List of nearest stars and brown dwarfs

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Rotating 3D image of the nearest stars
Animated 3D map of the nearest stars, centered on the Sun. 3d glasses red green.svg 3D red green glasses are recommended to view this image correctly.
Distance and angle conformal map of the celestial neighbourhood of Sol.

This list covers all known stars and brown dwarfs (incl. sub-brown dwarfs) within 5.0 parsecs (16.3 light-years) of the Solar System. So far 76 such objects have been found, of which only nine are bright enough in visible light to reach or exceed the dimmest brightness to be visible to the naked eye from Earth, 6.5 apparent magnitude.[1] The stars and (sub-) brown dwarfs are currently moving through or with interstellar clouds like the Local Interstellar Cloud and the G-Cloud, all of which are, along with the nearest and unaided-visible moving group of Ursa Major or the closest visible star cluster the Hyades, within the Local Bubble. In the galactic context the Local Bubble is a small part, unlike the wider Gould Belt, of the Orion Arm, which contains most unaided visible stars.

The currently known 76 objects are bound in 54 stellar systems. The closest system is Alpha Centauri, with Proxima Centauri as the closest system star at 4.25 light-years from Earth. The brightest among these systems, as well as the brightest in Earth's night sky, is Sirius. Of the population of currently known objects 61 are main sequence stars, with 50 being red dwarfs and the remaining 13 having greater mass. Additionally astronomers have found four white dwarfs (extremely dense collapsed cores that remain after stars such as our Sun have exhausted all fusable hydrogen in their core and have shed slowly their outer layers), as well as 10 brown dwarfs and the closest and only sub-brown dwarf WISE 0855−0714 (an object of planetary-mass, not quite massive enough to fuse hydrogen, therefore also the nearest known rogue planet).

Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will possibly approach the Solar System to less than 5 parsecs in the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec (3.3 light-years) and another 7 within 0.5 parsecs (1.6 light-years).[2] This number is likely much higher, due to the sheer number of stars needed to be surveyed; a star approaching the Solar System 10 million years ago, moving at a typical Sun-relative 20–200 kilometers per second, would be 600–6,000 light-years from the Sun at present day, with millions of stars closer to the Sun. The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun.[3] It is currently predicted to pass 19,300 ± 3,200 astronomical units (0.305 ± 0.051 light-years) from the Sun in 1.280+0.041
−0.039
million years from the present, close enough to significantly disturb the Solar System's Oort cloud.[2][3]

The easiest way to determine stellar distance to the Sun for objects at these distances is parallax, which measures how much stars appear to move against background objects over the course of Earth's orbit around the Sun. As a parsec (parallax-second) is defined by the distance of an object that would appear to move exactly one second of arc against background objects, stars less than 5 parsecs away will have measured parallaxes of over 0.2 arcseconds, or 200 milliarcseconds. Determining past and future positions relies on accurate astrometric measurements of their parallax and total proper motions (how far they move across the sky due to their actual velocity relative to the Sun), along with spectroscopically determined radial velocities (their speed directly towards or away from us, which combined with proper motion defines their true movement through the sky relative to the Sun). Both of these measurements are subject to increasing and significant errors over very long time spans, especially over the several thousand-year time spans it takes for stars to noticeably move relative to each other.[4]

List[edit]

Key
# Visible to the unaided eye
§ Brown dwarf or Sub-brown dwarf
white dwarf White dwarf

The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible color bands (U, B or V). Absolute magnitude (with electromagnetic wave, 'light' band denoted in subscript) is a measurement at a 10-parsec distance across imaginary empty space devoid of all its sparse dust and gas. Some of the parallaxes and resultant distances are rough measurements.[5]

Known star systems within 5.0 parsecs (16.3 light-years)
Designation Distance[6]
(light-years (±err))
Stellar
class
Mass Magnitude (mV[5] or mJ) Epoch J2000.0 Parallax
(mas (±err))

[5][note 1]
Notes and additional
references
System Star or (sub-) brown dwarf M Apparent Absolute Right ascension[5] Declination[5]
Solar System Sun (Sol) 0.0000158 G2V[5] 1 −26.74# 4.85 N/A N/A N/A eight known planets
Alpha Centauri Proxima Centauri (V645 Centauri) 4.2441±0.0011 M5.5Ve 0.122 11.09 15.53 14h 29m 43.0s −62° 40′ 46″ 768.50±0.20[7] flare star, two confirmed planets (b, 2016, and c, 2019)[8] and unconfirmed evidence for a third, sub-Earth sized, planet (d, 2020).[9]
α Centauri A (Rigil Kentaurus) 4.3650±0.0068 G2V[5] 1.100 0.01# 4.38 14h 39m 36.5s −60° 50′ 02″ 747.23±1.17
[10][11][12]
one directly-imaged habitable-zone planet candidate (Candidate 1) (2021)
α Centauri B (Toliman) K1V[5] 0.907 1.34# 5.71 14h 39m 35.1s −60° 50′ 14″ one suspected planet (c) (2013)
(planet b refuted in 2015)
Barnard's Star (BD+04°3561a) 5.9577±0.0032 M4.0Ve 0.144 9.53 13.22 17h 57m 48.5s +04° 41′ 36″ 547.45±0.29[7] flare star, largest-known proper motion,[13] one disputed planet (b)[14][15]
Luhman 16
(WISE 1049−5319)§
Luhman 16A§ 6.5029±0.0011 L8±1[16] 0.032 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 501.557±0.082[17] one refuted planet (Ab[18] in 2017[19])
Luhman 16B§ T1±2[16] 0.027
WISE 0855−0714§ 7.43±0.04[20] Y4 0.003-0.010 25.0 J 08h 55m 10.83s −07° 14′ 42.5″ 439.0±2.4[21] sub-brown dwarf
Wolf 359 (CN Leonis) 7.856±0.031 M6.0V[5] 0.090 13.44 16.55 10h 56m 29.2s +07° 00′ 53″ 415.16±1.62[22] flare star, has 2 known planets[14]
Lalande 21185 (BD+36°2147) 8.307±0.014 M2.0V[5] 0.390 7.47 10.44 11h 03m 20.2s +35° 58′ 12″ 392.64±0.67[23] two known planets (2019)(2021)[14]
Sirius
(α Canis Majoris)
Sirius A 8.659±0.010 A1V[5] 2.063 −1.46# 1.42 06h 45m 08.9s −16° 42′ 58″ 376.68±0.45[7] brightest star in the night sky
Sirius Bwhite dwarf DA2[5] 1.018 8.44 11.34
Luyten 726-8 Luyten 726-8 A (BL Ceti) 8.791±0.012 M5.5Ve 0.102 12.54 15.40 01h 39m 01.3s −17° 57′ 01″ 371.0±0.5[7] flare star (Archetypal member)
Luyten 726-8 B (UV Ceti) M6.0Ve 0.100 12.99 15.85
Ross 154 (V1216 Sagittarii) 9.7035±0.0019 M3.5Ve 0.17 10.43 13.07 18h 49m 49.4s −23° 50′ 10″ 336.123±0.064[7] flare star
Ross 248 (HH Andromedae) 10.2903±0.0041 M5.5Ve 0.136 12.29 14.79 23h 41m 54.7s +44° 10′ 30″ 316.96±0.13[7] flare star
Epsilon Eridani (Ran) 10.446±0.016 K2V[5] 0.820 3.73# 6.19 03h 32m 55.8s −09° 27′ 30″ 312.22±0.47[7] three circumstellar disks,
two suspected planets (AEgir (debated) and c) (2000 & 2002)[24]
Lacaille 9352 (Gliese 887) 10.7211±0.0016 M0.5V 0.486 7.34 9.75 23h 05m 52.0s −35° 51′ 11″ 304.219±0.045[7] two planets, b and c, with equivocal evidence for a third in the habitable zone (2020)[25]
Ross 128 (FI Virginis) 11.0074±0.0026 M4.0Vn 0.168 11.13 13.51 11h 47m 44.4s +00° 48′ 16″ 296.307±0.070[7] flare star, one planet (b) (2017)[26]
EZ Aquarii
(Gliese 866, Luyten 789-6)
EZ Aquarii A 11.109±0.034 M5.0Ve 0.11 13.33 15.64 22h 38m 33.4s −15° 17′ 57″ 293.60±0.9[27] A & B flare stars
EZ Aquarii B M? 0.11 13.27 15.58
EZ Aquarii C M? 0.10 14.03 16.34
61 Cygni 61 Cygni A (BD+38°4343) 11.4008±0.0012 K5.0V[5] 0.70 5.21# 7.49 21h 06m 53.9s +38° 44′ 58″ 286.08±0.03[7] First star (besides Sun) to have measured distance.[28]
B flare star and brightest red dwarf in night sky, with possible planet or brown dwarf.[29]
Possible circumstellar disk.
61 Cygni B (BD+38°4344) K7.0V[5] 0.63 6.03# 8.31 21h 06m 55.3s +38° 44′ 31″
Procyon
(α Canis Minoris)
Procyon A 11.402±0.032 F5IV–V[5] 1.499 0.38# 2.66 07h 39m 18.1s +05° 13′ 30″ 286.05±0.81
[10][11]
Procyon Bwhite dwarf DQZ[5] 0.602 10.70 12.98
Struve 2398
(Gliese 725, BD+59°1915)
Struve 2398 A (HD 173739) 11.4880±0.0012 M3.0V[5] 0.334 8.90 11.16 18h 42m 46.7s +59° 37′ 49″ 283.91±0.03[7] flare stars, star B has 2 known planets[14]
Struve 2398 B (HD 173740) M3.5V[5] 0.248 9.69 11.95 18h 42m 46.9s +59° 37′ 37″
Groombridge 34
(Gliese 15)
Groombridge 34 A (GX Andromedae) 11.6182±0.0008 M1.5V[5] 0.38 8.08 10.32 00h 18m 22.9s +44° 01′ 23″ 280.73±0.02[7] flare star, two suspected planets (Ac, 2017) and Ab, 2014)[30]
Groombridge 34 B (GQ Andromedae) M3.5V[5] 0.15 11.06 13.30 flare star
DX Cancri (G 51-15) 11.6780±0.0056 M6.5Ve 0.09 14.78 16.98 08h 29m 49.5s +26° 46′ 37″ 279.29±0.13[7] flare star
Tau Ceti (BD−16°295) 11.753±0.022 G8.5Vp[5] 0.783 3.49# 5.68 01h 44m 04.1s −15° 56′ 15″ 277.52±0.52[7] one debris disk
four confirmed planets (e, f, g, and h) (2012, 2017),
four candidate planets (b, c, d, and "i") (2012, 2019), and 1 predicted planet (2020).
Epsilon Indi
(CPD−57°10015)
Epsilon Indi A 11.869±0.011 K5Ve[5] 0.754 4.69# 6.89 22h 03m 21.7s −56° 47′ 10″ 274.80±0.25[7] one planet (Ab) (2018)[31]
Epsilon Indi Ba§ T1.0V 0.065 12.3 J[32] 22h 04m 10.5s −56° 46′ 58″
Epsilon Indi Bb§ T6.0V 0.050 13.2 J[32]
Gliese 1061 (LHS 1565) 11.9803±0.0029 M5.5V[5] 0.113 13.09 15.26 03h 35m 59.7s −44° 30′ 45″ 272.245±0.066[7] has 3 known planets (2019)[33][34][35]
YZ Ceti (LHS 138) 12.1084±0.0035 M4.5V[5] 0.130 12.02 14.17 01h 12m 30.6s −16° 59′ 56″ 269.363±0.078[7] flare star, three planets (b, c, and d) (2017),[36]
one suspected planet (e)
Luyten's Star (BD+05°1668) 12.199±0.036 M3.5Vn 0.26 9.86 11.97 07h 27m 24.5s +05° 13′ 33″ 267.36±0.79[37] two planets (b, c) (2017)[38] and two suspected planets (d, e) (2019)[39]
Teegarden's Star (SO025300.5+165258) 12.496±0.013 M6.5V 0.08 15.14 17.22 02h 53m 00.9s +16° 52′ 53″ 261.01±0.27[7] tentative radial velocity variation (2010)[35][40] has 2 known planets (2019)[41][42]
Kapteyn's Star (CD−45°1841) 12.8294±0.0013 M1.5VI[5] 0.281 8.84 10.87 05h 11m 40.6s −45° 01′ 06″ 254.226±0.026[7] two disputed planets (b and c) (2014)[43][44]
Lacaille 8760 (AX Microscopii) 12.9515±0.0029 M0.0V[5] 0.60 6.67 8.69 21h 17m 15.3s −38° 52′ 03″ 251.829±0.056[7] brightest M dwarf star in night sky, flare star
SCR 1845-6357 SCR 1845-6357 A 13.050±0.008 M8.5V[5] 0.07 17.39 19.41 18h 45m 05.3s −63° 57′ 48″ 249.91±0.16[7] [35]
SCR 1845-6357 B§ T6[45] 0.03[5] 13.3 J[32] 18h 45m 02.6s −63° 57′ 52″
Kruger 60
(BD+56°2783)
Kruger 60 A 13.0724±0.0052 M3.0V[5] 0.271 9.79 11.76 22h 27m 59.5s +57° 41′ 45″ 249.5±0.1[7] B flare star
Kruger 60 B (DO Cephei) M4.0V[5] 0.176 11.41 13.38
DEN 1048-3956§ 13.1932±0.0066 M8.5V[5] 0.08 17.39 19.37 10h 48m 14.7s −39° 56′ 06″ 247.22±0.12[7] [46][47]
Ross 614
(V577 Monocerotis, Gliese 234)
Ross 614A (LHS 1849) 13.424±0.049 M4.5V[5] 0.223 11.15 13.09 06h 29m 23.4s −02° 48′ 50″ 242.97±0.88[7] A flare star
Ross 614B (LHS 1850) M5.5V 0.111 14.23 16.17
UGPS J0722-0540§ 13.43±0.13 T9[5] 0.010-0.025 16.52 J[48] 07h 22m 27.3s –05° 40′ 30″ 242.8±2.4[49] [50]
Wolf 1061 (Gliese 628, BD−12°4523) 14.0458±0.0038 M3.0V[5] 0.294 10.07 11.93 16h 30m 18.1s −12° 39′ 45″ 232.210±0.063[7] three planets (b, c, and d) (2015)[51]
Wolf 424
(FL Virginis, LHS 333, Gliese 473)
Wolf 424 A 14.05±0.26 M5.5Ve 0.143 13.18 14.97 12h 33m 17.2s +09° 01′ 15″ 232.2±4.3[52] flare stars
Wolf 424 B M7Ve 0.131 13.17 14.96
Van Maanen's star (Gliese 35, LHS 7)white dwarf 14.0744±0.0023 DZ7[5] 0.67 12.38 14.21 00h 49m 09.9s +05° 23′ 19″ 231.737±0.038[7] closest-known free-floating white dwarf,
third-known white dwarf
possible debris disk (1917),
possible planet (b) (2004) (debated)
Gliese 1 (CD−37°15492) 14.1725±0.0037 M1.5 V[5] 0.45-0.48 8.55 10.35 00h 05m 24.4s −37° 21′ 27″ 230.133±0.060[7]
L 1159-16 (TZ Arietis, Gliese 83.1) 14.5843±0.0070 M4.5V[5] 0.14 12.27 14.03 02h 00m 13.2s +13° 03′ 08″ 223.63±0.11[7] flare star, has two known planets (b and c) and one candidate (d)[14]
Gliese 674 (LHS 449) 14.8387±0.0033 M3.0V[5] 0.35 9.38 11.09 17h 28m 39.9s −46° 53′ 43″ 219.801±0.049[7] one planet (b) (2007)[53]
Gliese 687 (LHS 450, BD+68°946) 14.8401±0.0022 M3.0V[5] 0.401 9.17 10.89 17h 36m 25.9s +68° 20′ 21″ 219.781±0.032[7] possible flare star, two planets (b) (2014)[54] and (c) (2020)[55]
LHS 292 (LP 731-58) 14.885±0.011 M6.5V[5] 0.08 15.60 17.32 10h 48m 12.6s −11° 20′ 14″ 219.12±0.16[7] flare star
LP 145-141 (WD 1142-645, Gliese 440)white dwarf 15.1182±0.0023 DQ6[5] 0.75 11.50 13.18 11h 45m 42.9s −64° 50′ 29″ 215.737±0.032[7]
Gliese 1245 G 208-44 A

(Gliese 1245 A)

15.2090±0.0050 M5.5V[5] 0.11 13.46 15.17 19h 53m 54.2s +44° 24′ 55″ 214.45±0.07[7] flare stars
G 208-45

(Gliese 1245 B)

M6.0V[5] 0.10 14.01 15.72 19h 53m 55.2s +44° 24′ 56″
G 208-44 B

(Gliese 1245 C)

M5.5 0.07 16.75 18.46 19h 53m 54.2s +44° 24′ 55″
WISE 1741+2553§ 15.2±0.2 T9 16.53 J 18.18 J 17h 41m 24.2s +25° 53′ 19″ 214±2.8[21]
Gliese 876 (Ross 780) 15.2504±0.0054 M3.5V[5] 0.37 10.17 11.81 22h 53m 16.7s −14° 15′ 49″ 213.867±0.076[7] four planets (d (2005), c (2001), b (1998), and e (2010))[56]
two possible planets (f and g) (2014) (debated)
WISE 1639-6847§ 15.45±0.04 Y0.5 20.57 J 22.10 J 16h 39m 40.9s −68° 47′ 46″ 211.11±0.56[57]
LHS 288 (Luyten 143-23) 15.7703±0.0056 M5.5V[5] 0.11[5] 13.90 15.51 10h 44m 21.2s −61° 12′ 36″ 206.817±0.074[7] one tentative planet (b) (2007)[35]
Gliese 1002 15.8164±0.0098 M5.5V[5] 0.11 13.76 15.40 00h 06m 43.8s −07° 32′ 22″ 206.21±0.13[7]
Groombridge 1618 (Gliese 380) 15.8797±0.0026 K7.0V[5] 0.67 6.59 8.16 10h 11m 22.1s +49° 27′ 15″ 205.392±0.034[7] brightest single red dwarf in night sky, flare star, one suspected debris disk,
one suspected planet (b) (1989) (tentative)
DEN 0255-4700§ 15.885±0.020 L7.5V[5] 0.025-0.065 22.92 24.44 02h 55m 03.7s −47° 00′ 52″ 205.33±0.25[7] [47]
Gliese 412 Gliese 412 A 15.983±0.013 M1.0V[5] 0.48 8.77 10.34 11h 05m 28.6s +43° 31′ 36″ 204.06±0.17[7]
Gliese 412 B (WX Ursae Majoris) M5.5V[5] 0.10 14.48 16.05 11h 05m 30.4s +43° 31′ 18″ flare star
Gliese 832 16.1939±0.0034 M1.5 V[5] 0.45 8.66 10.20 21h 33m 34.0s −49° 00′ 32″ 201.407±0.043[7] possible flare star, two planets (b (2008) and c (2014))[58][59]
AD Leonis 16.1970±0.0055 M3.0V[5] 0.39-0.42 9.32 10.87 10h 19m 36.4s +19° 52′ 10″ 201.368±0.068[7] flare star, 1 refuted planet (b[14] in 2020)[60]
40 Eridani Keid

(40 Eridani A)

16.26±0.02 K0.5V 0.84 4.43# 5.93 04h 15m 16.3s −07° 39′ 10″ 200.62±0.23 one planet (Ab) (2018)[61]
Gliese 1005 Gliese 1005 A 16.26±0.76[note 2] M4V[62] 0.179 11.48[62] 12.70 00h 15m 28.11s −16° 08′ 01.6″ 200.5±9.4[62]
Gliese 1005 B M7V 0.112 ? 15.12
System Star or (sub-) brown dwarf Distance[6]
(Light-years (±err))
Stellar
class
Apparent Absolute Right ascension[5] Declination[5] Parallax
(mas (±err))

[5][note 1]
Notes and Additional
references
Designation Magnitude (mV[5] or mJ) Epoch J2000.0

Distant future and past encounters[edit]

Graph of the distances of various stars from the Sun during the past 20,000 to future 80,000 years.
Distances of the nearest stars from 20,000 years ago until 80,000 years in the future

Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astrometric measurements of parallax and total proper motions, along with spectroscopically determined radial velocities. Although predictions can be extrapolated back into the past or forward into the future, they are subject to increasing significant cumulative errors over very long periods.[4] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[63]

One of the first stars known to approach the Sun particularly close is Gliese 710. The star, whose mass is roughly half that of the Sun, is currently 62 light-years from the Solar System. It was first noticed in 1999 using data from the Hipparcos satellite, and was estimated to pass less than 1.3 light-years (0.40 pc) from the Sun in 1.4 million years.[64] With the release of Gaia's observations of the star, it has since been refined to a much closer 0.178 light-years (0.055 pc), close enough to significantly disturb objects in the Oort cloud, which extends out to 1.2 light-years (0.37 pc) from the Sun.[65]

The second-closest object known to approach the Sun was only discovered in 2018 after Gaia's second data release, known as 2MASS J0610-4246. Its approach has not been fully described due to it being a distant binary star with a red dwarf, but almost certainly passed less than 1 light-year from the Solar System roughly 1.16 million years ago.

Stars that are known to have passed or will pass within 5 light-years of the Sun in the past or future[66][67]
Star name HIP
number
Minimum distance
(light-years)
Date of approach
in thousands of years
Current distance
(light-years)
Stellar
classification
Mass in M Current
apparent magnitude
Current Constellation Current
Right ascension
Current
Declination
Gliese 710 89825 0.166+0.014
−0.013
1286+41
−38
62.248±0.020 K7V 0.4–0.6 9.6 Serpens 18h 19m 50.843s −01° 56′ 18.98″
HD 7977 N/A 0.483+0.109
−0.081
−2795+43
−44
246.74±0.60 G0V ~1.2 9.04 Cassiopeia 01h 20m 31.597s +61° 52′ 57.08″
Scholz's star and companion brown dwarf N/A 0.82+0.37
−0.22
−78.5±0.7 22.2±0.2 A: M9V
B: T5
A: 0.095
B: 0.063
18.3 Monoceros 07h 20m 03.20s −08° 46′ 51.2″
2MASS J2146+3813 N/A 1.56+0.13
−0.11
71.6+5.8
−5.0
22.9858±0.0034 M5V ~0.15 10.82 Cygnus 21h 46m 22.285s +38° 13′ 03.12″
CD-69 2001 N/A 1.614+0.071
−0.070
−1905±12 332.61±0.55 K4V 0.61 11.13 Indus 21h 40m 31.514s −69° 25′ 14.58″
2MASS J0621-0101 N/A 1.69+0.47
−0.40
−3179+95
−99
428.8±3.1 G5V 0.96 11.9 Orion 06h 21m 34.807s −01° 01′ 55.01″
HD 49995 N/A 1.79+0.24
−0.21
−4200+160
−170
439.74±0.59 A: F3V
B: M1V
A: 1.48
B: 0.49
8.78 Canis Major 06h 50m 20.810s −18° 37′ 30.58″
2MASS J0634-7449 N/A 2.043+0.043
−0.042
−894±12 212.41±0.15 mid K ~0.6 12.69 Mensa 06h 34m 29.385s −74° 49′ 47.12″
UCAC2 15719371 N/A 2.44+0.12
−0.11
−4239+90
−93
280.80±0.26 K4V 0.66 12.58 Antlia 09h 44m 09.884s −37° 45′ 31.09″
TYC 1662-1962-1 N/A 2.615+0.066
−0.064
−1524±15 286.51±0.40 Early K ~0.8 10.95 Vulpecula 21h 14m 32.911s +21° 53′ 32.76″
BD-21 1529 N/A 2.699+0.063
−0.062
−1659+8.7
−8.8
368.48±0.56 G5V ~0.95 9.67 Canis Major 06h 37m 48.004s −21° 22′ 21.94″
2MASS J0409+0245 N/A 2.756+0.055
−0.054
914±12 101.570±0.086 Early M ~0.4 11.73 Taurus 04h 09m 02.050s +02° 45′ 38.32″
Gliese 3649 N/A 2.954+0.077
−0.073
−510±12 54.435±0.023 M1 0.49 10.85 Leo 11h 12m 38.97s +18° 56′ 05.4″
2MASS J1921-1244 N/A 2.98+0.32
−0.27
−3370+220
−250
376.46±0.73 K6V 0.69 12.46 Sagittarius 19h 21m 58.124s −12° 43′ 58.61″
Ross 248 N/A 3.02763±0.00096 38.3166±0.0073 10.3057±0.0014 M6V 0.136 12.29 Andromeda 23h 41m 54.99s +44° 10′ 40.8″
Proxima Centauri 70890 3.1062±0.0024 28.673±0.042 4.24646±0.00028 M5Ve 0.15 11.05 Centaurus 14h 29m 42.949s −62° 40′ 46.14″
TYC 9387-2515-1 N/A 3.198+0.082
−0.081
−1498.7+9.6
−9.8
401.96±0.54 K1V 0.86 11.45 Mensa 06h 18m 54.643s −80° 19′ 16.54″
Alpha Centauri AB A: 71683
B: 71685
3.242±0.060 29.63+1.00
−0.98
4.321±0.024 A: G2V
B: K1V
A: 1.100
B: 0.907[68]
A: -0.01
B: +1.33
Centaurus 14h 39m 36.495s −60° 50′ 02.31″
2MASS J1638-6355 N/A 3.34+0.32
−0.30
−1417+32
−33
468.5±4.2 K2V 0.82 12.44 Triangulum Australe 16h 38m 21.759s −63° 55′ 13.16″
HIP 117795 117795 3.4135±0.0054 93.277±0.097 87.166±0.031 K8V ~0.5 10.6 Cassiopeia 23h 53m 20.014s +59° 56′ 42.95″
Gliese 445 57544 3.44376±0.00086 46.1489±0.0056 17.1368±0.0017 M4 0.15? 10.8 Camelopardalis 11h 47m 41.377s +78° 41′ 28.18″
2MASS J0542+3217 N/A 3.52+0.89
−0.82
6040+220
−200
884.6±2.4 A: G4V
B: K0V
A: 1.01
B: 0.85
12.80 Auriga 05h 42m 38.349s +32° 17′ 29.85″
2MASS J0625-2408 N/A 3.636+0.102
−0.099
−1841+24
−25
534.88±0.93 K/M ~0.5 12.91 Canis Major 06h 25m 42.744s −24° 08′ 35.02″
Barnard's Star 87937 3.77059±0.00046 11.7374±0.0013 5.96290±0.00044 sdM4 0.144 9.54 Ophiuchus 17h 57m 48.498s +04° 41′ 36.25″
BD+05 1792 N/A 3.957+0.043
−0.042
−960.6+3.6
−3.7
239.73±0.33 G2V 1.07 8.58 Gemini 07h 48m 07.037s +05° 27′ 22.51″
2MASS J2241-2759 N/A 4.01±0.16 −2784+41
−42
411.06±0.76 K7V ~0.5 12.28 Piscis Austrinus 22h 41m 50.996s −27° 59′ 47.04″
StKM 1-554 N/A 4.191+0.047
−0.046
−546.5+4.4
−4.5
151.97±0.19 M0V 0.65 12.17 Orion 05h 14m 01.871s +05° 22′ 56.26″
Gliese 3379 N/A 4.1915±0.0023 −156.190±0.051 16.9861±0.0027 M3.5V 0.19 11.31 Orion 06h 00m 03.824s +02° 42′ 22.97″
2MASS J1724-0522 N/A 4.24+0.44
−0.40
3120+170
−160
489.5±1.3 K0V 0.86 12.73 Ophiuchus 17h 24m 55.056s −05° 22′ 11.45″
2MASS J1936+3627 N/A 4.28+0.64
−0.59
3880+130
−120
671.6±3.4 G5.5V 0.95 12.2 Cygnus 19h 36m 57.294s +36° 27′ 57.71″
2MASS J0710+5228 N/A 4.325+0.074
−0.072
510.1+7.9
−7.7
90.949±0.050 M3V 0.33 12.52 Lynx 07h 10m 52.167s +52° 28′ 18.49″
StKM 1-1456 N/A 4.330+0.060
−0.059
1219±11 144.934±0.095 A: K5V
B: M8V
A: 0.81
B: 0.09
10.58 Hercules 17h 17m 31.118s +15° 34′ 55.35″
HD 146248 N/A 4.345+0.054
−0.053
−1142.5+7.3
−7.4
334.87±0.47 G2/3IV 1.23 9.47 Triangulum Australe 16h 19m 27.875s −64° 50′ 34.38″
Zeta Leporis 27288 4.43+0.33
−0.30
−878+42
−46
72.81±0.40 A2Vann 2.0 3.55 Lepus 05h 46m 57.341s −14° 49′ 19.02″
HD 68814 40317 4.668+0.086
−0.085
−2213±11 259.85±0.30 G6V 0.98 9.57 Hydra 08h 13m 57.112s −04° 03′ 12.56″
Lalande 21185 54035 4.6965±0.0044 22.010±0.026 8.30437±0.00068 M2V 0.39 7.52 Ursa Major 11h 03m 20.194s +35° 58′ 11.55″
2MASS J1724+0355 N/A 4.74+0.16
−0.15
2130+52
−50
254.99±0.26 G8V 0.85 12.54 Ophiuchus 17h 24m 34.633s +03° 55′ 26.75″
2MASS J1941-4602 N/A 4.868+0.074
−0.072
−461.7+6.3
−6.5
66.848±0.033 M4-M6 ~0.15 12.4 Telescopium 19h 41m 53.18s −46° 02′ 31.4″
TYC 94-1074-1 N/A 5.00±0.11 −1068.2+8.3
−8.4
316.37±0.71 K4V 0.72 11.25 Taurus 04h 34m 35.456s +06° 30′ 26.18″


See also[edit]

Notes[edit]

  1. ^ a b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
  2. ^ Might not be within 5 parsecs of the Sun.

References[edit]

  1. ^ Weaver, Harold F. (1947). "The Visibility of Stars Without Optical Aid". Publications of the Astronomical Society of the Pacific. 59 (350): 232–243. Bibcode:1947PASP...59..232W. doi:10.1086/125956.
  2. ^ a b Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616 (37): A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
  3. ^ a b Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
  4. ^ a b Matthews, R. A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. 35: 1. Bibcode:1994QJRAS..35....1M.
  5. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap aq ar as at au av aw ax ay az ba bb bc bd be bf "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). 17 September 2007. Retrieved 6 November 2007.
  6. ^ a b From parallax.
  7. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao Gaia Collaboration. "Gaia DR2". gea.esac.esa.int. Retrieved 10 May 2018.
  8. ^ Drake, Nadia (12 April 2019). "A new super-Earth may orbit the star next door". National Geographic. Retrieved 21 April 2019. Video of discovery being discussed (accidentally announced?)
  9. ^ Suárez Mascareño, A.; Faria, J. P.; et al. (2020). "Revisiting Proxima with ESPRESSO". Astronomy & Astrophysics. 639: A77. arXiv:2005.12114. Bibcode:2020A&A...639A..77S. doi:10.1051/0004-6361/202037745. ISSN 0004-6361.
  10. ^ a b General Catalogue of Trigonometric Parallaxes.
  11. ^ a b Hipparcos Catalogue.
  12. ^ Söderhjelm, Staffan (1999). "Visual binary orbits and masses POST HIPPARCOS". Astronomy & Astrophysics. 341: 121. Bibcode:1999A&A...341..121S.
  13. ^ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
  14. ^ a b c d e f Tuomi, M.; el, al. (11 June 2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
  15. ^ Lubin, Jack; Robertson, Paul; Stefansson, Gudmundur; Ninan, Joe; Mahadevan, Suvrath; Endl, Michael; Ford, Eric; Wright, Jason T.; Beard, Corey; Bender, Chad; Cochran, William D.; Diddams, Scott A.; Fredrick, Connor; Halverson, Samuel; Kanodia, Shubham; Metcalf, Andrew J.; Ramsey, Lawrence; Roy, Arpita; Schwab, Christian; Terrien, Ryan (2021), Stellar Activity Manifesting at a One Year Alias Explains Barnard b as a False Positive, arXiv:2105.07005
  16. ^ a b Luhman, K. L. (2013). "Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun". The Astrophysical Journal Letters. 767 (1): L1. arXiv:1303.2401. Bibcode:2013ApJ...767L...1L. doi:10.1088/2041-8205/767/1/L1. S2CID 8419422.
  17. ^ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". Astronomy & Astrophysics. 618: A111. arXiv:1808.07835. Bibcode:2018A&A...618A.111L. doi:10.1051/0004-6361/201833626. S2CID 119540451.
  18. ^ Boffin, H. M. J.; et al. (2013). "Possible astrometric discovery of a substellar companion to the closest binary brown dwarf system WISE J104915.57-531906.1". Astronomy & Astrophysics. 561: L4. arXiv:1312.1303. Bibcode:2014A&A...561L...4B. doi:10.1051/0004-6361/201322975. S2CID 33043358.
  19. ^ Bedin L. R.; et al. (27 June 2017). "Hubble Space Telescope astrometry of the closest brown dwarf binary system - I. Overview and improved orbit". Monthly Notices of the Royal Astronomical Society. 470 (1): 1140–1155. arXiv:1706.00657. Bibcode:2017MNRAS.470.1140B. doi:10.1093/mnras/stx1177. hdl:10150/625503. S2CID 119385778. Retrieved 27 June 2017.
  20. ^ Luhman, K. L. (21 April 2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal Letters. 786 (2): L18. arXiv:1404.6501. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18. S2CID 119102654.
  21. ^ a b Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; Marocco, Federico; Cayago, Alfred J.; Smart, R. L.; Eisenhardt, Peter R.; Kuchner, Marc J. (2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 7. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. S2CID 227126954.
  22. ^ Davison, Cassy L.; et al. (19 February 2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal. 149 (3): 106. arXiv:1501.05012. Bibcode:2015AJ....149..106D. doi:10.1088/0004-6256/149/3/106. ISSN 1538-3881. S2CID 9719725.
  23. ^ van Leeuwen, F. (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. ISSN 0004-6361. S2CID 18759600.
  24. ^ Janson, M.; et al. (September 2008), "A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches", Astronomy & Astrophysics, 488 (2): 771–780, arXiv:0807.0301, Bibcode:2008A&A...488..771J, doi:10.1051/0004-6361:200809984, S2CID 119113471
  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. ^ ESO. "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs" (PDF). Retrieved 15 November 2017.
  27. ^ Torres, G.; Andersen, J.; Giménez, A. (2010). "Accurate masses and radii of normal stars: modern results and applications". The Astronomy & Astrophysics Review. 18 (1–2): 67–126. arXiv:0908.2624. Bibcode:2010A&ARv..18...67T. doi:10.1007/s00159-009-0025-1. S2CID 14006009.
  28. ^ Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel". Astronomische Nachrichten (in German). 16 (5–6): 65–96. Bibcode:1838AN.....16...65B. doi:10.1002/asna.18390160502. (page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist A parallax of 313.6 mas yields a distance of 10.4 light years
  29. ^ Kervella, Pierre; Arenou, Frédéric; et al. (2019). "Stellar and substellar companions of nearby stars from Gaia DR2". Astronomy & Astrophysics. 623. doi:10.1051/0004-6361/201834371. S2CID 119491061. This PMa offset between 61 Cyg A and B points at the possible presence of a third body in the system, likely orbiting around 61 Cyg B.
  30. ^ Bailer-Jones, C. A. L.; et al. (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): 51. arXiv:1408.5645. Bibcode:2014ApJ...794...51H. doi:10.1088/0004-637X/794/1/51. S2CID 17361592.
  31. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2018). "Detection of the closest Jovian exoplanet in the Epsilon Indi triple system". arXiv:1803.08163 [astro-ph.EP].
  32. ^ a b c Chris Gelino, Davy Kirkpatrick, Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Retrieved 10 June 2012.CS1 maint: multiple names: authors list (link) (main page)
  33. ^ 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. (13 August 2019). "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. arXiv:1908.04717. doi:10.1093/mnras/staa248. S2CID 199551874.
  34. ^ Henry, Todd J.; Ianna, Philip A.; Kirkpatrick, J. Davy; Jahreiss, Hartmut (July 1997). "The solar neighborhood IV: discovery of the twentieth nearest star". The Astronomical Journal. 114 (1): 388–395. Bibcode:1997AJ....114..388H. doi:10.1086/118482.
  35. ^ a b c d Henry, Todd J.; Jao, Wei-Chun; Subasavage, John P.; Beaulieu, Thomas D.; Ianna, Philip A.; Costa, Edgardo; Méndez, René A. (December 2006). "The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample". The Astronomical Journal. 132 (6): 2360–2371. arXiv:astro-ph/0608230. Bibcode:2006AJ....132.2360H. doi:10.1086/508233. S2CID 15002841.
  36. ^ Astudillo-Defru, Nicola; Díaz, Rodrigo F.; Bonfils, Xavier; Almenara, José M.; Delisle, Jean-Baptiste; Bouchy, François; Delfosse, Xavier; Forveille, Thierry; Lovis, Christophe; Mayor, Michel; Murgas, Felipe; Pepe, Francesco; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Wünsche, Anaël (2017). "The HARPS search for southern extra-solar planets. XLII. A system of Earth-mass planets around the nearby M dwarf YZ Ceti". Astronomy & Astrophysics. 605: L11. arXiv:1708.03336. Bibcode:2017A&A...605L..11A. doi:10.1051/0004-6361/201731581. S2CID 119393757.
  37. ^ Gatewood, George (1 July 2008). "Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions". The Astronomical Journal. 136 (1): 452–460. Bibcode:2008AJ....136..452G. doi:10.1088/0004-6256/136/1/452.
  38. ^ 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.
  39. ^ Pozuelos, Francisco J.; et al. (2020). "GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec". Astronomy & Astrophysics. 641: A23. arXiv:2006.09403. Bibcode:2020A&A...641A..23P. doi:10.1051/0004-6361/202038047. S2CID 219721292.
  40. ^ Barnes, J. R.; et al. (2012). "ROPS: A New Search for Habitable Earths in the Southern Sky". Monthly Notices of the Royal Astronomical Society. 424 (1): 591–604. arXiv:1204.6283. Bibcode:2012MNRAS.424..591B. doi:10.1111/j.1365-2966.2012.21236.x.
  41. ^ "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF).
  42. ^ 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.
  43. ^ Anglada-Escude, G.; et al. (2014). "Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf". Monthly Notices of the Royal Astronomical Society: Letters. 443: L89–L93. arXiv:1406.0818. Bibcode:2014MNRAS.443L..89A. doi:10.1093/mnrasl/slu076. hdl:2299/19219. S2CID 67807856.
  44. ^ 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.
  45. ^ Kasper, M.; Biller, B. A.; Burrows, A.; Brandner, W.; Budaj, J.; Close, L. M. (2007). "The very nearby M/T dwarf binary SCR 1845-6357". Astronomy & Astrophysics. 471 (2): 655. arXiv:0706.3824. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881. S2CID 1860702.
  46. ^ Jao, Wei-Chun; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer L.; Costa, Edgardo; Méndez, René A. (2005). "The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr−1 (MOTION Sample)". The Astronomical Journal. 129 (4): 1954. arXiv:astro-ph/0502167. Bibcode:2005AJ....129.1954J. doi:10.1086/428489. S2CID 16164903.
  47. ^ a b Costa, Edgardo; Méndez, René A.; Jao, W. -C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer (2005). "The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation-First Results from the 1.5 m Telescope Program". The Astronomical Journal. 130 (1): 337. Bibcode:2005AJ....130..337C. doi:10.1086/430473.
  48. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (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. arXiv:1004.0317. Bibcode:2010MNRAS.408L..56L. doi:10.1111/j.1745-3933.2010.00927.x. S2CID 16032606.
  49. ^ Leggett, Sandy K.; Saumon, Didier; Marley, Mark S.; Lodders, Katharina; Canty, J.; Lucas, Philip W.; Smart, Richard L.; Tinney, Chris G.; Homeier, Derek; Allard, France; Burningham, Ben; Day-Jones, Avril; Fegley, Bruce; Ishii, Miki; Jones, Hugh R. A.; Marocco, Federico; Pinfield, David J.; Tamura, Motohide (2012). "The Properties of the 500 K Dwarf UGPS J072227.51-054031.2 and a Study of the Far-red Flux of Cold Brown Dwarfs". The Astrophysical Journal. 748 (2): 74. arXiv:1201.2973. Bibcode:2012ApJ...748...74L. doi:10.1088/0004-637X/748/2/74. S2CID 14171934.
  50. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2010). "Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System". arXiv:1004.0317v1 [astro-ph.SR].
  51. ^ "Nearby star hosts closest alien planet in the 'habitable zone'". Phys.org. 16 December 2015. Retrieved 16 December 2015. The planet, more than four times the mass of the Earth, is one of three that the team detected around a red dwarf star called Wolf 1061.
  52. ^ Gliese, W. and Jahreiß, H. (1991). "Gl 473". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 10 May 2018.CS1 maint: multiple names: authors list (link)
  53. ^ "The Extrasolar Planet Encyclopaedia — Catalog Listing".
  54. ^ The Lick–Carnegie exoplanet survey: Gliese 687 b: A Neptune-mass planet orbiting a nearby red dwarf Archived March 27, 2014, at the Wayback Machine
  55. ^ Feng, Fabo; Shectman, Stephen A.; Clement, Matthew S.; Vogt, Steven S.; Tuomi, Mikko; Teske, Johanna K.; Burt, Jennifer; Crane, Jeffrey D.; Holden, Bradford; Sharon Xuesong Wang; Thompson, Ian B.; Diaz, Matias R.; Paul Butler, R. (2020), Search for Nearby Earth Analogs. III. Detection of ten new planets, three planet candidates, and confirmation of three planets around eleven nearby M dwarfs, arXiv:2008.07998, doi:10.3847/1538-4365/abb139, S2CID 221150644 Accepted for publication by ApJS
  56. ^ Rivera, Eugenio J.; et al. (July 2010). "The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration". The Astrophysical Journal. 719 (1): 890–899. arXiv:1006.4244. Bibcode:2010ApJ...719..890R. doi:10.1088/0004-637X/719/1/890. S2CID 118707953.
  57. ^ Fontanive, C.; Bedin, L. R.; Bardalez Gagliuffi, D. C. (1 February 2021). "The Y dwarf population with HST: unlocking the secrets of our coolest neighbours - I. Overview and first astrometric results". Monthly Notices of the Royal Astronomical Society. 501 (1): 911–915. arXiv:2011.13873. Bibcode:2021MNRAS.501..911F. doi:10.1093/mnras/staa3732. ISSN 0035-8711.
  58. ^ Bailey, Jeremy; et al. (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal. 690 (1): 743–747. arXiv:0809.0172. Bibcode:2009ApJ...690..743B. doi:10.1088/0004-637X/690/1/743. S2CID 17172233.
  59. ^ Wittenmyer, R. A.; Tuomi; et al. (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal. 791 (2): 114. arXiv:1406.5587. Bibcode:2014ApJ...791..114W. doi:10.1088/0004-637X/791/2/114. S2CID 12157837.
  60. ^ Carleo, I.; et al. (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 Leo b". Astronomy & Astrophysics. A5: 638. arXiv:2002.10562. Bibcode:2020A&A...638A...5C. doi:10.1051/0004-6361/201937369. S2CID 211296466.
  61. ^ Ma, Bo; et al. (19 July 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. doi:10.1093/mnras/sty1933. eISSN 1365-2966. ISSN 0035-8711.
  62. ^ a b c "G 158-50 - SIMBAD". SIMBAD. Retrieved 12 September 2015.
  63. ^ See also: Stellar kinematics.
  64. ^ García-Sánchez, Joan; Preston, Robert A.; Jones, Dayton L.; Weissman, Paul R.; Lestrade, Jean-François; Latham, David W.; Stefanik, Robert P. (February 1999). "Stellar Encounters with the Oort Cloud Based on [ITAL]Hipparcos[/ITAL] Data". The Astronomical Journal. 117 (2): 1042–1055. Bibcode:1999AJ....117.1042G. doi:10.1086/300723.
  65. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (13 August 2018). "New stellar encounters discovered in the second data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
  66. ^ Table 3, Bobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System". Astronomy Letters. 36 (3): 220–226. arXiv:1003.2160. Bibcode:2010AstL...36..220B. doi:10.1134/S1063773710030060.
  67. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (19 May 2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616 (37): A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456.
  68. ^ "A Family Portrait of the Alpha Centauri System - VLT Interferometer Studies the Nearest Stars". European Southern Observatory. 15 March 2003. Retrieved 24 January 2011.

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