List of nearest stars
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
# | Visible to the unaided eye |
§ | Brown 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]
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 | 0.0000158 | 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), tentative evidence for second planet (c) (2019)[8] |
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 [9][10][11] |
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[12], one suspected planet | |
Luhman 16 (WISE 1049−5319)§ |
Luhman 16A§ | 6.5029±0.0011 | L8±1[13] | 10.7 J | 14.2 J | 10h 49m 15.57s | −53° 19′ 06″ | 501.557±0.082[14] | 2013 | one refuted planet (Ab[15] in 2017[16]) |
Luhman 16B§ | T1±2[13] | |||||||||
WISE 0855−0714§ | 7.26±0.13[17] | Y2 | 25.0 J | 08h 55m 10.83s | −07° 14′ 42.5″ | 449±8[18] | 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[19] | 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[20] | 1801 | one suspected planet (2017)[21] | |
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 B‡ | 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)[22] | |
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)[23] | |
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[24] | 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[25] 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 [9][10] |
N/A | |
Procyon B‡ | 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)[26] |
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)[27] |
Epsilon Indi Ba§ | T1.0V | 12.3 J[28] | 22h 04m 10.5s | −56° 46′ 58″ | 2003 | |||||
Epsilon Indi Bb§ | T6.0V | 13.2 J[28] | 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 | [29][30] | |
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),[31] 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[32] | 1935 | two planets (b, c) (2017)[33] | |
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)[30][34] | |
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 | [30] |
SCR 1845-6357 B§ | T6[35] | 13.3 J[28] | 18h 45m 02.6s | −63° 57′ 52″ | 2006 | |||||
Kapteyn's Star (CD−45°1841) | 12.8294±0.0013 | M1.5VI[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)[36] | |
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 1048-3956§ | 13.1932±0.0066 | M8.5V[5] | 17.39 | 19.37 | 10h 48m 14.7s | −39° 56′ 06″ | 247.22±0.12[7] | 2001 | [37][38] | |
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 J0722-0540§ | 13.43±0.13 | T9[5] | 16.52 J[39] | 07h 22m 27.3s | –05° 40′ 30″ | 242.8±2.4[40] | 2010 | [41] | ||
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)[42] | |
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[43] | 1919 | flare stars |
Wolf 424 B | M7Ve | 13.17 | 14.96 | 1941 | ||||||
Van Maanen's star (Gliese 35, LHS 7)‡ | 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 1639-6847§ | 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[44] | 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)[45] | |
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)[46] | |
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+1025§ | 16.3±4.2 | T7.5[47] | 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 | 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] | 1967 | flare stars |
G 208-45 | M6.0V[5] | 14.01 | 15.72 | 19h 53m 55.2s | +44° 24′ 56″ | 1967 | ||||
G 208-44 B | M5.5 | 16.75 | 18.46 | 19h 53m 54.2s | +44° 24′ 55″ | 1984 | ||||
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))[48] 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)[30] | |
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 0255-4700§ | 15.885±0.020 | L7.5V[5] | 22.92 | 24.44 | 02h 55m 03.7s | −47° 00′ 52″ | 205.33±0.25[7] | 1999 | [38] | |
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))[49][50] | |
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[51] | 11.48[51] | 00h 15m 28.11s | −16° 08′ 01.6″ | 200.5±9.4[51] | 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
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.[52]
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.[53] 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.[54]
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.
See also
- Lists of astronomical objects
- Interstellar travel
- List of brightest stars
- List of star systems within 20–25 light-years
- List of star systems within 25–30 light-years
- List of nearest bright stars
- List of nearest exoplanets
- List of nearest galaxies
- Lists of stars
- Nearby Stars Database
- Stars and planetary systems in fiction
- The Magnificent Seven
- List of Solar System objects by greatest aphelion
- List of trans-Neptunian objects
Notes
- ^ a b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
- ^ a b Before 1900: earliest certain recorded observation. 1900–1930: first catalogued. After 1930: earliest trigonometric or spectroscopic parallax.
- ^ Systems with their first accurate trigonometric parallaxes measured by RECONS
- ^ a b Might not be within 5 parsecs of the Sun.
References
- ^ 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.
- ^ 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.
- ^ a b Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
- ^ 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.
- ^ 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). September 17, 2007. Retrieved 2007-11-06.
- ^ a b From parallax.
- ^ 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.
- ^ 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 (accidently announced?)
- ^ a b General Catalogue of Trigonometric Parallaxes.
- ^ a b Hipparcos Catalogue.
- ^ Söderhjelm, Staffan (1999). "Visual binary orbits and masses POST HIPPARCOS". Astronomy and Astrophysics. 341: 121. Bibcode:1999A&A...341..121S.
- ^ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
- ^ 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.
- ^ 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].
- ^ 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.
- ^ 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. Retrieved 27 June 2017.
{{cite journal}}
: CS1 maint: unflagged free DOI (link) - ^ 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:1404.6501. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18.
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(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist
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External links
- "The 100 nearest star systems", Research Consortium on Nearby Stars
- "NStars database". Northern Arizona University. Archived from the original on October 30, 2005. Retrieved October 24, 2005.
{{cite web}}
: Unknown parameter|deadurl=
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suggested) (help) - Nemiroff, R.; Bonnell, J., eds. (March 18, 2001). "Map of the 25 nearest star systems". Astronomy Picture of the Day. NASA. Retrieved 2005-10-24.
- "Notable Nearby Stars". SolStation. Retrieved 2005-10-24.
- "Cool stars in the solar Neighbourhood". D. Montes, UCM. Retrieved 2005-11-14.
- The dynamics of the closest stars
- Takeda, G.; E. B. Ford; A. Sills; F. A. Rasio; D. A. Fischer; J. A. Valenti (2006). "Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~ 1000 Cool Stars from the SPOCS Catalog". California & Carnegie Planet Search. Retrieved 2006-10-13.
- 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.
- http://phl.upr.edu/projects/nearby-stars-catalog