List of nearest exoplanets

Last updated

Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023. Epsilon Indi Ab (MIRI Image).png
Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023.
Distribution of nearest known exoplanets as of March 2018 Distances to nearest confirmed exoplanets in light years.png
Distribution of nearest known exoplanets as of March 2018

There are 7,408 known exoplanets, or planets outside the Solar System that orbit a star, as of January 26, 2024; only a small fraction of these are located in the vicinity of the Solar System. [2] Within 10 parsecs (32.6 light-years ), there are 106 exoplanets listed as confirmed by the NASA Exoplanet Archive. [note 1] [3] Among the over 500 known stars and brown dwarfs within 10 parsecs, [4] [note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye, [note 3] [6] eight of which have planetary systems.

Contents

The first report of an exoplanet within this range was in 1998 for a planet orbiting around Gliese 876 (15.3 light-years (ly) away), and the latest as of 2024 is one around Struve 2398 A (11.5 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is Proxima Centauri 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was Proxima Centauri b, in 2016. HD 219134 (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.

Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around YZ Ceti, Gliese 367, Proxima Centauri, and Barnard's Star which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and GJ 1002 b (15.8 ly) considered among the most likely candidates. [7] The International Astronomical Union has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the NameExoWorlds project. Planets named in the 2015 event include the planets around Epsilon Eridani (10.5 ly) and Fomalhaut, [note 4] [10] while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367. [11]

Exoplanets within 10 parsecs

Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
#Confirmed multiplanetary systems
↑Exoplanets believed to be potentially habitable [7]
Confirmed exoplanets [3]
Host star system Companion exoplanet (in order from star)Notes and additional planetary observations
Name Distance
(ly)
Apparent
magnitude
(V)		 Mass
(M☉)
Label
[note 5] 		Mass
(ME) [note 6]
Radius
(R🜨)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(°)
Discovery
method 		Discovery year
Sun °0.000016−26.71 Mercury 0.0550.38290.38788.00.205————
Earth 111365.30.0167———
Jupiter 317.810.9735.204,3330.0488———
Proxima Centauri #4.246511.130.123 d ≥0.26—0.02895.1220.04— RV 2022 [13] [14] one disputed candidate (c) [15] [16] [17] [18]
b ↑≥1.07—0.048611.190.02— RV 2016
Barnard's Star 5.96299.510.162 b ≥0.37—0.02293.1530.16— RV 2024 [19] [20]
Lalande 21185 #8.3047.520.46 b ≥2.69—0.078812.940.06— RV 20191 candidate [21]
c ≥13.6—2.942,9460.13— RV 2021
Epsilon Eridani 10.4893.730.781 Ægir 242—3.532,6890.26166.5 RV 20001 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc [22] [23]
Lacaille 9352 #10.7247.340.489 b ≥4.2—0.0689.2620.03— RV 20191 candidate [24] [25]
c ≥7.6—0.12021.790.03— RV 2019
Ross 128 11.00711.10.168 b ↑≥1.40—0.04969.8660.12— RV 2017 [26]
Gliese 725 A11.4918.940.330 b ≥2.78—0.06811.22010.0— RV 2024 [27]
Groombridge 34 A#11.6198.10.38 b ≥3.03—0.07211.440.09~54? RV 2014 [28] [29]
c ≥36—5.47,6000.27~54? RV 2018
Epsilon Indi A11.8674.830.762 b 2005—28.463,4000.40103.7 RV 2018nearest exoplanet directly imaged [30] [31]
Tau Ceti #11.9123.500.78 g ≥1.75—0.13320.00.06~35? RV 20174 disputed candidates
[32] [33] [7] [34] [35] [36]
h ≥1.8—0.24349.40.23~35? RV 2017
e ≥3.9—0.5381630.18~35? RV 2017
f ≥3.9—1.336400.16~35? RV 2017
GJ 1061 #11.9847.520.113 b ≥1.37—0.0213.204<0.31— RV 2019two solutions for d's orbit [37]
c ↑≥1.74—0.0356.689<0.29— RV 2019
d ↑≥1.64—0.05413.03<0.53— RV 2019
YZ Ceti #12.12212.10.130 b ≥0.70—0.01632.0210.06— RV 2017 [38]
c ≥1.14—0.02163.0600.0— RV 2017
d ≥1.09—0.02854.6560.07— RV 2017
Luyten's Star #12.34811.940.29 c ≥1.18—0.03654.7230.10— RV 2017 [39] [24]
b ↑≥2.89—0.091118.650.17— RV 2017
d ≥10.8—0.7124140.17— RV 2019
e ≥9.3—0.8495420.03— RV 2019
Teegarden's Star #12.49715.400.08 b ↑≥1.16—0.02594.9060.03— RV 2019 [40] [41]
c ↑≥1.05—0.045511.420.04— RV 2019
d ≥0.82—0.079126.130.07— RV 2024
Wolf 1061 #14.05010.10.25 b ≥1.91—0.03754.8870.15— RV 2015 [39]
c ↑≥3.41—0.089017.870.11— RV 2015
d ≥7.7—0.4702170.55— RV 2015
TZ Arietis 14.57812.300.14 b ≥67—0.887710.46— RV 20192 refuted candidates [24] [42] [43]
Gliese 687 #14.8399.150.41 b ≥17.2—0.16338.140.17— RV 2014 [24] [42]
c ≥16.0—1.1657280.40— RV 2019
Gliese 674 14.8499.380.35 b ≥11.1—0.0394.6940.20— RV 2007 [44]
Gliese 876 #15.23810.20.33 d 6.68—0.02101.9380.0456.7 RV 2005 [45]
c 235—0.130930.100.2656.7 RV 2000
b 749—0.209861.100.0356.7 RV 1998
e 16—0.3355123.60.0556.7 RV 2010
GJ 1002 #15.80613.840.12 b ↑≥1.08—0.045710.35—— RV 2022 [46]
c ↑≥1.36—0.073821.2—— RV 2022
Gliese 832 16.2008.670.45 b 315—3.73,8530.0551 or 134 RV 20081 refuted candidate [47] [48]
GJ 3323 #17.53112.20.164 b ≥2.0—0.03285.360.2— RV 2017 [39]
c ≥2.3—0.12640.50.2— RV 2017
Gliese 251 18.2159.650.372 b ≥4.0—0.081814.20.10— RV 2020 [49]
Gliese 229 A#18.7918.140.58 c ↑≥7.3—0.3391220.19— RV 2020Ab not confirmed until 2020 [50]
b ≥8.5—0.8985260.10— RV 2014
Gliese 752 A19.2929.130.46 b ≥12.2—0.3431060.10— RV 2018 [51] [52]
82 G. Eridani #19.7044.260.79 b ≥2.15—0.12618.30.06— RV 2011 [53]
c ≥2.98—0.36389.70.08— RV 2011
d ↑≥5.82—1.3546480.45— RV 2023
Gliese 555 20.39511.320.29 b ≥5.5—0.14236.10.08— RV 20231 candidate [54]
EQ Pegasi A20.40010.380.436 b 718—0.6432840.3569.2 Astrometry 2022 [55]
Gliese 581 #20.54910.50.295 e 2.5—0.02803.150.0147 RV 20093 refuted candidates and a disc [56]
b 20.5—0.03995.370.0347 RV 2005
c 6.8—0.071812.90.0347 RV 2007
Gliese 338 B20.6587.00.64 b ≥10.3—0.14124.50.11— RV 2020 [57]
Gliese 625 21.13110.20.30 b ≥2.8—0.078414.6~0.1— RV 2017 [58]
HD 219134 #21.3365.570.78 b 4.71.600.03883.09~085.05 RV 2015 [59] [60] [61]
c 4.41.510.0656.770.06287.28 RV 2015
d ≥16—0.23746.90.138~87? RV 2015
f ≥7.3—0.14622.70.148~87? RV 2015
g ≥11—0.37594.20~87? RV 2015
h (e)≥108—3.112,2470.06~87? RV 2015
LTT 1445 A#22.38710.530.26 c 1.541.150.02663.12<0.2287.43 Transit 20211 candidate [62] [63] [64]
b 2.871.300.03815.36<0.1189.68 Transit 2019
Gliese 393 22.9538.650.41 b ≥1.71—0.05407.030.00— RV 2019 [24] [65]
Gliese 667 C#23.62310.20.33 b ≥5.4—0.0497.200.13~52? RV 20095 dubious candidates
[66] [7] [67] [68] [24]
c ↑≥3.9—0.125128.20.03~52? RV 2011
Gliese 514 24.8789.030.53 b ≥5.2—0.4211400.45— RV 2022 [69]
GJ 1151 26.23114.010.164 c ≥10.6—0.571390—— RV 20231 refuted candidate [70] [71] [72] [73]
Gliese 486 26.35111.3950.32 Su 2.81.310.01731.47<0.0588.4 Transit 2021 [74]
Gliese 686 26.6139.580.42 b ≥7.1—0.09715.50.04— RV 2019 [75] [24]
GJ 1289 27.27512.67 [76] 0.21 b ≥6.3—0.271120— RV 2024 [77]
61 Virginis #27.8364.740.95 b ≥6.1—0.054.220.05~77? RV 2009a debris disc [78]
c ≥17.9—0.2238.10.06~77? RV 2009
d ≥10.5—0.471230.12~77? RV 2009
CD Ceti 28.05214.0010.161 b ≥3.95—0.01852.290— RV 2020 [79]
Gliese 785 #28.7396.130.78 b ≥17—0.32750.13— RV 2010 [80]
c ≥24—1.18530~0.3— RV 2011
Gliese 849 #28.75010.40.49 b ≥270—2.261,9100.05— RV 2006 [81] [24]
c ≥300—4.825,5200.087— RV 2006
Gliese 433 #29.6059.790.48 b ≥6.0—0.0627.370.04— RV 2009 [82] [24] [50]
d ≥5.2—0.17836.10.07— RV 2020
c ≥32—4.825,0900.12— RV 2012
HD 102365 A30.3964.890.85 b ≥16—0.461220.34— RV 2010 [83]
Gliese 367 #30.7199.980.45 Tahay 0.630.700.00710.3220.0679.89 Transit 2021 [84] [85]
c ≥4.1—0.07711.50.09~80? RV 2023
d ≥6.0—0.15934.40.14~80? RV 2023
Gliese 357 #30.77610.90.34 b 6.11.170.0353.930.0288.92 Transit 2019 [86] [24]
c ≥3.6—0.0619.130.04~89? RV 2019
d ↑≥7.7—0.20455.70.03~89? RV 2019
Gliese 176 30.93710.10.45 b ≥8.0—0.0668.770.08— RV 20071 disputed candidate [87] [88] [24]
GJ 3512 #30.97613.110.123 b ≥147—0.3382040.44— RV 2019 [89]
c ≥54—>1.2>1390—— RV 2019
Wolf 1069 31.22913.990.167 b ↑≥1.26—0.067215.6—— RV 2023 [90]
AU Microscopii #31.6838.630.50 b 174.380.06458.4630.1089.03 Transit 20202 candidates [91] [92] [93] [94]
c <283.510.110118.86088.62 Transit 2020
Gliese 436 31.88210.670.41 Awohali 21.44.330.02802.640.1585.8 RV 2004 [95] [96]
Gliese 49 32.1588.90.57 b ≥16.4—0.10617.30.03— RV 2019 [97]
GJ 3988 32.31613.60.184 b ≥3.7—0.04056.9440— RV 2023 [98]
HD 260655 #32.6089.770.439 b 2.141.2400.02932.7800.03987.35 Transit 2022 [99]
c 3.091.5330.04755.7060.03887.79 Transit 2022

Excluded objects

Unlike for bodies within the Solar System, there is no clearly established method for officially recognizing an exoplanet. According to the International Astronomical Union, an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery. [100] There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include Wolf 359 (7.9 ly, in 2019), [24] LHS 288 (15.8 ly, in 2007), [101] and Gliese 682 (16.3 ly, in 2014). [50] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly), [102] Barnard's Star (5.96 ly), [103] [104] Kapteyn's Star (12.8 ly), [105] Van Maanen 2 (14.1 ly), [106] Groombridge 1618 (15.9 ly), [107] AD Leonis (16.2 ly), [108] 40 Eridani A (16.3 ly), [109] [110] VB 10 (19.3 ly), [111] and Fomalhaut (25.1 ly). [112]

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed. [113] Another candidate planet, Candidate 1, was directly imaged around Alpha Centauri A, though it may also be a clump of asteroids or an artifact of the discovery mechanism. [114] Candidate planets around Luyten 726-8 (8.77 ly) [115] and GJ 3378 (25.2 ly) were reported in 2024. [77]

The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of deuterium. Some studies have calculated this to be somewhere around 13 times the mass of Jupiter, and therefore objects more massive than this are usually classified as brown dwarfs. [116] Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: SCR 1845-6357 B (13.1 ly), [117] SDSS J1416+1348 B (30.3 ly), [118] and WISE 1217+1626 B (30 ly). [119]

Excluded from the current list are known examples of potential free-floating sub-brown dwarfs, or "rogue planets", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: WISE 0855−0714 (7.4 ly), [120] UGPS 0722-05, (13.4 ly) [121] WISE 1541−2250 (18.6 ly), [122] and SIMP J01365663+0933473 (20.0 ly). [123]

See also

Notes

  1. ↑ Listed values are primarily taken from NASA Exoplanet Archive , [3] but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:
    "Exoplanet Catalog". Extrasolar Planets Encyclopaedia . 1995. Full table.
    "Exoplanets Data Explorer". Exoplanet Orbit Database. California Planet Survey. Click the "+" button to visualize additional parameters.
    "Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. Archived from the original on 2017-09-02. Retrieved 2015-02-14.
  2. ↑ For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly). [4]
  3. ↑ According to the Bortle scale, an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an apparent magnitude smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort). [5]
  4. ↑ The star Epsilon Eridani was named Ran (after Rán, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Ægir, Rán's husband), [8] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god” [9] ). [10]
  5. ↑ Exoplanet naming convention assigns uncapitalized letters starting from b to each planet based on chronological order of their initial report, and in increasing order of distance from the parent star for planets reported at the same time. Omitted letters signify planets that have yet to be confirmed, or planets that have been retracted altogether.
  6. ↑ Most reported exoplanet masses have very large error margins (typically, between 10% and 30%). The mass of an exoplanet has generally been inferred from measurements on changes in the radial velocity of the host star, but this kind of measurement only allows for an estimate on the exoplanet's orbital parameters, but not on their orbital inclination (i). As such, most exoplanets only have an estimated minimum mass (Mreal*sin(i)), where their true masses are statistically expected to come close to this minimum, with only about 13% chance for the mass of an exoplanet to be more than double its minimum mass. [12]

Related Research Articles

<span class="mw-page-title-main">Gliese 436</span> Star in the constellation Leo

Gliese 436 is a red dwarf located 31.9 light-years away in the zodiac constellation of Leo. It has an apparent visual magnitude of 10.67, which is much too faint to be seen with the naked eye. However, it can be viewed with even a modest telescope of 2.4 in (6 cm) aperture. In 2004, the existence of an extrasolar planet, Gliese 436 b, was verified as orbiting the star. This planet was later discovered to transit its host star.

TZ Arietis is a red dwarf in the northern constellation of Aries. With a normal apparent visual magnitude of 12.3, it is too faint to be seen by the naked eye, although it lies relatively close at a distance of 14.6 light-years. It is a flare star, which means it can suddenly increase in brightness for short periods of time.

Gliese 674(GJ 674) is a small red dwarf star with an exoplanetary companion in the southern constellation of Ara. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.38 and an absolute magnitude of 11.09. The system is located at a distance of 14.85 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −2.9 km/s. It is a candidate member of the 200 million year old Castor stream of co-moving stars.

Gliese 849, or GJ 849, is a small, solitary star in the equatorial constellation of Aquarius. It has a reddish hue and is invisible to the naked eye with an apparent visual magnitude of 10.41. The distance to this star is 28.8 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.3 km/s. It has a pair of confirmed gas giant companions.

GJ 3323 is a nearby single star located in the equatorial constellation Eridanus, about 0.4° to the northwest of the naked eye star Psi Eridani. It is invisible to the naked eye with an apparent visual magnitude 12.20. Parallax measurements give a distance estimate of 17.5 light-years from the Sun. It is drifting further away with a radial velocity of +42.3 km/s. Roughly 104,000 years ago, the star is believed to have come to within 7.34 ± 0.16 light-years of the Solar System.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located 18.2 light-years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

GJ 625 is a small red dwarf star with an exoplanetary companion in the northern constellation of Draco. The system is located at a distance of 21.1 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 10.13 and an absolute magnitude of 11.06.

Gliese 880 is a red dwarf star 22.4 light-years away in the northern constellation of Pegasus. No stellar companions to Gliese 880 have been discovered as of 2020.

Gliese 393, or GJ 393, is a single star with an orbiting exoplanet companion in the equatorial constellation of Sextans, positioned about 1.5° to the NNW of Beta Sextantis. At an apparent visual magnitude of 9.65, it is much too faint to be seen with the unaided eye. This star is located at a distance of 22.9 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8.3 km/s. It has a large proper motion, traversing the celestial sphere at the rate of 0.950″ per year. The net velocity of this star relative to the Sun is 32.9 km/s. It shares a similar space motion as members of the AB Doradus moving group, but is considered a random interloper.

GJ 3512 is a nearby star in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye but can be observed using a telescope, having an apparent visual magnitude of +15.05. The star is located at a distance of 31 light-years from the Sun based on parallax. It has a high proper motion, traversing the celestial sphere at the rate of 1.311″ yr−1. The measurement of the star's radial velocity is poorly constrained, but it appears to be drifting further away at a rate of ~8 km/s.

<span class="mw-page-title-main">Gliese 15 Ac</span> Subjovian planet orbiting Gliese 15 A

Gliese 15 Ac is an exoplanet orbiting the nearby red dwarf star Gliese 15 A, which is part of a binary star system located about 11.6 light-years from the Sun. The planet was first proposed in October 2017 using radial velocity data from the CARMENES spectrograph, combined with measurements from the HARPS and HIRES spectrographs, and its existence was confirmed in April 2018 using HARPS-N data. It has a minimum mass 36 times that of Earth and orbits at around 5.4 astronomical units with a period of 7,600 days, an orbit which may have been sculpted by interaction with the companion star, Gliese 15 B. As of 2020, Gliese 15 Ac is the longest-period sub-Jovian planet discovered by radial velocity.

References

  1. ↑ "NASA's Webb Images Cold Exoplanet 12 Light-Years Away". nasa.gov. NASA Webb Mission Team. Retrieved Jul 24, 2024.
  2. ↑ Schneider, Jean (1995). "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia . Archived from the original on 2012-02-12. Retrieved 2018-03-20.
  3. 1 2 3 "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18.
  4. 1 2 Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics . 650: A201. arXiv: 2104.14972 . Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID   233476431. Data available at https://gruze.org/10pc/
  5. ↑ Bortle, John E. (2001). "Light Pollution And Astronomy: The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2014-05-20.
  6. ↑ Powell, Richard (2006). "Stars within 50 light years". An Atlas of the Universe. Archived from the original on 2014-06-27. Retrieved 2014-05-17.
  7. 1 2 3 4 "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico in Arecibo. 2015-09-01. Archived from the original on 2016-01-09. Retrieved 2015-09-17.
  8. ↑ "epsilon Eridani". NameExoWorlds. International Astronomical Union. Archived from the original on 2018-02-15. Retrieved 2018-05-14.
  9. ↑ "Fomalhaut (alpha Piscis Austrini)". Nameexoworlds. International Astronomical Union. Archived from the original on 2017-04-30. Retrieved 2018-05-14.
  10. 1 2 "Final Results of NameExoWorlds Public Vote Released" (Press release). International Astronomical Union. 2015-12-15. Archived from the original on 2018-05-15. Retrieved 2018-03-17.
  11. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
  12. ↑ Cumming, Andrew; Butler, R. Paul; Marcy, Geoffrey W.; et al. (2008). "The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets". Publications of the Astronomical Society of the Pacific. 120 (867): 531–554. arXiv: 0803.3357 . Bibcode:2008PASP..120..531C. doi:10.1086/588487. S2CID   10979195.
  13. ↑ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv: 1609.03449 . Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID   27558064. S2CID   4451513.
  14. ↑ Faria, J. P.; Suárez Mascareño, A.; et al. (January 4, 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. European Southern Observatory: 17. arXiv: 2202.05188 . Bibcode:2022A&A...658A.115F. doi: 10.1051/0004-6361/202142337 .
  15. ↑ Damasso, Mario; Del Sordo, Fabio; Anglada-Escudé, Guillem; et al. (15 January 2020). "A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU". Science Advances . 6 (3). eaax7467. Bibcode:2020SciA....6.7467D. doi:10.1126/sciadv.aax7467. PMC   6962037 . PMID   31998838.
  16. ↑ Kervella, Pierre; Arenou, Frédéric; Schneider, Jean (2020). "Orbital inclination and mass of the exoplanet candidate Proxima c". Astronomy & Astrophysics. 635: L14. arXiv: 2003.13106 . Bibcode:2020A&A...635L..14K. doi:10.1051/0004-6361/202037551. ISSN   0004-6361. S2CID   214713486.
  17. ↑ Benedict, G. Fritz; McArthur, Barbara E. (16 June 2020). "A Moving Target—Revising the Mass of Proxima Centauri c". Research Notes of the AAS . 4 (6): 86. Bibcode:2020RNAAS...4...86B. doi: 10.3847/2515-5172/ab9ca9 . S2CID   225798015.
  18. ↑ Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; Donati, Jean-Françcois; Moutou, Claire; Delfosse, Xavier; Fouqué, Pascal; Martioli, Eder; Bouchy, François; Parsons, Jasmine; Carmona, Andres; Dumusque, Xavier; Astudillo-Defru, Nicola; Bonfils, Xavier; Mignon, Lucille (2022). "Line-by-line Velocity Measurements: An Outlier-resistant Method for Precision Velocimetry". The Astronomical Journal. 164 (3): 84. arXiv: 2207.13524 . Bibcode:2022AJ....164...84A. doi: 10.3847/1538-3881/ac7ce6 . S2CID   251105120.
  19. ↑ ESO. "Scientists discover planet orbiting closest single star to our sun". phys.org. Retrieved 2024-10-05.
  20. ↑ Hernández, J. I. González; Mascareño, A. Suárez; Silva, A. M.; Stefanov, A. K.; Faria, J. P.; Tabernero, H. M.; Sozzetti, A.; Rebolo, R.; Pepe, F.; Santos, N. C.; Cristiani, S.; Lovis, C.; Dumusque, X.; Figueira, P.; Lillo-Box, J. (2024-10-01). "A sub-Earth-mass planet orbiting Barnard's star". Astronomy & Astrophysics. 690: A79. arXiv: 2410.00569 . doi:10.1051/0004-6361/202451311. ISSN   0004-6361.
  21. ↑ Hurt, Spencer A.; Fulton, Benjamin; Isaacson, Howard; Rosenthal, Lee J.; Howard, Andrew W.; Weiss, Lauren M.; Petigura, Erik A. (2021), "Confirmation of the Long-Period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate", The Astronomical Journal, 163 (5): 218, arXiv: 2107.09087 , Bibcode:2022AJ....163..218H, doi: 10.3847/1538-3881/ac5c47 , S2CID   236134034
  22. ↑ Booth, Mark; Pearce, Tim D; Krivov, Alexander V; Wyatt, Mark C; Dent, William R F; Hales, Antonio S; Lestrade, Jean-François; Cruz-Sáenz de Miera, Fernando; Faramaz, Virginie C; Löhne, Torsten; Chavez-Dagostino, Miguel (2023-03-30). "The clumpy structure of ϵ Eridani's debris disc revisited by ALMA". Monthly Notices of the Royal Astronomical Society. 521 (4). Oxford University Press (OUP): 6180–6194. arXiv: 2303.13584 . Bibcode:2023MNRAS.521.6180B. doi: 10.1093/mnras/stad938 . ISSN   0035-8711.
  23. ↑ Feng, Fabo; Butler, R. Paul; et al. (July 2023). "Revised orbits of the two nearest Jupiters". Monthly Notices of the Royal Astronomical Society . 525 (1): 607–619. arXiv: 2307.13622 . Bibcode:2023MNRAS.525..607F. doi: 10.1093/mnras/stad2297 .
  24. 1 2 3 4 5 6 7 8 9 10 11 12 Barnes, J. R.; Kiraga, M.; Diaz, M.; Berdiñas, Z.; Jenkins, J. S.; Keiser, S.; Thompson, I.; Crane, J. D.; Shectman, S. A.; Teske, J. K.; Holden, B.; Laughlin, G.; Burt, J.; Vogt, S. S.; Arriagada, P.; Butler, R. P.; Anglada-Escudé, G.; Jones, H. R. A.; Tuomi, M. (11 June 2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv: 1906.04644 [astro-ph.EP].
  25. ↑ Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; Luque, R.; et al. (2020), "A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887", Science, 368 (6498): 1477–1481, arXiv: 2006.16372 , Bibcode:2020Sci...368.1477J, doi:10.1126/science.aaz0795, PMID   32587019, S2CID   220075207
  26. ↑ Bonfils, Xavier (2017). "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs". Astronomy and Astrophysics . 613: A25. arXiv: 1711.06177 . Bibcode:2018A&A...613A..25B. doi:10.1051/0004-6361/201731973. S2CID   37148632.
  27. ↑ Cortes-Zuleta, P.; Boisse, I.; Ould-Elhkim, M.; Wilson, T. G.; Larue, P.; Carmona, A.; Delfosse, X.; Donati, J.-F.; Forveille, T. (2024-11-14), Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc, doi:10.48550/arXiv.2411.09506 , retrieved 2024-11-27
  28. ↑ Howard, Andrew W.; et al. (October 2014). "The NASA-UC-UH ETA-Earth Program. IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth". The Astrophysical Journal. 794 (1): 9. arXiv: 1408.5645 . Bibcode:2014ApJ...794...51H. doi:10.1088/0004-637X/794/1/51. S2CID   17361592. 51.
  29. ↑ Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv: 1804.03476 . Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID   54990041.
  30. ↑ Feng, Fabo; Anglada-Escudé, Guillem; Tuomi, Mikko; Jones, Hugh R. A.; Chanamé, Julio; Butler, Paul R.; Janson, Markus (14 October 2019). "Detection of the nearest Jupiter analog in radial velocity and astrometry data". Monthly Notices of the Royal Astronomical Society. 490 (4): 5002–5016. arXiv: 1910.06804 . Bibcode:2019MNRAS.490.5002F. doi: 10.1093/mnras/stz2912 . S2CID   204575783.
  31. ↑ Matthews, E. C.; Carter, A. L.; et al. (July 2024). "A temperate super-Jupiter imaged with JWST in the mid-infrared". Nature . 633 (8031): 789–792. Bibcode:2024Natur.633..789M. doi: 10.1038/s41586-024-07837-8 . PMC   11424479 . PMID   39048015.
  32. ↑ "tau Cet". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  33. ↑ "tau Ceti". Open Exoplanet Catalogue. Archived from the original on 2014-03-14. Retrieved 2014-05-17.
  34. ↑ "tau Cet b". Extrasolar Planets Encyclopaedia . Archived from the original on 2017-11-07. Retrieved 2018-03-22.
  35. ↑ "tau Cet c". Extrasolar Planets Encyclopaedia . Archived from the original on 2017-12-01. Retrieved 2018-03-22.
  36. ↑ "tau Cet d". Extrasolar Planets Encyclopaedia . Archived from the original on 2017-12-01. Retrieved 2018-03-22.
  37. ↑ Dreizler, S.; Jeffers, S. V.; Rodríguez, E.; Zechmeister, M.; Barnes, J.R.; Haswell, C.A.; Coleman, G. A. L.; Lalitha, S.; Hidalgo Soto, D.; Strachan, J.B.P.; Hambsch, F-J.; López-González, M. J.; Morales, N.; Rodríguez López, C.; Berdiñas, Z. M.; Ribas, I.; Pallé, E.; Reiners, Ansgar; Anglada-Escudé, G. (2019-08-13). "Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061". Monthly Notices of the Royal Astronomical Society . 493 (1): 536. arXiv: 1908.04717 . Bibcode:2020MNRAS.493..536D. doi: 10.1093/mnras/staa248 . S2CID   199551874.
  38. ↑ Stock, S.; et al. (2020). "The CARMENES search for exoplanets around M dwarfs". Astronomy & Astrophysics. 636: A119. arXiv: 2002.01772 . Bibcode:2020A&A...636A.119S. doi:10.1051/0004-6361/201936732. S2CID   211032169.
  39. 1 2 3 Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier; et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics. 602. A88. arXiv: 1703.05386 . Bibcode:2017A&A...602A..88A. doi:10.1051/0004-6361/201630153. S2CID   119418595.
  40. ↑ Caballero, J. A.; Reiners, Ansgar; Ribas, I.; Dreizler, S.; Zechmeister, M.; et al. (12 June 2019). "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF). Astronomy & Astrophysics. 627: A49. arXiv: 1906.07196 . Bibcode:2019A&A...627A..49Z. doi:10.1051/0004-6361/201935460. ISSN   0004-6361. S2CID   189999121.
  41. ↑ Dreizler, S.; Luque, R.; et al. (April 2024). "Teegarden's Star revisited: A nearby planetary system with at least three planets". Astronomy & Astrophysics . 684: A117. arXiv: 2402.00923 . Bibcode:2024A&A...684A.117D. doi:10.1051/0004-6361/202348033.
  42. 1 2 Feng, Fabo; et al. (October 2020). "Search for Nearby Earth Analogs. III. Detection of 10 New Planets, 3 Planet Candidates, and Confirmation of 3 Planets around 11 Nearby M Dwarfs". The Astrophysical Journal Supplement Series . 250 (2): 29. arXiv: 2008.07998 . Bibcode:2020ApJS..250...29F. doi: 10.3847/1538-4365/abb139 . S2CID   221150644.
  43. ↑ Quirrenbach, A.; Passegger, V. M.; Trifonov, T.; Amado, P. J.; Caballero, J. A.; Reiners, A.; Ribas, I.; Aceituno, J.; Béjar, V. J. S.; Chaturvedi, P.; González-Cuesta, L.; Henning, T.; Herrero, E.; Kaminski, A.; Kürster, M.; Lalitha, S.; Lodieu, N.; López-González, M. J.; Montes, D.; Pallé, E.; Perger, M.; Pollacco, D.; Reffert, S.; Rodríguez, E.; López, C. Rodríguez; Shan, Y.; Tal-Or, L.; Osorio, M. R. Zapatero; Zechmeister, M. (2022). "The CARMENES search for exoplanets around M dwarfs". Astronomy & Astrophysics. 663: A48. arXiv: 2203.16504 . Bibcode:2022A&A...663A..48Q. doi:10.1051/0004-6361/202142915. S2CID   247835988.
  44. ↑ Bonfils, X.; et al. (2007). "The HARPS search for southern extra-solar planets. X. A m sin i = 11 M🜨 planet around the nearby spotted M dwarf GJ 674". Astronomy and Astrophysics. 474 (1): 293–299. arXiv: 0704.0270 . Bibcode:2007A&A...474..293B. doi:10.1051/0004-6361:20077068. S2CID   119671420.
  45. ↑ Moutou, C.; Delfosse, X.; et al. (July 2023). "Characterizing planetary systems with SPIRou: M-dwarf planet-search survey and the multiplanet systems GJ 876 and GJ 1148". Astronomy & Astrophysics . 678: A207. arXiv: 2307.11569 . Bibcode:2023A&A...678A.207M. doi:10.1051/0004-6361/202346813.
  46. ↑ Suárez Mascareño, A.; González-Alvarez, E.; et al. (December 2022). "Two temperate Earth-mass planets orbiting the nearby star GJ 1002". Astronomy & Astrophysics . 670: A5. arXiv: 2212.07332 . Bibcode:2023A&A...670A...5S. doi:10.1051/0004-6361/202244991. S2CID   254353639.
  47. ↑ Gorrini, P.; Astudillo-Defru, N.; Dreizler, S.; Damasso, M.; Díaz, R. F.; Bonfils, X.; Jeffers, S. V.; Barnes, J. R.; Del Sordo, F.; Almenara, J. -M.; Artigau, E.; Bouchy, F.; Charbonneau, D.; Delfosse, X.; Doyon, R.; Figueira, P.; Forveille, T.; Haswell, C. A.; López-González, M. J.; Melo, C.; Mennickent, R. E.; Gaisné, G.; Morales, N.; Murgas, F.; Pepe, F.; Rodríguez, E.; Santos, N. C.; Tal-Or, L.; Tsapras, Y.; Udry, S. (2022). "Detailed stellar activity analysis and modelling of GJ 832". Astronomy & Astrophysics. 664: A64. arXiv: 2206.07552 . Bibcode:2022A&A...664A..64G. doi:10.1051/0004-6361/202243063. S2CID   249674385.
  48. ↑ Philipot, F.; Lagrange, A.-M.; et al. (August 2023). "Multi techniques approach to identify and/or constrain radial velocity sub-stellar companions". Astronomy & Astrophysics . 678. arXiv: 2308.05417 . Bibcode:2023A&A...678A.107P. doi:10.1051/0004-6361/202346612.
  49. ↑ Stock, S.; et al. (2020), "The CARMENES search for exoplanets around M dwarfs Three temperate-to-warm super-Earths", Astronomy & Astrophysics, A112: 643, arXiv: 2010.00474 , Bibcode:2020A&A...643A.112S, doi:10.1051/0004-6361/202038820, S2CID   222090233
  50. 1 2 3 Feng, Fabo; Butler, R. Paul; Shectman, Stephen A.; Crane, Jeffrey D.; Vogt, Steve; Chambers, John; Jones, Hugh R. A.; Wang, Sharon Xuesong; Teske, Johanna K.; Burt, Jenn; Díaz, Matías R.; Thompson, Ian B. (8 January 2020). "Search for Nearby Earth Analogs. II. Detection of Five New Planets, Eight Planet Candidates, and Confirmation of Three Planets around Nine Nearby M Dwarfs". The Astrophysical Journal Supplement Series. 246 (1): 11. arXiv: 2001.02577 . Bibcode:2020ApJS..246...11F. doi: 10.3847/1538-4365/ab5e7c . S2CID   210064560.
  51. ↑ Kaminski, Adrian; Trifonov, Trifon; Caballero, José A.; Quirrenbach, Andreas; Ribas, Ignasi; Reiners, Ansgar; Amado, Pedro J.; Zechmeister, Mathias; Dreizler, Stefan; Perger, Manuel; Tal-Or, Lev; Bonfils, Xavier; Mayor, Michel; Astudillo-Defru, Nicola; Bauer, Florian F.; Béjar, Victor J. S.; Cifuentes, Carlos; Colomé, Josep; Cortés-Contreras, Miriam; Delfosse, Xavier; Díez-Alonso, Enrique; Forveille, Thierry; Guenther, Eike W.; Hatzes, Artie P.; Henning, Thomas K.; Jeffers, Sandra V.; Kürster, Martin; Lafarga, Marina; Luque, Rafael; Mandel, Holger; Montes, David; Morales, Juan Carlos; Passegger, Vera Maria; Pedraz, Sandos; Reffert, Sabine; Sadegi, Sepideh; Schweitzer, Andreas; Seifert, Walter; Stahl, Otmar; Udry, Stéphane (3 August 2018). "The CARMENES search for exoplanets around M dwarfs. A Neptune-mass planet traversing the habitable zone around HD 180617". Astronomy & Astrophysics. 618: A115. arXiv: 1808.01183 . Bibcode:2018A&A...618A.115K. doi:10.1051/0004-6361/201833354. S2CID   118980171.
  52. ↑ Burt, Jennifer; Feng, Fabo; et al. (January 2021). "A Collage of Small Planets from the Lick-Carnegie Exoplanet Survey: Exploring the Super-Earth and Sub-Neptune Mass Regime". The Astronomical Journal . 161 (1): 10. arXiv: 2011.08867 . Bibcode:2021AJ....161...10B. doi: 10.3847/1538-3881/abc2d0 .
  53. ↑ Nari, N.; Dumusque, X. (January 2025). "Revisiting the multi-planetary system of the nearby star HD 20794". Astronomy & Astrophysics . 693: A297. doi: 10.1051/0004-6361/202451769 .
  54. ↑ González-Álvarez, E.; Kemmer, J.; et al. (July 2023). "The CARMENES search for exoplanets around M dwarfs. A sub-Neptunian mass planet in the habitable zone of HN Lib". Astronomy & Astrophysics . 675: A141. arXiv: 2305.19677 . Bibcode:2023A&A...675A.141G. doi:10.1051/0004-6361/202346276.
  55. ↑ Curiel, Salvador; Ortiz-León, Gisela N.; Mioduszewski, Amy J.; Sanchez-Bermudez, Joel (September 2022). "3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion". The Astronomical Journal . 164 (3): 93. arXiv: 2208.14553 . Bibcode:2022AJ....164...93C. doi: 10.3847/1538-3881/ac7c66 . S2CID   251953478.
  56. ↑ von Stauffenberg, A.; Trifonov, T.; Quirrenbach, A.; et al. (2024-06-05). "The CARMENES search for exoplanets around M dwarfs. Revisiting the GJ 581 multi-planetary system with new Doppler measurements from CARMENES, HARPS, and HIRES". Astronomy & Astrophysics. arXiv: 2407.11520 . doi:10.1051/0004-6361/202449375. ISSN   0004-6361.
  57. ↑ González-Álvarez, E.; Osorio, M. R. Zapatero; Caballero, J. A.; Sanz-Forcada, J.; Béjar, V. J. S.; González-Cuesta, L.; Dreizler, S.; Bauer, F. F.; Rodríguez, E.; Tal-Or, L.; Zechmeister, M.; Montes, D.; López-González, M. J.; Ribas, I.; Reiners, Ansgar; Quirrenbach, A.; Amado, P. J.; Anglada-Escudé, G.; Azzaro, M.; Cortés-Contreras, M.; Hatzes, A. P.; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Morales, J. C.; Pallé, E.; Perger, M.; Schmitt, J. H. M. M. (29 March 2020). "The CARMENES search for exoplanets around M dwarfs. A super-Earth planet orbiting HD 79211 (GJ 338 B)". Astronomy & Astrophysics. A93: 637. arXiv: 2003.13052 . Bibcode:2020A&A...637A..93G. doi:10.1051/0004-6361/201937050. S2CID   214714124.
  58. ↑ "GJ 625". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  59. ↑ Vogt, Steven S.; et al. (November 2015). "Six Planets Orbiting HD 219134". The Astrophysical Journal . 814 (1): 12. arXiv: 1509.07912 . Bibcode:2015ApJ...814...12V. doi:10.1088/0004-637X/814/1/12. S2CID   45438051.
  60. ↑ Johnson, Marshall C.; et al. (April 2016). "A 12-year Activity Cycle for the Nearby Planet Host Star HD 219134". The Astrophysical Journal . 821 (2): 74. arXiv: 1602.05200 . Bibcode:2016ApJ...821...74J. doi: 10.3847/0004-637X/821/2/74 . S2CID   118651905.
  61. ↑ Gillon, Michaël; et al. (2017). "Two massive rocky planets transiting a K-dwarf 6.5 parsecs away". Nature Astronomy. 1 (3). 0056. arXiv: 1703.01430 . Bibcode:2017NatAs...1E..56G. doi:10.1038/s41550-017-0056. S2CID   56075932.
  62. ↑ Almenara, Jose-Manuel; Berlind, Perry; Bouchy, Franois; Burke, Chris J.; Delfosse, Xavier; Díaz, Rodrigo F.; Dressing, Courtney D.; Esquerdo, Gilbert A.; Figueira, Pedro; Forveille, Thierry; Fur'esz, G'abor; Henze, Christopher E.; Jao, Wei-Chun; L'epine, S'ebastien; Levine, Alan M.; Lovis, Christophe; Mink, Jessica; Muirhead, Philip S.; Murgas, Felipe; Pepe, Francesco; Tenenbaum, Peter; Teske, Johanna K.; Twicken, Dr Joseph D.; Udry, St'ephane; Jenkins, Jon M.; Winn, Joshua N.; Seager, Sara; Latham, David W.; Vanderspek, Roland; Ricker, George R.; Bonfils, Xavier; Winston, Elaine; Diamond-Lowe, Hannah; Henry, Todd J.; Vrijmoet, Eliot; Eastman, Jason D.; Horch, Elliott P.; Astudillo-Defru, Nicola; Charbonneau, David; Irwin, Jonathan M.; Medina, Amber A.; Winters, Jennifer G. (24 June 2019). "Three Red Suns in the Sky: A Transiting, Terrestrial Planet in a Triple M Dwarf System at 6.9 Parsecs". The Astronomical Journal . 158 (4): 152. arXiv: 1906.10147 . Bibcode:2019AJ....158..152W. doi: 10.3847/1538-3881/ab364d . S2CID   195584444.
  63. ↑ Winters, Jennifer G.; Cloutier, Ryan; Medina, Amber A.; Irwin, Jonathan M.; Charbonneau, David; Astudillo-Defru, Nicola; Bonfils, Xavier; Howard, Andrew W.; Isaacson, Howard; Bean, J. L.; Seifahrt, A.; Teske, J. K.; Eastman, Jason D.; Twicken, Joseph D.; Collins, K. A.; Jensen, E. L. N.; Quinn, S. N.; Payne, M. J.; Kristiansen, M. H.; Spencer, A.; Vanderburg, Andrew; Zechmeister, Mathias; Weiss, L. M.; Wang, S. X.; Wang, G.; Udry, Stéphane; Terentev, I. A.; Sturmer, J.; Stefansson, G.; Shectman, Stephen A.; Sefako, R.; Schwengeler, H. M.; Schwarz, R. P.; Scarsdale, N.; Rubenzahl, R. A.; Roy, A.; Rosenthal, L. J.; Robertson, P.; Petigura, Erik A.; Pepe, Francesco; Omohundro, M.; Murphy, J. M. A.; Murgas, Felipe; Movcnik, T.; Montet, B. T.; Mennickent, R.; Mayo, A. W.; Massey, B.; Lubin, J.; Lovis, Christophe; Lewin, P.; Kasper, D.; Kane, S. R.; Jenkins, J. M.; Huber, D.; Horne, K.; Hill, M. L.; Gorrini, P.; Giacalone, S.; Fulton, Benjamin J.; Forveille, Thierry; Figueira, Pedro; Fetherolf, T.; Dressing, Courtney D.; Díaz, Rodrigo F.; Delfosse, Xavier; Dalba, P. A.; Dai, F.; Cortes, C. C.; Crossfield, Ian J. M.; Crane, Jeffrey D.; Conti, D. M.; Collins, K. I.; Chontos, A.; Butler, R. Paul; Brown, P.; Brady, M.; Bouchy, François; Behmard, A.; Beard, C.; Batalha, Natalie M.; Almenara, José M. (2022). "A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds". The Astronomical Journal. 163 (4): 168. arXiv: 2107.14737 . Bibcode:2022AJ....163..168W. doi: 10.3847/1538-3881/ac50a9 . S2CID   236635391.
  64. ↑ Lavie, B.; Bouchy, F.; et al. (May 2023). "Planetary system around LTT 1445A unveiled by ESPRESSO: Multiple planets in a triple M-dwarf system". Astronomy & Astrophysics . 673: A69. arXiv: 2210.09713 . Bibcode:2023A&A...673A..69L. doi:10.1051/0004-6361/202143007.
  65. ↑ Amado, Pedro J.; Bauer, Florian F.; Rodríguez López, Cristina; Rodríguez, Eloy; Cardona Guillén, C.; Perger, M.; Caballero, José A.; López-González, Maria J.; Muñoz Rodríguez, I.; Pozuelos, F. J.; Sánchez-Rivero, A.; Schlecker, M.; Quirrenbach, Andreas; Ribas, Ignasi; Reiners, Ansgar; Almenara, J.; Astudillo-Defru, N.; Azzaro, M.; Béjar, Victor J. S.; Bohemann, R.; Bonfils, X.; Bouchy, F.; Cifuentes, C.; Cortés-Contreras, M.; Delfosse, Xavier; Dreizler, Stefan; Forveille, Thierry; Hatzes, Artie P.; Henning, Thomas K.; Jeffers, Sandra V.; Kaminski, Adrian; Kürster, Martin; Lafarga, M.; Lodieu, Nicolas; Lovis, C.; Mayor, M.; Montes, David; Morales, Juan Carlos; Morales, Nicolás; Murgas, F.; Ortiz, José L.; Pepe, F.; Perdelwitz, V.; Pollaco, D.; Santos, N. C.; Schöfer, P.; Schweitzer, A.; Ségransan, N. C.; Shan, Y.; Stock, S.; Tal-Or, Lev; Udry, S.; Zapatero-Osorio, María Rosa; Zechmeister, Mathias (2021-05-28). "The CARMENES search for exoplanets around M dwarfs". Astronomy & Astrophysics. 650: A188. arXiv: 2105.13785 . doi:10.1051/0004-6361/202140633. S2CID   235248027.
  66. ↑ "GJ 667 C". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  67. ↑ "GJ 667 C d". Extrasolar Planets Encyclopaedia . Archived from the original on 2017-12-01. Retrieved 2018-03-22.
  68. ↑ "GJ 667 C h". Extrasolar Planets Encyclopaedia . 2016-02-23. Archived from the original on 2017-12-01. Retrieved 2018-03-22.
  69. ↑ Damasso, M.; Perger, M.; Almenara, J. M.; Nardiello, D.; Pérez-Torres, M.; Sozzetti, A.; Hara, N. C.; Quirrenbach, A.; Bonfils, X.; Osorio, M. R. Zapatero; Astudillo-Defru, N.; Hernández, J. I. González; Mascareño, A. Suárez; Amado, P. J.; Forveille, T.; Lillo-Box, J.; Alibert, Y.; Caballero, J. A.; Cifuentes, C.; Delfosse, X.; Figueira, P.; Galadí-Enríquez, D.; Hatzes, A. P.; Henning, Th; Kaminski, A.; Mayor, M.; Murgas, F.; Montes, D.; Pinamonti, M.; Reiners, A.; Ribas, I.; Béjar, V. J. S.; Schweitzer, A.; Zechmeister, M. (13 April 2022). "A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514". Astronomy & Astrophysics. 666: A187. arXiv: 2204.06376 . doi:10.1051/0004-6361/202243522. S2CID   248157318.
  70. ↑ Vedantham, H. K.; Callingham, J. R.; Shimwell, T. W.; Tasse, C.; Pope, B. J. S.; Bedell, M.; Snellen, I.; Best, P.; Hardcastle, M. J.; Haverkorn, M.; Mechev, A.; O’Sullivan, S. P.; Röttgering, H. J. A.; White, G. J. (June 2020). "Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction". Nature Astronomy. 4 (6): 577–583. arXiv: 2002.08727 . Bibcode:2020NatAs...4..577V. doi:10.1038/s41550-020-1011-9. S2CID   211204712.
  71. ↑ Mahadevan, Suvrath; Stefánsson, Guðmundur; Robertson, Paul; Terrien, Ryan C.; Ninan, Joe P.; Holcomb, Rae J.; Halverson, Samuel; Cochran, William D.; Kanodia, Shubham; Ramsey, Lawrence W.; Wolszczan, Alexander; Endl, Michael; Bender, Chad F.; Diddams, Scott A.; Fredrick, Connor; Hearty, Fred; Monson, Andrew; Metcalf, Andrew J.; Roy, Arpita; Schwab, Christian (3 February 2021). "The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star". The Astrophysical Journal Letters. 919 (1): L9. arXiv: 2102.02233 . Bibcode:2021ApJ...919L...9M. doi: 10.3847/2041-8213/abe2b2 . S2CID   231802021.
  72. ↑ Perger, M.; Ribas, I.; Anglada-Escudé, G.; Morales, J. C.; Amado, P. J.; Caballero, J. A.; Quirrenbach, A.; Reiners, A.; Béjar, V. J. S.; Dreizler, S.; Galadí-Enríquez, D.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Montes, D.; Pallé, E.; Rodríguez-López, C.; Schweitzer, A.; Zapatero Osorio, M. R.; Zechmeister, M. (2021), "The CARMENES search for exoplanets around M dwarfs, No evidence for a super-Earth in a 2-day orbit around GJ 1151", Astronomy & Astrophysics, 649: L12, arXiv: 2103.10216 , Bibcode:2021A&A...649L..12P, doi:10.1051/0004-6361/202140786, S2CID   126038821
  73. ↑ Blanco-Pozo, J.; Perger, M.; et al. (March 2023). "The CARMENES search for exoplanets around M dwarfs. A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data". Astronomy & Astrophysics . 671: A50. arXiv: 2301.04442 . Bibcode:2023A&A...671A..50B. doi:10.1051/0004-6361/202245053.
  74. ↑ Trifonov, T.; Caballero, J. A.; Morales, J. C.; Seifahrt, A.; Ribas, I.; Reiners, Ansgar; Bean, J. L.; Luque, R.; Parviainen, H.; Pallé, E.; Stock, S.; Zechmeister, M.; Amado, P. J.; Anglada-Escudé, G.; Azzaro, M.; Barclay, T.; Béjar, V. J. S.; Bluhm, P.; Casasayas-Barris, N.; Cifuentes, C.; Collins, K. A.; Collins, K. I.; Cortés-Contreras, M.; de Leon, J.; Dreizler, S.; Dressing, C. D.; Esparza-Borges, E.; Espinoza, N.; Fausnaugh, M.; Fukui, A.; Hatzes, A. P.; Hellier, C.; Henning, Th.; Henze, C. E.; Herrero, E.; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kaminski, A.; Kasper, D.; Kossakowski, D.; Kürster, M.; Lafarga, M.; Latham, D. W.; Mann, A. W.; Molaverdikhani, K.; Montes, D.; Montet, B. T.; Murgas, F.; Narita, N.; Oshagh, M.; Passegger, V. M.; Pollacco, D.; Quinn, S. N.; Quirrenbach, A.; Ricker, G. R.; Rodríguez López, C.; Sanz-Forcada, J.; Schwarz, R. P.; Schweitzer, A.; Seager, S.; Shporer, A.; Stangret, M.; Stürmer, J.; Tan, T. G.; Tenenbaum, P.; Twicken, J. D.; Vanderspek, R.; Winn, J. N. (5 March 2021). "A nearby transiting rocky exoplanet that is suitable for atmospheric investigation". Science. 371 (6533): 1038–1041. arXiv: 2103.04950 . Bibcode:2021Sci...371.1038T. doi:10.1126/science.abd7645. PMID   33674491. S2CID   232124642.
  75. ↑ Affer, L.; Damasso, M.; Micela, G.; Poretti, E.; Scandariato, G.; Maldonado, J.; Lanza, A. F.; Covino, E.; Rubio, A. Garrido; Hernandez, J. I. Gonzalez; Gratton, R.; Leto, G.; Maggio, A.; Perger, M.; Sozzetti, A.; Mascareno, A. Suarez; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Desidera, S.; Molinari, E.; Pedani, M.; Pinamonti, M.; Rebolo, R.; Ribas, I.; Toledo-Padron, B. (16 January 2019). "HADES RV programme with HARPS-N at TNG. X. A super-Earth around the M dwarf Gl686". Astronomy & Astrophysics. A193: 622. arXiv: 1901.05338 . Bibcode:2019A&A...622A.193A. doi:10.1051/0004-6361/201834868. S2CID   118863481.
  76. ↑ "GJ 1289". SIMBAD . Centre de données astronomiques de Strasbourg.
  77. 1 2 Moutou, C.; Ould-Elhkim, M.; Donati, J.-F.; Charpentier, P.; Cadieux, C.; Delfosse, X.; Artigau, E.; Arnold, L.; Baruteau, C. (2024-06-14), Characterizing planetary systems with SPIRou: a temperate sub-Neptune exoplanet orbiting the nearby fully-convective star GJ 1289 and a candidate around GJ 3378, arXiv: 2406.10384
  78. ↑ Cretignier, M.; Dumusque, X.; et al. (August 2023). "YARARA V2: Reaching sub-m s−1 precision over a decade using PCA on line-by-line radial velocities". Astronomy & Astrophysics. 678: A2. arXiv: 2308.11812 . Bibcode:2023A&A...678A...2C. doi:10.1051/0004-6361/202347232. S2CID   261076243.
  79. ↑ Bauer, F. F.; Zechmeister, M.; Kaminski, A.; López, C. Rodríguez; Caballero, J. A.; Azzaro, M.; Stahl, O.; Kossakowski, D.; Quirrenbach, A.; Jarque, S. Becerril; Rodríguez, E.; Amado, P. J.; Seifert, W.; Reiners, Ansgar; Schäfer, S.; Ribas, I.; Béjar, V. J. S.; Cortés-Contreras, M.; Dreizler, S.; Hatzes, A.; Henning, T.; Jeffers, S. V.; Kürster, M.; Lafarga, M.; Montes, D.; Morales, J. C.; Schmitt, J. H. M. M.; Schweitzer, A.; Solano, E. (2 June 2020). "The CARMENES search for exoplanets around M dwarfs. Measuring precise radial velocities in the near infrared: the example of the super-Earth CD Cet b". Astronomy and Astrophysics. 640: A50. arXiv: 2006.01684 . Bibcode:2020A&A...640A..50B. doi:10.1051/0004-6361/202038031. S2CID   219179889.
  80. ↑ "HD 192310". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  81. ↑ "GJ 849". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  82. ↑ "GJ 433". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  83. ↑ "HD 102365". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  84. ↑ Lam, Kristine W. F.; Csizmadia, Szilárd; Astudillo-Defru, Nicola; Bonfils, Xavier; Gandolfi, Davide; Padovan, Sebastiano; Esposito, Massimiliano; Hellier, Coel; Hirano, Teruyuki; Livingston, John; Murgas, Felipe; Smith, Alexis M. S.; Collins, Karen A.; Mathur, Savita; Garcia, Rafael A.; Howell, Steve B.; Santos, Nuno C.; Dai, Fei; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Albrecht, Simon; Almenara, Jose M.; Artigau, Etienne; Barragán, Oscar; Bouchy, François; Cabrera, Juan; Charbonneau, David; Chaturvedi, Priyanka; Chaushev, Alexander; Christiansen, Jessie L.; Cochran, William D.; De Meideiros, José R.; Delfosse, Xavier; Díaz, Rodrigo F.; Doyon, René; Eigmüller, Philipp; Figueira, Pedro; Forveille, Thierry; Fridlund, Malcolm; Gaisné, Guillaume; Goffo, Elisa; Georgieva, Iskra; Grziwa, Sascha; Guenther, Eike; Hatzes, Artie P.; Johnson, Marshall C.; Kabáth, Petr; Knudstrup, Emil; Korth, Judith; Lewin, Pablo; Lissauer, Jack J.; Lovis, Christophe; Luque, Rafael; Melo, Claudio; Morgan, Edward H.; Morris, Robert; Mayor, Michel; Narita, Norio; Osborne, Hannah L. M.; Palle, Enric; Pepe, Francesco; Persson, Carina M.; Quinn, Samuel N.; Rauer, Heike; Redfield, Seth; Schlieder, Joshua E.; Ségransan, Damien; Serrano, Luisa M.; Smith, Jeffrey C.; Šubjak, Ján; Twicken, Joseph D.; Udry, Stéphane; Van Eylen, Vincent; Vezie, Michael (3 December 2021). "GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star" (PDF). Science. 374 (6572): 1271–1275. arXiv: 2112.01309 . Bibcode:2021Sci...374.1271L. doi:10.1126/science.aay3253. PMID   34855492. S2CID   244799656.
  85. ↑ Goffo, Elisa; Gandolfi, Davide; et al. (September 2023). "Company for the ultra-high density, ultra-short period sub-Earth GJ 367 b: discovery of two additional low-mass planets at 11.5 and 34 days". The Astrophysical Journal Letters . 955 (1): L3. arXiv: 2307.09181 . Bibcode:2023ApJ...955L...3G. doi: 10.3847/2041-8213/ace0c7 .
  86. ↑ Wohler, B.; Winn, J. W.; Wang, S. X.; Twicken, J. D.; Teske, J.; Tamura, M.; Shectman, S. A.; Rowden, P.; Ricker, G. R.; Ribas, I.; Pedraz, S.; Nagel, E.; Murgas, F.; Morales, J. C.; Montañés-Rodríguez, P.; McDermott, S.; Latham, D. W.; Lafarga, M.; Kotani, T.; Klahr, H.; Kaminski, A.; Jenkins, J. M.; Feng, F.; Dynes, S.; Dressing, C. D.; Crane, J. D.; Collins, K. I.; Collins, K. A.; Chen, G.; Caldwell, D. A.; Butler, R. P.; Burt, J.; Burke, C. J.; Bluhm, P.; Bauer, F. F.; Batalha, N. E.; Anderson, D. R.; Amado, P. J.; Zechmeister, M.; Osorio, M. R. Zapatero; Trifonov, T.; Stock, S.; Schlecker, M.; Rodríguez-López, C.; Reiners, Ansgar; Reffert, S.; Quirrenbach, A.; Parviainen, H.; Oshagh, M.; Ofir, A.; Nowak, G.; Narita, N.; Montes, D.; Molaverdikhani, K.; Kürster, M.; Kaltenegger, L.; Jeffers, S. V.; Henning, T.; Hellier, C.; Hatzes, A.; Díez-Alonso, E.; Cortés-Contreras, M.; Caballero, J. A.; Béjar, V. J. S.; Anglada-Escudé, G.; Espinoza, N.; Kemmer, J.; Dreizler, S.; Kossakowski, D.; Pallé, E.; Luque, R. (29 April 2019). "A planetary system around the nearby M dwarf Gl 357 including a transiting hot Earth-sized planet optimal for atmospheric characterisation". Astronomy & Astrophysics. A39: 628. arXiv: 1904.12818 . Bibcode:2019A&A...628A..39L. doi:10.1051/0004-6361/201935801. S2CID   139102184.
  87. ↑ "HD 285968". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2018-03-22.
  88. ↑ "GJ 176 c". Extrasolar Planets Encyclopaedia . 2010-12-17. Archived from the original on 2014-02-23. Retrieved 2014-05-20.
  89. ↑ Morales, J. C.; et al. (2019). "A giant exoplanet orbiting a very-low-mass star challenges planet formation models". Science. 365 (6460): 1441–1445. arXiv: 1909.12174 . Bibcode:2019Sci...365.1441M. doi:10.1126/science.aax3198. ISSN   0036-8075. PMID   31604272. S2CID   202888425.
  90. ↑ Kossakowski, D.; Kürster, M.; et al. (January 2023). "The CARMENES search for exoplanets around M dwarfs, Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star". Astronomy & Astrophysics . 670. arXiv: 2301.02477 . Bibcode:2023A&A...670A..84K. doi:10.1051/0004-6361/202245322.
  91. ↑ Plavchan, Peter; Barclay, Thomas; Gagné, Jonathan; et al. (2020). "A planet within the debris disk around the pre-main-sequence star AU Microscopii". Nature. 582 (7813): 497–500. arXiv: 2006.13248 . Bibcode:2020Natur.582..497P. doi:10.1038/s41586-020-2400-z. PMC   7323865 . PMID   32581383. S2CID   220042005.
  92. ↑ Martioli, E.; et al. (2021). "New constraints on the planetary system around the young active star AU Mic. Two transiting warm Neptunes near mean-motion resonance". Astronomy & Astrophysics. A177: 649. arXiv: 2012.13238 . Bibcode:2021A&A...649A.177M. doi:10.1051/0004-6361/202040235. S2CID   229371309.
  93. ↑ Wittrock, Justin M.; et al. (2023), "Validating AU Microscopii d with Transit Timing Variations", The Astronomical Journal, 166 (6): 232, arXiv: 2302.04922 , Bibcode:2023AJ....166..232W, doi: 10.3847/1538-3881/acfda8
  94. ↑ Donati, J-F; Cristofari, P I; Finociety, B; et al. (24 April 2023). "The magnetic field and multiple planets of the young dwarf AU Mic". Monthly Notices of the Royal Astronomical Society . 525: 455–475. arXiv: 2304.09642 . doi: 10.1093/mnras/stad1193 . ISSN   0035-8711. S2CID   258212637.
  95. ↑ Gillon, M.; et al. (2007). "Detection of transits of the nearby hot Neptune GJ 436 b". Astronomy and Astrophysics. 472 (2): L13 –L16. arXiv: 0705.2219 . Bibcode:2007A&A...472L..13G. doi:10.1051/0004-6361:20077799. S2CID   13552824.
  96. ↑ Lanotte, A. A.; et al. (2014). "A global analysis of Spitzer and new HARPS data confirms the loneliness and metal-richness of GJ 436 b". Astronomy and Astrophysics. 572. A73. arXiv: 1409.4038 . Bibcode:2014A&A...572A..73L. doi:10.1051/0004-6361/201424373. S2CID   55405647.
  97. ↑ Perger, M.; et al. (April 2019). "Gliese 49: Activity evolution and detection of a super-Earth". Astronomy & Astrophysics. 624: 19. arXiv: 1903.04808 . Bibcode:2019A&A...624A.123P. doi:10.1051/0004-6361/201935192. ISSN   0004-6361. S2CID   85497416. A123.
  98. ↑ Gorrini, P.; Kemmer, J.; et al. (December 2023). "Planetary companions orbiting the M dwarfs GJ 724 and GJ 3988. A CARMENES and IRD collaboration". Astronomy & Astrophysics . 680: A28. arXiv: 2310.05599 . Bibcode:2023A&A...680A..28G. doi:10.1051/0004-6361/202347108.
  99. ↑ Luque, R.; et al. (2022). "The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc". Astronomy & Astrophysics. 664: A199. arXiv: 2204.10261 . Bibcode:2022A&A...664A.199L. doi:10.1051/0004-6361/202243834. S2CID   248300168.
  100. ↑ Lee, Rhodi (2015-09-18). "Want To Name An Exoplanet? Here's Your Chance". Tech Times. Archived from the original on 2015-09-07. Retrieved 2015-09-17.
  101. ↑ Bartlett, Jennifer L; Ianna, Philip A; Begam, Michael C (2009). "A Search for Astrometric Companions to Stars in the Southern Hemisphere". Publications of the Astronomical Society of the Pacific. 121 (878): 365. Bibcode:2009PASP..121..365B. doi:10.1086/599044. S2CID   122529477.
  102. ↑ Rajpaul, Vinesh (19 October 2015). "Ghost in the time series: no planet for Alpha Cen B". Monthly Notices of the Royal Astronomical Society: Letters. 456 (1): L6 –L10. arXiv: 1510.05598 . Bibcode:2016MNRAS.456L...6R. doi: 10.1093/mnrasl/slv164 .
  103. ↑ Ribas, I.; Tuomi, M.; Reiners, Ansgar; Butler, R. P.; et al. (2018-11-14). "A candidate super-Earth planet orbiting near the snow line of Barnard's star" (PDF). Nature . 563 (7731). Holtzbrinck Publishing Group: 365–368. arXiv: 1811.05955 . Bibcode:2018Natur.563..365R. doi:10.1038/s41586-018-0677-y. hdl:2299/21132. ISSN   0028-0836. OCLC   716177853. PMID   30429552. S2CID   256769911. Archived (PDF) from the original on 2019-03-26.
  104. ↑ Lubin, Jack; Robertson, Paul; Stefansson, Gudmundur; et al. (15 July 2021). "Stellar Activity Manifesting at a One-year Alias Explains Barnard b as a False Positive". The Astronomical Journal. 162 (2). American Astronomical Society: 61. arXiv: 2105.07005 . Bibcode:2021AJ....162...61L. doi: 10.3847/1538-3881/ac0057 . ISSN   0004-6256. S2CID   234741985.
  105. ↑ Bortle, Anna; et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal. 161 (5): 230. arXiv: 2103.02709 . Bibcode:2021AJ....161..230B. doi: 10.3847/1538-3881/abec89 . S2CID   232110395.
  106. ↑ Farihi, J.; Becklin, E. E.; Macintosh, B. A. (June 2004). "Mid-Infrared Observations of van Maanen 2: No Substellar Companion". Astrophysical Journal Letters. 608 (2): L109 –L112. arXiv: astro-ph/0405245 . Bibcode:2004ApJ...608L.109F. doi:10.1086/422502. S2CID   17166073.
  107. ↑ Heinze, A. N.; Hinz, Philip M.; Sivanandam, Suresh; et al. (May 2010). "Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations". The Astrophysical Journal. 714 (2): 1551–1569. arXiv: 1003.5340 . Bibcode:2010ApJ...714.1551H. doi:10.1088/0004-637X/714/2/1551. S2CID   119199321.
  108. ↑ Carleo, I.; et al. (June 2020). "The GAPS Programme at TNG. XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis b". Astronomy & Astrophysics . 638: A5. arXiv: 2002.10562 . Bibcode:2020A&A...638A...5C. doi:10.1051/0004-6361/201937369. S2CID   211296466.
  109. ↑ Ma, Bo; Ge, Jian; Muterspaugh, Matthew; Singer, Michael A; Henry, Gregory W; González Hernández, Jonay I; Sithajan, Sirinrat; Jeram, Sarik; Williamson, Michael; Stassun, Keivan; Kimock, Benjamin; Varosi, Frank; Schofield, Sidney; Liu, Jian; Powell, Scott; Cassette, Anthony; Jakeman, Hali; Avner, Louis; Grieves, Nolan; Barnes, Rory; Zhao, Bo; Gilda, Sankalp; Grantham, Jim; Stafford, Greg; Savage, David; Bland, Steve; Ealey, Brent (October 2018). "The first super-Earth detection from the high cadence and high radial velocity precision Dharma Planet Survey". Monthly Notices of the Royal Astronomical Society. 480 (2): 2411–2422. arXiv: 1807.07098 . Bibcode:2018MNRAS.480.2411M. doi: 10.1093/mnras/sty1933 . S2CID   54871108.
  110. ↑ Burrows, Abigail; Halverson, Samuel; et al. (April 2024). "The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity". The Astronomical Journal . 167 (5): 243. arXiv: 2404.17494 . Bibcode:2024AJ....167..243B. doi: 10.3847/1538-3881/ad34d5 .
  111. ↑ "VB 10 b". Extrasolar Planets Encyclopaedia . Archived from the original on 2015-09-29. Retrieved 2015-09-17.
  112. ↑ Gáspár, András; Rieke, George H. (April 20, 2020). "New HST data and modeling reveal a massive planetesimal collision around Fomalhaut". PNAS . 117 (18): 9712–9722. arXiv: 2004.08736 . Bibcode:2020PNAS..117.9712G. doi: 10.1073/pnas.1912506117 . PMC   7211925 . PMID   32312810. S2CID   215827666.
  113. ↑ Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George (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. arXiv: 2101.08801 . Bibcode:2021AJ....161..157H. doi: 10.3847/1538-3881/abdec8 . S2CID   231693198.
  114. ↑ Wagner, K.; Boehle, A.; Pathak, P.; Kasper, M.; Arsenault, R.; Jakob, G.; Käufl, U.; Leveratto, S.; Maire, A.-L.; Pantin, E.; Siebenmorgen, R. (2021-02-10). "Imaging low-mass planets within the habitable zone of α Centauri". Nature Communications. 12 (1): 922. arXiv: 2102.05159 . Bibcode:2021NatCo..12..922W. doi: 10.1038/s41467-021-21176-6 . ISSN   2041-1723. PMC   7876126 . PMID   33568657.
  115. ↑ Abuter, R.; et al. (GRAVITY Collaboration) (May 2024). "Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY". Astronomy & Astrophysics . 685: L9. arXiv: 2404.08746 . Bibcode:2024A&A...685L...9G. doi:10.1051/0004-6361/202449547.
  116. ↑ Boss, Alan P.; Butler, R. Paul; Hubbard, William B.; et al. (2007). "Working Group on Extrasolar Planets". Proceedings of the International Astronomical Union. 1 (T26A): 183. Bibcode:2007IAUTA..26..183B. doi: 10.1017/S1743921306004509 .
  117. ↑ "SCR 1845 b". Extrasolar Planets Encyclopaedia . 2012-04-13. Archived from the original on 2015-10-01. Retrieved 2015-09-17.
  118. ↑ "SDSS 141624 b". Extrasolar Planets Encyclopaedia . 2010-01-18. Archived from the original on 2014-02-23. Retrieved 2014-05-20.
  119. ↑ "WISE 1217+16A b". Extrasolar Planets Encyclopaedia . Archived from the original on 2017-06-12. Retrieved 2014-05-17.
  120. ↑ Clavin, Whitney; Harrington, J. D. (2014-04-25). "NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun". NASA. Archived from the original on 2014-04-26. Retrieved 2015-09-17.
  121. ↑ Lucas, P. W.; Tinney, C. G.; Burningham, B.; et al. (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". Monthly Notices of the Royal Astronomical Society. 408 (1): L56 –L60. arXiv: 1004.0317 . Bibcode:2010MNRAS.408L..56L. doi: 10.1111/j.1745-3933.2010.00927.x . S2CID   16032606.
  122. ↑ Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; et al. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal. 743 (1): 50. arXiv: 1108.4678 . Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50. S2CID   286881.
  123. ↑ "Astronomers discover a nearby free-range planet with incredible magne". 3 August 2018.

This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.