List of nearest stars and brown dwarfs

There are 52 stellar systems beyond our own Solar system that currently lie within 5.0 parsecs (16.3 light-years) of the Sun. These systems contain a total of 63 stars, of which 50 are red dwarfs, by far the most common type of star in the Milky Way. Much more massive stars, such as our own, make up the remaining 13. In addition to these "true" stars, there are 11 brown dwarfs (objects not quite massive enough to fuse hydrogen), and 4 white dwarfs (extremely dense objects that remain after stars such as our Sun exhaust all fusable hydrogen in their core and slowly shed their outer layers while only the collapsed core remains). Despite the relative proximity of these objects to Earth, only nine (not including the Sun) are brighter than 6.5 apparent magnitude, the dimmest magnitude visible to the naked eye from Earth.[1] All of these objects are located in the Local Bubble, a region within the Orion–Cygnus Arm of the Milky Way.

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 5.0 parsecs (16 light-years) over 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 our 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

Key
# Visible to the unaided eye
brown dwarf 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 colors. Some of the parallax and distance results are preliminary measurements.[5]

Known star systems within 5.0 parsecs (16.3 light-years)
Designation Distance[6]
(light-years (±err))		 Stellar class Apparent magnitude
(mV[5] or mJ)		 Absolute magnitude
(MV[5] or MJ)		 Epoch J2000.0 Parallax
(mas (±err))
[5][note 1]		 Discovery
date
[note 2]		 Notes and additional
references
System Star Right ascension[5] Declination[5]
Solar System Sun 0 G2V[5] −26.74# 4.85 N/A N/A N/A N/A eight planets
Alpha Centauri
(Rigil Kentaurus)		 Proxima Centauri (V645 Centauri) 4.2441±0.0011 M5.5Ve 11.09 15.53 14h 29m 43.0s −62° 40′ 46″ 768.50±0.20[7] 1915 flare star, one planet (b) (2016)
α Centauri A (HD 128620) 4.3650±0.0068 G2V[5] 0.01# 4.38 14h 39m 36.5s −60° 50′ 02″ 747.23±1.17
[8][9][10]		 N/A
α Centauri B (HD 128621) K1V[5] 1.34# 5.71 14h 39m 35.1s −60° 50′ 14″ 1689 one suspected planet (c) (2013)
(planet b refuted in 2015)
Barnard's Star (BD+04°3561a) 5.9577±0.0032 M4.0Ve 9.53 13.22 17h 57m 48.5s +04° 41′ 36″ 547.45±0.29[7] 1916 flare star, largest known proper motion[11]
Luhman 16
(WISE 1049−5319)brown dwarf		 Luhman 16Abrown dwarf 6.5029±0.0011 L8±1[12] 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 501.557±0.082[13] 2013 one refuted planet (Ab[14] in 2017[15])
Luhman 16Bbrown dwarf T1±2[12]
WISE 0855−0714brown dwarf 7.26±0.13[16] Y2 25.0 J 08h 55m 10.83s −07° 14′ 42.5″ 449±8[17] 2014 sub-brown dwarf
Wolf 359 (CN Leonis) 7.856±0.031 M6.0V[5] 13.44 16.55 10h 56m 29.2s +07° 00′ 53″ 415.16±1.62[18] 1919 flare star
Lalande 21185 (BD+36°2147) 8.307±0.014 M2.0V[5] 7.47 10.44 11h 03m 20.2s +35° 58′ 12″ 392.64±0.67[19] 1801 one suspected planet (2017)[20]
Sirius
(α Canis Majoris)		 Sirius A 8.659±0.010 A1V[5] −1.46# 1.42 06h 45m 08.9s −16° 42′ 58″ 376.68±0.45[7] N/A brightest star in the night sky
Sirius Bwhite dwarf DA2[5] 8.44 11.34 1844
Luyten 726-8 Luyten 726-8 A (BL Ceti) 8.791±0.012 M5.5Ve 12.54 15.40 01h 39m 01.3s −17° 57′ 01″ 371.0±0.5[7] 1949 flare star (Archetypal member)
Luyten 726-8 B (UV Ceti) M6.0Ve 12.99 15.85
Ross 154 (V1216 Sagittarii) 9.7035±0.0019 M3.5Ve 10.43 13.07 18h 49m 49.4s −23° 50′ 10″ 336.123±0.064[7] 1925 flare star
Ross 248 (HH Andromedae) 10.2903±0.0041 M5.5Ve 12.29 14.79 23h 41m 54.7s +44° 10′ 30″ 316.96±0.13[7] 1925 flare star
Epsilon Eridani (BD−09°697) 10.446±0.016 K2V[5] 3.73# 6.19 03h 32m 55.8s −09° 27′ 30″ 312.22±0.47[7] 150 three circumstellar disks,
two suspected planets (AEgir (debated) and c) (2000 & 2002)[21]
Lacaille 9352 (CD−36°15693) 10.7211±0.0016 M0.5V 7.34 9.75 23h 05m 52.0s −35° 51′ 11″ 304.219±0.045[7] 1753
Ross 128 (FI Virginis) 11.0074±0.0026 M4.0Vn 11.13 13.51 11h 47m 44.4s +00° 48′ 16″ 296.307±0.070[7] 1925 flare star, one planet (b) (2017)[22]
EZ Aquarii
(Gliese 866, Luyten 789-6)		 EZ Aquarii A 11.109±0.034 M5.0Ve 13.33 15.64 22h 38m 33.4s −15° 17′ 57″ 293.60±0.9[23] 1937 A & B flare stars
EZ Aquarii B M? 13.27 15.58 1937
EZ Aquarii C M? 14.03 16.34 1995
61 Cygni 61 Cygni A (BD+38°4343) 11.4008±0.0012 K5.0V[5] 5.21# 7.49 21h 06m 53.9s +38° 44′ 58″ 286.08±0.03[7] N/A B flare star, first star (besides Sun) to have measured distance[24]
possible circumstellar disk.
61 Cygni B (BD+38°4344) K7.0V[5] 6.03# 8.31 21h 06m 55.3s +38° 44′ 31″ 1725
Procyon
(α Canis Minoris)		 Procyon A 11.402±0.032 F5V–IV[5] 0.38# 2.66 07h 39m 18.1s +05° 13′ 30″ 286.05±0.81
[8][9]		 N/A
Procyon Bwhite dwarf DQZ[5] 10.70 12.98 1844
Struve 2398
(Gliese 725, BD+59°1915)		 Struve 2398 A (HD 173739) 11.4880±0.0012 M3.0V[5] 8.90 11.16 18h 42m 46.7s +59° 37′ 49″ 283.91±0.03[7] 1835 flare stars
Struve 2398 B (HD 173740) M3.5V[5] 9.69 11.95 18h 42m 46.9s +59° 37′ 37″ 1835
Groombridge 34
(Gliese 15)		 Groombridge 34 A (GX Andromedae) 11.6182±0.0008 M1.5V[5] 8.08 10.32 0h 18m 22.9s +44° 01′ 23″ 280.73±0.02[7] 1813 flare star, two suspected planets (Ac, 2017) and Ab, 2014)[25]
Groombridge 34 B (GQ Andromedae) M3.5V[5] 11.06 13.30 1813 flare star
DX Cancri (G 51-15) 11.6780±0.0056 M6.5Ve 14.78 16.98 08h 29m 49.5s +26° 46′ 37″ 279.29±0.13[7] 1972 flare star
Tau Ceti (BD−16°295) 11.753±0.022 G8Vp[5] 3.49# 5.68 01h 44m 04.1s −15° 56′ 15″ 277.52±0.52[7] N/A one debris disk
two planets (e and f) (2012),
three suspected planets (d, g and h) (2012, 2017),
two refuted planets (b and c in 2017)
Epsilon Indi
(CPD−57°10015)		 Epsilon Indi A 11.869±0.011 K5Ve[5] 4.69# 6.89 22h 03m 21.7s −56° 47′ 10″ 274.80±0.25[7] N/A one planet (b) (2018)[26]
Epsilon Indi Babrown dwarf T1.0V 12.3 J[27] 22h 04m 10.5s −56° 46′ 58″ 2003
Epsilon Indi Bbbrown dwarf T6.0V 13.2 J[27] 2003
GJ 1061 (LHS 1565) 11.9803±0.0029 M5.5V[5] 13.09 15.26 03h 35m 59.7s −44° 30′ 45″ 272.245±0.066[7] 1995 [28][29]
YZ Ceti (LHS 138) 12.1084±0.0035 M4.5V[5] 12.02 14.17 01h 12m 30.6s −16° 59′ 56″ 269.363±0.078[7] 1961 flare star, three planets (b, c, and d) (2017),[30]
one suspected planet (e)
Luyten's Star (BD+05°1668) 12.199±0.036 M3.5Vn 9.86 11.97 07h 27m 24.5s +05° 13′ 33″ 267.36±0.79[31] 1935 two planets (b, c) (2017)[32]
Teegarden's Star (SO025300.5+165258) 12.496±0.013 M6.5V 15.14 17.22 02h 53m 00.9sg +16° 52′ 53″ 261.01±0.27[7] 2003 tentative radial velocity variation (2010)[29][33]
SCR 1845-6357 SCR 1845-6357 A 12.571±0.054 M8.5V[5] 17.39 19.41 18h 45m 05.3s −63° 57′ 48″ 259.45±1.11
[note 3]		 2004 [29]
SCR 1845-6357 Bbrown dwarf T6[34] 13.3 J[27] 18h 45m 02.6s −63° 57′ 52″ 2006
Kapteyn's Star (CD−45°1841) 12.8294±0.0013 M1.5V[5] 8.84 10.87 05h 11m 40.6s −45° 01′ 06″ 254.226±0.026[7] 1898 two suspected planets (b and c) (2014)[35]
Lacaille 8760 (AX Microscopii) 12.9515±0.0029 M0.0V[5] 6.67 8.69 21h 17m 15.3s −38° 52′ 03″ 251.829±0.056[7] 1753 flare star
Kruger 60
(BD+56°2783)		 Kruger 60 A 13.0724±0.0052 M3.0V[5] 9.79 11.76 22h 27m 59.5s +57° 41′ 45″ 249.5±0.1[7] 1880 B flare star
Kruger 60 B (DO Cephei) M4.0V[5] 11.41 13.38 1890?
DEN 1048-3956brown dwarf 13.1932±0.0066 M8.5V[5] 17.39 19.37 10h 48m 14.7s −39° 56′ 06″ 247.22±0.12[7] 2001 [36][37]
Ross 614
(V577 Monocerotis, Gliese 234)		 Ross 614A (LHS 1849) 13.424±0.049 M4.5V[5] 11.15 13.09 06h 29m 23.4s −02° 48′ 50″ 242.97±0.88[7] 1927 A flare star
Ross 614B (LHS 1850) M5.5V 14.23 16.17 1936
UGPS J0722-0540brown dwarf 13.43±0.13 T9[5] 16.52 J[38] 07h 22m 27.3s –05° 40′ 30″ 242.8±2.4[39] 2010 [40]
Wolf 1061 (Gliese 628, BD−12°4523) 14.0458±0.0038 M3.0V[5] 10.07 11.93 16h 30m 18.1s −12° 39′ 45″ 232.210±0.063[7] 1919 three planets (b, c, and d) (2015)[41]
Wolf 424
(FL Virginis, LHS 333, Gliese 473)		 Wolf 424 A 14.05±0.26 M5.5Ve 13.18 14.97 12h 33m 17.2s +09° 01′ 15″ 232.2±4.3[42] 1919 flare stars
Wolf 424 B M7Ve 13.17 14.96 1941
Van Maanen's star (Gliese 35, LHS 7)white dwarf 14.0744±0.0023 DZ7[5] 12.38 14.21 00h 49m 09.9s +05° 23′ 19″ 231.737±0.038[7] 1896 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] 8.55 10.35 00h 05m 24.4s −37° 21′ 27″ 230.133±0.060[7] 1884
WISE 1639-6847brown dwarf 14.30±0.56[note 4] Y0.5 20.57 J 22.10 J 16h 39m 40.9s −68° 47′ 46″ 228.1±8.9[43] 2012
L 1159-16 (TZ Arietis, Gliese 83.1) 14.5843±0.0070 M4.5V[5] 12.27 14.03 02h 00m 13.2s +13° 03′ 08″ 223.63±0.11[7] unknown flare star
Gliese 674 (LHS 449) 14.8387±0.0033 M3.0V[5] 9.38 11.09 17h 28m 39.9s −46° 53′ 43″ 219.801±0.049[7] unknown one planet (b) (2007)[44]
Gliese 687 (LHS 450, BD+68°946) 14.8401±0.0022 M3.0V[5] 9.17 10.89 17h 36m 25.9s +68° 20′ 21″ 219.781±0.032[7] unknown possible flare star, one planet (b) (2014)[45]
LHS 292 (LP 731-58) 14.885±0.011 M6.5V[5] 15.60 17.32 10h 48m 12.6s −11° 20′ 14″ 219.12±0.16[7] unknown flare star
WISE J0521+1025brown dwarf 15±3[note 4] T7.5[46] 15.26 J 16.95 J 05h 21m 26.3s +10° 25′ 28″ 217.5±40 2012 distance highly uncertain
LP 145-141 (WD 1142-645, Gliese 440)white dwarf 15.1182±0.0023 DQ6[5] 11.50 13.18 11h 45m 42.9s −64° 50′ 29″ 215.737±0.032[7] 1917
G 208-44
G 208-45
(GJ 1245)		 G 208-44 A (V1581 Cyg) 15.2090±0.0050 M5.5V[5] 13.46 15.17 19h 53m 54.2s +44° 24′ 55″ 214.45±0.07[7] unknown flare stars
G 208-45 M6.0V[5] 14.01 15.72 19h 53m 55.2s +44° 24′ 56″ unknown
G 208-44 B M5.5 16.75 18.46 19h 53m 54.2s +44° 24′ 55″ unknown
Gliese 876 (Ross 780) 15.2504±0.0054 M3.5V[5] 10.17 11.81 22h 53m 16.7s −14° 15′ 49″ 213.867±0.076[7] unknown four planets (d (2005), c (2001), b (1998), and e (2010))[47]
two possible planets (f and g) (2014) (debated)
LHS 288 (Luyten 143-23) 15.7703±0.0056 M5.5V[5] 13.90 15.51 10h 44m 21.2s −61° 12′ 36″ 206.817±0.074[7] unknown one tentative planet (b) (2007)[29]
GJ 1002 15.8164±0.0098 M5.5V[5] 13.76 15.40 00h 06m 43.8s −07° 32′ 22″ 206.21±0.13[7] unknown
Groombridge 1618 (Gliese 380) 15.8797±0.0026 K7.0V[5] 6.59 8.16 10h 11m 22.1s +49° 27′ 15″ 205.392±0.034[7] 1838 flare star, one suspected debris disk,
one suspected planet (b) (1989) (tentative)
DEN 0255-4700brown dwarf 15.885±0.020 L7.5V[5] 22.92 24.44 02h 55m 03.7s −47° 00′ 52″ 205.33±0.25[7] 1999 [37]
Gliese 412 Gliese 412 A 15.983±0.013 M1.0V[5] 8.77 10.34 11h 05m 28.6s +43° 31′ 36″ 204.06±0.17[7] 1850s?
Gliese 412 B (WX Ursae Majoris) M5.5V[5] 14.48 16.05 11h 05m 30.4s +43° 31′ 18″ 1850s? flare star
Gliese 832 16.1939±0.0034 M1.5 V[5] 8.66 10.20 21h 33m 34.0s −49° 00′ 32″ 201.407±0.043[7] 1910s? possible flare star, two planets (b (2008) and c (2014))[48][49]
AD Leonis 16.1970±0.0055 M3.0V[5] 9.32 10.87 10h 19m 36.4s +19° 52′ 10″ 201.368±0.068[7] 1850s? flare star
GJ 1005 GJ 1005 A 16.26±0.76[note 4] M4V[50] 11.48[50] 00h 15m 28.11s −16° 08′ 01.6″ 200.5±9.4[50] unknown
GJ 1005 B M7V ? ? unknown
System Star Distance[6]
(Light-years (±err))		 Stellar class Apparent magnitude
(mV[5] or mJ)		 Absolute magnitude
(MV[5] or MJ)		 Right ascension[5] Declination[5] Parallax
(mas (±err))
[5][note 1]		 Discovery
date
[note 2]		 Notes and Additional
references
Designation Epoch J2000.0

Maps of nearby stars

graph of the nearest stars within 15 light years of the Sun, projected from the equatorial plane.
This map shows all of the star systems within 14 light-years of the Sun (shown as Sol), except for brown dwarfs discovered after 2009. Double and triple stars are shown "stacked", but the true location is the star closest to the central plane. Color corresponds to the table above.
Anaglyph 3D image of the nearest stars to the Sun within 14 light years
This is a 3D map of the nearest stars using the coordinates listed above. The stars in the front have a right ascension of 18h. An animated version is available here. 3D red green glasses are recommended to view this image correctly.
The four nearest known star systems to the Sun, Proxima Centauri and Alpha Centauri, Barnard's Star, Luhman 16, and WISE 0855-0714.
The locations of the four star systems closest to the Sun. Two, a brown dwarf and a free planet were found by the WISE satellite. The year when the distance to each system was determined is listed after the system's name.

Distant future and past encounters

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.[51]

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.[52] 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.[53]

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.

Distances of the nearest stars from 20,000 years ago until 80,000 years in the future
Known stars that have passed or will pass within 5 light-years of the Sun within ±3 million years[54][55]
Star name HIP
number		 Minimum distance
(light-years)		 Date of approach
in 1000s of years		 Current distance
(light-years)		 Stellar
classification		 Mass in M☉ Current
apparent magnitude		 Current Constellation Current
Right ascension		 Current
Declination
Gliese 710 89825 0.178+0.043
−0.036		 1280+41
−39		 62.103±0.057 K7V 0.4–0.6 9.6 Serpens 18h 19m 50.843s −01° 56′ 18.98″
2MASS J0610-4246 N/A 0.755+0.084
−0.090		 −1164.4+8.8
−8.9		 319.75±0.60 early K ~0.8 11.79 Puppis 06h 10m 55.448s −42° 46′ 03.39″
Scholz's star and companion brown dwarf N/A 0.82+0.37
−0.22		 −69+10
−14		 19.6±3.4 M9+T5 0.15 18.3 Monoceros 07h 20m 03.20s −08° 46′ 51.2″
HD 283856 N/A 1.13+0.75
−0.55		 374+40
−34		 290±17 K0V (binary?) ~0.8 10.46 Taurus 04h 48m 28.124s +27° 00′ 39.06″
TYC 1662-1962-1 N/A 1.84+0.22
−0.21		 −1513+18
−19		 284.5±1.0 Early K ~0.8 10.95 Vulpecula 21h 14m 32.911s +21° 53′ 32.76″
HD 7977 N/A 1.88+0.18
−0.16		 −2798+44
−46		 247.03±0.70 G0V ~1.2 9.04 Cassiopeia 01h 20m 31.597s +61° 52′ 57.08″
2MASS J2146+3813 N/A 1.89+0.18
−0.15		 84.4+8.0
−6.8		 22.9603±0.0083 M5V ~0.15 10.82 Cygnus 21h 46m 22.285s +38° 13′ 03.12″
2MASS J0634-7449 N/A 2.169+0.083
−0.080		 −898+12
−13		 213.28±0.29 mid K ~0.6 12.69 Mensa 06h 34m 29.385s −74° 49′ 47.12″
TYC 2730-1701-1 N/A 2.31+0.31
−0.29		 −714+21
−22		 829.1±9.1 G? ~1 9.44 Pegasus 21h 50m 41.029s +36h 20m 46.73s
2MASS J0409+0245 N/A 2.684+0.088
−0.091		 912±13 101.40±0.18 Early M ~0.4 11.73 Taurus 04h 09m 02.050s +02° 45′ 38.32″
Gliese 3649 N/A 2.975+0.093
−0.089		 −509±12 54.415±0.048 M1 0.49 10.85 Leo 11h 12m 38.97s +18° 56′ 05.4″
2MASS J0605+4020 N/A 2.9+4.5
−2.1		 −860+210
−350		 248±20 K ~0.5 12.07 Auriga 06h 05m 05.077s +40° 20′ 37.72″
2MASS J1818-4038 N/A 3.0+1.3
−1.1		 1049+54
−50		 191.4±5.6 K/M ~0.5 11.97 Corona Australis 18h 18m 17.213s −40° 38′ 39.48″
BD-21 1529 N/A 3.01+0.29
−0.28		 −1685+14
−15		 374.1±1.8 G5V ~0.95 9.67 Canis Major 06h 37m 48.004s −21° 22′ 21.94″
Ross 248 N/A 3.11+0.15
−0.14		 39.2+1.9
−1.8		 10.2903±0.0041 M6V 0.136 12.29 Andromeda 23h 41m 54.99s +44° 10′ 40.8″
Proxima Centauri 70890 3.1034±0.0033 28.677±0.054 4.2441±0.0011 M5Ve 0.15 11.05 Centaurus 14h 29m 42.949s −62° 40′ 46.14″
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[56]		 A: -0.01
B: +1.33		 Centaurus 14h 39m 36.495s −60° 50′ 02.31″
Gliese 445 57544 3.3365±0.0050 46.301±0.052 17.1424±0.0043 M4 0.15? 10.8 Camelopardalis 11h 47m 41.377s +78° 41′ 28.18″
HIP 117795 117795 3.433±0.013 93.46±0.21 87.336±0.075 K8V ~0.5 10.6 Cassiopeia 23h 53m 20.014s +59° 56′ 42.95″
2MASS J0625-2408 N/A 3.59+0.25
−0.27		 −1849+30
−31		 537.1±2.7 K/M ~0.5 12.91 Canis Major 06h 25m 42.744s −24° 08′ 35.02″
Barnard's Star 87937 3.7604±0.0074 11.731±0.027 5.9577±0.0032 sdM4 0.144 9.54 Ophiuchus 17h 57m 48.498s +04° 41′ 36.25″
2MASS J2241-2759 N/A 3.79+0.67
−0.62		 −2809+53
−55		 414.7±2.6 K7V ~0.5 12.28 Piscis Austrinus 22h 41m 50.996s −27° 59′ 47.04″
Gliese 3379 N/A 4.194±0.016 −156.13±0.52 16.9813±0.0063 M3.5V 0.19 11.31 Orion 06h 00m 03.824s +02° 42′ 22.97″
Zeta Leporis 27288 4.70+0.59
−0.51		 −860+45
−49		 71.34±0.65 A2Vann 2.0 3.55 Lepus 05h 46m 57.341s −14° 49′ 19.02″
Lalande 21185 54035 4.692±0.018 22.039+0.082
−0.081		 8.307±0.014 M2V 0.39 7.52 Ursa Major 11h 03m 20.194s +35° 58′ 11.55″
2MASS J1941-4602 N/A 4.854+0.087
−0.085		 −463.7+6.5
−6.7		 66.996±0.066 M4-M6 ~0.15 12.4 Telescopium 19h 41m 53.18s −46° 02′ 31.4″

See also

Notes

  1. 1 2 Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
  2. 1 2 Before 1900: earliest certain recorded observation. 1900–1930: first catalogued. After 1930: earliest trigonometric or spectroscopic parallax.
  3. ↑ Systems with their first accurate trigonometric parallaxes measured by RECONS
  4. 1 2 3 Might not be within 5 parsecs of the Sun.

References

  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. 1 2 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.
  3. 1 2 Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
  4. 1 2 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. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). September 17, 2007. Retrieved 2007-11-06.
  6. 1 2 From parallax.
  7. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 Gaia Collaboration. "Gaia DR2". gea.esac.esa.int. Retrieved 10 May 2018.
  8. 1 2 General Catalogue of Trigonometric Parallaxes.
  9. 1 2 Hipparcos Catalogue.
  10. ↑ Söderhjelm, Staffan (1999). "Visual binary orbits and masses POST HIPPARCOS". Astronomy and Astrophysics. 341: 121. Bibcode:1999A&A...341..121S.
  11. ↑ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
  12. 1 2 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.
  13. ↑ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". arXiv:1808.07835 [astro-ph.SR].
  14. ↑ 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.
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  17. ↑ Luhman, K. L.; Esplin, T. L. (6 September 2016). "The Spectral Energy Distribution of the Coldest Known Brown Dwarf". The Astronomical Journal. 152 (3): 78. arXiv:1605.06655. Bibcode:2016AJ....152...78L. doi:10.3847/0004-6256/152/3/78. ISSN 1538-3881.
  18. ↑ 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.
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  23. ↑ Torres, G.; Andersen, J.; Giménez, A. (2010). "Accurate masses and radii of normal stars: modern results and applications". The Astronomy and Astrophysics Review. 18 (1–2): 67–126. arXiv:0908.2624. Bibcode:2010A&ARv..18...67T. doi:10.1007/s00159-009-0025-1.
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  25. ↑ 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: 51. arXiv:1408.5645. doi:10.1088/0004-637X/794/1/51.
  26. ↑ 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].
  27. 1 2 3 Chris Gelino, Davy Kirkpatrick, Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Retrieved 2012-06-10. (main page)
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  29. 1 2 3 4 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.
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  31. ↑ 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.
  32. ↑ Bailer-Jones, C. A. L.; 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 & Astrophysics. 602: A88. arXiv:1703.05386. doi:10.1051/0004-6361/201630153.
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  34. ↑ 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 and Astrophysics. 471 (2): 655. arXiv:0706.3824. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881.
  35. ↑ 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.
  36. ↑ 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. Bibcode:2005AJ....129.1954J. doi:10.1086/428489.
  37. 1 2 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.
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  51. ↑ See also: Stellar kinematics.
  52. ↑ 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. doi:10.1086/300723.
  53. ↑ 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. doi:10.1051/0004-6361/201833456.
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  • Nearest Stars 3D View
  • Table 4 "The Census of Stars and Brown Dwarfs within 8 Parsecs of the Sun" in Bailer-Jones, C. A. L.; et al. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 156. arXiv:1205.2122. doi:10.1088/0004-637X/753/2/156.
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