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List of nearest stars

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Rotating 3D image of the nearest stars
Animated 3D map of the nearest stars, centered on the Sun. 3D red green glasses are recommended to view this image correctly.

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 exceed 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] although this number is likely, in reality, 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 200 kilometers per second, would be more than 6,000 light years from the Sun at present day, with hundreds of 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 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.[4]

List

Key
# 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]

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

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 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.[4] 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.[3]
  • 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.[4]
  • 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.

Template:Solar encounters

See also

Template:Wikipedia books

Notes

  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

  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. doi:10.1051/0004-6361/201833456.{{cite journal}}: CS1 maint: extra punctuation (link) CS1 maint: multiple names: authors list (link)
  3. ^ a b c Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
  4. ^ a b c 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 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). 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.
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  50. ^ See also: Stellar kinematics.
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  55. ^ Coryn Bailer-Jones (2015-01-01). "The closest encounter is Hip 85605. How reliable is this?". Retrieved 2015-01-05.
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