List of exoplanet extremes

Short description: none

The following are lists of extremes among the known exoplanets. The properties listed here are those for which values are known reliably. It is important to note that the study of exoplanets is one of the most dynamic emerging fields of science, and these values may change wildly as new discoveries are made.

## Contents

* 1 Extremes from Earth's viewpoint
* 2 Planetary characteristics
* 3 Orbital characteristics
* 4 Stellar characteristics
* 5 System characteristics
* 6 See also
* 7 Notes and references
* 8 External links

## Extremes from Earth's viewpoint

Title  | Planet  | Star  | Data  | Notes

|
|
|
|

Most distant discovered  | SWEEPS-11 / SWEEPS-04 | SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6  | 27,710 light-years[1] | Several candidate extragalactic planets have been detected.

The most distant potentially habitable planet confirmed is Kepler-1606b, at 2,870 light-years distant,[2] although the unconfirmed planet KOI-5889.01 is over 5,000 light-years distant.

On 31 March 2022, K2-2016-BLG-0005Lb was reported to be the most distant exoplanet discovered by Kepler telescope, at 17,000 light-years away.[3]

Least distant | Proxima Centauri b, c and d | Proxima Centauri | 4.25 light-years  | Proxima Centauri b and d are the closest rocky exoplanets, b is the closest potentially habitable exoplanet known, and c is the closest mini-Neptune and potentially ringed planet. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25,000 years), this is an absolute record.
Most distant directly visible  | CT Chamaeleontis b | CT Chamaeleontis | 622 light-years[4] | The disputed planet candidate CVSO 30 c may be more distant, at 1,200 light-years.
Closest directly visible  | COCONUTS-2b | L 34-26  | 35.5 light-years[4] | WISE 1217+1626 B is closer, but is generally considered a brown dwarf. Proxima Centauri c (confirmed in 2020 using archival Hubble data from 1995+) may have been directly imaged.[5]
Star with the brightest apparent magnitude with a planet  | Pollux b | Pollux[6] | Apparent magnitude is 1.14  | Alpha Centauri A (apparent magnitude 0.01) has a unconfirmed planet candidate. The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.[7] As of 2021[update], a candidate planet around Vega has been detected.[8]
Star with the faintest apparent magnitude with a planet  | MOA-bin-29Lb  | MOA-bin-29L  | Apparent magnitude is 44.61[4] |
Largest angular distance separation from its host star  | COCONUTS-2b | COCONUTS-2 | 594 arcseconds[9] |

## Planetary characteristics

Title  | Planet  | Star  | Data  | Notes

|
|
|
|

Least massive  | PSR B1257+12 b | PSR B1257+12 | 0.020±0.002 M🜨[4] | The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 M⊕.[9]
Most massive  | The candidate for the most massive planet is contentious, as it is difficult to distinguish between a highly massive planet and a brown dwarf (the border between them approximately from 13 to 80 MJ). So it is estimated the largest planets are approximately a dozen Jupiter masses.
Largest radius | Proplyd 133-353  | 7.4±0.3 – 8±1.1 [[Astronomy:Jupiter radius | J}}}}}}]][10][lower-alpha 1] | Proplyd 133-353 could be a sub-brown dwarf or an rogue planet, with a photoevaporating disk.

HAT-P-67b has the largest accurately measured radius, at 2.085+0.096
−0.071 RJ.[11]

Smallest radius | Kepler-37b | Kepler-37 | 0.296±0.037 R🜨[4] | The extrasolar planetesimals SDSS J1228+1040 b[12] and WD 1145+017 b are smaller.
Most dense  | TOI-4603b  | HD 245134  | 14.1+1.7−1.6 g/cm3 [13] | TOI-4603b has a mass of 12.89+0.58−0.57 MJ and a radius of 1.042+0.038−0.035 RJ.[14]

KELT-1b is denser, with 22.1+5.62−9.16 g/cm3.[15] But, with a mass of 27.23 MJ, it is likely a brown dwarf.

Kepler-131c might be more dense at 77.7+55
−55 g/cm3,[16] but the value is very uncertain.

Least dense  | Kepler-51c, b and/or possibly d[17] | Kepler-51[17] | ~ 0.03 g/cm3[17] | The densities of Kepler-51 b and c have been constrained to be below 0.05 g/cm3 (expected value 0.03 g/cm3 for each). The density of Kepler-51d is determined to be 0.046 ± 0.009 g/cm3.[17]
Hottest (irradiated hot Jupiter)  | KELT-9b | KELT-9  | 4,050±180 K[4](3777 °C)  | The unconfirmed planets Kepler-70b and Kepler-70c may be hotter, both at >6,800 K.[18]
Hottest (self-luminous)  | AB Aurigae b | AB Aurigae | 3,800 K (3,530 °C)[19] |
Coldest |  OGLE-2005-BLG-390Lb |  OGLE-2005-BLG-390L | 50 K (−223.2 °C)[20] | The disputed planet Proxima Centauri c may be cooler, at 39 K (−234.2 °C).[21]
Highest albedo | LTT 9779 b | LTT 9779 | 0.8[22] | For comparison, Earth is 0.3 and Venus is 0.76.
Lowest albedo  | TrES-2b | GSC 03549-02811 | Geometric albedo < 1%[23] | Best-fit model for albedo gives 0.04% (0.0004).[18]
Youngest  | CI Tauri b  | CI Tauri | 2 Myr[24]
Oldest  | WASP-183b  | WASP-183  | 14.9±1.7 Gyr[4] | The estimated age of the universe is 13.8 billion years, within the margin of error.

## Orbital characteristics

Title  | Planet  | Star  | Data  | Notes

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|
|
|

Longest orbital period
(Longest year) | COCONUTS-2b | COCONUTS-2  | 1.1 million years[25] | 2MASS J2126–8140 previously held this record at ~900,000 years.
Shortest orbital period
(Shortest year) | SWIFT J1756.9-2508 b | SWIFT J1756.9-2508 | 48 minutes, 56.5 seconds[26] | K2-137b has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.[27]
Most eccentric orbit | HD 20782 b[28] | HD 20782 | 0.956±0.004 | [29] Record among confirmed planets. The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.[30] HD 80606 b previously held this record at 0.93226+0.00064
−0.00069.
Highest orbital inclination | HD 204313 e | HD 204313 | 176.092°+0.963°
−2.122° | [31][32]
Lowest orbital inclination  | HD 331093 b  | HD 331093  | >0.3704° | [33][32] HD 43197 c has the lowest orbital inclination that is not a lower limit, of 11.42°+5.388°
−3.07°.[32]
Largest orbit around a single star  | COCONUTS-2b | COCONUTS-2  | 7,506+5,205
−2,060 astronomical unit|AU[4] | Projected separation of 6,471 AU.[25] Next largest are 2MASS J2126–8140 with 6,900 AU and HD 106906 b[34] with ~738 AU.
Smallest orbit  | PSR J1719-1438 b | PSR J1719−1438 | 0.0044 AU (658,230 km)  | [35]
Smallest orbit around binary star  | Kepler-47b | Kepler-47AB | 0.2877+0.0014
−0.0011 AU[4] | [36]
Smallest ratio of semi-major axis of a planet orbit to binary star orbit  | Kepler-16b | Kepler-16AB | 3.14 ± 0.01  | [37]
Largest orbit around binary star  | SR 12 (AB) c  | SR 12 AB  | ≈1100 AU[38] | SR 12 (AB) c has a mass of 0.013±0.007 M☉.[38]

ROXs 42B (AB) b is lower in mass at 9.0+6−3 |♃|J}}}}}}, however also in projected separation of ≈150 AU.[39]

DT Virginis c, also known as Ross 458 (AB) c, at a projected separation of ≈1200 AU, with several mass estimates below the deuterium burning limit, has a latest mass determination of 27±4 MJ.[40]

Largest orbit around a single star in a multiple star system  | ROXs 12 b | ROXs 12 | 210±20 AU[4] |
Largest separation between binary stars with a circumbinary planet  | SR 12 (AB) c  | SR 12 AB  | ≈26 AU[38] | SR 12 (AB) c has a mass of 0.013±0.007 M☉ at a projected separation of ≈1100 AU.[38]

FW Tauri b orbits at a projected separation of 330±30 astronomical unit|AU around a ≈11 AU separated binary.[41] It was shown to be more likely a 0.1 M☉ star surrounded by a protoplanetary disk than a planetary-mass companion.[42]

Closest orbit between stars with a planet orbiting one of the stars  | OGLE-2013-BLG-0341LBb | OGLE-2013-BLG-0341LB | ~12–17 AU
(10 or 14 AU projected distance)[43] | OGLE-2013-BLG-0341L b's semi-major axis is 0.7 AU.[43]
Smallest semi-major-axis difference between consecutive planets  | Kepler-70b and Kepler-70c[18] | Kepler-70 | 0.0016 AU (240,000 km)  | During closest approach, Kepler-70c would appear 5 times the size of the Moon in Kepler-70b's sky.[needs update]
Smallest semi-major axis ratio between consecutive planets  | Kepler-36b and Kepler-36c | Kepler-36 | 11%  | Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively, c is 11% further from star than b.

## Stellar characteristics

Title  | Planet  | Star  | Data  | Notes

|
|
|
|

Highest metallicity | HD 126614 Ab | HD 126614 A | +0.56 dex | Located in a triple star system.
Lowest metallicity  | K2-344b  | K2-344  | −0.95±0.02 dex[4] | BD+20°2457 may be the lowest-metallicity planet host ([Fe/H]=−1.00); however, the proposed planetary system is dynamically unstable.[44] Kapteyn's Star may also be the lowest-metallicity planet host ([Fe/H]=−0.99±0.04), but its planets are most likely artifacts of stellar activity and rotation.[45]

Planets were announced around even the extremely low-metallicity stars HIP 13044 and HIP 11952; however, these claims have since been disproven.[46]

Highest stellar mass  | Mu2 Scorpii b | Mu2 Scorpii | 9.1±0.3 M☉[47] | M51-ULS-1b, listed as a candidate planet with 4 sigma confidence, may be the planet with the highest-mass host star. The host is a massive O-class supergiant and a black hole orbiting each other at 0.8 AU, with a combined system mass of >60 solar masses. The planet is a Saturn-sized (0.72 Jupiter radii) object orbiting the black-hole/supergiant binary at 10 AU. The host stars giving off a combined 1 million solar luminosities, the planet receives the equivalent irradiation of 51 Pegasi b, which orbits its star at 0.045 AU. M51-ULS-1b would also be one of the youngest planets ever discovered, with a system age of <10 million years according to evolutionary models.[48]

Because M51-ULS-1b requires further confirmation, the object V921 Sco b, a 60-Jupiter-mass object orbiting a 20-solar-mass 30,000 K Herbig Haro B0IV-class subgiant at 835 AU, may actually be the record holder. Despite the large distance, V921 Sco b receives a comparable amount of irradiation as Mars, owing to the large mass and luminosity of the host star. At 20 solar masses, V921 Sco is the most massive object to host a substellar object. Normally, V921 Sco b would be considered a brown dwarf, but given the high mass of the host star, and the growing studies that confirm the correlation of more massive planets around more massive stars, this object could be considered a planet. Hatzes and Rauer quote an upper limit of 60 MJup for a core-accretion formation of high-mass gas giants, which is how heavy this object is. Furthermore, the Extrasolar Planets Encyclopedia lists objects up to 60 Jupiter masses as planets if they orbit stars.[49]

b Centauri has a mass of 6 solar masses.

The stars R126 (HD 37974) and R66 (HD 268835) in the Large Magellanic Cloud have masses of 70 and 30 solar masses and have dust discs but no planets have been detected yet.

Lowest stellar mass (main sequence)  | OGLE-2016-BLG-1195Lb | OGLE-2016-BLG-1195L  | 0.078+0.016
−0.012 M☉[4] | Could also be OGLE-2015-BLG-1771L, at 0.077+0.119
−0.044 M☉.[4]
Lowest stellar mass (brown dwarf)  | 2MASS J1119-1137 B  | 2MASS J1119–1137 A  | 0.0033 M☉ | The system 2MASS J1119-1137 AB is a pair of binary rogue planets approximately 3.7 MJup each.[50]
Largest stellar radius  | HD 240237 b | HD 240237 | 71.23±17.07 R☉[4] | HD 81817 and Mirach (β Andromedae) are larger, at 83.8±7.8 R☉[4] and 86.4 R☉[51] respectively, but their planetary companions may actually be brown dwarfs, and in the case of HD 81817 it companion may be a red dwarf. R Leonis (299 or 320-350 R☉)[52][53] has a candidate planet. It is a Mira variable.

The stars R126 and R66 in the Large Magellanic Cloud have radius of 78 R☉ and 131 R☉[54] and have dust discs but no planets have been detected yet.

Smallest stellar radius (main sequence star)  | Teegarden's Star b and c | Teegarden's Star | 0.107±0.004 R☉[4] | VB 10 (0.102 R☉)[55] has a disproven planet candidate.
Smallest stellar radius (brown dwarf)  | 2M 0746+20 b[56] | 2M 0746+20  | 0.089 (± 0.003) R☉ | Planet's mass is very uncertain at 30.0 (± 25.0) MJup.
Smallest stellar radius (stellar remnant)  | PSR B0943+10 b and c[57][58][59] | PSR B0943+10 | 0.000003737 R☉ (2.5998 km)[60] |
Highest stellar luminosity  | Beta Andromedae b | Mirach | 1675 L☉ | [61][32] With a mass of 28.26+2.05
−2.17 MJ, the planet is likely a brown dwarf. Beta Cancri, with a luminosity of 794 L☉, is the most luminous star to host a planet (Beta Cancri b) that is not a potential brown dwarf.[62][32]

The stars R126 and R66 in the Large Magellanic Cloud have luminosity of 1400000 L☉ and 320000 L☉[54] and have dust discs but no planets have been detected yet.

Lowest stellar luminosity (main sequence star)  | TRAPPIST-1 planets  | TRAPPIST-1 | 0.0005495 L☉ | [63][32]
Oldest star  | WASP-183b  | WASP-183  | 14.9±1.7 Gyr[4] | The estimated age of the universe is 13.8 billion years, within the margin of error.
Hottest star with a planet  | NSVS 14256825 b | NSVS 14256825 | 40,000 K[64] | NN Serpentis is hotter, with a temperature of 57,000 K,[4] but the existence of its planets is disputed.[65]
Hottest main-sequence star with a planet  | b Centauri b | b Centauri | 18,310±320 K[66] | V921 Scorpii b orbits a hotter star, at 30,000 K. Its host star is a 20-solar-mass B0IV-class subgiant.[49] However, at 60 Jupiter masses, it is not considered a planet under most definitions.

The candidate planet M51-ULS-1b's supergiant primary is an O5-class supergiant with an estimated surface temperature of 40,000 K, but as the star is a supergiant, does not count as on the main sequence.

Coolest star with a planet  | TRAPPIST-1b, c, d, e, f, g and h | TRAPPIST-1 | 2,511 K  | Technically Oph 162225-240515, CFBDSIR 1458+10 and WISE 1217+1626 are cooler, but are classified as brown dwarfs.

## System characteristics

Title  | System(s)  | Planet(s)  | Star(s)  | Notes

|
|
|
|

System with most planets  | Kepler-90 | 8  | 1

HD 10180 has six confirmed planets and potentially three more planets.[67]

System with most planets in habitable zone  | TRAPPIST-1 | 7  | 1  | Four planets in this system (d, e, f and g) orbit within the habitable zone.[68]
System with most stars  | Kepler-64 | PH1b (Kepler-64b)  | 4  | PH1b has a circumbinary orbit.

30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system until later studies revealed a true mass well above 80 MJup.[69]

Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star)  | Kepler-42 | b, c, d | 1  | Kepler-42 b, c and d have a semi-major axis of only 0.0116, 0.006 and 0.0154 AU, respectively.

Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively.

Multiplanetary system with largest mean semi-major axis (planets are farthest from their star)  | TYC 8998-760-1 | b, c | 1  | TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.[4]
Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet)  | Kepler-42 | b, c, d | 1  | Kepler-42 b, c and d have a semi-major axis of only 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is only 0.0094 AU.

Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. The separation between closest and furthest is only 0.0016 AU (239,356 km).

Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet)  | TYC 8998-760-1 | b, c | 1  | TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.[4] The separation between closest and furthest is 158 AU.
System with smallest total planetary mass  | Kepler-444 | b, c, d, e, f  | 3  | The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
System with largest total planetary mass  | Nu Ophiuchi | b, c  | 1  | Nu Ophiuchi b and c have masses of 22.206 and 24.662 Jupiter masses, respectively.[4] They may be brown dwarfs.
Multiplanetary system with smallest mean planetary mass  | Kepler-444 | b, c, d, e, f  | 3  | The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
Multiplanetary system with largest mean planetary mass  | Nu Ophiuchi | b, c  | 1  | Nu Ophiuchi b and c have masses of 22.206 and 24.662 Jupiter masses, respectively.[4] They may be brown dwarfs.
Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets)  | Teegarden's Star | b, c  | 1  | Teegarden b and c are estimated to have masses of 1.05 and 1.11 Earth masses, respectively.
Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets)  | Kepler-37 | b, d | 1  | Mercury and Jupiter have a mass ratio of 5,750 to 1. Kepler-37 d and b may have a mass ratio between 500 and 1,000, and Gliese 676 c and d have a mass ratio of 491.

## See also

* Extremes on Earth
* Lists of exoplanets
* List of exoplanet firsts
* List of stars with proplyds
* Methods of detecting exoplanets
* List of potentially habitable exoplanets

## Notes and references

1. ↑ "HEC: Top 10 Exoplanets". University of Puerto Rico at Arecibo. 5 December 2015. http://phl.upr.edu/projects/habitable-exoplanets-catalog/top10.
2. ↑ "Exoplanet-catalog-Exoplanet exploration-Kepler-1606b". https://exoplanets.nasa.gov/exoplanet-catalog/2252/kepler-1606-b/.
3. ↑ Specht, D. (2023). "Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing". Monthly Notices of the Royal Astronomical Society 520 (4): 6350–6366. doi:10.1093/mnras/stad212.
4. ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 4.13 4.14 4.15 4.16 4.17 4.18 4.19 4.20 4.21 "Planetary Systems Composite Data". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars.
5. ↑ Gratton, R. (June 2020). "Searching for the near-infrared counterpart of Proxima c using multi-epoch high-contrast SPHERE data at VLT". Astronomy & Astrophysics 638: A120. doi:10.1051/0004-6361/202037594. Bibcode: 2020A&A...638A.120G.
6. ↑ Lee, T. A. (October 1970), "Photometry of high-luminosity M-type stars", The Astrophysical Journal 162: 217, doi:10.1086/150648, Bibcode: 1970ApJ...162..217L
7. ↑ "NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega" (Press release). Whitney Clavin, NASA. 8 January 2013. Retrieved 4 March 2013.
8. ↑ Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth et al. (21 January 2021). "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets". The Astronomical Journal 161 (4): 157. doi:10.3847/1538-3881/abdec8. Bibcode: 2021AJ....161..157H.
9. ↑ 9.0 9.1 "The Extrasolar Planet Encyclopaedia — Catalog Listing". Extrasolar Planets Encyclopaedia. 11 January 1995. https://exoplanet.eu/catalog/. Retrieved 2019-05-04.
10. ↑ Fang, Min; Kim, Jinyoung Serena; Pascucci, Ilaria; Apai, Dániel; Manara, Carlo Felice (2016-12-12). "A candidate planetary-mass object with a photoevaporating disk in Orion". The Astrophysical Journal 833 (2): L16. doi:10.3847/2041-8213/833/2/L16. ISSN 2041-8213. Bibcode: 2016ApJ...833L..16F.
11. ↑ Manitowoc, Terrence Gollata (2018-11-27). "What's the diameter of the largest exoplanet found so far?" (in en-US). https://www.astronomy.com/science/whats-the-diameter-of-the-largest-exoplanet-found-so-far/.
12. ↑ "Planet SDSS J1228+1040 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/sdss_j1228_1040_b--7079/. Retrieved 2019-08-05.
13. ↑ Khandelwal, Akanksha; Sharma, Rishikesh; Chakraborty, Abhijit; Chaturvedi, Priyanka; Ulmer-Moll, Solène; Ciardi, David R.; Boyle, Andrew W.; Baliwal, Sanjay et al. (2023-04-14). "Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603". Astronomy & Astrophysics 672: L7. doi:10.1051/0004-6361/202245608. ISSN 0004-6361. Bibcode: 2023A&A...672L...7K. https://www.aanda.org/10.1051/0004-6361/202245608.
14. ↑ "Planet TOI-4603 b". https://exoplanetarchive.ipac.caltech.edu/overview/TOI-4603.
15. ↑ Johns, Daniel; Marti, Connor; Huff, Madison; McCann, Jacob; Wittenmyer, Robert A.; Horner, Jonathan; Wright, Duncan J. (2018-11-16). "Revised Exoplanet Radii and Habitability Using Gaia Data Release 2". The Astrophysical Journal Supplement Series 239 (1): 14. doi:10.3847/1538-4365/aae5fb. ISSN 1538-4365. Bibcode: 2018ApJS..239...14J.
16. ↑ Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew W.; Rowe, Jason F.; Jenkins, Jon M.; Bryson, Stephen T.; Latham, David W.; Howell, Steve B. et al. (2014-01-13). "Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets". The Astrophysical Journal Supplement Series 210 (2): 20. doi:10.1088/0067-0049/210/2/20. ISSN 0067-0049. Bibcode: 2014ApJS..210...20M.
17. ↑ 17.0 17.1 17.2 17.3 Very Low-Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event: Kento Masuda
18. ↑ 18.0 18.1 18.2 Charpinet, S. et al. (21 December 2011). "A compact system of small planets around a former red-giant star". Nature 480 (7378): 496–499. doi:10.1038/nature10631. ISSN 1476-4687. PMID 22193103. Bibcode: 2011Natur.480..496C.
19. ↑ Zhou, Yifan; Sanghi, Aniket; Bowler, Brendan P.; Wu, Ya-Lin; Close, Laird M.; Long, Feng; Ward-Duong, Kimberly; Zhu, Zhaohuan et al. (July 2022). "HST/WFC3 Hα Direct-imaging Detection of a Pointlike Source in the Disk Cavity of AB Aur" (in en). The Astrophysical Journal Letters 934 (1): L13. doi:10.3847/2041-8213/ac7fef. ISSN 2041-8205. Bibcode: 2022ApJ...934L..13Z.
20. ↑ Beaulieu, J. -P.; Bennett, D. P.; Fouqué, P.; Williams, A.; Dominik, M.; Jørgensen, U. G.; Kubas, D.; Cassan, A. et al. (2006-01-01). "Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing". Nature 439 (7075): 437–440. doi:10.1038/nature04441. ISSN 0028-0836. PMID 16437108. Bibcode: 2006Natur.439..437B.
21. ↑ Damasso, Mario; Del Sordo, Fabio; Anglada-Escudé, Guillem; Giacobbe, Paolo; Sozzetti, Alessandro; Morbidelli, Alessandro; Pojmanski, Grzegorz; Barbato, Domenico et al. (2020-01-01). "A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU". Science Advances 6 (3): eaax7467. doi:10.1126/sciadv.aax7467. PMID 31998838. Bibcode: 2020SciA....6.7467D.
22. ↑ Hoyer, S.; Jenkins, J. S.; Parmentier, V.; Deleuil, M.; Scandariato, G.; Wilson, T. G.; Díaz, M. R.; Crossfield, I. J. M. et al. (10 July 2023). "The extremely high albedo of LTT 9779 b revealed by CHEOPS". Astronomy & Astrophysics 675: A81. doi:10.1051/0004-6361/202346117. https://www.aanda.org/articles/aa/full_html/2023/07/aa46117-23/aa46117-23.html. Retrieved 12 July 2023.
23. ↑ David M. Kipping (2011). "Detection of visible light from the darkest world". Monthly Notices of the Royal Astronomical Society 417 (1): L88–L92. doi:10.1111/j.1745-3933.2011.01127.x. Bibcode: 2011MNRAS.417L..88K. http://www.astro.princeton.edu/~dsp/PrincetonSite/Home_files/darkest_world.pdf. Retrieved 2011-08-12.
24. ↑ Flagg, Laura; Johns-Krull, Christopher M.; Nofi, Larissa; Llama, Joe; Prato, L.; Sullivan, Kendall; Jaffe, D. T.; Mace, Gregory (2019-06-21). "CO Detected in CI Tau b: Hot Start Implied by Planet Mass and M K". The Astrophysical Journal 878 (2): L37. doi:10.3847/2041-8213/ab276d. ISSN 2041-8213. Bibcode: 2019ApJ...878L..37F.
25. ↑ 25.0 25.1 Zhang, Zhoujian; Liu, Michael C.; Claytor, Zachary R.; Best, William M. J.; Dupuy, Trent J.; Siverd, Robert J. (2021). "The Second Discovery from the COCONUTS Program: A Cold Wide-orbit Exoplanet around a Young Field M Dwarf at 10.9 pc". The Astrophysical Journal Letters 916 (2): L11. doi:10.3847/2041-8213/ac1123. Bibcode: 2021ApJ...916L..11Z.
26. ↑ "The Extrasolar Planet Encyclopaedia — SWIFT J1756-2508". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/swift_j1756_2508--1515/. Retrieved 2018-08-22.
27. ↑ "The Extrasolar Planet Encyclopaedia — K2-137 b.". Extrasolar Planets Encyclopaedia. 2018. https://exoplanet.eu/catalog/k2_137_b--6591/.
28. ↑ "HD 20781 b". http://www.openexoplanetcatalogue.com/system.html?id=HD+20781+b.
29. ↑ "The Extrasolar Planet Encyclopaedia — HD 20782 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/hd_20782_b--319/. Retrieved 2019-05-04.
30. ↑ "The Extrasolar Planet Encyclopaedia — VB 10 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/vb_10_b--550/. Retrieved 2020-02-12.
31. ↑ Feng, Fabo; Butler, R. Paul; Vogt, Steven S.; Clement, Matthew S.; Tinney, C. G.; Cui, Kaiming; Aizawa, Masataka; Jones, Hugh R. A. et al. (2022-09-01). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series 262 (1): 21. doi:10.3847/1538-4365/ac7e57. ISSN 0067-0049. Bibcode: 2022ApJS..262...21F.
32. ↑ 32.0 32.1 32.2 32.3 32.4 32.5 "Planetary Systems". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PS.
33. ↑ Dalal, S.; Kiefer, F.; Hébrard, G.; Sahlmann, J.; Sousa, S. G.; Forveille, T.; Delfosse, X.; Arnold, L. et al. (2021-07-01). "The SOPHIE search for northern extrasolar planets. XVII. A wealth of new objects: Six cool Jupiters, three brown dwarfs, and 16 low-mass binary stars". Astronomy and Astrophysics 651: A11. doi:10.1051/0004-6361/202140712. ISSN 0004-6361. Bibcode: 2021A&A...651A..11D. https://ui.adsabs.harvard.edu/abs/2021A&A...651A..11D.
34. ↑ De Rosa, Robert J.; Kalas, Paul (February 2019). "A Near-coplanar Stellar Flyby of the Planet Host Star HD 106906". The Astronomical Journal 157 (3): 125. doi:10.3847/1538-3881/ab0109. Bibcode: 2019AJ....157..125D.
35. ↑ "PSR J1719-1438 | NASA Exoplanet Archive". https://exoplanetarchive.ipac.caltech.edu/overview/PSR J1719-1438 b.
36. ↑ Orosz, J. et al. (2012). "Kepler-47: A Transiting Circumbinary Multi-Planet System". Science 337 (6101): 1511–4. doi:10.1126/science.1228380. PMID 22933522. Bibcode: 2012Sci...337.1511O.
37. ↑ Laurance R. Doyle et al. (2011). "Kepler-16: A Transiting Circumbinary Planet". Science 333 (6049): 1602–1606. doi:10.1126/science.1210923. PMID 21921192. Bibcode: 2011Sci...333.1602D.
38. ↑ 38.0 38.1 38.2 38.3 Kuzuhara, M.; Tamura, M.; Ishii, M.; Kudo, T.; Nishiyama, S.; Kandori, R. (2011-04-01). "The Widest-Separation Substellar Companion Candidate to a Binary T Tauri Star". The Astronomical Journal 141 (4): 119. doi:10.1088/0004-6256/141/4/119. ISSN 0004-6256. Bibcode: 2011AJ....141..119K. https://iopscience.iop.org/article/10.1088/0004-6256/141/4/119.
39. ↑ Currie, Thayne; Daemgen, Sebastian; Debes, John; Lafreniere, David; Itoh, Yoichi; Jayawardhana, Ray; Ratzka, Thorsten; Correia, Serge (2014). "Direct Imaging and Spectroscopy of a Candidate Companion Below/Near the Deuterium-Burning Limit In The Young Binary Star System, ROXs 42B". The Astrophysical Journal Letters 780 (2): 30. doi:10.1088/2041-8205/780/2/L30. Bibcode: 2014ApJ...780L..30C.
40. ↑ Gaarn, Josefine; Burningham, Ben; Faherty, Jacqueline K; Visscher, Channon; Marley, Mark S; Gonzales, Eileen C; Calamari, Emily; Bardalez Gagliuffi, Daniella et al. (2023-03-31). "The puzzle of the formation of T8 dwarf Ross 458c" (in en). Monthly Notices of the Royal Astronomical Society 521 (4): 5761–5775. doi:10.1093/mnras/stad753. ISSN 0035-8711. Bibcode: 2023MNRAS.521.5761G. https://academic.oup.com/mnras/article/521/4/5761/7078574.
41. ↑ Kraus, Adam; J. Ireland, Michael; A. Cieza, Lucas; Hinkley, Sasha; J. Dupuy, Trent; P. Bowler, Brendan; C. Liu, Michael (2 January 2014). "Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B". The Astrophysical Journal 781 (1): 1311. doi:10.1088/0004-637X/781/1/20. Bibcode: 2014ApJ...781...20K.
42. ↑ Mora, Ariel; Wu, Ya-Lin; Bowler, Brendan P.; Sheehan, Patrick (2020-01-01). "Measuring the Mass of the Faint Companion to FW Tau with ALMA". Research Notes of the AAS 4 (1): 9. doi:10.3847/2515-5172/ab6852. ISSN 2515-5172. Bibcode: 2020RNAAS...4....9M.
43. ↑ 43.0 43.1 Gould, A. et al. (3 July 2014). "A terrestrial planet in a ~1-AU orbit around one member of a 15-AU binary". Science 345 (6192): 46–49. doi:10.1126/science.1251527. ISSN 0036-8075. PMID 24994642. Bibcode: 2014Sci...345...46G. "these projected separations are good proxies for the semi-major axis (afterupward adjustment by 3/2 to correct for projection effects)".
44. ↑ Horner, J.; Wittenmyer, R. A.; Hinse, T. C.; Marshall, J. P. (2014). "A dynamical investigation of the proposed BD +20 2457 system". Monthly Notices of the Royal Astronomical Society 439 (1): 1176. doi:10.1093/mnras/stu081. Bibcode: 2014MNRAS.439.1176H.
45. ↑ Bortle, Anna et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal 161 (5): 230. doi:10.3847/1538-3881/abec89. Bibcode: 2021AJ....161..230B.
46. ↑ Jones, M. I.; Jenkins, J. S. (2014). "No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044". Astronomy and Astrophysics 562: A129. doi:10.1051/0004-6361/201322132. Bibcode: 2014A&A...562A.129J.
47. ↑ "Notes for mu2 scorpii". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/mu2_sco_b--8201/. Retrieved 2022-05-06.
48. ↑ "Notes for planet M51-ULS-1b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/m51_uls_1_b--7496/. Retrieved 2021-07-18.
49. ↑ 49.0 49.1 "V921 Sco b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/v921_sco_b--7107/. Retrieved 2021-07-18.
50. ↑ "Notes for planet 2MASSS J1119-1137 B". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/2mass_j1119_1137_b--6572/. Retrieved 2017-08-29.
51. ↑ Lee, Byeong-Cheol; Do, Hee-Jin; Park, Myeong-Gu; Lim, Beomdu; Choi, Yeon-Ho; Koo, Jae-Rim; Bang, Tae-Yang; Oh, Hyeong-Ill et al. (2023-10-01). "Long-period radial velocity variations of nine M red giants - The detection of substellar companions around HD 6860 and HD 112300" (in en). Astronomy & Astrophysics 678: A106. doi:10.1051/0004-6361/202243725. ISSN 0004-6361. Bibcode: 2023A&A...678A.106L. https://www.aanda.org/articles/aa/abs/2023/10/aa43725-22/aa43725-22.html.
52. ↑ De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics 523: A18. doi:10.1051/0004-6361/200913771. Bibcode: 2010A&A...523A..18D.
53. ↑ Fedele (2005). "The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI". Astronomy & Astrophysics 431 (3): 1019–1026. doi:10.1051/0004-6361:20042013. Bibcode: 2005A&A...431.1019F.
54. ↑ 54.0 54.1 Kastner, J. H.; Buchanan, C. L.; Sargent, B.; Forrest, W. J. (2006). "SpitzerSpectroscopy of Dusty Disks around B\e] Hypergiants in the Large Magellanic Cloud". The Astrophysical Journal 638 (1): L29–L32. doi:10.1086/500804. Bibcode: 2006ApJ...638L..29K.
55. ↑ Linsky, Jeffrey L.; Wood, Brian E.; Brown, Alexander; Giampapa, Mark S.; Ambruster, Carol (December 1995). "Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10". The Astrophysical Journal 455: 670. doi:10.1086/176614. ISSN 0004-637X. Bibcode: 1995ApJ...455..670L.
56. ↑ "The Extrasolar Planet Encyclopaedia — 2M 0746+20 b". Extrasolar Planets Encyclopaedia. http://exoplanet.eu/catalog/2m_0746+20_b/. Retrieved 8 March 2014.
57. ↑ Suleymanova, S. A.; Rodin, A. E. (2014-11-01). "Detection of regular variations in the intensity and pulse time of arrival of the anomalous pulsar PSR B0943+10" (in en). Astronomy Reports 58 (11): 796–807. doi:10.1134/S1063772914110067. ISSN 1562-6881. Bibcode: 2014ARep...58..796S. https://doi.org/10.1134/S1063772914110067.
58. ↑ "The Extrasolar Planet Encyclopaedia — PSR B0943+10 c". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/psr_b0943_10_c--6642/. Retrieved 2023-01-18.
59. ↑ "The Extrasolar Planet Encyclopaedia — PSR B0943+10 b". Extrasolar Planets Encyclopaedia. https://exoplanet.eu/catalog/psr_b0943_10_b--6641/. Retrieved 2023-01-18.
60. ↑ Yue, Y. L.; Cui, X. H.; Xu, R. X. (2006-10-01). "Is PSR B0943+10 a low-mass quark star?". The Astrophysical Journal 649 (2): L95–L98. doi:10.1086/508421. ISSN 0004-637X. Bibcode: 2006ApJ...649L..95Y.
61. ↑ Lee, Byeong-Cheol; Do, Hee-Jin; Park, Myeong-Gu; Lim, Beomdu; Choi, Yeon-Ho; Koo, Jae-Rim; Bang, Tae-Yang; Oh, Hyeong-Ill et al. (2023-10-01). "Long-period radial velocity variations of nine M red giants. The detection of substellar companions around HD 6860 and HD 112300". Astronomy and Astrophysics 678: A106. doi:10.1051/0004-6361/202243725. ISSN 0004-6361. Bibcode: 2023A&A...678A.106L. https://ui.adsabs.harvard.edu/abs/2023A&A...678A.106L.
62. ↑ Lee, B. -C.; Han, I.; Park, M. -G.; Mkrtichian, D. E.; Hatzes, A. P.; Kim, K. -M. (2014-06-01). "Planetary companions in K giants β Cancri, μ Leonis, and β Ursae Minoris". Astronomy and Astrophysics 566: A67. doi:10.1051/0004-6361/201322608. ISSN 0004-6361. Bibcode: 2014A&A...566A..67L. https://ui.adsabs.harvard.edu/abs/2014A&A...566A..67L.
63. ↑ Agol, Eric; Dorn, Caroline; Grimm, Simon L.; Turbet, Martin; Ducrot, Elsa; Delrez, Laetitia; Gillon, Michaël; Demory, Brice-Olivier et al. (2021-02-01). "Refining the Transit-timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides". The Planetary Science Journal 2 (1): 1. doi:10.3847/PSJ/abd022. ISSN 2632-3338. Bibcode: 2021PSJ.....2....1A.
64. ↑ Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; De Lee, Nathan; Collins, Kevin; Latham, David W. et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256. Bibcode: 2019AJ....158..138S.
65. ↑ Pulley, D.; Sharp, I. D.; Mallett, J.; von Harrach, S. (August 2022). "Eclipse timing variations in post-common envelope binaries: Are they a reliable indicator of circumbinary companions?". Monthly Notices of the Royal Astronomical Society 514 (4): 5725–5738. doi:10.1093/mnras/stac1676. Bibcode: 2022MNRAS.514.5725P.
66. ↑ Janson, Markus; Gratton, Raffaele; Rodet, Laetitia; Vigan, Arthur; Bonnefoy, Mickaël; Delorme, Philippe; Mamajek, Eric E.; Reffert, Sabine et al. (2021). "A wide-orbit giant planet in the high-mass b Centauri binary system". Nature 600 (7888): 231–234. doi:10.1038/s41586-021-04124-8. PMID 34880428. Bibcode: 2021Natur.600..231J.
67. ↑ Tuomi, Mikko (6 April 2012). "Evidence for 9 planets in the 10180 system". Astronomy & Astrophysics 543: A52. doi:10.1051/0004-6361/201118518. Bibcode: 2012A&A...543A..52T.
68. ↑ "NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star". Exoplanet Exploration: Planets Beyond our Solar System. nasa.gov. 21 February 2017. https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/.
69. ↑ Kiefer, F. et al. (January 2021). "Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets". Astronomy & Astrophysics 645. doi:10.1051/0004-6361/202039168. Bibcode: 2021A&A...645A...7K.

1. ↑ Based on the estimated temperature and luminosity.

## External links

* WiredScience, Top 5 Most Extreme Exoplanets, Clara Moskowitz, 21 January 2009

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