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Pole star project/Red dwarfs

< Pole star project

With respect to the color 'red', there are studies of the redness of objects such as the red dwarf AZ Cancri shown in the visual image at right. Cool stars of spectral class M appear red; they are (depending on their size) referred to as "red giants" or "red dwarfs".

AZ Cancri. Credit: SDSS Data Release 6.

A red dwarf is a small and relatively cool star on the main sequence, either late K or M spectral type. Red dwarfs are by far the most common type of star in the Galaxy, at least in the neighborhood of the Sun. Proxima Centauri, the nearest star to the Sun, is a red dwarf. Due to their low luminosity, individual red dwarfs cannot easily be observed. From Earth, none are visible to the naked eye.[1]

Dwarf stars

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"Ideally all intrinsic colours should be found from unreddened stars. This is possible for dwarf and giant stars later than about A0 (Johnson, 1964) ... However, it cannot be used for stars of other spectral classes since they are all relatively infrequent in space, and generally reddened."[2]

Red wavelengths

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A very important wavelength in this region is the Balmer alpha line, 656.28 nm. It is emitted or absorbed by hydrogen atoms when electrons move between the second and third electron shells. Other Balmer lines, known as beta, gamma and delta, have wavelengths of 486.13, 434.05 and 410.17 nm respectively;[3] these are also in the visual range but are less important than the alpha line.

M class stars

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Typical characteristics[4]
Stellar
Class 		Mass
(Mʘ) 		Radius
(Rʘ) 		Luminosity
(Lʘ) 		Teff
(K)
M0V 60% 62% 7.2% 3,800
M1V 49% 49% 3.5% 3,600
M2V 44% 44% 2.3% 3,400
M3V 36% 39% 1.5% 3,250
M4V 20% 26% 0.55% 3,100
M5V 14% 20% 0.22% 2,800
M6V 10% 15% 0.09% 2,600
M7V 9% 12% 0.05% 2,500
M8V 8% 11% 0.03% 2,400
M9V 7.5% 8% 0.015% 2,300

Exoplanets

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"[O]ut [of] a sample of 3,897 red dwarfs ... the Kepler Space Telescope has identified 95 exoplanet candidates circling them. Three of these candidates are roughly Earth-size and orbit within their stars' "Goldilocks zone," where liquid water (and possibly life as we know it) can exist."[5]

Proxima Centauri

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Proxima Centauri, the closest star to the Sun, at a distance of 4.2 ly, is a red dwarf. Credit: ESA/Hubble & NASA.{{free media}}

Proxima Centauri, the nearest star to the Sun, is a red dwarf, as are fifty of the sixty nearest stars.

Coolest and smallest red dwarfs near the Sun

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The coolest red dwarfs near the Sun have a surface temperature of ~2,000 K and the smallest have radii of ~9% that of the Sun, with masses about ~7.5% that of the Sun. These red dwarfs have spectral classes of L0 to L2. There is some overlap with the properties of brown dwarfs, since the most massive brown dwarfs at lower metallicity can be as hot as 3,600 K and have late M spectral types.

Known star systems

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The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible color bands (U, B or V). Absolute magnitude (with electromagnetic wave, 'light' band denoted in subscript) is a measurement at a 10-parsec distance across imaginary empty space devoid of all its sparse dust and gas. Some of the parallaxes and resultant distances are rough measurements.[6]

Key
# Visible to the unaided eye
§ Brown dwarf or Sub-brown dwarf
‡ White dwarf
Known star systems within 5.0 parsecs (16.3 light-years)
Designation Distance[7]
(light-years margin of error (±err)) 		Stellar
class 		Mass Magnitude (mV[6] or mJ) Epoch J2000.0 Stellar parallax
(milliarcsecond (mas) margin of error (±err))
[6][8] 		additional
references
Stellar system Star or (sub-) brown dwarf M☉ Apparent magnitude Absolute magnitude Right ascension[6] Declination[6]
Solar System Sun (Sol) 0.0000158 G-type main-sequence star (G2V)[6] 1 −26.74# 4.85 N/A N/A N/A eight known planets
Alpha Centauri Proxima Centauri (V645 Centauri) 4.2441 ± 0.0011 red dwarf M5.5Ve 0.122 11.09 15.53 14h 29m 43.0s −62° 40′ 46″ 768.50 ± 0.20[9] flare star, two confirmed planets (Proxima b, 2016, and Proxima Centauri c, 2019)[10] and unconfirmed evidence for a third, sub-Earth sized, planet (d, 2020).[11]
α Centauri A (Rigil Kentaurus) 4.3650 ± 0.0068}} G-type main-sequence star (G2V)[6] 1.100 0.01# 4.38 14h 39m 36.5s −60° 50′ 02″ 747.23 ± 1.17
[12][13][14] 		one directly-imaged habitable-zone planet candidate (Candidate 1) (2021)
α Centauri B (Toliman) K-type main-sequence star (K1V)[6] 0.907 1.34# 5.71 14h 39m 35.1s −60° 50′ 14″ one suspected planet (Alpha Centauri Bc) (2013)
(planet Alpha Centauri Bb refuted in 2015)
Barnard's Star (BD+04°3561a) 5.9577 ± 0.0032 red dwarf M4.0Ve 0.144 9.53 13.22 17h 57m 48.5s +04° 41′ 36″ 547.45 ± 0.29[9] flare star, largest-known proper motion,[15] one disputed planet (Barnard's Star b)[16][17]
Luhman 16
(WISE 1049−5319)§ 		Luhman 16A§ 6.5029 ± 0.0011 Brown dwarf Spectral class L (L8±1)[18] 0.032 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 501.557 ± 0.082[19] one refuted planet (Ab[20] in 2017[21])
Luhman 16B§ Brown dwarf Spectral class T (T1±2)[18] 0.027
WISE 0855−0714 § 7.43 ± 0.04[22] Brown dwarf Spectral class Y (Y4) 0.003-0.010 25.0 J 08h 55m 10.83s -07° 14′ 42.5″ 439.0 ± 2.4[23] sub-brown dwarf
Wolf 359 (CN Leonis) 7.856 ± 0.031 red dwarf M6.0V[6] 0.090 13.44 16.55 10h 56m 29.2s +07° 00′ 53″ 415.16 ± 1.62[24] flare star, has 2 known planets[16]
Lalande 21185 (BD+36°2147) 8.307 ± 0.014 red dwarf M2.0V[6] 0.390 7.47 10.44 11h 03m 20.2s +35° 58′ 12″ 392.64 ± 0.67[25] two known planets (2019)(2021)[16]
Sirius
(α Canis Majoris) 		Sirius A 8.659 ± 0.010}} A-type main-sequence A1V[6] 2.063 −1.46# 1.42 06h 45m 08.9s −16° 42′ 58″ 376.68 ± 0.45[9] brightest star in the night sky
Sirius B‡ White dwarf DA2[6] 1.018 8.44 11.34
Luyten 726-8 Luyten 726-8 A (BL Ceti) 8.791 ± 0.012 red dwarf M5.5Ve 0.102 12.54 15.40 01h 39m 01.3s −17° 57′ 01″ 371.0 ± 0.5[9] flare star (Archetypal member)
Luyten 726-8 B (UV Ceti) red dwarf M6.0Ve 0.100 12.99 15.85
Ross 154 (V1216 Sagittarii) 9.7035 ± 0.0019 red dwarf M3.5Ve 0.17 10.43 13.07 18h 49m 49.4s −23° 50′ 10″ 336.123 ± 0.064[9] flare star
Ross 248 (HH Andromedae) 10.2903 ± 0.0041 red dwarf M5.5Ve 0.136 12.29 14.79 23h 41m 54.7s +44° 10′ 30″ 316.96 ± 0.13[9] flare star
Epsilon Eridani (Ran) 10.446 ± 0.016 K-type main-sequence star (K2V)[6] 0.820 3.73# 6.19 03h 32m 55.8s −09° 27′ 30″ 312.22 ± 0.47[9] three circumstellar disks,
two suspected planets (Epsilon Eridani b (AEgir) (debated) and Epsilon Eridani c) (2000 & 2002)[26]
Lacaille 9352 (Gliese Catalogue of Nearby Stars, Gliese 887) 10.7211 ± 0.0016 red dwarf M0.5V 0.486 7.34 9.75 23h 05m 52.0s −35° 51′ 11″ 304.219 ± 0.045[9] two planets, b and c, with equivocal evidence for a third in the habitable zone (2020)[27]
Ross 128 (FI Virginis) 11.0074 ± 0.0026 red dwarf M4.0Vn 0.168 11.13 13.51 11h 47m 44.4s +00° 48′ 16″ 296.307 ± 0.070}}[9] flare star, one planet (Ross 128 b) (2017)[28]
EZ Aquarii
(Gliese 866, Luyten 789-6) 		EZ Aquarii A 11.109 ± 0.034 red dwarf M5.0Ve 0.11 13.33 15.64 22h 38m 33.4s −15° 17′ 57″ 293.60 ± 0.9[29] A & B flare stars
EZ Aquarii B red dwarf M? 0.11 13.27 15.58
EZ Aquarii C red dwarf M? 0.10 14.03 16.34
61 Cygni 61 Cygni A (BD+38°4343) 11.4008 ± 0.0012 K-type main-sequence star (K5.0V)[6] 0.70 5.21# 7.49 21h 06m 53.9s +38° 44′ 58″ 286.08 ± 0.03[9] B flare star and brightest red dwarf in night sky, first star (besides Sun) to have measured distance[30]
possible circumstellar disk.
61 Cygni B (BD+38°4344) K-type main-sequence star (K7.0V)[6] 0.63 6.03# 8.31 21h 06m 55.3s +38° 44′ 31″
Procyon
(α Canis Minoris) 		Procyon A 11.402 ± 0.032 F-type main-sequence star (F5IV–V)[6] 1.499 0.38# 2.66 07h 39m 18.1s +05° 13′ 30″ 286.05 ± 0.81
[12][13]
Procyon B‡ White dwarf (DQZ)[6] 0.602 10.70 12.98
Struve 2398
(Gliese 725, BD+59°1915) 		Struve 2398 A (HD 173739) 11.4880 ± 0.0012 red dwarf M3.0V[6] 0.334 8.90 11.16 18h 42m 46.7s +59° 37′ 49″ 283.91 ± 0.03[9] flare stars, star B has 2 known planets[16]
Struve 2398 B (HD 173740) red dwarf M3.5V[6] 0.248 9.69 11.95 18h 42m 46.9s +59° 37′ 37″
Groombridge 34
(Gliese 15) 		Groombridge 34 A (GX Andromedae) 11.6182 ± 0.0008 red dwarf M1.5V[6] 0.38 8.08 10.32 00h 18m 22.9s +44° 01′ 23″ 280.73 ± 0.02[9] flare star, two suspected planets (Gliese 15 Ac, 2017) and Gliese 15 Ab, 2014)[31]
Groombridge 34 B (GQ Andromedae) red dwarf M3.5V[6] 0.15 11.06 13.30 flare star
DX Cancri (G 51-15) 11.6780 ± 0.0056 red dwarf M6.5Ve 0.09 14.78 16.98 08h 29m 49.5s +26° 46′ 37″ 279.29 ± 0.13[9] flare star
Tau Ceti (BD−16°295) 11.753 ± 0.022 G-type main-sequence star G8.5Vp[6] 0.783 3.49# 5.68 01h 44m 04.1s −15° 56′ 15″ 277.52 ± 0.52[9] one debris disk
four confirmed planets (Tau Ceti e), Tau Ceti f, g, and h) (2012, 2017),
four candidate planets (b, c, d, and "i") (2012, 2019), and 1 predicted planet (2020).
Epsilon Indi
(CPD−57°10015) 		Epsilon Indi A 11.869 ± 0.011 K-type main-sequence star K5Ve[6] 0.754 4.69# 6.89 22h 03m 21.7s −56° 47′ 10″ 274.80 ± 0.25[9] one planet (Ab) (2018)[32]
Epsilon Indi Ba§ Brown dwarf Spectral class T T1.0V 0.065 12.3 J[33] 22h 04m 10.5s −56° 46′ 58″
Epsilon Indi Bb§ Brown dwarf Spectral class T T6.0V 0.050 13.2 J[33]
Gliese 1061 (LHS 1565) 11.9803 ± 0.0029 red dwarf M5.5V[6] 0.113 13.09 15.26 03h 35m 59.7s −44° 30′ 45″ 272.245 ± 0.066[9] has 3 known planets (2019)[34][35][36]
YZ Ceti (LHS 138) 12.1084 ± 0.0035 red dwarf M4.5V[6] 0.130 12.02 14.17 01h 12m 30.6s −16° 59′ 56″ 269.363 ± 0.078[9] flare star, three planets (b, c, and d) (2017),[37]
one suspected planet (e)
Luyten's Star (BD+05°1668) 12.199 ± 0.036 red dwarf M3.5Vn 0.26 9.86 11.97 07h 27m 24.5s +05° 13′ 33″ 267.36 ± 0.79[38] two planets (Luyten b, c) (2017)[39] and two suspected planets (d, e) (2019)[40]
Teegarden's Star (SO025300.5+165258) 12.496 ± 0.013 red dwarf M6.5V 0.08 15.14 17.22 02h 53m 00.9s +16° 52′ 53″ 261.01 ± 0.27[9] tentative radial velocity variation (2010)[36][41] has 2 known planets (2019)[42][43]
Kapteyn's Star (CD−45°1841) 12.8294 ± 0.0013 red dwarf M1.5 subdwarf Cool subdwarfs VI[6] 0.281 8.84 10.87 05h 11m 40.6s −45° 01′ 06″ 254.226 ± 0.026[9] two disputed planets (b and c) (2014)[44][45]
Lacaille 8760 (AX Microscopii) 12.9515 ± 0.0029 red dwarf M0.0V[6] 0.60 6.67 8.69 21h 17m 15.3s −38° 52′ 03″ 251.829 ± 0.056[9] brightest M dwarf star in night sky, flare star
SCR 1845-6357 SCR 1845-6357 A 13.050 ± 0.008 red dwarf M8.5V[6] 0.07 17.39 19.41 18h 45m 05.3s −63° 57′ 48″ 249.91 ± 0.16[9] [36]
SCR 1845-6357 B§ Brown dwarf Spectral class T|T6[46] 0.03[6] 13.3 J[33] 18h 45m 02.6s −63° 57′ 52″
Kruger 60
(BD+56°2783) 		Kruger 60 A 13.0724 ± 0.0052 red dwarf M3.0V[6] 0.271 9.79 11.76 22h 27m 59.5s +57° 41′ 45″ 249.5 ± 0.1[9] B flare star
Kruger 60 B (DO Cephei) red dwarf M4.0V[6] 0.176 11.41 13.38
DEN 1048-3956|DEN 1048-3956§ 13.1932 ± 0.0066 red dwarf M8.5V[6] 0.08 17.39 19.37 10h 48m 14.7s −39° 56′ 06″ 247.22 ± 0.12[9] [47][48]
Ross 614
(V577 Monocerotis, Gliese 234) 		Ross 614A (LHS 1849) 13.424 ± 0.049 red dwarf M4.5V[6] 0.223 11.15 13.09 06h 29m 23.4s −02° 48′ 50″ 242.97 ± 0.88[9] A flare star
Ross 614B (LHS 1850) red dwarf M5.5V 0.111 14.23 16.17
UGPS J0722-0540§ 13.43 ± 0.13 brown dwarf Spectral class T|T9[6] 0.010-0.025 16.52 J[49] 07h 22m 27.3s –05° 40′ 30″ 242.8 ± 2.4[50] [51]
Wolf 1061 (Gliese 628, BD−12°4523) 14.0458 ± 0.0038 red dwarf M3.0V[6] 0.294 10.07 11.93 16h 30m 18.1s −12° 39′ 45″ 232.210 ± 0.063[9] three planets (Wolf 1061 b, Wolf 1061 c, and Wolf 1061 d) (2015)[52]
Wolf 424
(FL Virginis, LHS 333, Gliese 473) 		Wolf 424 A 14.05 ± 0.26 red dwarf M5.5Ve 0.143 13.18 14.97 12h 33m 17.2s +09° 01′ 15″ 232.2 ± 4.3[53] flare stars
Wolf 424 B red dwarf M7Ve 0.131 13.17 14.96
Van Maanen's star (Gliese 35, LHS 7)‡ 14.0744 ± 0.0023 White dwarf DZ7[6] 0.67 12.38 14.21 00h 49m 09.9s +05° 23′ 19″ 231.737 ± 0.038[9] 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 red dwarf M1.5 V[6] 0.45-0.48 8.55 10.35 00h 05m 24.4s −37° 21′ 27″ 230.133 ± 0.060[9]
L 1159-16 (TZ Arietis, Gliese 83.1) 14.5843 ± 0.0070 red dwarf M4.5V[6] 0.14 12.27 14.03 02h 00m 13.2s +13° 03′ 08″ 223.63 ± 0.11[9] flare star, has two known planets (b and c) and one candidate (d)[16]
Gliese 674 (LHS 449) 14.8387 ± 0.0033 red dwarf M3.0V[6] 0.35 9.38 11.09 17h 28m 39.9s −46° 53′ 43″ 219.801 ± 0.049[9] one planet (b) (2007)[54]
Gliese 687 (LHS 450, BD+68°946) 14.8401 ± 0.0022 red dwarf M3.0V[6] 0.401 9.17 10.89 17h 36m 25.9s +68° 20′ 21″ 219.781 ± 0.032[9] possible flare star, two planets (b) (2014)[55] and (c) (2020)[56]
LHS 292 (LP 731-58) 14.885 ± 0.011 red dwarf M6.5V[6] 0.08 15.60 17.32 10h 48m 12.6s −11° 20′ 14″ 219.12 ± 0.16[9] flare star
LP 145-141 (WD 1142-645, Gliese 440)‡ 15.1182 ± 0.0023 White dwarf DQ6[6] 0.75 11.50 13.18 11h 45m 42.9s −64° 50′ 29″ 215.737 ± 0.032[9]
GJ 1245|Gliese 1245 G 208-44 A

(Gliese 1245 A)

15.2090 ± 0.0050 red dwarf M5.5V[6] 0.11 13.46 15.17 19h 53m 54.2s +44° 24′ 55″ 214.45 ± 0.07[9] flare stars
G 208-45

(Gliese 1245 B)

red dwarf M6.0V[6] 0.10 14.01 15.72 19h 53m 55.2s +44° 24′ 56″
G 208-44 B

(Gliese 1245 C)

red dwarf M5.5 0.07 16.75 18.46 19h 53m 54.2s +44° 24′ 55″
WISEPA J174124.26+255319.5|WISE 1741+2553§ 15.2 ± 0.2 Brown dwarf Spectral class T|T9 16.53 J 18.18 J 17h 41m 24.2s +25° 53′ 19″ 214 ± 2.8[23]
Gliese 876 (Ross 780) 15.2504 ± 0.0054 red dwarf M3.5V[6] 0.37 10.17 11.81 22h 53m 16.7s −14° 15′ 49″ 213.867 ± 0.076[9] four planets (Gliese 876 d (2005), Gliese 876 c (2001), Gliese 876 b (1998), and Gliese 876 e (2010))[57]
two possible planets (f and g) (2014) (debated)
WISE 1639-6847§ 15.45 ± 0.04 brown dwarf Spectral class Y Y0.5 20.57 J 22.10 J 16h 39m 40.9s -68° 47′ 46″ 211.11 ± 0.56[58]
LHS 288 (Luyten 143-23) 15.7703 ± 0.0056 red dwarf M5.5V[6] 0.11[6] 13.90 15.51 10h 44m 21.2s −61° 12′ 36″ 206.817 ± 0.074[9] one tentative planet (b) (2007)[36]
GJ 1002|Gliese 1002 15.8164 ± 0.0098 red dwarf M5.5V[6] 0.11 13.76 15.40 00h 06m 43.8s −07° 32′ 22″ 206.21 ± 0.13[9]
Groombridge 1618 (Gliese 380) 15.8797 ± 0.0026 K-type main-sequence K7.0V[6] 0.67 6.59 8.16 10h 11m 22.1s +49° 27′ 15″ 205.392 ± 0.034[9] brightest single red dwarf in night sky, flare star, one suspected debris disk,
one suspected planet (b) (1989) (tentative)
DEN 0255-4700|DEN 0255-4700§ 15.885 ± 0.020 Brown dwarf Spectral class L|L7.5V[6] 0.025-0.065 22.92 24.44 02h 55m 03.7s −47° 00′ 52″ 205.33 ± 0.25[9] [48]
Gliese 412 Gliese 412 A 15.983 ± 0.013 red dwarf M1.0V[6] 0.48 8.77 10.34 11h 05m 28.6s +43° 31′ 36″ 204.06 ± 0.17[9]
Gliese 412 B (WX Ursae Majoris) red dwarf M5.5V[6] 0.10 14.48 16.05 11h 05m 30.4s +43° 31′ 18″ flare star
Gliese 832 16.1939 ± 0.0034 red dwarf M1.5 V[6] 0.45 8.66 10.20 21h 33m 34.0s −49° 00′ 32″ 201.407 ± 0.043[9] b (2008) and Gliese 832 c|c (2014))[59][60]
AD Leonis 16.1970 ± 0.0055 red dwarf M3.0V[6] 0.39-0.42 9.32 10.87 10h 19m 36.4s +19° 52′ 10″ 201.368 ± 0.068[9] flare star, 1 refuted planet (b[16] in 2020)[61]
40 Eridani Keid

(40 Eridani A)

16.26 ± 0.02 K-type main-sequence star K0.5V 0.84 4.43# 5.93 04h 15m 16.3s −07° 39′ 10″ 200.62 ± 0.23
GJ 1005 Gliese 1005 Gliese 1005 A 16.26 ± 0.76[note 1] red dwarf M4V[62] 0.179 11.48[62] 12.70 00h 15m 28.11s -16° 08′ 01.6″ 200.5 ± 9.4[62]
Gliese 1005 B red dwarf M7V 0.112 ? 15.12
System Star or (sub-) brown dwarf Distance[7]
(Light-years margin of error (±err)) 		Stellar
class 		Apparent magnitude Absolute magnitude Right ascension[6] Declination[6] Stellar parallax
(milliarcsecond (mas) margin of error (±err))
[6][8] 		Additional
references
Designation Magnitude (mV[6] or mJ) Epoch J2000.0

Milky Way

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According to some estimates, red dwarfs make up three-quarters of the stars in the Milky Way.[63]

Gaseous giants

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The volume and mass of Jupiter are VJ = 1.4313 x 1015 km3 and MJ = 1.8982 x 1027 kg.

The volume and mass of Saturn are VS = 8.2713 x 1014 km3 and MS = 5.6834 x 1026 kg.

The volume and mass of Uranus are VU = 6.833 x 1013 km3 and MU = 8.6810 x 1025 kg.

The volume and mass of Neptune are VN = 6.254 x 1013 km3 and MN = 1.021 x 1026 kg.

The minimal volume and mass for the small star Helios (H) that may have interacted with the Sun some 13,000 to 100,000 years ago: VH = 2.389 x 1015 km3 (0.00169 V⊙) and MH = 2.656 x 1027 kg (0.00136 M⊙).

Sun

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The volume and mass of the Sun are V⊙ = 1.41 x 1018 km3 and M⊙ = 1.9885 x 1030 kg.

Nearby small stars

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There are 66 stars within 5.0 parsecs (16.3 light-years) of the Sun.

Key
# Visible to the unaided eye
§ Brown dwarf or Sub-brown dwarf
‡ White dwarf
Known small star systems within 5.0 parsecs (16.3 light-years)
Designation Distance[7]
(light-years margin of error (±err)) 		Stellar
class 		Mass Magnitude (mV[6] or mJ) Epoch J2000.0 Stellar parallax
(milliarcsecond (mas) margin of error (±err))
[6][8] 		Stellar
volume
1015 km3 		additional
references
Stellar system Star or (sub-) brown dwarf M☉ Apparent magnitude Absolute magnitude Right ascension[6] Declination[6]
Alpha Centauri Proxima Centauri (V645 Centauri) 4.2441 ± 0.0011 red dwarf M5.5Ve 0.122 11.09 15.53 14h 29m 43.0s −62° 40′ 46″ 768.50 ± 0.20[9] 5.1856 flare star, two confirmed planets (Proxima b, 2016, and Proxima Centauri c, 2019)[10] and unconfirmed evidence for a third, sub-Earth sized, planet (d, 2020).[11]
Barnard's Star (BD+04°3561a) 5.9577 ± 0.0032 red dwarf M4.0Ve 0.144 9.53 13.22 17h 57m 48.5s +04° 41′ 36″ 547.45 ± 0.29[9] 1 flare star, largest-known proper motion,[15] one disputed planet (Barnard's Star b)[16][17]
Luhman 16
(WISE 1049−5319)§ 		Luhman 16A§ 6.5029 ± 0.0011 Brown dwarf Spectral class L8±1[18] 0.032 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 501.557 ± 0.082[64] 1 one refuted planet (Ab[65] in 2017[21])
Luhman 16B§ Brown dwarf Spectral class T1±2[18] 0.027 0.5
WISE 0855−0714 § 7.43 ± 0.04[22] Brown dwarf Spectral class Y4 0.003-0.010 25.0 J 08h 55m 10.83s -07° 14′ 42.5″ 439.0 ± 2.4[23] 1 sub-brown dwarf
Wolf 359 (CN Leonis) 7.856 ± 0.031 red dwarf M6.0V[6] 0.090 13.44 16.55 10h 56m 29.2s +07° 00′ 53″ 415.16 ± 1.62[24] 1 flare star, has 2 known planets[16]
Lalande 21185 (BD+36°2147) 8.307 ± 0.014 red dwarf M2.0V[6] 0.390 7.47 10.44 11h 03m 20.2s +35° 58′ 12″ 392.64 ± 0.67[25] 1 two known planets (2019)(2021)[16]
Sirius
(α Canis Majoris) 		Sirius B‡ 8.659 ± 0.010 White dwarf DA2[6] 1.018 8.44 11.34 06h 45m 08.9s −16° 42′ 58″ 376.68 ± 0.45[9] 0.000838
Luyten 726-8 Luyten 726-8 A (BL Ceti) 8.791 ± 0.012 red dwarf M5.5Ve 0.102 12.54 15.40 01h 39m 01.3s −17° 57′ 01″ 371.0 ± 0.5[9] 1 flare star (Archetypal member)
Luyten 726-8 B (UV Ceti) red dwarf M6.0Ve 0.100 12.99 15.85 0.5
Ross 154 (V1216 Sagittarii) 9.7035 ± 0.0019 red dwarf M3.5Ve 0.17 10.43 13.07 18h 49m 49.4s −23° 50′ 10″ 336.123 ± 0.064[9] 1 flare star
Ross 248 (HH Andromedae) 10.2903 ± 0.0041 red dwarf M5.5Ve 0.136 12.29 14.79 23h 41m 54.7s +44° 10′ 30″ 316.96 ± 0.13[9] 1 flare star
Lacaille 9352 (Gliese Catalogue of Nearby Stars, Gliese 887) 10.7211 ± 0.0016 red dwarf M0.5V 0.486 7.34 9.75 23h 05m 52.0s −35° 51′ 11″ 304.219 ± 0.045[9] 1 two planets, b and c, with equivocal evidence for a third in the habitable zone (2020)[27]
Ross 128 (FI Virginis) 11.0074 ± 0.0026 red dwarf M4.0Vn 0.168 11.13 13.51 11h 47m 44.4s +00° 48′ 16″ 296.307 ± 0.070}}[9] 1 flare star, one planet (Ross 128 b) (2017)[28]
EZ Aquarii
(Gliese 866, Luyten 789-6) 		EZ Aquarii A 11.109 ± 0.034 red dwarf M5.0Ve 0.11 13.33 15.64 22h 38m 33.4s −15° 17′ 57″ 293.60 ± 0.9[29] 1 A & B flare stars
EZ Aquarii B red dwarf M? 0.11 13.27 15.58 1
EZ Aquarii C red dwarf M? 0.10 14.03 16.34 1
Procyon
(α Canis Minoris) 		Procyon B‡ 11.402 ± 0.032 White dwarf (DQZ)[6] 0.602 10.70 12.98 07h 39m 18.1s +05° 13′ 30″ 286.05 ± 0.81
[12][13] 		1
Struve 2398
(Gliese 725, BD+59°1915) 		Struve 2398 A (HD 173739) 11.4880 ± 0.0012 red dwarf M3.0V[6] 0.334 8.90 11.16 18h 42m 46.7s +59° 37′ 49″ 283.91 ± 0.03[9] 1 flare stars, star B has 2 known planets[16]
Struve 2398 B (HD 173740) red dwarf M3.5V[6] 0.248 9.69 11.95 18h 42m 46.9s +59° 37′ 37″ 1
Groombridge 34
(Gliese 15) 		Groombridge 34 A (GX Andromedae) 11.6182 ± 0.0008 red dwarf M1.5V[6] 0.38 8.08 10.32 00h 18m 22.9s +44° 01′ 23″ 280.73 ± 0.02[9] 1 flare star, two suspected planets (Gliese 15 Ac, 2017) and Gliese 15 Ab, 2014)[66]
Groombridge 34 B (GQ Andromedae) red dwarf M3.5V[6] 0.15 11.06 13.30 1 flare star
DX Cancri (G 51-15) 11.6780 ± 0.0056 red dwarf M6.5Ve 0.09 14.78 16.98 08h 29m 49.5s +26° 46′ 37″ 279.29 ± 0.13[9] 1 flare star
Epsilon Indi
(CPD−57°10015) 		Epsilon Indi Ba§ 11.869 ± 0.011 Brown dwarf Spectral class T1.0V 0.065 12.3 J[33] 22h 04m 10.5s −56° 46′ 58″ 274.80 ± 0.25[9] 1
Epsilon Indi Bb§ Brown dwarf Spectral class T6.0V 0.050 13.2 J[33] 1
Gliese 1061 (LHS 1565) 11.9803 ± 0.0029 red dwarf M5.5V[6] 0.113 13.09 15.26 03h 35m 59.7s −44° 30′ 45″ 272.245 ± 0.066[9] 1 has 3 known planets (2019)[67][35][36]
YZ Ceti (LHS 138) 12.1084 ± 0.0035 red dwarf M4.5V[6] 0.130 12.02 14.17 01h 12m 30.6s −16° 59′ 56″ 269.363 ± 0.078[9] 1 flare star, three planets (b, c, and d) (2017),[68]
one suspected planet (e)
Luyten's Star (BD+05°1668) 12.199 ± 0.036 red dwarf M3.5Vn 0.26 9.86 11.97 07h 27m 24.5s +05° 13′ 33″ 267.36 ± 0.79[38] 1 two planets (Luyten b, c) (2017)[69] and two suspected planets (d, e) (2019)[40]
Teegarden's Star (SO025300.5+165258) 12.496 ± 0.013 red dwarf M6.5V 0.08 15.14 17.22 02h 53m 00.9s +16° 52′ 53″ 261.01 ± 0.27[9] 1 tentative radial velocity variation (2010)[36][41] has 2 known planets (2019)[70][71]
Kapteyn's Star (CD−45°1841) 12.8294 ± 0.0013 red dwarf M1.5 subdwarf Cool subdwarfs VI[6] 0.281 8.84 10.87 05h 11m 40.6s −45° 01′ 06″ 254.226 ± 0.026[9] 1 two disputed planets (b and c) (2014)[44][45]
Lacaille 8760 (AX Microscopii) 12.9515 ± 0.0029 red dwarf M0.0V[6] 0.60 6.67 8.69 21h 17m 15.3s −38° 52′ 03″ 251.829 ± 0.056[9] 1 brightest M dwarf star in night sky, flare star
SCR 1845-6357 SCR 1845-6357 A 13.050 ± 0.008 red dwarf M8.5V[6] 0.07 17.39 19.41 18h 45m 05.3s −63° 57′ 48″ 249.91 ± 0.16[9] 1 has 3 known planets (2019)?[36]
SCR 1845-6357 B§ Brown dwarf Spectral class T6[46] 0.03[6] 13.3 J[33] 18h 45m 02.6s −63° 57′ 52″ 1
Kruger 60
(BD+56°2783) 		Kruger 60 A 13.0724 ± 0.0052 red dwarf M3.0V[6] 0.271 9.79 11.76 22h 27m 59.5s +57° 41′ 45″ 249.5 ± 0.1[9] 1 B flare star
Kruger 60 B (DO Cephei) red dwarf M4.0V[6] 0.176 11.41 13.38 1
DEN 1048-3956§ 13.1932 ± 0.0066 red dwarf M8.5V[6] 0.08 17.39 19.37 10h 48m 14.7s −39° 56′ 06″ 247.22 ± 0.12[9] 1 μ >= 1.0" yr−1[72][48]
Ross 614
(V577 Monocerotis, Gliese 234) 		Ross 614A (LHS 1849) 13.424 ± 0.049 red dwarf M4.5V[6] 0.223 11.15 13.09 06h 29m 23.4s −02° 48′ 50″ 242.97 ± 0.88[9] 1 A flare star
Ross 614B (LHS 1850) red dwarf M5.5V 0.111 14.23 16.17 1
UGPS J0722-0540§ 13.43 ± 0.13 brown dwarf Spectral class T9[6] 0.010-0.025 16.52 J[73] 07h 22m 27.3s –05° 40′ 30″ 242.8 ± 2.4[50] 1 very cool brown dwarf[51]
Wolf 1061 (Gliese 628, BD−12°4523) 14.0458 ± 0.0038 red dwarf M3.0V[6] 0.294 10.07 11.93 16h 30m 18.1s −12° 39′ 45″ 232.210 ± 0.063[9] 1 three planets (Wolf 1061 b, Wolf 1061 c, and Wolf 1061 d) (2015)[74]
Wolf 424
(FL Virginis, LHS 333, Gliese 473) 		Wolf 424 A 14.05 ± 0.26 red dwarf M5.5Ve 0.143 13.18 14.97 12h 33m 17.2s +09° 01′ 15″ 232.2 ± 4.3[53] 1 flare stars
Wolf 424 B red dwarf M7Ve 0.131 13.17 14.96 1
Van Maanen's star (Gliese 35, LHS 7)‡ 14.0744 ± 0.0023 White dwarf DZ7[6] 0.67 12.38 14.21 00h 49m 09.9s +05° 23′ 19″ 231.737 ± 0.038[9] 1 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 red dwarf M1.5 V[6] 0.45-0.48 8.55 10.35 00h 05m 24.4s −37° 21′ 27″ 230.133 ± 0.060[9] 1
L 1159-16 (TZ Arietis, Gliese 83.1) 14.5843 ± 0.0070 red dwarf M4.5V[6] 0.14 12.27 14.03 02h 00m 13.2s +13° 03′ 08″ 223.63 ± 0.11[9] 1 flare star, has two known planets (b and c) and one candidate (d)[16]
Gliese 674 (LHS 449) 14.8387 ± 0.0033 red dwarf M3.0V[6] 0.35 9.38 11.09 17h 28m 39.9s −46° 53′ 43″ 219.801 ± 0.049[9] 1 one planet (b) (2007)[75]
Gliese 687 (LHS 450, BD+68°946) 14.8401 ± 0.0022 red dwarf M3.0V[6] 0.401 9.17 10.89 17h 36m 25.9s +68° 20′ 21″ 219.781 ± 0.032[9] 1 possible flare star, two planets (b) (2014)[55] and (c) (2020)[56]
LHS 292 (LP 731-58) 14.885 ± 0.011 red dwarf M6.5V[6] 0.08 15.60 17.32 10h 48m 12.6s −11° 20′ 14″ 219.12 ± 0.16[9] 1 flare star
LP 145-141 (WD 1142-645, Gliese 440)‡ 15.1182 ± 0.0023 White dwarf DQ6[6] 0.75 11.50 13.18 11h 45m 42.9s −64° 50′ 29″ 215.737 ± 0.032[9] 1
Gliese 1245 G 208-44 A

(Gliese 1245 A)

15.2090 ± 0.0050 red dwarf M5.5V[6] 0.11 13.46 15.17 19h 53m 54.2s +44° 24′ 55″ 214.45 ± 0.07[9] 1 flare stars
G 208-45

(Gliese 1245 B)

red dwarf M6.0V[6] 0.10 14.01 15.72 19h 53m 55.2s +44° 24′ 56″ 1
G 208-44 B

(Gliese 1245 C)

red dwarf M5.5 0.07 16.75 18.46 19h 53m 54.2s +44° 24′ 55″ 1
WISE 1741+2553§ 15.2 ± 0.2 Brown dwarf Spectral class T9 16.53 J 18.18 J 17h 41m 24.2s +25° 53′ 19″ 214 ± 2.8[23] 1
Gliese 876 (Ross 780) 15.2504 ± 0.0054 red dwarf M3.5V[6] 0.37 10.17 11.81 22h 53m 16.7s −14° 15′ 49″ 213.867 ± 0.076[9] 1 four planets (Gliese 876 d (2005), Gliese 876 c (2001), Gliese 876 b (1998), and Gliese 876 e (2010))[76]
two possible planets (f and g) (2014) (debated)
WISE 1639-6847§ 15.45 ± 0.04 brown dwarf Spectral class Y0.5 20.57 J 22.10 J 16h 39m 40.9s -68° 47′ 46″ 211.11 ± 0.56[77] 1
LHS 288 (Luyten 143-23) 15.7703 ± 0.0056 red dwarf M5.5V[6] 0.11[6] 13.90 15.51 10h 44m 21.2s −61° 12′ 36″ 206.817 ± 0.074[9] 1 one tentative planet (b) (2007)[36]
Gliese 1002 15.8164 ± 0.0098 red dwarf M5.5V[6] 0.11 13.76 15.40 00h 06m 43.8s −07° 32′ 22″ 206.21 ± 0.13[9] 1
Groombridge 1618 (Gliese 380) 15.8797 ± 0.0026 K-type main-sequence K7.0V[6] 0.67 6.59 8.16 10h 11m 22.1s +49° 27′ 15″ 205.392 ± 0.034[9] 1 brightest single red dwarf in night sky, flare star, one suspected debris disk,
one suspected planet (b) (1989) (tentative)
DEN 0255-4700§ 15.885 ± 0.020 Brown dwarf Spectral class L7.5V[6] 0.025-0.065 22.92 24.44 02h 55m 03.7s −47° 00′ 52″ 205.33 ± 0.25[9] 1 μ >= 1.0" yr−1[48]
Gliese 412 Gliese 412 A 15.983 ± 0.013 red dwarf M1.0V[6] 0.48 8.77 10.34 11h 05m 28.6s +43° 31′ 36″ 204.06 ± 0.17[9] 1
Gliese 412 B (WX Ursae Majoris) red dwarf M5.5V[6] 0.10 14.48 16.05 11h 05m 30.4s +43° 31′ 18″ 1 flare star
Gliese 832 16.1939 ± 0.0034 red dwarf M1.5 V[6] 0.45 8.66 10.20 21h 33m 34.0s −49° 00′ 32″ 201.407 ± 0.043[9] 1 b (2008) and Gliese 832 c|c (2014))[78][79]
AD Leonis 16.1970 ± 0.0055 red dwarf M3.0V[6] 0.39-0.42 9.32 10.87 10h 19m 36.4s +19° 52′ 10″ 201.368 ± 0.068[9] 1 flare star, 1 refuted planet (b[16] in 2020)[61]
40 Eridani Keid

(40 Eridani A)

16.26 ± 0.02 K-type main-sequence star K0.5V 0.84 4.43# 5.93 04h 15m 16.3s −07° 39′ 10″ 200.62 ± 0.23 1
GJ 1005 Gliese 1005 Gliese 1005 A 16.26 ± 0.76[note 1] red dwarf M4V[62] 0.179 11.48[62] 12.70 00h 15m 28.11s -16° 08′ 01.6″ 200.5 ± 9.4[62] 1
Gliese 1005 B red dwarf M7V 0.112 ? 15.12 1
System Star or (sub-) brown dwarf Distance[7]
(Light-years margin of error (±err)) 		Stellar
class 		Mass Apparent magnitude Absolute magnitude Right ascension[6] Declination[6] Stellar parallax
(milliarcsecond (mas) margin of error (±err))
[6][8] 		Stellar
volume
1015 km3 		Additional
references
Designation M☉ Magnitude (mV[6] or mJ) Epoch J2000.0

Past encounters

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Distances of the nearest stars from 20,000 years ago until 80,000 years in the future. Credit: SternFuchs.{{free media}}

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.[80] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[81]

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.[82] 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.[83]

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.

List of past encounters

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Stars that are known to have passed within 5 light-years of the Sun in the past[84][85]
Star name Hipparcos Catalogue (HIP
number) 		Minimum distance
(light-years) 		Date of approach
in thousands of years 		Current distance
(light-years) 		Stellar
classification 		Mass in M☉ Current
apparent magnitude 		Current Constellation Current
Right ascension 		Current
Declination
HD 7977 N/A 0.483 +0.109
-0.081 		-2795 +43
-44 		246.74±0.60 G0V ~1.2 9.04 Cassiopeia 01h 20m 31.597s +61° 52′ 57.08″
Scholz's star and companion brown dwarf N/A 0.82 +0.37
-0.22 		−78.5±0.7 22.2±0.2 A: M9V
B: T5 		A: 0.095
B: 0.063 		18.3 Monoceros 07h 20m 03.20s -08° 46′ 51.2″
CD-69 2001 N/A 1.614 +0.071
-0.070 		−1905±12 332.61±0.55 K4V 0.61 11.13 Indus 21h 40m 31.514s -69° 25′ 14.58″
2MASS J0621-0101 N/A 1.69 +0.47
-0.40 		-3179 +95
-99 		428.8±3.1 G5V 0.96 11.9 Orion 06h 21m 34.807s -01° 01′ 55.01″
HD 49995 N/A 1.79 +0.24
-0.21 		-4200 +160
-170 		439.74±0.59 A: F3V
B: M1V 		A: 1.48
B: 0.49 		8.78 Canis Major 06h 50m 20.810s -18° 37′ 30.58″
2MASS J0634-7449 N/A 2.043 +0.043
-0.042 		−894±12 212.41±0.15 mid K ~0.6 12.69 Mensa 06h 34m 29.385s -74° 49′ 47.12″
UCAC2 15719371 N/A 2.44 +0.12
-0.11 		-4239 +90
-93 		280.80±0.26 K4V 0.66 12.58 Antlia 09h 44m 09.884s -37° 45′ 31.09″
TYC 1662-1962-1 N/A 2.615 +0.066
-0.064 		−1524±15 286.51±0.40 Early K ~0.8 10.95 Vulpecula 21h 14m 32.911s +21° 53′ 32.76″
BD-21 1529 N/A 2.699 +0.063
-0.062 		-1659 +8.7
-8.8 		368.48±0.56 G5V ~0.95 9.67 Canis Major 06h 37m 48.004s -21° 22′ 21.94″
Gliese 3649 N/A 2.954 +0.077
-0.073 		−510±12 54.435±0.023 M1 0.49 10.85 Leo 11h 12m 38.97s +18° 56′ 05.4″
2MASS J1921-1244 N/A 2.98 +0.32
-0.27 		-3370 +220
-250 		376.46±0.73 K6V 0.69 12.46 Sagittarius 19h 21m 58.124s -12° 43′ 58.61″
TYC 9387-2515-1 N/A 3.198 +0.082
-0.081 		-1498.7 +9.6
-9.8 		401.96±0.54 K1V 0.86 11.45 Mensa 06h 18m 54.643s -80° 19′ 16.54″
2MASS J1638-6355 N/A 3.34 +0.32
-0.30 		-1417 +32
-33 		468.5±4.2 K2V 0.82 12.44 Triangulum Australe 16h 38m 21.759s -63° 55′ 13.16″
2MASS J0625-2408 N/A 3.636 +0.102
-0.099 		-1841 +24
-25 		534.88±0.93 K/M ~0.5 12.91 Canis Major 06h 25m 42.744s -24° 08′ 35.02″
BD+05 1792 N/A 3.957 +0.043
-0.042 		-960.6 +3.6
-3.7 		239.73±0.33 G2V 1.07 8.58 Gemini 07h 48m 07.037s +05° 27′ 22.51″
2MASS J2241-2759 N/A 4.01|0.16}} -2784 +41
-42 		411.06±0.76 K7V ~0.5 12.28 Piscis Austrinus 22h 41m 50.996s -27° 59′ 47.04″
StKM 1-554 N/A 4.191 +0.047
-0.046 		-546.5 +4.4
-4.5 		151.97±0.19 M0V 0.65 12.17 Orion 05h 14m 01.871s +05° 22′ 56.26″
Gliese 3379 N/A 4.1915±0.0023 −156.190±0.051 16.9861±0.0027 M3.5V 0.19 11.31 Orion 06h 00m 03.824s +02° 42′ 22.97″
HD 146248 N/A 4.345 +0.054
-0.053 		-1142.5 +7.3
-7.4 		334.87±0.47 G2/3IV 1.23 9.47 Triangulum Australe 16h 19m 27.875s -64° 50′ 34.38″
Zeta Leporis 27288 4.43 +0.33
-0.30 		-878 +42
-46 		72.81±0.40 A2Vann 2.0 3.55 Lepus 05h 46m 57.341s −14° 49′ 19.02″
HD 68814 40317 4.668 +0.086
-0.085 		−2213±11 259.85±0.30 G6V 0.98 9.57 Hydra 08h 13m 57.112s -04° 03′ 12.56″
2MASS J1941-4602 N/A 4.868 +0.074
-0.072 		-461.7 +6.3
-6.5 		66.848±0.033 M4-M6 ~0.15 12.4 Telescopium 19h 41m 53.18s -46° 02′ 31.4″
TYC 94-1074-1 N/A 5.00 ± 0.11 -1068.2 +8.3
-8.4 		316.37 ± 0.71 K4V 0.72 11.25 Taurus 04h 34m 35.456s +06° 30′ 26.18″

Hypotheses

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Main resource: Hypotheses
  1. The sums of the masses and volumes of Jupiter, Saturn, Uranus, and Neptune are the minima for the small star that may have interacted with the Sun some 13,000 to 100,000 years ago.
  2. The small star may have been called Helios or Sol, if this interaction was observed at some point by hominins on Earth.

See also

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Notes

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  1. ↑ 1.0 1.1 Might not be within 5 parsecs of the Sun.

References

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  1. ↑ "The Brightest Red Dwarf", by Ken Croswell (Accessed 6/7/08)
  2. ↑ M. Pim FitzGerald (February 1970). "The Intrinsic Colours of Stars and Two-Colour Reddening Lines". Astronomy and Astrophysics 4 (2): 234-43. 
  3. ↑ http://www.phys.utk.edu/labs/modphys/BalmerSeries.pdf
  4. ↑ Lisa Kaltenegger, Wesley A. Traub (June 2009). "Transits of Earth-like Planets". The Astrophysical Journal 698 (1): 519-527. doi:10.1088/0004-637X/698/1/519. 
  5. ↑ Elizabeth Howell (February 7, 2013). "Closest 'Alien Earth' May Be 13 Light-Years Away". Yahoo! News. Retrieved 2013-02-07.
  6. ↑ 6.000 6.001 6.002 6.003 6.004 6.005 6.006 6.007 6.008 6.009 6.010 6.011 6.012 6.013 6.014 6.015 6.016 6.017 6.018 6.019 6.020 6.021 6.022 6.023 6.024 6.025 6.026 6.027 6.028 6.029 6.030 6.031 6.032 6.033 6.034 6.035 6.036 6.037 6.038 6.039 6.040 6.041 6.042 6.043 6.044 6.045 6.046 6.047 6.048 6.049 6.050 6.051 6.052 6.053 6.054 6.055 6.056 6.057 6.058 6.059 6.060 6.061 6.062 6.063 6.064 6.065 6.066 6.067 6.068 6.069 6.070 6.071 6.072 6.073 6.074 6.075 6.076 6.077 6.078 6.079 6.080 6.081 6.082 6.083 6.084 6.085 6.086 6.087 6.088 6.089 6.090 6.091 6.092 6.093 6.094 6.095 6.096 6.097 6.098 6.099 6.100 6.101 6.102 6.103 6.104 "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). September 17, 2007. http://www.astro.gsu.edu/RECONS/TOP100.posted.htm. Retrieved 2007-11-06. 
  7. ↑ 7.0 7.1 7.2 7.3 From parallax.
  8. ↑ 8.0 8.1 8.2 8.3 Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
  9. ↑ 9.00 9.01 9.02 9.03 9.04 9.05 9.06 9.07 9.08 9.09 9.10 9.11 9.12 9.13 9.14 9.15 9.16 9.17 9.18 9.19 9.20 9.21 9.22 9.23 9.24 9.25 9.26 9.27 9.28 9.29 9.30 9.31 9.32 9.33 9.34 9.35 9.36 9.37 9.38 9.39 9.40 9.41 9.42 9.43 9.44 9.45 9.46 9.47 9.48 9.49 9.50 9.51 9.52 9.53 9.54 9.55 9.56 9.57 9.58 9.59 9.60 9.61 9.62 9.63 9.64 9.65 9.66 9.67 9.68 9.69 9.70 9.71 9.72 9.73 9.74 9.75 9.76 9.77 9.78 Gaia Collaboration. "Gaia DR2". gea.esac.esa.int. Retrieved 10 May 2018.
  10. ↑ 10.0 10.1 Drake, Nadia (12 April 2019). "A new super-Earth may orbit the star next door". National Geographic. Retrieved 21 April 2019. Video of discovery being discussed (accidentally announced?)
  11. ↑ 11.0 11.1 Suárez Mascareño, A.; Faria, J. P.; Figueira, P.; Lovis, C.; Damasso, M.; González Hernández, J. I.; Rebolo, R.; Cristiano, S. et al. (2020). "Revisiting Proxima with ESPRESSO". Astronomy & Astrophysics 639: A77. doi:10.1051/0004-6361/202037745. ISSN 0004-6361. 
  12. ↑ 12.0 12.1 12.2 General Catalogue of Trigonometric Parallaxes.
  13. ↑ 13.0 13.1 13.2 Hipparcos Catalogue.
  14. ↑ Söderhjelm, Staffan (1999). "Visual binary orbits and masses POST HIPPARCOS". Astronomy & Astrophysics 341: 121. 
  15. ↑ 15.0 15.1 Barnard, Edward Emerson (1916). "A small star with large proper motion". Astronomical Journal 29 (695): 181. doi:10.1086/104156. 
  16. ↑ 16.00 16.01 16.02 16.03 16.04 16.05 16.06 16.07 16.08 16.09 16.10 16.11 Tuomi, M.; el, al. (2019-06-11). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
  17. ↑ 17.0 17.1 Lubin, Jack; Robertson, Paul; Stefansson, Gudmundur; Ninan, Joe; Mahadevan, Suvrath; Endl, Michael; Ford, Eric; Wright, Jason T.; Beard, Corey; Bender, Chad; Cochran, William D.; Diddams, Scott A.; Fredrick, Connor; Halverson, Samuel; Kanodia, Shubham; Metcalf, Andrew J.; Ramsey, Lawrence; Roy, Arpita; Schwab, Christian; Terrien, Ryan (2021), Stellar Activity Manifesting at a One Year Alias Explains Barnard b as a False Positive, arXiv:2105.07005
  18. ↑ 18.0 18.1 18.2 18.3 Luhman, K. L. (2013). "Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun". The Astrophysical Journal Letters 767 (1): L1. doi:10.1088/2041-8205/767/1/L1. 
  19. ↑ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". Astronomy & Astrophysics 618: A111. doi:10.1051/0004-6361/201833626. 
  20. ↑ Boffin, H. M. J. (2013). "Possible astrometric discovery of a substellar companion to the closest binary brown dwarf system WISE J104915.57-531906.1". Astronomy & Astrophysics 561: L4. doi:10.1051/0004-6361/201322975. 
  21. ↑ 21.0 21.1 Bedin L. R. (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. doi:10.1093/mnras/stx1177. https://academic.oup.com/mnras/article/470/1/1140/3896221. Retrieved 27 June 2017. 
  22. ↑ 22.0 22.1 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. doi:10.1088/2041-8205/786/2/L18. 
  23. ↑ 23.0 23.1 23.2 23.3 Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; Marocco, Federico; Cayago, Alfred J. et al. (2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and y Dwarfs". The Astrophysical Journal Supplement Series 253 (1): 7. doi:10.3847/1538-4365/abd107. 
  24. ↑ 24.0 24.1 Davison, Cassy L. (19 February 2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal 149 (3): 106. doi:10.1088/0004-6256/149/3/106. ISSN 1538-3881. 
  25. ↑ 25.0 25.1 van Leeuwen, F. (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. ISSN 0004-6361. 
  26. ↑ Janson, M.; Reffert, S.; Brandner, W.; Henning, T.; Lenzen, R.; Hippler, S. (September 2008), "A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches", Astronomy & Astrophysics, 488 (2): 771–780, arXiv:0807.0301, Bibcode:2008A&A...488..771J, doi:10.1051/0004-6361:200809984
  27. ↑ 27.0 27.1 Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; Luque, R.; Zechmeister, M.; Vogt, S. S.; Jenkins, J. S.; Pallé, E.; Berdi Ñas, Z. M.; Coleman, G. A. L.; Díaz, M. R.; Ribas, I.; Jones, H. R. A.; Butler, R. P.; Tinney, C. G.; Bailey, J.; Carter, B. D.; o'Toole, S.; Wittenmyer, R. A.; Crane, J. D.; Feng, F.; Shectman, S. A.; Teske, J.; Reiners, Ansgar; Amado, P. J. (2020), "A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887", Science, 368 (6498): 1477–1481, arXiv:2006.16372, Bibcode:2020Sci...368.1477J, doi:10.1126/science.aaz0795, PMID 32587019
  28. ↑ 28.0 28.1 ESO. "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs" (PDF). Retrieved 15 November 2017.
  29. ↑ 29.0 29.1 Torres, G.; Andersen, J.; Giménez, A. (2010). "Accurate masses and radii of normal stars: modern results and applications". The Astronomy & Astrophysics Review 18 (1–2): 67–126. doi:10.1007/s00159-009-0025-1. 
  30. ↑ Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel". Astronomische Nachrichten 16 (5–6): 65–96. doi:10.1002/asna.18390160502. https://zenodo.org/record/1424605. "(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
  31. ↑ Bailer-Jones, C. A. L. (2014). "The NASA-UC-UH Eta-Earth Program: IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth". The Astrophysical Journal 794 (1): 51. doi:10.1088/0004-637X/794/1/51. 
  32. ↑ 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].
  33. ↑ 33.0 33.1 33.2 33.3 33.4 33.5 Chris Gelino, J. Davy Kirkpatrick, Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Retrieved 2012-06-10.{{cite web}}: CS1 maint: multiple names: authors list (link) (main page)
  34. ↑ Dreizler, S.; Jeffers, S. V.; Rodríguez, E.; Zechmeister, M.; Barnes, J.R.; Haswell, C.A.; Coleman, G. A. L.; Lalitha, S. et al. (2019-08-13). "Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061". Monthly Notices of the Royal Astronomical Society. doi:10.1093/mnras/staa248. 
  35. ↑ 35.0 35.1 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. doi:10.1086/118482. 
  36. ↑ 36.0 36.1 36.2 36.3 36.4 36.5 36.6 36.7 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. doi:10.1086/508233. 
  37. ↑ Bailer-Jones, C. A. L. (2017). "The HARPS search for southern extra-solar planets XLII. A system of Earth-mass planets around the nearby M dwarf YZ Ceti". Astronomy and Astrophysics 605: L11. doi:10.1051/0004-6361/201731581. 
  38. ↑ 38.0 38.1 Gatewood, George (1 July 2008). "Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions". The Astronomical Journal 136 (1): 452–460. doi:10.1088/0004-6256/136/1/452. 
  39. ↑ Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics 602: A88. doi:10.1051/0004-6361/201630153. https://www.aanda.org/articles/aa/full_html/2017/06/aa30153-16/aa30153-16.html. 
  40. ↑ 40.0 40.1 Pozuelos, Francisco J. et al. (2020). "GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec". Astronomy & Astrophysics 641: A23. doi:10.1051/0004-6361/202038047. 
  41. ↑ 41.0 41.1 Barnes, J. R. (2012). "ROPS: A New Search for Habitable Earths in the Southern Sky". Monthly Notices of the Royal Astronomical Society 424 (1): 591–604. doi:10.1111/j.1365-2966.2012.21236.x. 
  42. ↑ "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF).
  43. ↑ Caballero, J. A.; Reiners, Ansgar; Ribas, I.; Dreizler, S.; Zechmeister, M. (12 June 2019). "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star". Astronomy & Astrophysics 627: A49. doi:10.1051/0004-6361/201935460. ISSN 0004-6361. https://www.aanda.org/articles/aa/pdf/forth/aa35460-19.pdf. 
  44. ↑ 44.0 44.1 Anglada-Escude, G. (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. doi:10.1093/mnrasl/slu076. 
  45. ↑ 45.0 45.1 Bortle, Anna et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal 161 (5): 230. doi:10.3847/1538-3881/abec89. 
  46. ↑ 46.0 46.1 Kasper, M.; Biller, B. A.; Burrows, A.; Brandner, W.; Budaj, J.; Close, L. M. (2007). "The very nearby M/T dwarf binary SCR 1845-6357". Astronomy & Astrophysics 471 (2): 655. doi:10.1051/0004-6361:20077881. 
  47. ↑ 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. doi:10.1086/428489. 
  48. ↑ 48.0 48.1 48.2 48.3 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. doi:10.1086/430473. 
  49. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". Monthly Notices of the Royal Astronomical Society 408 (1): L56. doi:10.1111/j.1745-3933.2010.00927.x. 
  50. ↑ 50.0 50.1 Leggett, Sandy K.; Saumon, Didier; Marley, Mark S.; Lodders, Katharina; Canty, J.; Lucas, Philip W.; Smart, Richard L.; Tinney, Chris G. et al. (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. doi:10.1088/0004-637X/748/2/74. 
  51. ↑ 51.0 51.1 Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2010). "Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System". arXiv:1004.0317v1 [astro-ph.SR].
  52. ↑ "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.
  53. ↑ 53.0 53.1 Gliese, W. and Jahreiß, H. (1991). "Gl 473". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 10 May 2018.{{cite web}}: CS1 maint: multiple names: authors list (link)
  54. ↑ "The Extrasolar Planet Encyclopaedia — Catalog Listing".
  55. ↑ 55.0 55.1 "The Lick–Carnegie exoplanet survey: Gliese 687 b: A Neptune-mass planet orbiting a nearby red dwarf" (PDF). March 27, 2014.
  56. ↑ 56.0 56.1 Feng, Fabo; Shectman, Stephen A.; Clement, Matthew S.; Vogt, Steven S.; Tuomi, Mikko; Teske, Johanna K.; Burt, Jennifer; Crane, Jeffrey D.; Holden, Bradford; Sharon Xuesong Wang; Thompson, Ian B.; Diaz, Matias R.; Paul Butler, R. (2020), Search for Nearby Earth Analogs. III. Detection of ten new planets, three planet candidates, and confirmation of three planets around eleven nearby M dwarfs, arXiv:2008.07998, doi:10.3847/1538-4365/abb139 Accepted for publication by The Astrophysical Journal Supplement Series|ApJS
  57. ↑ 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. doi:10.1088/0004-637X/719/1/890. 
  58. ↑ Fontanive, C.; Bedin, L. R.; Bardalez Gagliuffi, D. C. (2021-02-01). "The Y dwarf population with HST: unlocking the secrets of our coolest neighbours - I. Overview and first astrometric results". Monthly Notices of the Royal Astronomical Society 501 (1): 911–915. doi:10.1093/mnras/staa3732. ISSN 0035-8711. 
  59. ↑ Bailey, Jeremy (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal 690 (1): 743–747. doi:10.1088/0004-637X/690/1/743. 
  60. ↑ Wittenmyer, R. A.; Tuomi (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal 791 (2): 114. doi:10.1088/0004-637X/791/2/114. 
  61. ↑ 61.0 61.1 Carleo, I. et al. (2020). "The GAPS Programme at TNG XXI – A GIARPS case-study of known young planetary candidates: Confirmation of HD 285507 b and refutation of AD Leo b". Astronomy & Astrophysics A5: 638. doi:10.1051/0004-6361/201937369. 
  62. ↑ 62.0 62.1 62.2 62.3 62.4 62.5 "G 158-50 - SIMBAD". SIMBAD. Retrieved 2015-09-12.
  63. ↑ Jason Palmer (6 February 2013). "Exoplanets near red dwarfs suggest another Earth nearer". BBC. Retrieved 2019-07-10.
  64. ↑ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". Astronomy & Astrophysics 618: A111. doi:10.1051/0004-6361/201833626. 
  65. ↑ Boffin, H. M. J. (2013). "Possible astrometric discovery of a substellar companion to the closest binary brown dwarf system WISE J104915.57-531906.1". Astronomy & Astrophysics 561: L4. doi:10.1051/0004-6361/201322975. 
  66. ↑ Bailer-Jones, C. A. L. (2014). "The NASA-UC-UH Eta-Earth Program: IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth". The Astrophysical Journal 794 (1): 51. doi:10.1088/0004-637X/794/1/51. 
  67. ↑ Dreizler, S.; Jeffers, S. V.; Rodríguez, E.; Zechmeister, M.; Barnes, J.R.; Haswell, C.A.; Coleman, G. A. L.; Lalitha, S. et al. (2019-08-13). "Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061". Monthly Notices of the Royal Astronomical Society. doi:10.1093/mnras/staa248. 
  68. ↑ Bailer-Jones, C. A. L. (2017). "The HARPS search for southern extra-solar planets XLII. A system of Earth-mass planets around the nearby M dwarf YZ Ceti". Astronomy and Astrophysics 605: L11. doi:10.1051/0004-6361/201731581. 
  69. ↑ Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics 602: A88. doi:10.1051/0004-6361/201630153. https://www.aanda.org/articles/aa/full_html/2017/06/aa30153-16/aa30153-16.html. 
  70. ↑ "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF).
  71. ↑ Caballero, J. A.; Reiners, Ansgar; Ribas, I.; Dreizler, S.; Zechmeister, M. (12 June 2019). "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star". Astronomy & Astrophysics 627: A49. doi:10.1051/0004-6361/201935460. ISSN 0004-6361. https://www.aanda.org/articles/aa/pdf/forth/aa35460-19.pdf. 
  72. ↑ 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. doi:10.1086/428489. 
  73. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". Monthly Notices of the Royal Astronomical Society 408 (1): L56. doi:10.1111/j.1745-3933.2010.00927.x. 
  74. ↑ "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.
  75. ↑ "The Extrasolar Planet Encyclopaedia — Catalog Listing".
  76. ↑ 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. doi:10.1088/0004-637X/719/1/890. 
  77. ↑ Fontanive, C.; Bedin, L. R.; Bardalez Gagliuffi, D. C. (2021-02-01). "The Y dwarf population with HST: unlocking the secrets of our coolest neighbours - I. Overview and first astrometric results". Monthly Notices of the Royal Astronomical Society 501 (1): 911–915. doi:10.1093/mnras/staa3732. ISSN 0035-8711. 
  78. ↑ Bailey, Jeremy (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal 690 (1): 743–747. doi:10.1088/0004-637X/690/1/743. 
  79. ↑ Wittenmyer, R. A.; Tuomi (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal 791 (2): 114. doi:10.1088/0004-637X/791/2/114. 
  80. ↑ Matthews, R. A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society 35: 1. 
  81. ↑ See also: Stellar kinematics.
  82. ↑ 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 Hipparcos Data". The Astronomical Journal 117 (2): 1042–1055. doi:10.1086/300723. 
  83. ↑ 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. doi:10.1051/0004-6361/201833456. 
  84. ↑ Table 3, Bobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System". Astronomy Letters 36 (3): 220–226. doi:10.1134/S1063773710030060. 
  85. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (19 May 2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics 616 (37): A37. doi:10.1051/0004-6361/201833456. 
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