List of nearest stars and brown dwarfs

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Video showing the space around the nearest stars to the Sun.

The following two lists include all the known stars and brown dwarfs that are within 5.0 parsecs (16.3 light-years) of the Sun, or were/will be within 5.0 light-years (1.53 parsecs) in the astronomically near past or future. The easiest way to determine stellar distance to the Sun for these objects 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.

The first table is based on the most accurate observed parallaxes of the stars. The second table additionally lists stars that in the past have come or in the future will come within 1.5 parsecs (4.9 light-years). Determining which stars fall within the stated range 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 spectroscopic 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.[1]

There are 52 stellar systems beyond our own Solar system that currently lie within this 5 parsec distance. 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 exceed 6.5 apparent magnitude, meaning only about 12% of these objects can be observed with the naked eye.[2] Besides the Sun, only three are first-magnitude stars: Alpha Centauri, Sirius, and Procyon. All of these objects are located in the Local Bubble, a region within the Orion–Cygnus Arm of the Milky Way.

Based on the latest Gaia DR2 astrometric results released in 2018 of stars brighter than 13.8G apparent magnitude, an estimated 694 solar-like or cooler stars will possibly approach the solar system to less than 5 parsecs over the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec and another 7 within 0.5 parsecs.[3] The closest encounter to the Sun so far predicted is the low mass orange K7 spectral type star Gliese 710 / HIP 89825.[4] Minimum perihelion distance is 0.0676±0.0157 parsecs or 13900±3200 AU about 1.281 million years from now.[3] This is easily within the predicted maximum size of the Oort cloud,[3] whose approach will likely be disruptive enough to affect the orbits of cometary bodies.[4]

List[edit]

Stars visible to the unaided eye have their magnitude shown in light blue below. Brown dwarfs are shown with their designations in brown. White dwarfs are shown with their designation in beige. 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]

Nearest star systems
Designation Distance[6]
(light-years (±err))
Stellar class Apparent magnitude (mV or mJ) Absolute magnitude (MV 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[5] 4.85[5] eight planets
Alpha Centauri
(Rigil Kentaurus)
Proxima Centauri (V645 Centauri) 4.2441±0.0011 M5.5Ve 11.09[5] 15.53[5] 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[5] 4.38[5] 14h 39m 36.5s −60° 50′ 02″ 747.23±1.17
[8][9][10]
α Centauri B (HD 128621) K1V[5] 1.34[5] 5.71[5] 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[5] 13.22[5] 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)
Luhman 16A 6.5049±0.0012 L8±1[12] 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 501.398±0.093[13] 2013 one refuted planet (Ab[14] in 2017[13])
Luhman 16B T1±2[12]
WISE 0855−0714 7.26±0.13[15] Y2 25.0 J 08h 55m 10.83s −07° 14′ 42.5″ 449±8[16] 2014 sub-brown dwarf
Wolf 359 (CN Leonis) 7.856±0.031 M6.0V[5] 13.44[5] 16.55[5] 10h 56m 29.2s +07° 00′ 53″ 415.16±1.62[17] 1919 flare star
Lalande 21185 (BD+36°2147) 8.307±0.014 M2.0V[5] 7.47[5] 10.44[5] 11h 03m 20.2s +35° 58′ 12″ 392.64±0.67[18] 1801 one suspected planet (2017)[19]
Sirius
(α Canis Majoris)
Sirius A 8.659±0.010 A1V[5] −1.46[5] 1.42[5] 06h 45m 08.9s −16° 42′ 58″ 376.68±0.45[7] brightest star in the night sky
Sirius B DA2[5] 8.44[5] 11.34[5] 1844
Luyten 726-8 Luyten 726-8 A (BL Ceti) 8.791±0.012 M5.5Ve 12.54[5] 15.40[5] 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[5] 15.85[5]
Ross 154 (V1216 Sagittarii) 9.7035±0.0019 M3.5Ve 10.43[5] 13.07[5] 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[5] 14.79[5] 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[5] 6.19[5] 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)[20]
Lacaille 9352 (CD−36°15693) 10.7211±0.0016 M0.5V 7.34[5] 9.75[5] 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[5] 13.51[5] 11h 47m 44.4s +00° 48′ 16″ 296.307±0.070[7] 1925 flare star, one planet (b) (2017)[21]
EZ Aquarii
(Gliese 866, Luyten 789-6)
EZ Aquarii A 11.109±0.034 M5.0Ve 13.33[5] 15.64[5] 22h 38m 33.4s −15° 17′ 57″ 293.60±0.9[22] 1937 A & B flare stars
EZ Aquarii B M? 13.27[5] 15.58[5] -
EZ Aquarii C M? 14.03[5] 16.34[5] 1995
61 Cygni 61 Cygni A (BD+38°4343) 11.4008±0.0012 K5.0V[5] 5.21[5] 7.49[5] 21h 06m 53.9s +38° 44′ 58″ 286.08±0.03[7] 1725 B flare star, first star (besides Sun) to have measured distance[23]
possible circumstellar disk.
61 Cygni B (BD+38°4344) K7.0V[5] 6.03[5] 8.31[5] 21h 06m 55.3s +38° 44′ 31″ -
Procyon
(α Canis Minoris)
Procyon A 11.402±0.032 F5V–IV[5] 0.38[5] 2.66[5] 07h 39m 18.1s +05° 13′ 30″ 286.05±0.81
[8][9]
Procyon B DQZ[5] 10.70[5] 12.98[5] 1844
Struve 2398
(Gliese 725, BD+59°1915)
Struve 2398 A (HD 173739) 11.4880±0.0012 M3.0V[5] 8.90[5] 11.16[5] 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[5] 11.95[5] 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[5] 10.32[5] 0h 18m 22.9s +44° 01′ 23″ 280.73±0.02[7] 1813 flare star, two suspected planets (Ac, 2017) and Ab, 2014)[24]
Groombridge 34 B (GQ Andromedae) M3.5V[5] 11.06[5] 13.30[5] - flare star
DX Cancri (G 51-15) 11.6780±0.0056 M6.5Ve 14.78[5] 16.98[5] 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] 5.68[5] 01h 44m 04.1s −15° 56′ 15″ 277.52±0.52[7] 150 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[5] 6.89[5] 22h 03m 21.7s −56° 47′ 10″ 274.80±0.25[7] 1597 one planet (b) (2018)[25]
Epsilon Indi Ba T1.0V 12.3 J[26] 22h 04m 10.5s −56° 46′ 58″ 2003
Epsilon Indi Bb T6.0V 13.2 J[26] 2003
GJ 1061 (LHS 1565) 11.9803±0.0029 M5.5V[5] 13.09[5] 15.26[5] 03h 35m 59.7s −44° 30′ 45″ 272.245±0.066[7] 1995 [27][28]
YZ Ceti (LHS 138) 12.1084±0.0035 M4.5V[5] 12.02[5] 14.17[5] 01h 12m 30.6s −16° 59′ 56″ 269.363±0.078[7] 1961 flare star, three planets (b, c, and d) (2017),[29]
one suspected planet (e)
Luyten's Star (BD+05°1668) 12.199±0.036 M3.5Vn 9.86[5] 11.97[5] 07h 27m 24.5s +05° 13′ 33″ 267.36±0.79[30] 1935 two planets (b, c) (2017)[31]
Teegarden's Star (SO025300.5+165258) 12.496±0.013 M6.5V 15.14[5] 17.22[5] 02h 53m 00.9sg +16° 52′ 53″ 261.01±0.27[7] 2003 tentative radial velocity variation (2010)[28][32]
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 [28]
SCR 1845-6357 B T6[33] 13.3 J[26] 18h 45m 02.6s −63° 57′ 52″ 2006
Kapteyn's Star (CD−45°1841) 12.8294±0.0013 M1.5V[5] 8.84[5] 10.87[5] 05h 11m 40.6s −45° 01′ 06″ 254.226±0.026[7] 1898 two suspected planets (b and c) (2014)[34]
Lacaille 8760 (AX Microscopii) 12.9515±0.0029 M0.0V[5] 6.67[5] 8.69[5] 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[5] 11.76[5] 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[5] 13.38[5] 1890?
DEN 1048-3956 13.1932±0.0066 M8.5V[5] 17.39[5] 19.37[5] 10h 48m 14.7s −39° 56′ 06″ 247.22±0.12[7] 2001 [35][36]
Ross 614
(V577 Monocerotis, Gliese 234)
Ross 614A (LHS 1849) 13.424±0.049 M4.5V[5] 11.15[5] 13.09[5] 06h 29m 23.4s −02° 48′ 50″ 242.97±0.88[7] 1927 A flare star
Ross 614B (LHS 1850) M5.5V 14.23[5] 16.17[5] 1936
UGPS J0722-0540 13.43±0.13 T9[5] 16.52 J[37] 07h 22m 27.3s –05° 40′ 30″ 242.8±2.4[38] 2010 [39]
Wolf 1061 (Gliese 628, BD−12°4523) 14.0458±0.0038 M3.0V[5] 10.07[5] 11.93[5] 16h 30m 18.1s −12° 39′ 45″ 232.210±0.063[7] 1919 three planets (b, c, and d) (2015)[40]
Wolf 424
(FL Virginis, LHS 333, Gliese 473)
Wolf 424 A 14.05±0.26 M5.5Ve 13.18[5] 14.97[5] 12h 33m 17.2s +09° 01′ 15″ 232.2±4.3[41] 1919 flare stars
Wolf 424 B M7Ve 13.17[5] 14.96[5] 1941
Van Maanen's star (Gliese 35, LHS 7) 14.0744±0.0023 DZ7[5] 12.38[5] 14.21[5] 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[5] 10.35[5] 00h 05m 24.4s −37° 21′ 27″ 230.133±0.060[7] 1884
L 1159-16 (TZ Arietis, Gliese 83.1) 14.5843±0.0070 M4.5V[5] 12.27[5] 14.03[5] 02h 00m 13.2s +13° 03′ 08″ 223.63±0.11[7] flare star
Gliese 674 (LHS 449) 14.8387±0.0033 M3.0V[5] 9.38[5] 11.09[5] 17h 28m 39.9s −46° 53′ 43″ 219.801±0.049[7] one planet (b) (2007)[42]
Gliese 687 (LHS 450, BD+68°946) 14.8401±0.0022 M3.0V[5] 9.17[5] 10.89[5] 17h 36m 25.9s +68° 20′ 21″ 219.781±0.032[7] possible flare star, one planet (b) (2014)[43]
LHS 292 (LP 731-58) 14.885±0.011 M6.5V[5] 15.60[5] 17.32[5] 10h 48m 12.6s −11° 20′ 14″ 219.12±0.16[7] flare star
WISE J0521+1025 15±3[note 4] T7.5[44] 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) 15.1182±0.0023 DQ6[5] 11.50[5] 13.18[5] 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[5] 15.17[5] 19h 53m 54.2s +44° 24′ 55″ 214.45±0.07[7] flare stars
G 208-45 M6.0V[5] 14.01[5] 15.72[5] 19h 53m 55.2s +44° 24′ 56″
G 208-44 B M5.5 16.75[5] 18.46[5] 19h 53m 54.2s +44° 24′ 55″
Gliese 876 (Ross 780) 15.2504±0.0054 M3.5V[5] 10.17[5] 11.81[5] 22h 53m 16.7s −14° 15′ 49″ 213.867±0.076[7] four planets (d (2005), c (2001), b (1998), and e (2010))[45]
two possible planets (f and g) (2014) (debated)
LHS 288 (Luyten 143-23) 15.7703±0.0056 M5.5V[5] 13.90[5] 15.51[5] 10h 44m 21.2s −61° 12′ 36″ 206.817±0.074[7] one tentative planet (b) (2007)[28]
GJ 1002 15.8164±0.0098 M5.5V[5] 13.76[5] 15.40[5] 00h 06m 43.8s −07° 32′ 22″ 206.21±0.13[7]
Groombridge 1618 (Gliese 380) 15.8797±0.0026 K7.0V[5] 6.59[5] 8.16[5] 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 0255-4700 15.885±0.020 L7.5V[5] 22.92[5] 24.44[5] 02h 55m 03.7s −47° 00′ 52″ 205.33±0.25[7] 1999 [36]
Gliese 412 Gliese 412 A 15.983±0.013 M1.0V[5] 8.77[5] 10.34[5] 11h 05m 28.6s +43° 31′ 36″ 204.06±0.17[7] 1850s?
Gliese 412 B (WX Ursae Majoris) M5.5V[5] 14.48[5] 16.05[5] 11h 05m 30.4s +43° 31′ 18″ 1850s? flare star
WISE 1639-6847 16.12±0.25[note 4] Y0.5 20.57 J 22.10 J 16h 39m 40.9s −68° 47′ 46″ 202.3±3.1[46] 2012
Gliese 832 16.1939±0.0034 M1.5 V[5] 8.66[5] 10.20[5] 21h 33m 34.0s −49° 00′ 32″ 201.407±0.043[7] 1910s? possible flare star, two planets (b (2008) and c (2014))[47][48]
AD Leonis 16.1970±0.0055 M3.0V[5] 9.32[5] 10.87[5] 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[49] 11.48[49] 00h 15m 28.11s −16° 08′ 01.6″ 200.5±9.4[49]
GJ 1005 B M7V ? ?
System Star # Distance[6]
Light-years (±err)
Stellar class Apparent magnitude (mV or mJ) Absolute magnitude (MV or MJ) Right ascension[5] Declination[5] Parallax[5][note 1]
mas (±err)
Discovery date Additional
references
Designation Epoch J2000.0

Maps of nearby stars[edit]

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.
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 glasses red green.svg 3D red green glasses are recommended to view this image correctly.
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[edit]

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 astromertic measurements of parallax and total proper motions, along with spectroscopic 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.[1] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[50]

Distances of the nearest stars from 20,000 years ago until 80,000 years in the future

Examples of notable predicted stellar encounters falling within 5 parsecs from the Sun appear in the list below. A summary of the more likely candidates include:

  • Scholz's star and its companion brown dwarf is thought to have passed about 52,000 astronomical units (0.25 parsecs; 0.82 light-years) from the Sun about 70,000 years ago.[51]
  • Gamma Microscopii approximately 3.8 million years ago has been predicted to approach as close as 6 light-years from the Sun. Maximum apparent magnitude possibly reached −3, being brighter than the current brightest star, Sirius.[citation needed] More recent examination of measurement errors now suggests it may or may not have passed within 5.0 parsecs.
  • Gliese 710 / HIP 89825 is the low mass orange K7 spectral type star that currently lies about 63.8 light-years (19.6 parsecs) from the Sun. Based on past and 2007 Hipparcos data,[52] was first estimated to approach just under one light year from the Sun some 1.4 million years from now to appear as a first-magnitude star roughly equal in brightness to Antares. As total proper motion of Gliese 710 is very small and a radial velocity of −119 km/s is fairly high, this suggests it is traveling at a similar and relatively close-approach trajectory to the Solar System. Gaia DR2 in 2018 now predicts the closest known encounter so far known: Minimum perihelion distance is 0.0676±0.0157 parsecs or 13900±3200 AU about 1.281 million years in the future. The Gliese 710 close approach will likely cause the greatest known gravitational perturbation on celestial objects within in the Solar System.[4]
  • Ross 248 is presently about 10.3 light-years away from the Sun and in about 31,000 years from now it may be the closest star for several millennia, with a minimum distance of 0.927 parsecs (3.02 light-years) in 36,000 years.[1]
  • Gliese 445 present distance is 17.6 light-years but in about 40,000 years it will become the closest star for a period of several thousand years.
  • HIP 85605 in 2014 was estimated to approach the Sun between 0.13 to 0.65 light-years (8,200 to 41,100 astronomical units; 0.040 to 0.199 parsecs) within the next 240,000 to 470,000 years.[53][54][55] With the release of Gaia DR2, it was determined that HIP 85605 is actually a much more distant 1790±30 light-years away, and as such will not be passing remotely close to the Sun at any point in time.
Known stars that have passed or will pass within 5.1 light-years of the Sun within ±3 million years:[52][56]
Star name HIP# Minimum distance
(light-years)
Date of approach
in kiloyears
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 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 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 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 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 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 1.89+0.18
−0.15
84.4+8.0
−6.8
22.9603±0.0083 M5V ~0.015 10.82 Cygnus 21h 46m 22.285s +38° 13′ 03.12″
2MASS J0634-7449 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 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 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 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 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 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 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 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 71683
71685
3.242±0.060 29.63+1.00
−0.98
4.321±0.024 G2V+K1V 1.100
0.907[57]
-0.01
+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 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 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 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 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[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. ^ 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. ^ a b c Might not be within 5 parsecs of the Sun.

References[edit]

  1. ^ a b c Matthews, R.A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. Royal Astronomical Society. 35: 1. Bibcode:1994QJRAS..35....1M. 
  2. ^ 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. 
  3. ^ a b c Bailer-Jones, C.A.L.; Rybizki, J,; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". arXiv:1805.07581Freely accessible [astro-ph.SR]. 
  4. ^ a b c Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018. 
  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 bg bh bi bj bk bl bm bn bo bp bq br bs bt bu bv bw bx by bz ca cb cc cd ce cf cg ch ci cj ck cl cm cn co cp cq cr cs ct cu cv cw cx cy cz da db dc dd de df dg dh di dj dk dl dm dn do dp dq dr ds dt du dv dw dx dy dz ea eb ec ed ee ef eg eh ei ej ek el em en eo ep eq er es et eu ev ew ex ey ez fa fb fc fd fe ff fg fh fi fj fk fl fm fn fo fp fq fr fs ft fu fv fw fx "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). Georgia State University. September 17, 2007. Retrieved 2007-11-06. 
  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 Gaia Collaboration. "Gaia DR2". gea.esac.esa.int. Retrieved 10 May 2018. 
  8. ^ a b General Catalogue of Trigonometric Parallaxes.
  9. ^ a b Hipparcos Catalogue.
  10. ^ Visual binary orbits and masses post Hipparcos, Staffan Söderhjelm, Astronomy and Astrophysics 341 (January 1999), pp. 121–140.
  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. ^ a b Luhman, K. L. (2013). "Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun" (PDF). The Astrophysical Journal Letters. 767: L1. arXiv:1303.2401Freely accessible. Bibcode:2013ApJ...767L...1L. doi:10.1088/2041-8205/767/1/L1. [permanent dead link]
  13. ^ a b 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:1706.00657Freely accessible. Bibcode:2017MNRAS.470.1140B. doi:10.1093/mnras/stx1177. Retrieved 27 June 2017. 
  14. ^ Boffin, H. M. J.; Pourbaix, D.; Muzic, K.; Ivanov, V. D.; Kurtev, R.; Beletsky, Y.; Mehner, A.; Berger, J. P.; Girard, J. H.; Mawet, D. (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:1312.1303Freely accessible. Bibcode:2014A&A...561L...4B. doi:10.1051/0004-6361/201322975. 
  15. ^ Luhman, K. L. (April 21, 2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal Letters. 786 (2): L18. arXiv:1404.6501Freely accessible. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18. 
  16. ^ 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:1605.06655Freely accessible. Bibcode:2016AJ....152...78L. doi:10.3847/0004-6256/152/3/78. ISSN 1538-3881. 
  17. ^ Davison, Cassy L.; White, Russel J.; Henry, Todd J.; Riedel, Adric R.; Jao, Wei-Chun; Bailey III, John I.; Quinn, Samuel N.; Cantrell, Justin R.; Subasavage, John P.; Winters, Jen G. (19 February 2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal. 149 (3): 106. arXiv:1501.05012Freely accessible. Bibcode:2015AJ....149..106D. doi:10.1088/0004-6256/149/3/106. ISSN 1538-3881. 
  18. ^ van Leeuwen, F. (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. ISSN 0004-6361. 
  19. ^ "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey". Butler et al. (2017)
  20. ^ 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 and Astrophysics, 488 (2): 771–780, arXiv:0807.0301Freely accessible, Bibcode:2008A&A...488..771J, doi:10.1051/0004-6361:200809984 
  21. ^ ESO. "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs" (PDF). Retrieved 15 November 2017. 
  22. ^ Torres, G.; Andersen, J.; Giménez, A. (7 October 2009). "Accurate masses and radii of normal stars: modern results and applications". The Astronomy and Astrophysics Review. 18 (1–2): 67–126. arXiv:0908.2624Freely accessible. Bibcode:2010A&ARv..18...67T. doi:10.1007/s00159-009-0025-1. Retrieved 10 May 2018. 
  23. ^ 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. 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
  24. ^ "The NASA-UC-UH Eta-Earth Program: IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth". Andrew W. Howard, Geoffrey W. Marcy, Debra A. Fischer, Howard Isaacson, Philip S. Muirhead, Gregory W. Henry, Tabetha S. Boyajian, Kaspar von Braun, Juliette C. Becker, Jason T. Wright, John Asher Johnson. Accessed August 26, 2014.
  25. ^ "Detection of the closest Jovian exoplanet in the Epsilon Indi triple system". Fabo Feng, Mikko Tuomi, Hugh R. A. Jones. Accessed 21 March 2018.
  26. ^ a b c 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)
  27. ^ 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. 
  28. ^ 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/0608230Freely accessible. Bibcode:2006AJ....132.2360H. doi:10.1086/508233. 
  29. ^ "The HARPS search for southern extra-solar planets XLII. A system of Earth-mass planets around the nearby M dwarf YZ Cet". N. Astudillo-Defru1 , R. F. Díaz, X. Bonfils , J.M. Almenara, J.-B. Delisle, F. Bouchy, X. Delfosse, T. Forveille, C. Lovis, M. Mayor, F. Murgas, F. Pepe, N. C. Santos, D. Ségransan, S. Udry, A. Wünsche (August 10, 2017).
  30. ^ 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. 
  31. ^ "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". N. Astudillo-Defru, T. Forveille, X. Bonfils, D. Ségransan, F. Bouchy, X. Delfosse, C. Lovis, M. Mayor, F. Murgas, F. Pepe, N. C. Santos, S. Udry, A. Wunsche (March 15, 2017).
  32. ^ 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:1204.6283Freely accessible. Bibcode:2012MNRAS.424..591B. doi:10.1111/j.1365-2966.2012.21236.x. 
  33. ^ The very nearby M/T dwarf binary SCR 1845-6357, Markus Kasper, Beth A. Biller, Adam Burrows, Wolfgang Brandner, Jano Budaj, and Laird M. Close, Astronomy and Astrophysics 471, #2 (August 2007), pp. 655–659. doi:10.1051/0004-6361:20077881
  34. ^ Guillem Anglada-Escudé; Pamela Arriagada; Mikko Tuomi; Mathias Zechmeister; James S. Jenkins; Aviv Ofir; Stefan Dreizler; Enrico Gerlach; Chris J. Marvin; Ansgar Reiners; Sandra V. Jeffers; R. Paul Butler; Steven S. Vogt; Pedro J. Amado; Cristina Rodríguez-López; Zaira M. Berdiñas; Julian Morin; Jeff D. Crane; Stephen A. Shectman; Ian B. Thompson; Matías Díaz; Eugenio Rivera; Luis F. Sarmiento; Hugh R.A. Jones (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:1406.0818v1Freely accessible [astro-ph.EP]. Bibcode:2014MNRAS.443L..89A. doi:10.1093/mnrasl/slu076. 
  35. ^ The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr−1 (Motion sample), Wei-Chun Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, Jennifer L. Bartlett, Edgardo Costa, René A. Méndez, The Astronomical Journal 129, #4 (April 2005), pp. 1954–1967. doi:10.1086/428489
  36. ^ a b The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation—First Results from the 1.5 m Telescope Program, Edgardo Costa, René A. Méndez, W.-C. Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, and Jennifer Bartlett, The Astronomical Journal 130, #1 (July 2005), pp. 337–349. doi:10.1086/430473
  37. ^ Lucas; Tinney; Ben Burningham; Leggett; Pinfield; Richard Smart; Jones; Federico Marocco; Barber (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". arXiv:1004.0317v2Freely accessible [astro-ph.SR]. 
  38. ^ Leggett, S. K.; Saumon, D.; Marley, M. S.; Lodders, K.; Canty, J.; Lucas, P.; Smart, R. L.; Tinney, C. G.; Homeier, D.; Allard, F.; Burningham, Ben; Day-Jones, A.; Fegley, B.; Ishii, Miki; Jones, H. R. A.; Marocco, F.; Pinfield, D. J.; Tamura, M. (1 April 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:1201.2973Freely accessible. Bibcode:2012ApJ...748...74L. doi:10.1088/0004-637X/748/2/74. ISSN 0004-637X. 
  39. ^ Lucas, Philip W.; Tinney; Burningham; Leggett; Pinfield; Smart; et al. (2010). "Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System". arXiv:1004.0317v1Freely accessible [astro-ph.SR]. 
  40. ^ "Nearby star hosts closest alien planet in the 'habitable zone'". Phys.org. December 16, 2015. Retrieved 2015-12-16. 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. 
  41. ^ Gliese, W. and Jahreiß, H. (1991). "Gl 473". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 10 May 2018. 
  42. ^ "The Extrasolar Planet Encyclopaedia — Catalog Listing". 
  43. ^ 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.
  44. ^ Bihain, G.; Scholz, R.-D.; Storm, J.; Schnurr, O. (26 August 2013). "An overlooked brown dwarf neighbour (T7.5 at ~ 5 pc) of the Sun and two additional T dwarfs at about 10 pc". Astronomy & Astrophysics. 557: A43. arXiv:1307.2722Freely accessible. Bibcode:2013A&A...557A..43B. doi:10.1051/0004-6361/201322141. 
  45. ^ 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:1006.4244Freely accessible. Bibcode:2010ApJ...719..890R. doi:10.1088/0004-637X/719/1/890. 
  46. ^ Tinney, C. G.; Faherty, Jacqueline K.; Kirkpatrick, J. Davy; Cushing, Mike; Morley, Caroline V.; Wright, Edward L. (4 November 2014). "THE LUMINOSITIES OF THE COLDEST BROWN DWARFS". The Astrophysical Journal. 796 (1): 39. arXiv:1410.0746Freely accessible. Bibcode:2014ApJ...796...39T. doi:10.1088/0004-637X/796/1/39. ISSN 1538-4357. 
  47. ^ Bailey, Jeremy; et al. (2008). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal. 690 (1): 743–747. arXiv:0809.0172Freely accessible. Bibcode:2009ApJ...690..743B. doi:10.1088/0004-637X/690/1/743. 
  48. ^ Wittenmyer, R. A.; Tuomi, Mikko; Butler, R. P.; Jones, H. R. A.; Anglada-Escude, Guillem; Horner, Jonathan; Tinney, C. G.; Marshall, J. P.; Carter, B. D.; Bailey, J.; Salter, G. S.; O'Toole, S. J.; Wright, D.; Crane, J. D.; Schectman, S. A.; Arriagada, P.; Thompson, I.; Minniti, D.; Jenkins, J. S.; Diaz, M. (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal. 791 (2): 114. arXiv:1406.5587Freely accessible. Bibcode:2014ApJ...791..114W. doi:10.1088/0004-637X/791/2/114. 
  49. ^ a b c "G 158-50 - SIMBAD". SIMBAD. Retrieved 2015-09-12. 
  50. ^ See also: Stellar kinematics.
  51. ^ "Featured Research: Closest known flyby of star to our solar system: Dim star passed through Oort Cloud 70,000 years ago". Science Daily. February 17, 2015. Retrieved 2015-02-21. 
  52. ^ a b Table 3, Bobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System". Astronomy Letters. 36 (3): 220–226. arXiv:1003.2160Freely accessible. Bibcode:2010AstL...36..220B. doi:10.1134/S1063773710030060. 
  53. ^ Coryn A.L. Bailer-Jones (Dec 11, 2014). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: A35. arXiv:1412.3648Freely accessible. Bibcode:2014yCat..35750035B. doi:10.1051/0004-6361/201425221. 
  54. ^ Mamajek, Eric E.; Barenfeld, Scott A.; Ivanov, Valentin D. (2015). "The Closest Known Flyby of a Star to the Solar System". The Astrophysical Journal. 800 (1): L17. arXiv:1502.04655Freely accessible. Bibcode:2015ApJ...800L..17M. doi:10.1088/2041-8205/800/1/L17. 
  55. ^ Coryn Bailer-Jones (2015-01-01). "The closest encounter is Hip 85605. How reliable is this?". Retrieved 2015-01-05. 
  56. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (19 May 2018). "New stellar encounters discovered in the second Gaia data release". Retrieved 23 May 2018. 
  57. ^ A Family Portrait of the Alpha Centauri System (eso0307), European Southern Observatory. 15 March 2003. Accessed online 24 January 2011.

External links[edit]