright et al. 2012; Howard et al. 2012), generally involves early (e.g., Type II), or late migration scenarios (following planet-planet scattering or secular perturbations from more distant…”
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) · University of Southern Queensland ePrints (University of Southern Queensland) · Cited by 23
Self-citationGaidos, E. J., Fischer, D. A., Mann, A. W., & Howard, A. W. (2013) · Cited by 23
Self-citationLimits to the presence of transiting circumbinary planets in CoRoT Data
Klagyivik, P., Deeg, H. J., Cabrera, J., Csizmadia, S., & Almenara, J. M. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628244 · Cited by 22
“The fraction of single stars with hot Jupiters (P < 10 days) is 1.2% ± 0.38% from the Doppler sample of Wright et al. (2012) and 0.6% ± 0.1% from the Kepler photometric sample (Wang et al. 2015b).”
BackgroundInfluentialSearch for giant planets in M67 IV: survey results
Brucalassi, A., Koppenhoefer, J., Saglia, R. P., Pasquini, L., Ruíz, M. T., Bonifacio, P., Bedin, L. R., Libralato, M., Biazzo, K., Melo, C., et al. (2017) · MPG.PuRe (Max Planck Society) · doi:10.48550/arxiv.1703.04296 · Cited by 22
“These values appear to be higher than what is observed in field stars (Wright et al. 2012; Howard et al. 2011).”
BackgroundLongmore, S. N., Chevance, M., & Kruijssen, J. M. D. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/abeb22 · Cited by 22
“Rows 4 and 5 in Table 1 show the exoplanet multiplicity distributions of the field and overdensities when remov- ing systems with hot Jupiters (HJs; here defined by masses > 50M⊕ and semi-major axes < 0.2 au) from the Winter et al. (2020) sample.”
BackgroundInfluentialStellar companions and Jupiter-like planets in young associations
Gratton, R., Bonavita, M., Mesa, D., Desidera, S., Zurlo, A., Marino, S., D’Orazi, V., Rigliaco, E., Nascimbeni, V., Barbato, D., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348393 · Cited by 22
Quantifying the Influence of Jupiter on the Earth’s Orbital Cycles
Horner, J., Vervoort, P., Kane, S. R., Ceja, A. Y., Waltham, D., Gilmore, J., & Turner, S. K. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab5365 · Cited by 22
Evolution of galaxy habitability
Gobat, R. A. S., & Hong, S. E. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628834 · Cited by 21
“012 for solar-type stars (Wright et al. 2012) and, in both cases, set f T , 0 = 0 .”
BackgroundInfluentialBoisse, I., Hartman, J. D., Bakos, G. Á., Penev, K., Csubry, Z., Béky, B., Latham, D. W., Bieryla, A., Torres, G., Kovács, G., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201220993 · Cited by 21
“Radial velocity (RV) surveys with well defined sample limits estimated an occurrence rate of hot Jupiters in the Solar neighborhood to be around one percent (Udry & Santos 2007; Wright et al. 2012).”
BackgroundTransit probabilities in secularly evolving planetary systems
Read, M. J., Wyatt, M. C., & Triaud, A. H. M. J. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx798 · Cited by 20
“This is large compared with the occurrence rate of Hot Jupiters (∼ 1 − 2% e.g. Marcy et al. (2005); Cumming et al. (2008); Mayor et al. (2011); Wright et al. (2012); Santerne et al. (2016)).”
Result
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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