This list covers all known stars, white dwarfs, brown dwarfs, and sub-brown dwarfs within 20 light-years (6.13 parsecs) of the Sun. So far, 131 such objects have been found. Only 22 are bright enough to be visible without a telescope, for which the star's visible light needs to reach or exceed the dimmest brightness visible to the naked eye from Earth, 6.5 apparent magnitude.[1]
3D red green glasses are recommended to view this image correctly..png)
The known 131 objects are bound in 94 stellar systems. Of those, 103 are main sequence stars: 80 red dwarfs and 23 "typical" stars having greater mass. Additionally, astronomers have found 6 white dwarfs (stars that have exhausted all fusible hydrogen), 21 brown dwarfs, as well as 1 sub-brown dwarf, WISE 0855−0714 (possibly a rogue planet). The closest system is Alpha Centauri, with Proxima Centauri as the closest star in that system, at 4.2465 light-years from Earth. The brightest, most massive and most luminous object among those 131 is Sirius A, which is also the brightest star in Earth's night sky; its white dwarf companion Sirius B is the hottest object among them. The largest object within the 20 light-years is Procyon.
The Solar System, and the other stars/dwarfs listed here, are currently moving within (or near) the Local Interstellar Cloud, roughly 30 light-years (9.2 pc) across. The Local Interstellar Cloud is, in turn, contained inside the Local Bubble, a cavity in the interstellar medium about 300 light-years (92.0 pc) across. It contains Ursa Major and the Hyades star cluster, among others. The Local Bubble also contains the neighboring G-Cloud, which contains the stars Alpha Centauri and Altair. In the galactic context, the Local Bubble is a small part of the Orion Arm, which contains most stars that we can see without a telescope. The Orion Arm is one of the spiral arms of our Milky Way galaxy.
Astrometrics
editThe 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.[2]
Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will approach the Solar System to less than 5 parsecs in 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).[3] 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.[4] It is currently predicted to pass 0.1696±0.0065 ly (10635±500 au) from the Sun in 1.290±0.04 million years from the present, close enough to significantly disturb the Solar System's Oort cloud.[5]
List
edit| # | Visible to the unaided eye (apparent magnitude of +6.5 or brighter) |
| $ | Luminous star (absolute magnitude of +8.5 or brighter) |
| ‡ | White dwarf |
| § | Brown dwarf |
| & | Sub-brown dwarf or rogue planet |
| * | Nearest in constellation |
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 necessarily 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]
| Designation | Distance (ly (±err))[7]→→ |
Coordinates: RA, Dec (Ep J2000, Eq J2000)[6] |
Stellar class |
Mass | Magnitude (mV[6] or mJ) | Parallax (mas (±err)) [6][note 1] |
Notes and additional references | |||
|---|---|---|---|---|---|---|---|---|---|---|
| System | Star or (sub-) brown dwarf | M☉ | App. | Abs. | ||||||
| Solar System | Sun (Sol)$ | 0.0000158 | N/A | N/A | G2V[6] | 1 | −26.74# | 4.85 | N/A | eight recognized planets and more dwarf planets |
| Alpha Centauri | Proxima Centauri (C, V645 Centauri) | 4.2465 ±0.0003 |
Cen* | 14h 29m 43.0s −62° 40′ 46″ |
M5.5Ve | 0.122 | 11.09 | 15.53 | 768.0665 ±0.0499[8] |
flare star, one confirmed planet (b, 2016, and two candidate planets, (d, 2022)[9][10] and (c, 2019)[11][12] |
| Rigil Kentaurus (A)$ | 4.3441 ±0.0022 |
14h 39m 36.5s −60° 50′ 02″ |
G2V[6] | 1.079 | 0.01# | 4.38 | 750.81 ±0.38[13] |
one directly imaged habitable-zone planet candidate (Candidate 1) (2021) | ||
| Toliman (B)$ | 14h 39m 35.1s −60° 50′ 14″ |
K1V[6] | 0.909 | 1.34# | 5.71 | planet b refuted in 2015 | ||||
| Barnard's Star (BD+04°3561a) | 5.9629 ±0.0004 |
Oph* | 17h 57m 48.5s +04° 41′ 36″ |
M4.0Ve | 0.144 | 9.53 | 13.22 | 546.9759 ±0.0401[8] |
flare star, largest-known proper motion,[14] one confirmed planet (b)[15] | |
| Luhman 16 (WISE 1049−5319) |
A§ | 6.5029 ±0.0011 |
Vel* | 10h 49m 18.9s −53° 19′ 10″ |
L8±1[16] | 0.032 | 10.7 J | 14.2 J | 501.557 ±0.082[17] |
nearest brown dwarfs |
| B§ | T1±2[16] | 0.027 | ||||||||
| WISE 0855−0714& | 7.430 ±0.041 |
Hya* | 08h 55m 10.8s −07° 14′ 43″ |
Y4 | 0.003-0.010 | 25.0 J | 28.2 J | 439.0 ±2.4[18] |
sub-brown dwarf | |
| Wolf 359 (CN Leonis) | 7.8558 ±0.0013 |
Leo* | 10h 56m 29.2s +07° 00′ 53″ |
M6.0V[6] | 0.090 | 13.44 | 16.55 | 415.1794 ±0.0684[8] |
flare star, has 1 candidate & 1 refuted planet[19][20] | |
| Lalande 21185 (BD+36°2147, Gliese 411, HD 95735) | 8.3044 ±0.0007 |
UMa* | 11h 03m 20.2s +35° 58′ 12″ |
M2.0V[6] | 0.390 | 7.47 | 10.44 | 392.7529 ±0.0321[8] |
two known planets (2019, 2021)[21] | |
| Alpha Canis Majoris | Sirius (A)$ | 8.7094 ±0.0054 |
CMa* | 06h 45m 08.9s −16° 42′ 58″ |
A1V[6] | 2.063 | −1.46# | 1.42 | 374.4896 ±0.2313[8] |
brightest star in the night sky |
| B‡ | DA2[6] | 1.018 | 8.44 | 11.34 | ||||||
| Gliese 65 (Luyten 726–8) | A (BL Ceti) | 8.724 ±0.012 |
Cet* | 01h 39m 01.3s −17° 57′ 01″ |
M5.5Ve | 0.102 | 12.54 | 15.40 | 373.8443 ±0.5009[8] |
flare star (Archetypal member), has 1 candidate planet[22] |
| B (UV Ceti) | M6.0Ve | 0.100 | 12.99 | 15.85 | ||||||
| Ross 154 (V1216 Sagittarii) | 9.7063 ±0.0009 |
Sgr* | 18h 49m 49.4s −23° 50′ 10″ |
M3.5Ve | 0.17 | 10.43 | 13.07 | 336.0266 ±0.0317[8] |
flare star | |
| Ross 248 (HH Andromedae) | 10.3057 ±0.0014 |
And* | 23h 41m 54.7s +44° 10′ 30″ |
M5.5Ve | 0.136 | 12.29 | 14.79 | 316.4812 ±0.0444[8] |
flare star | |
| Epsilon Eridani (Ran)$ | 10.4749 ±0.0037 |
Eri* | 03h 32m 55.8s −09° 27′ 30″ |
K2V[6] | 0.820 | 3.73# | 6.19 | 311.37 ±0.11[23] |
three circumstellar disks, one confirmed planet (AEgir, 2000) and one candidate (c, 2002)[24] | |
| Lacaille 9352 (Gliese 887) | 10.7241 ±0.0007 |
PsA* | 23h 05m 52.0s −35° 51′ 11″ |
M0.5V | 0.486 | 7.34 | 9.75 | 304.1354 ±0.0200[8] |
two planets, b and c, with equivocal evidence for a third in the habitable zone (2020)[25] | |
| Ross 128 (FI Virginis) | 11.0074 ±0.0011 |
Vir* | 11h 47m 44.4s +00° 48′ 16″ |
M4.0Vn | 0.168 | 11.13 | 13.51 | 296.3053 ±0.0302[8] |
flare star, one planet (b) (2017)[26] | |
| EZ Aquarii (Gliese 866, Luyten 789-6) |
A | 11.109 ±0.034 |
Aqr* | 22h 38m 33.4s −15° 17′ 57″ |
M5.0Ve | 0.11 | 13.33 | 15.64 | 293.60 ±0.9[27] |
A & B flare stars |
| B | M? | 0.11 | 13.27 | 15.58 | ||||||
| C | M? | 0.10 | 14.03 | 16.34 | ||||||
| Alpha Canis Minoris | Procyon (A)$ | 11.402 ±0.032 |
CMi* | 07h 39m 18.1s +05° 13′ 30″ |
F5IV–V[6] | 1.499 | 0.38# | 2.66 | 286.05 ±0.81 [28][29] |
|
| B‡ | DQZ[6] | 0.602 | 10.70 | 12.98 | ||||||
| 61 Cygni | A (BD+38°4343)$ | 11.4039 ±0.0012 |
Cyg* | 21h 06m 53.9s +38° 44′ 58″ |
K5.0V[6] | 0.70 | 5.21# | 7.49 | 286.0054 ±0.0289[8] |
First star (besides Sun) to have measured distance.[30] B flare star, with possible planet or brown dwarf.[31] Possible circumstellar disk. |
| B (BD+38°4344)$ | 21h 06m 55.3s +38° 44′ 31″ |
K7.0V[6] | 0.63 | 6.03# | 8.31 | |||||
| Struve 2398 (Gliese 725, BD+59°1915) |
A (HD 173739) | 11.4908 ±0.0009 |
Dra* | 18h 42m 46.7s +59° 37′ 49″ |
M3.0V[6] | 0.334 | 8.90 | 11.16 | 283.8401 ±0.0220[8] |
flare stars, star B has 2 candidate planets[19] |
| B (HD 173740) | 18h 42m 46.9s +59° 37′ 37″ |
M3.5V[6] | 0.248 | 9.69 | 11.95 | |||||
| Groombridge 34 (Gliese 15) |
A (GX Andromedae) | 11.6191 ±0.0008 |
And | 00h 18m 22.9s +44° 01′ 23″ |
M1.5V[6] | 0.38 | 8.08 | 10.32 | 280.7068 ±0.0203[8] |
flare star, two known planets (Ab, 2014, and Ac, 2018)[32] |
| B (GQ Andromedae) | M3.5V[6] | 0.15 | 11.06 | 13.30 | flare star | |||||
| DX Cancri (G 51-15) | 11.6797 ±0.0027 |
Cnc* | 08h 29m 49.5s +26° 46′ 37″ |
M6.5Ve | 0.09 | 14.78 | 16.98 | 279.2496 ±0.0637[8] |
flare star | |
| Epsilon Indi (CPD−57°10015) |
A$ | 11.8670 ±0.0041 |
Ind* | 22h 03m 21.7s −56° 47′ 10″ |
K5Ve[6] | 0.754 | 4.69# | 6.89 | 274.8431 ±0.0956[8] |
one planet (Ab) (2018)[33] |
| Ba§ | 22h 04m 10.5s −56° 46′ 58″ |
T1.0V | 0.065 | 12.3 J[34] | 14.5 J | |||||
| Bb§ | T6.0V | 0.050 | 13.2 J[34] | 15.4 J | ||||||
| Tau Ceti (BD−16°295)$ | 11.9118 ±0.0074 |
Cet | 01h 44m 04.1s −15° 56′ 15″ |
G8.5Vp[6] | 0.783 | 3.49# | 5.68 | 273.8097 ±0.1701[8] |
one debris disk four confirmed planets (e, f, g, and h) (2012, 2017), four candidate planets (b, c, d, and "i") (2012, 2019) | |
| GJ 1061 (LHS 1565) | 11.9839 ±0.0014 |
Hor* | 03h 35m 59.7s −44° 30′ 45″ |
M5.5V[6] | 0.113 | 13.09 | 15.26 | 272.1615 ±0.0316[8] |
has 3 known planets (2019)[35][36][37] | |
| YZ Ceti (LHS 138) | 12.1222 ±0.0015 |
Cet | 01h 12m 30.6s −16° 59′ 56″ |
M4.5V[6] | 0.130 | 12.02 | 14.17 | 269.0573 ±0.0337[8] |
flare star, three planets (b, c, and d) (2017)[38] | |
| Luyten's Star (BD+05°1668) | 12.3485 ±0.0019 |
CMi | 07h 27m 24.5s +05° 13′ 33″ |
M3.5Vn | 0.26 | 9.86 | 11.97 | 264.1269 ±0.0413[8] |
two planets (b, c) (2017)[39] and two suspected planets (d, e) (2019)[40] | |
| Teegarden's Star (SO025300.5+165258) | 12.4970 ±0.0045 |
Ari* | 02h 53m 00.9s +16° 52′ 53″ |
M6.5V | 0.08 | 15.14 | 17.22 | 260.9884 ±0.0934[8] |
has 3 known planets (2019, 2024)[41][42] | |
| Kapteyn's Star (CD−45°1841) | 12.8308 ±0.0008 |
Pic* | 05h 11m 40.6s −45° 01′ 06″ |
M1.5VI[6] | 0.281 | 8.84 | 10.87 | 254.1986 ±0.0168[8] |
two refuted planets (b and c) (2014)[43][44] | |
| Lacaille 8760 (AX Microscopii) | 12.9472 ±0.0018 |
Mic* | 21h 17m 15.3s −38° 52′ 03″ |
M0.0V[6] | 0.60 | 6.67 | 8.69 | 251.9124 ±0.0352[8] |
brightest M dwarf star in night sky, flare star | |
| SCR 1845−6357 | A | 13.0638 ±0.0070 |
Pav* | 18h 45m 05.3s −63° 57′ 48″ |
M8.5V[6] | 0.07 | 17.39 | 19.41 | 249.6651 ±0.1330[8] |
[37] |
| B§ | 18h 45m 02.6s −63° 57′ 52″ |
T6[45] | 0.03[6] | 13.3 J[34] | 15.3 J | |||||
| Kruger 60 (BD+56°2783) |
A | 13.0724 ±0.0052 |
Cep* | 22h 27m 59.5s +57° 41′ 45″ |
M3.0V[6] | 0.271 | 9.79 | 11.76 | 249.5 ±0.1[46] |
B flare star |
| B (DO Cephei) | M4.0V[6] | 0.176 | 11.41 | 13.38 | ||||||
| DENIS J1048−3956 | 13.1932 ±0.0027 |
Ant* | 10h 48m 14.7s −39° 56′ 06″ |
M8.5V[6] | 0.08 | 17.39 | 19.37 | 247.2156 ±0.0512[8] |
[47][48] | |
| Ross 614 (V577 Monocerotis, Gliese 234) |
A (LHS 1849) | 13.363 ±0.040 |
Mon* | 06h 29m 23.4s −02° 48′ 50″ |
M4.5V[6] | 0.223 | 11.15 | 13.09 | 244.07 ±0.73[49] |
A flare star |
| B (LHS 1850) | M5.5V | 0.111 | 14.23 | 16.17 | ||||||
| UGPS J0722-0540§ | 13.43 ±0.13 |
Mon | 07h 22m 27.3s –05° 40′ 30″ |
T9[6] | 0.010-0.025 | 16.52 J[50] | 18.45 J | 242.8 ±2.4[51] |
[52] | |
| Wolf 1061 (Gliese 628, BD−12°4523) | 14.0500 ±0.0016 |
Oph | 16h 30m 18.1s −12° 39′ 45″ |
M3.0V[6] | 0.294 | 10.07 | 11.93 | 232.1390 ±0.0268[8] |
three planets (b, c, and d) (2015)[53] | |
| Van Maanen's Star (Gliese 35, LHS 7)‡ | 14.0718 ±0.0011 |
Psc* | 00h 49m 09.9s +05° 23′ 19″ |
DZ7[6] | 0.67 | 12.38 | 14.21 | 231.7800 ±0.0183[8] |
closest-known free-floating white dwarf, third-known white dwarf possible debris disk (1917) | |
| Gliese 1 (CD−37°15492) | 14.1747 ±0.0022 |
Scl* | 00h 05m 24.4s −37° 21′ 27″ |
M1.5 V[6] | 0.45-0.48 | 8.55 | 10.35 | 230.0970 ±0.0362[8] |
||
| TZ Arietis (Gliese 83.1, L 1159–16) | 14.5780 ±0.0046 |
Ari | 02h 00m 13.2s +13° 03′ 08″ |
M4.5V[6] | 0.14 | 12.27 | 14.03 | 223.7321 ±0.0699[8] |
flare star, has one confirmed planet (b)[54] | |
| Wolf 424 (FL Virginis, LHS 333, Gliese 473) |
A | 14.595 ±0.031 |
Vir | 12h 33m 17.2s +09° 01′ 15″ |
M5.5Ve | 0.143 | 13.18 | 14.97 | 223.4775 ±0.4665[8] |
flare stars |
| B | M7Ve | 0.131 | 13.17 | 14.96 | ||||||
| Gliese 687 (LHS 450, BD+68°946) | 14.8395 ±0.0014 |
Dra | 17h 36m 25.9s +68° 20′ 21″ |
M3.0V[6] | 0.401 | 9.17 | 10.89 | 219.7898 ±0.0210[8] |
possible flare star, two planets (b) (2014)[55] and (c) (2020)[56] | |
| Gliese 674 (LHS 449) | 14.8492 ±0.0018 |
Ara* | 17h 28m 39.9s −46° 53′ 43″ |
M3.0V[6] | 0.35 | 9.38 | 11.09 | 219.6463 ±0.0262[8] |
one planet (b) (2007)[57] | |
| LHS 292 (LP 731-58) | 14.8706 ±0.0041 |
Sex* | 10h 48m 12.6s −11° 20′ 14″ |
M6.5V[6] | 0.08 | 15.60 | 17.32 | 219.3302 ±0.0602[8] |
flare star | |
| Gliese 440 (WD 1142-645, LP 145-141)‡ | 15.1226 ±0.0013 |
Mus* | 11h 45m 42.9s −64° 50′ 29″ |
DQ6[6] | 0.75 | 11.50 | 13.18 | 215.6753 ±0.0181[8] |
||
| GJ 1245 | A (G 208-44 A) | 15.2001 ±0.0034 |
Cyg | 19h 53m 54.2s +44° 24′ 55″ |
M5.5V[6] | 0.11 | 13.46 | 15.17 | 214.5745 ±0.0476[8] |
flare stars |
| B (G 208-45) | 19h 53m 55.2s +44° 24′ 56″ |
M6.0V[6] | 0.10 | 14.01 | 15.72 | |||||
| C (G 208-44 B) | 19h 53m 54.2s +44° 24′ 55″ |
M5.5 | 0.07 | 16.75 | 18.46 | |||||
| WISE 1741+2553§ | 15.22 ±0.20 |
Her* | 17h 41m 24.2s +25° 53′ 19″ |
T9 | 16.53 J | 18.18 J | 214.3 ±2.8[58] |
|||
| Gliese 876 (Ross 780) | 15.2382 ±0.0025 |
Aqr | 22h 53m 16.7s −14° 15′ 49″ |
M3.5V[6] | 0.37 | 10.17 | 11.81 | 214.0380 ±0.0356[8] |
four planets (d (2005), c (2001), b (1998), and e (2010))[59] | |
| WISE 1639−6847§ | 15.450 ±0.041 |
TrA* | 16h 39m 40.9s −68° 47′ 46″ |
Y0.5 | 20.57 J | 22.10 J | 211.11 ±0.56[60] |
|||
| LHS 288 (Luyten 143-23) | 15.7586 ±0.0034 |
Car* | 10h 44m 21.2s −61° 12′ 36″ |
M5.5V[6] | 0.11[6] | 13.90 | 15.51 | 206.9698 ±0.0448[8] |
||
| GJ 1002 | 15.8060 ±0.0036 |
Cet | 00h 06m 43.8s −07° 32′ 22″ |
M5.5V[6] | 0.11 | 13.76 | 15.40 | 206.3500 ±0.0474[8] |
two known planets (b & c, 2022)[61] | |
| DENIS 0255−4700§ | 15.877 ±0.014 |
Eri | 02h 55m 03.7s −47° 00′ 52″ |
L7.5V[6] | 0.025-0.065 | 22.92 | 24.44 | 205.4251 ±0.1857[8] |
[48] | |
| Groombridge 1618 (Gliese 380)$ | 15.8857 ±0.0017 |
UMa | 10h 11m 22.1s +49° 27′ 15″ |
K7.0V[6] | 0.67 | 6.59 | 8.16 | 205.3148 ±0.0224[8] |
flare star, one suspected debris disk | |
| Gliese 412 | A | 15.9969 ±0.0026 |
UMa | 11h 05m 28.6s +43° 31′ 36″ |
M1.0V[6] | 0.48 | 8.77 | 10.34 | 203.8876 ±0.0332[8] |
|
| B (WX Ursae Majoris) | 11h 05m 30.4s +43° 31′ 18″ |
M5.5V[6] | 0.10 | 14.48 | 16.05 | flare star | ||||
| AD Leonis | 16.1939 ±0.0024 |
Leo | 10h 19m 36.4s +19° 52′ 10″ |
M3.0V[6] | 0.39-0.42 | 9.32 | 10.87 | 201.4064 ±0.0296[8] |
flare star, 1 refuted planet (b[19] in 2020)[62] | |
| Gliese 832 | 16.2005 ±0.0019 |
Gru* | 21h 33m 34.0s −49° 00′ 32″ |
M1.5 V[6] | 0.45 | 8.66 | 10.20 | 201.3252 ±0.0237[8] |
possible flare star, two planets; one confirmed (b (2008)),[63] and the other now refuted (c (2014))[64][65] | |
| Gliese 682 (CD-44 11909) | 16.3328 ±0.0026 |
Sco* | 17h 37m 03.7s –44° 19′ 09″ |
M4 V | 0.27 | 10.95 | 12.45 | 199.6944 ±0.0312[8] |
has 2 disputed planets | |
| Omicron2 Eridani (40 Eridani, Gliese 166) |
Keid (A)$ | 16.3330 ±0.0042 |
Eri | 04h 15m 16.3s −07° 39′ 10″ |
K0.5 V | 0.84 | 4.43# | 5.93 | 199.6911 ±0.0512[8] |
has 1 refuted planet |
| B‡ | 04h 15m 21.8s −07° 39′ 29″ |
DA4 | 0.573 | 9.52 | 11.02 | |||||
| C | 04h 15m 21.5s −07° 39′ 22″ |
M4 V | 0.2036 | 11.24 | 12.74 | |||||
| EV Lacertae | 16.4761 ±0.0018 |
Lac* | 22h 46m 49.7s +44° 20′ 02″ |
M3.5 V | 0.35 | 10.22 | 11.70 | 197.9573 ±0.0220[8] |
record setting stellar flare observed | |
| 70 Ophiuchi (Gliese 702) | A$ | 16.7074 ±0.0087 |
Oph | 18h 05m 27.4s +02° 29′ 59″ |
K0 V | 0.90 | 4.21# | 5.66 | 195.2166 ±0.1012[46] |
|
| B$ | 18h 05m 27.5s +02° 29′ 56″ |
K5 V | 0.70 | 6.01# | 7.46 | |||||
| Altair (Alpha Aquilae)$ | 16.730 ±0.049 |
Aql* | 19h 50m 47.0s +08° 52′ 06″ |
A7 IV-Vn | 1.79 | 0.77# | 2.22 | 194.95 ±0.57[66] |
||
| EI Cancri (GJ 1116, G 9-38) | A | 16.800 ±0.011 |
Cnc | 08h 58m 15.2s +19° 45′ 47″ |
M5.5 V | 0.12 | 14.06 | 15.50 | 194.1443 ±0.1228[8] |
|
| B | M V | 0.10 | 14.92 | 16.36 | ||||||
| WISE J150649.97+702736.1§ | 16.856 ±0.052 |
UMi* | 15h 06m 52.4s +70° 27′ 25″ |
T6 | 13.74 J | 15.17 J | 193.5 ±0.6[58] |
|||
| GJ 3379 (G 99-49) | 16.9861 ±0.0027 |
Ori* | 06h 00m 03.5s +02° 42′ 24″ |
M3.5 V | 0.2312 | 11.31 | 12.73 | 192.0135 ±0.0310[8] | ||
| DENIS J081730.0−615520§ | 17.002 ±0.037 |
Car | 08h 17m 30.1s −61° 55′ 16″ |
T6 | 0.015 | 13.61 J | 15.03 J | 191.8362 ±0.4186[8] |
||
| Gliese 445 (LHS 2459, G 254-29) | 17.1368 ±0.0017 |
Cam* | 11h 47m 41.4s +78° 41′ 28″ |
M3.5 V | 0.14 | 10.79 | 12.19 | 190.3251 ±0.0194[8] |
||
| 2MASS J15404342−5101357 | 17.3738 ±0.0046 |
Nor* | 15h 40m 43.5s −51° 01′ 36″ |
M7 V | 0.090 | 15.26 | 16.63 | 187.7290 ±0.0496[8] |
||
| 2MASS 0939−2448 | A§ | 17.41 ±0.44 |
Ant | 09h 39m 35.5s −24° 48′ 28″ |
T8 V | 0.019–0.048 | 15.61 J | 16.97 J | 187.3 ±4.6[67] |
binary brown dwarf |
| B§ | T8 V | 0.019–0.038 | ||||||||
| GJ 3323 (LHS 1723, LP 656-38) | 17.5309 ±0.0026 |
Eri | 05h 01m 57.4s −06° 56′ 46″ |
M4 V | 0.1705 | 12.22 | 13.57 | 186.0466 ±0.0277[8] |
has 2 known planets | |
| Gliese 526 (Wolf 498, HD 119850) | 17.7263 ±0.0024 |
Boo* | 13h 45m 43.8s +14° 53′ 29″ |
M1 V | 0.28 | 8.46 | 9.78 | 183.9962 ±0.0253[8] |
||
| Stein 2051 (Gliese 169.1, G 175-34) | A | 17.9925 ±0.0020 |
Cam | 04h 31m 11.5s +58° 58′ 37″ |
M4 V | 0.252 | 11.04 | 12.33 | 181.2730 ±0.0203[8] |
|
| B‡ | 04h 31m 12.6s +58° 58′ 41″ |
DC5 | 0.675 | 12.43 | 13.72 | |||||
| 2MASS J11145133−2618235§ | 18.20 ±0.14 |
Hya | 11h 14m 51.3s −26° 18′ 24″ |
T7.5 | 0.029–0.048 | 15.86 J | 17.12 J | 179.2 ±1.4[68] |
||
| Gliese 251 (Wolf 294, HD 265866) | 18.2146 ±0.0028 |
Gem* | 06h 54m 49.0s +33° 16′ 05″ |
M3 V | 0.360 | 10.02 | 11.29 | 179.0629 ±0.0280[8] |
has 1 known planet | |
| LP 816-60 | 18.3305 ±0.0038 |
Cap* | 20h 52m 33.0s −16° 58′ 29″ |
M3.5 V | 0.224 | 11.50 | 12.75 | 177.9312 ±0.0365[8] |
||
| WISE 0350−5658§ | 18.49 ±0.24 |
Ret* | 03h 50m 00.3s −56° 58′ 30″ |
Y1 | 22.47 J | 23.70 J | 176.4 ±2.3[18] |
|||
| LSR J1835+3259 | 18.5534 ±0.0049 |
Lyr* | 18h 35m 37.9s +32° 59′ 55″ |
M8.5 V | 0.053 | 18.27 | 19.50 | 175.7930 ±0.0468[8] |
||
| Gliese 205 (Wolf 1453, HD 36395) | 18.6042 ±0.0022 |
Ori | 05h 31m 27.4s −03° 40′ 38″ |
M1 V | 0.556 | 7.95 | 9.17 | 175.3131 ±0.0204[8] |
||
| 2MASS J04151954−0935066§ | 18.62 ±0.18 |
Eri | 04h 15m 19.5s −09° 35′ 07″ |
T8 | 0.03 | 15.34 J | 16.56 J | 175.2 ±1.7[68] |
||
| Gliese 229 (HD 42581) | A | 18.7906 ±0.0018 |
Lep* | 06h 10m 34.6s −21° 51′ 53″ |
M1.5 V | 0.579 | 8.14 | 9.34 | 173.5740 ±0.0170[8] |
has 2 known planets |
| B§ | T6 V | 0.058 | 14.01 J | 15.21 J | ||||||
| Alsafi (Sigma Draconis)$ | 18.7993 ±0.0081 |
Dra | 19h 32m 21.6s +69° 39′ 40″ |
G9 V | 0.85 | 4.67# | 5.87 | 173.4939 ±0.0748[8] |
||
| Ross 47 (Gliese 213) | 18.8883 ±0.0031 |
Ori | 05h 42m 09.3s +12° 29′ 21″ |
M4 V | 0.35 | 11.57 | 12.76 | 172.6762 ±0.0286[8] |
||
| Gliese 570 (Lalande 27173, 33 G. Librae) |
A$ | 19.1987 ±0.0074 |
Lib* | 14h 57m 28.0s −21° 24′ 56″ |
K4 V | 0.802 | 5.64# | 6.79 | 169.8843 ±0.0653[8] |
|
| B | M1.5 V | 0.55 | 8.30 | 9.45 | ||||||
| C | M | 0.35 | 9.96 | 11.11 | ||||||
| D§ | T7.5 | 0.05 | 15.32 J | 16.47 J | ||||||
| Gliese 693 (Luyten 205–128) | 19.2078 ±0.0053 |
Pav | 17h 46m 32.4s −57° 19′ 09″ |
M3 V | 0.26 | 10.76 | 11.91 | 169.8042 ±0.0465[8] |
||
| Gliese 754 (Luyten 347–14) | 19.2724 ±0.0067 |
Tel* | 19h 20m 48.0s −45° 33′ 30″ |
M4 V | 0.173 | 12.23 | 13.37 | 169.2351 ±0.0588[8] |
has 1 candidate planet | |
| Gliese 908 (Lalande 46650, BR Piscium) | 19.2745 ±0.0032 |
Psc | 23h 49m 12.5s +02° 24′ 04″ |
M1 V | 0.37 | 8.98 | 10.12 | 169.2163 ±0.0281[8] |
||
| Gliese 752 (Wolf 1055, HD 180617) | A | 19.2922 ±0.0027 |
Aql | 19h 16m 55.3s +05° 10′ 08″ |
M2.5 V | 0.46 | 9.10 | 10.24 | 169.0615 ±0.0239[8] |
has 1 known planet |
| B (VB 10) | 19h 16m 57.6s +05° 09′ 02″ |
M8 V | 0.075 | 17.45 | 18.59 | very small and very dim red dwarf | ||||
| Gliese 588 (CD-40 9712) | 19.2996 ±0.0031 |
Lup* | 15h 32m 12.9s −41° 16′ 32″ |
M2.5 V | 0.43 | 9.31 | 10.45 | 168.9965 ±0.0270[8] |
has 2 candidate planets | |
| Eta Cassiopeiae (Gliese 34) | Achird (A)$ | 19.3314 ±0.0025 |
Cas* | 00h 49m 06.3s +57° 48′ 55″ |
G3 V | 0.972 | 3.46# | 4.60 | 168.7186 ±0.0216[8] |
|
| B | K7 V | 0.57 | 7.51 | 8.65 | ||||||
| 36 Ophiuchi (Gliese 663) | Guniibuu (A)$ | 19.4185 ±0.0036 |
Oph | 17h 15m 20.9s −26° 36′ 09″ |
K1.5 V | 0.85 | 5.07# | 6.20 | 167.9617 ±0.0311[8] |
|
| B$ | 17h 15m 21.0s −26° 36′ 10″ |
K1 V | 0.85 | 5.08# | 6.21 | |||||
| C$ | 17h 16m 13.4s −26° 32′ 46″ |
K5 V | 0.71 | 6.32# | 7.45 | |||||
| YZ Canis Minoris (Ross 882, Gliese 285) | 19.5330 ±0.0040 |
CMi | 07h 44m 40.2s +03° 33′ 09″ |
M4 V | 0.308 | 11.19 | 12.30 | 166.9769 ±0.0343[8] |
||
| WISE 1541−2250§ | 19.54 ±0.24 |
Lib | 15h 41m 51.6s −22° 50′ 25″ |
Y0.5 | 0.011 | 20.99 J | 22.10 J | 166.9 ±2.0[18] |
||
| GJ 1005 (Luyten 722-22, G 158-50) | A | 19.577 ±0.035 |
Cet | 00h 15m 28.1s −16° 08′ 02″ |
M3.5 V | 0.179 | 11.60 | 12.71 | 166.6 ±0.3[69] |
distance uncertain: 16.28±0.75, 17.91±0.67, 17.0±1.5, 16.26±0.76, 17.26, 19.695±0.095 ly |
| B | M V | 0.112 | 14.02 | 15.13 | ||||||
| HR 7703 (279 G. Sagittarii, HD 191408, Gliese 783, IRAS 20079-3614) | A$ | 19.609 ±0.013 |
Sgr | 20h 11m 11.93s –36° 06′ 04″ |
K2.5 V | 0.65 | 5.31# | 6.41 | 166.3272 ±0.1065[8] |
|
| B | M4 V | 0.24 | 11.50 | 12.60 | ||||||
| 82 G. Eridani (e Eridani, Gliese 139, HD 20794)$ | 19.7045 ±0.0093 |
Eri | 03h 19m 55.7s −43° 04′ 11″ |
G8 V | 0.70 | 4.26# | 5.35 | 165.5242 ±0.0784[8] |
has 3 confirmed planets, 3 candidate planets, hot and cold dust disks | |
| Gliese 268 (Ross 986, QY Aurigae) | A | 19.7414 ±0.0076 |
Aur* | 07h 10m 01.8s +38° 31′ 46″ |
M4.5 V | 0.226 | 12.05 | 13.14 | 165.2147 ±0.0636[8] |
|
| B | M V | 0.192 | 12.45 | 13.54 | ||||||
| Delta Pavonis$ | 19.893 ±0.015 |
Pav | 20h 08m 43.6s −66° 10′ 55″ |
G8 IV | 1.051 | 3.55# | 4.62 | 163.9544 ±0.1222[8] |
has 1 candidate planet | |
| SIMP J013656.5+093347§ | 19.955 ±0.057 |
Psc | 01h 36m 56.5s +09° 33′ 47″ |
T2.5 | 0.012 | 13.25 J | 14.32 J | 163.4478 ±0.4629[8] |
rogue planet, 12.7 MJ | |
| 2MASS 0937+2931§ | 19.96 ±0.22 |
Leo | 09h 37m 34.9s +29° 31′ 41″ |
T7 | 0.040 | 14.65 J | 15.71 J | 163.39 ±1.76[70] |
||
| System | Star or (sub-) brown dwarf | Distance (ly (±err))[7] |
Coordinates: RA, Dec (Ep J2000, Eq J2000)[6] |
Stellar class |
Mass M☉ |
App. | Abs. | Parallax (mas (±err)) [6][note 1] |
Notes and additional references | |
| Designation | Magnitude (mV[6] or mJ) | |||||||||
Distant future and past encounters
edit
Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astrometric measurements of parallax and total proper motions, along with spectroscopically determined radial velocities. Although extrapolations can be made into the past or future, they are subject to increasingly significant cumulative errors over very long periods.[2] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[72]
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.[73] 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 1.2 light-years (0.37 pc) from the Sun.[74]
Gaia's third data release has provided updated values for many of the candidates in the table below.[75][76][77][78]
| Star name | 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 |
|---|---|---|---|---|---|---|---|---|---|
| Gliese 710 | 0.167±0.012 | 1296+24 −23 |
62.248±0.020 | K7V | 0.4–0.6 | 9.6 | Serpens | 18h 19m 50.843s | −01° 56′ 18.98″ |
| HD 7977 | 0.478+0.104 −0.078 |
−2764+28 −29 |
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 | 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″ |
| 2MASS J0628+1845 | 1.61+0.28 −0.24 |
1720+150 −130 |
272.28±0.80 | M2.5V | 0.28 | 16.2 | Gemini | 06h 28m 11.593s | +18° 45′ 12.91″ |
| 2MASS J0805+4624 | 1.610+0.099 −0.092 |
−363+13 −14 |
238.1±1.0 | M3V | 0.25 | 17.0 | Lynx | 08h 05m 29.038s | +46° 24′ 51.78″ |
| CD-69 2001 | 1.616+0.070 −0.068 |
−1907±10 | 332.61±0.55 | K4V | 0.61 | 11.13 | Indus | 21h 40m 31.514s | −69° 25′ 14.58″ |
| HD 49995 | 1.70+0.23 −0.20 |
−4034+94 −98 |
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 J0621-0101 | 1.71+0.46 −0.39 |
−3206+68 −66 |
428.8±3.1 | G5V | 0.96 | 11.9 | Orion | 06h 21m 34.807s | −01° 01′ 55.01″ |
| LSPM J2146+3813 | 1.8557±0.0048 | 84.59±0.19 | 22.9858±0.0034 | M5V | ~0.15 | 10.82 | Cygnus | 21h 46m 22.285s | +38° 13′ 03.12″ |
| 2MASS J0455+1144 | 1.94+0.16 −0.15 |
1702+58 −54 |
349.50±0.80 | M0V | 0.50 | 15.3 | Orion | 04h 55m 21.427s | +11° 44′ 41.25″ |
| 2MASS J0734-0637 | 1.950±0.021 | −554.6±3.3 | 130.66±0.12 | M0V | 0.50 | 12.9 | Monoceros | 07h 34m 39.097s | −06° 37′ 12.21″ |
| 2MASS J1151-0313 | 1.98+0.20 −0.18 |
1017+60 −54 |
125.88±0.41 | M3.5V | 0.23 | 15.3 | Virgo | 11h 51m 37.434s | −03° 13′ 45.24″ |
| UCAC4 076–006432 | 2.042+0.034 −0.033 |
−893.8+7.9 −8.0 |
212.41±0.15 | mid K | ~0.6 | 12.69 | Mensa | 06h 34m 29.385s | −74° 49′ 47.12″ |
| 2MASS J0120+4739 | 2.25+0.17 −0.15 |
473+27 −25 |
237.56±0.66 | M3.5V | 0.25 | 16.5 | Andromeda | 01h 20m 04.561s | +47° 39′ 46.56″ |
| TYC 6760–1510–1 | 2.46+0.19 −0.18 |
−1708+44 −47 |
102.89±0.16 | M1.5V | 0.58 | 11.5 | Hydra | 15h 00m 09.536s | −29° 05′ 27.67″ |
| UCAC2 15719371 | 2.46±0.10 | −4282+70 −73 |
280.80±0.26 | K4V | 0.66 | 12.58 | Antlia | 09h 44m 09.884s | −37° 45′ 31.09″ |
| TYC 1662–1962–1 | 2.637+0.055 −0.054 |
−1536.6+9.0 −9.1 |
286.51±0.40 | Early K | ~0.8 | 10.95 | Vulpecula | 21h 14m 32.911s | +21° 53′ 32.76″ |
| HD 179939 | 2.65±0.17 | 3020±25 | 334.32±0.88 | A3V | 1.7 | 7.23 | Aquila | 19h 14m 10.043s | +07° 45′ 50.72″ |
| BD-21 1529 | 2.701+0.059 −0.058 |
−1660.1±6.3 | 368.48±0.56 | G5V | ~0.95 | 9.67 | Canis Major | 06h 37m 48.004s | −21° 22′ 21.94″ |
| 2MASS J1310-1307 | 2.79+0.59 −0.47 |
−1520+150 −190 |
433.0±2.6 | M2.5V | 0.34 | 16.3 | Virgo | 13h 10m 30.804s | −13° 07′ 33.55″ |
| UPM J1121-5549 | 2.803±0.020 | −282.5+1.6 −1.7 |
72.498±0.029 | M3V | 0.29 | 13.5 | Centaurus | 11h 21m 18.136s | −55° 49′ 17.77″ |
| UCAC4 464–006057 | 2.812+0.052 −0.051 |
932±11 | 101.570±0.086 | Early M | ~0.4 | 11.73 | Taurus | 04h 09m 02.050s | +02° 45′ 38.32″ |
| UCAC4 213–008644 | 2.91+0.13 −0.12 |
−306+12 −13 |
80.987±0.048 | M5.0 | 0.17 | 16.4 | Puppis | 06h 21m 54.714s | −47° 25′ 31.33″ |
| GJ 3649 | 3.016±0.024 | −520.4±3.1 | 54.435±0.023 | M1 | 0.49 | 10.85 | Leo | 11h 12m 38.97s | +18° 56′ 05.4″ |
| Ross 248 | 3.0446±0.0077 | 38.500±0.096 | 10.3057±0.0014 | M6V | 0.136 | 12.29 | Andromeda | 23h 41m 54.99s | +44° 10′ 40.8″ |
| 2MASS J1921-1244 | 3.08+0.21 −0.19 |
−3490+120 −130 |
376.46±0.73 | K6V | 0.69 | 12.46 | Sagittarius | 19h 21m 58.124s | −12° 43′ 58.61″ |
| Proxima Centauri | 3.123±0.015 | 28.65±0.27 | 4.24646±0.00028 | M5Ve | 0.15 | 11.05 | Centaurus | 14h 29m 42.949s | −62° 40′ 46.14″ |
| TYC 9387–2515–1 | 3.220+0.081 −0.079 |
−1509.1+8.6 −8.7 |
401.96±0.54 | K1V | 0.86 | 11.45 | Mensa | 06h 18m 54.643s | −80° 19′ 16.54″ |
| Alpha Centauri AB | 3.242±0.060 | 29.63+1.00 −0.98 |
4.321±0.024 | A: G2V B: K1V |
A: 1.100 B: 0.907[82] |
A: -0.01 B: +1.33 |
Centaurus | 14h 39m 36.495s | −60° 50′ 02.31″ |
| Gliese 445 | 3.3400±0.0051 | 46.341±0.065 | 17.1368±0.0017 | M4 | 0.15? | 10.8 | Camelopardalis | 11h 47m 41.377s | +78° 41′ 28.18″ |
| 2MASS J1638-6355 | 3.37+0.29 −0.28 |
−1428+21 −22 |
468.5±4.2 | K2V | 0.82 | 12.44 | Triangulum Australe | 16h 38m 21.759s | −63° 55′ 13.16″ |
| 2MASS J0542+3217 | 3.43+0.75 −0.71 |
5823+89 −87 |
884.6±2.4 | A: G4V B: K0V |
A: 1.01 B: 0.85 |
12.80 | Auriga | 05h 42m 38.349s | +32° 17′ 29.85″ |
| 2MASS J0625-2408 | 3.700+0.082 −0.080 |
−1874±14 | 534.88±0.93 | K/M | ~0.5 | 12.91 | Canis Major | 06h 25m 42.744s | −24° 08′ 35.02″ |
| Barnard's Star | 3.7682±0.0031 | 11.735±0.013 | 5.96290±0.00044 | sdM4 | 0.144 | 9.54 | Ophiuchus | 17h 57m 48.498s | +04° 41′ 36.25″ |
| BD+05 1792 | 3.965±0.040 | −962.7±3.0 | 239.73±0.33 | G2V | 1.07 | 8.58 | Gemini | 07h 48m 07.037s | +05° 27′ 22.51″ |
| 2MASS J2241-2759 | 4.05±0.16 | −2810+37 −38 |
411.06±0.76 | K7V | ~0.5 | 12.28 | Piscis Austrinus | 22h 41m 50.996s | −27° 59′ 47.04″ |
| 2MASS J1724-0522 | 4.15+0.26 −0.25 |
3058+54 −52 |
489.5±1.3 | K0V | 0.86 | 12.73 | Ophiuchus | 17h 24m 55.056s | −05° 22′ 11.45″ |
| StKM 1–554 | 4.217+0.036 −0.035 |
−549.9+2.9 −3.0 |
151.97±0.19 | M0V | 0.65 | 12.17 | Orion | 05h 14m 01.871s | +05° 22′ 56.26″ |
| GJ 3379 | 4.227±0.024 | −157.43+0.93 −0.94 |
16.9861±0.0027 | M3.5V | 0.19 | 11.31 | Orion | 06h 00m 03.824s | +02° 42′ 22.97″ |
| 2MASS J1936+3627 | 4.23+0.62 −0.57 |
3830+120 −110 |
671.6±3.4 | G5.5V | 0.95 | 12.2 | Cygnus | 19h 36m 57.294s | +36° 27′ 57.71″ |
| 2MASS J0710+5228 | 4.303±0.039 | 507.6+3.8 −3.7 |
90.949±0.050 | M3V | 0.33 | 12.52 | Lynx | 07h 10m 52.167s | +52° 28′ 18.49″ |
| HD 146248 | 4.341+0.040 −0.039 |
−1141.5±3.7 | 334.87±0.47 | G2/3IV | 1.23 | 9.47 | Triangulum Australe | 16h 19m 27.875s | −64° 50′ 34.38″ |
| 2MASS J1724+0355 | 4.37±0.12 | 1991+38 −37 |
254.99±0.26 | G8V | 0.85 | 12.54 | Ophiuchus | 17h 24m 34.633s | +03° 55′ 26.75″ |
| StKM 1–1456 | 4.396±0.043 | 1240.2+6.9 −6.8 |
144.934±0.095 | A: K5V B: M8V |
A: 0.81 B: 0.09 |
10.58 | Hercules | 17h 17m 31.118s | +15° 34′ 55.35″ |
| Zeta Leporis | 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″ |
| Lalande 21185 | 4.6807±0.0055 | 21.973±0.033 | 8.30437±0.00068 | M2V | 0.39 | 7.52 | Ursa Major | 11h 03m 20.194s | +35° 58′ 11.55″ |
| HD 68814 | 4.724+0.090 −0.089 |
−2242±13 | 259.85±0.30 | G6V | 0.98 | 9.57 | Hydra | 08h 13m 57.112s | −04° 03′ 12.56″ |
| 2MASS J1941-4602 | 4.814+0.050 −0.049 |
−456.5+4.1 −4.2 |
66.848±0.033 | M4-M6 | ~0.15 | 12.4 | Telescopium | 19h 41m 53.18s | −46° 02′ 31.4″ |
See also
editRelated lists
edit- List of stars with resolved images
- List of brightest stars
- List of star systems within 20–25 light-years
- List of star systems within 25–30 light-years
- List of star systems within 30–35 light-years
- List of star systems within 35–40 light-years
- List of star systems within 40–45 light-years
- List of star systems within 45–50 light-years
- List of star systems within 50–55 light-years
- List of star systems within 55–60 light-years
- List of star systems within 60–65 light-years
- List of star systems within 65–70 light-years
- List of star systems within 70–75 light-years
- List of star systems within 75–80 light-years
- List of star systems within 80–85 light-years
- List of star systems within 85–90 light-years
- List of star systems within 90–95 light-years
- List of star systems within 95–100 light-years
- List of nearest giant stars
- List of nearest supergiants
- List of nearest bright stars
- List of nearest exoplanets
- List of nearest terrestrial exoplanet candidates
- List of nearest stars by spectral type
- List of nearby stellar associations and moving groups
- List of star-forming regions in the Local Group
- Lists of stars
- List of Solar System objects by greatest aphelion
- List of trans-Neptunian objects
- List of nearest known black holes
Notes
editReferences
edit- ^ 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 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.
- ^ 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. S2CID 56269929.
- ^ Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
- ^ de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (2022). "An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced". Research Notes of the AAS. 6 (6): 136. Bibcode:2022RNAAS...6..136D. doi:10.3847/2515-5172/ac7b95.
- ^ 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 "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). 17 September 2007. Retrieved 6 November 2007.
- ^ 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 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 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e).
- ^ Suárez Mascareño, A.; Faria, J. P.; et al. (2020). "Revisiting Proxima with ESPRESSO". Astronomy & Astrophysics. 639: A77. arXiv:2005.12114. Bibcode:2020A&A...639A..77S. doi:10.1051/0004-6361/202037745. ISSN 0004-6361.
- ^ Faria, J. P.; Suárez Mascareño, A.; Figueira, P.; et al. (2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. EDP Sciences: A115. arXiv:2202.05188. Bibcode:2022A&A...658A.115F. doi:10.1051/0004-6361/202142337.
- ^ Drake, Nadia (12 April 2019). "A new super-Earth may orbit the star next door". National Geographic. Archived from the original on 13 April 2019. Retrieved 21 April 2019. Video of discovery being discussed (accidentally announced?)
- ^ Artigau, Étienne; Cadieux, Charles; Cook, Neil J.; Doyon, René; Vandal, Thomas; et al. (23 June 2022). "Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry". The Astronomical Journal. 164:84 (3) (published 8 August 2022): 18pp. arXiv:2207.13524. Bibcode:2022AJ....164...84A. doi:10.3847/1538-3881/ac7ce6.
- ^ Akeson, Rachel; Beichman, Charles; Kervella, Pierre; Fomalont, Edward; Benedict, G. Fritz (20 April 2021). "Precision Millimeter Astrometry of the α Centauri AB System". The Astronomical Journal. 162 (1): 14. arXiv:2104.10086. Bibcode:2021AJ....162...14A. doi:10.3847/1538-3881/abfaff. S2CID 233307418.
- ^ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
- ^ González Hernández, J. I.; et al. (October 2024). "A sub-Earth-mass planet orbiting Barnard's star". Astronomy & Astrophysics. 690. arXiv:2410.00569. doi:10.1051/0004-6361/202451311. A79.
{{cite journal}}: CS1 maint: numeric names: authors list (link) - ^ 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. S2CID 8419422.
- ^ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". Astronomy & Astrophysics. 618: A111. arXiv:1808.07835. Bibcode:2018A&A...618A.111L. doi:10.1051/0004-6361/201833626. S2CID 119540451.
- ^ a b c Kirkpatrick, J. Davy; Gelino, Christopher R.; 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. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. S2CID 227126954.
- ^ a b c Tuomi, M.; el, al. (11 June 2019). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
- ^ Lafarga, M.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Azzaro, M.; Béjar, V. J. S.; Cortés-Contreras, M.; Dreizler, S.; Hatzes, A. P.; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Montes, D.; Morales, J. C.; Oshagh, M.; Rodríguez-López, C.; Schöfer, P.; Schweitzer, A.; Zechmeister, M. (2021). "The CARMENES search for exoplanets around M dwarfs. Mapping stellar activity indicators across the M dwarf domain". Astronomy and Astrophysics. 652: 652. arXiv:2105.13467. Bibcode:2021A&A...652A..28L. doi:10.1051/0004-6361/202140605. S2CID 235248016.
- ^ Hurt, Spencer A.; Fulton, Benjamin; Isaacson, Howard; Rosenthal, Lee J.; Howard, Andrew W.; Weiss, Lauren M.; Petigura, Erik A. (2021), "Confirmation of the Long-Period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate", The Astronomical Journal, 163 (5): 218, arXiv:2107.09087, Bibcode:2022AJ....163..218H, doi:10.3847/1538-3881/ac5c47, S2CID 236134034
- ^ Abuter, R.; et al. (GRAVITY Collaboration) (May 2024). "Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY". Astronomy & Astrophysics. 685: L9. arXiv:2404.08746. Bibcode:2024A&A...685L...9G. doi:10.1051/0004-6361/202449547.
- ^ Benedict, G. Fritz; McArthur, Barbara E.; Gatewood, George; Nelan, Edmund; Cochran, William D.; Hatzes, Artie; Endl, Michael; Wittenmyer, Robert; Baliunas, Sallie L.; Walker, Gordon A. H.; Yang, Stephenson; Kürster, Martin; Els, Sebastian; Paulson, Diane B. (November 2006), "The extrasolar planet e Eridani b – orbit and mass", The Astronomical Journal, 132 (5): 2206–2218, arXiv:astro-ph/0610247, Bibcode:2006AJ....132.2206B, doi:10.1086/508323, S2CID 18603036.
- ^ Janson, M.; et al. (September 2008), "A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches", Astronomy & Astrophysics, 488 (2): 771–780, arXiv:0807.0301, Bibcode:2008A&A...488..771J, doi:10.1051/0004-6361:200809984, S2CID 119113471
- ^ Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; Luque, R.; et al. (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, S2CID 220075207
- ^ ESO. "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs" (PDF). Retrieved 15 November 2017.
- ^ 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. arXiv:0908.2624. Bibcode:2010A&ARv..18...67T. doi:10.1007/s00159-009-0025-1. S2CID 14006009.
- ^ General Catalogue of Trigonometric Parallaxes.
- ^ Hipparcos Catalogue.
- ^ Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel". Astronomische Nachrichten (in German). 16 (5–6): 65–96. Bibcode:1838AN.....16...65B. doi:10.1002/asna.18390160502.
(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist
A parallax of 313.6 mas yields a distance of 10.4 light years - ^ Kervella, Pierre; Arenou, Frédéric; et al. (2019). "Stellar and substellar companions of nearby stars from Gaia DR2". Astronomy & Astrophysics. 623: A72. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. S2CID 119491061.
This PMa offset between 61 Cyg A and B points at the possible presence of a third body in the system, likely orbiting around 61 Cyg B.
- ^ Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv:1804.03476. Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID 54990041.
- ^ Feng, Fabo; Anglada-Escudé, Guillem; Tuomi, Mikko; Jones, Hugh R. A.; Chanamé, Julio; Butler, Paul R.; Janson, Markus (14 October 2019), "Detection of the nearest Jupiter analog in radial velocity and astrometry data", Monthly Notices of the Royal Astronomical Society, 490 (4): 5002–5016, arXiv:1910.06804, Bibcode:2019MNRAS.490.5002F, doi:10.1093/mnras/stz2912, S2CID 204575783
- ^ a b c Chris Gelino, Davy Kirkpatrick, Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Archived from the original on 13 November 2013. Retrieved 10 June 2012.
{{cite web}}: CS1 maint: multiple names: authors list (link) (main page) Archived 11 May 2019 at the Wayback Machine - ^ Dreizler, S.; Jeffers, S. V.; Rodríguez, E.; Zechmeister, M.; Barnes, J.R.; Haswell, C.A.; Coleman, G. A. L.; Lalitha, S.; Hidalgo Soto, D.; Strachan, J.B.P.; Hambsch, F-J.; López-González, M. J.; Morales, N.; Rodríguez López, C.; Berdiñas, Z. M.; Ribas, I.; Pallé, E.; Reiners, Ansgar; Anglada-Escudé, G. (13 August 2019). "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. 493 (1): 536–550. arXiv:1908.04717. Bibcode:2020MNRAS.493..536D. doi:10.1093/mnras/staa248. S2CID 199551874.
- ^ Henry, Todd J.; Ianna, Philip A.; Kirkpatrick, J. Davy; Jahreiss, Hartmut (July 1997). "The solar neighborhood IV: discovery of the twentieth nearest star". The Astronomical Journal. 114 (1): 388–395. Bibcode:1997AJ....114..388H. doi:10.1086/118482.
- ^ a b Henry, Todd J.; Jao, Wei-Chun; Subasavage, John P.; Beaulieu, Thomas D.; Ianna, Philip A.; Costa, Edgardo; Méndez, René A. (December 2006). "The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample". The Astronomical Journal. 132 (6): 2360–2371. arXiv:astro-ph/0608230. Bibcode:2006AJ....132.2360H. doi:10.1086/508233. S2CID 15002841.
- ^ Astudillo-Defru, Nicola; Díaz, Rodrigo F.; Bonfils, Xavier; Almenara, José M.; Delisle, Jean-Baptiste; Bouchy, François; Delfosse, Xavier; Forveille, Thierry; Lovis, Christophe; Mayor, Michel; Murgas, Felipe; Pepe, Francesco; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Wünsche, Anaël (2017). "The HARPS search for southern extra-solar planets. XLII. A system of Earth-mass planets around the nearby M dwarf YZ Ceti". Astronomy & Astrophysics. 605: L11. arXiv:1708.03336. Bibcode:2017A&A...605L..11A. doi:10.1051/0004-6361/201731581. S2CID 119393757.
- ^ 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. arXiv:1703.05386. Bibcode:2017A&A...602A..88A. doi:10.1051/0004-6361/201630153. S2CID 119418595.
- ^ 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. arXiv:2006.09403. Bibcode:2020A&A...641A..23P. doi:10.1051/0004-6361/202038047. S2CID 219721292.
{{cite journal}}: CS1 maint: numeric names: authors list (link) - ^ Caballero, J. A.; Reiners, Ansgar; Ribas, I.; Dreizler, S.; Zechmeister, M.; et al. (12 June 2019). "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF). Astronomy & Astrophysics. 627: A49. arXiv:1906.07196. Bibcode:2019A&A...627A..49Z. doi:10.1051/0004-6361/201935460. ISSN 0004-6361. S2CID 189999121.
- ^ Dreizler, S.; Luque, R.; et al. (April 2024). "Teegarden's Star revisited: A nearby planetary system with at least three planets". Astronomy & Astrophysics. 684: A117. arXiv:2402.00923. Bibcode:2024A&A...684A.117D. doi:10.1051/0004-6361/202348033.
- ^ Anglada-Escude, G.; et al. (2014). "Two planets around Kapteyn's star : a cold and a temperate super-Earth orbiting the nearest halo red-dwarf". Monthly Notices of the Royal Astronomical Society: Letters. 443: L89–L93. arXiv:1406.0818. Bibcode:2014MNRAS.443L..89A. doi:10.1093/mnrasl/slu076. hdl:2299/19219. S2CID 67807856.
- ^ Bortle, Anna; et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal. 161 (5): 230. arXiv:2103.02709. Bibcode:2021AJ....161..230B. doi:10.3847/1538-3881/abec89. S2CID 232110395.
- ^ 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. arXiv:0706.3824. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881. S2CID 1860702.
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.
- ^ 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. arXiv:astro-ph/0502167. Bibcode:2005AJ....129.1954J. doi:10.1086/428489. S2CID 16164903.
- ^ a b Costa, Edgardo; Méndez, René A.; Jao, W. -C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer (2005). "The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation-First Results from the 1.5 m Telescope Program". The Astronomical Journal. 130 (1): 337. Bibcode:2005AJ....130..337C. doi:10.1086/430473.
- ^ George Gatewood; et al. (2003). "An Astrometric Study of the Low-Mass Binary Star Ross 614" (PDF). The Astronomical Journal. 125 (3): 1530–1536. Bibcode:2003AJ....125.1530G. doi:10.1086/346143. S2CID 119597659. Archived from the original (PDF) on 19 December 2021. Retrieved 15 March 2022.
- ^ 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. arXiv:1004.0317. Bibcode:2010MNRAS.408L..56L. doi:10.1111/j.1745-3933.2010.00927.x. S2CID 16032606.
- ^ Leggett, Sandy K.; Saumon, Didier; Marley, Mark S.; Lodders, Katharina; Canty, J.; Lucas, Philip W.; Smart, Richard L.; Tinney, Chris G.; Homeier, Derek; Allard, France; Burningham, Ben; Day-Jones, Avril; Fegley, Bruce; Ishii, Miki; Jones, Hugh R. A.; Marocco, Federico; Pinfield, David J.; Tamura, Motohide (2012). "The Properties of the 500 K Dwarf UGPS J072227.51-054031.2 and a Study of the Far-red Flux of Cold Brown Dwarfs". The Astrophysical Journal. 748 (2): 74. arXiv:1201.2973. Bibcode:2012ApJ...748...74L. doi:10.1088/0004-637X/748/2/74. S2CID 14171934.
- ^ 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].
- ^ "Nearby star hosts closest alien planet in the 'habitable zone'". Phys.org. 16 December 2015. Retrieved 16 December 2015.
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.
- ^ Quirrenbach, A.; et al. (2022), "The CARMENES search for exoplanets around M dwarfs", Astronomy & Astrophysics, 663: A48, arXiv:2203.16504, Bibcode:2022A&A...663A..48Q, doi:10.1051/0004-6361/202142915, S2CID 247835988.
- ^ The Lick–Carnegie exoplanet survey: Gliese 687 b: A Neptune-mass planet orbiting a nearby red dwarf Archived March 27, 2014, at the Wayback Machine
- ^ 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", The Astrophysical Journal Supplement Series, 250 (2): 29, arXiv:2008.07998, Bibcode:2020ApJS..250...29F, doi:10.3847/1538-4365/abb139, S2CID 221150644 Accepted for publication by ApJS
- ^ "The Extrasolar Planet Encyclopaedia — Catalog Listing". Extrasolar Planets Encyclopaedia. Archived from the original on 2 July 2007.
- ^ a b Kirkpatrick, J. Davy; Martin, Emily C.; Smart, Richard L.; Cayago, Alfred J.; Beichman, Charles A.; Marocco, Federico; Gelino, Christopher R.; Faherty, Jacqueline K.; Cushing, Michael C.; Schneider, Adam C.; Mace, Gregory N.; Tinney, Christopher G.; Wright, Edward L.; Lowrance, Patrick J.; Ingalls, James G.; Vrba, Frederick J.; Munn, Jeffrey A.; Dahm, Scott E.; McLean, Ian S. (2019). "Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime". The Astrophysical Journal Supplement. 240 (19): 19. arXiv:1812.01208. Bibcode:2019ApJS..240...19K. doi:10.3847/1538-4365/aaf6af. S2CID 119451195.
- ^ Rivera, Eugenio J.; et al. (July 2010). "The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration". The Astrophysical Journal. 719 (1): 890–899. arXiv:1006.4244. Bibcode:2010ApJ...719..890R. doi:10.1088/0004-637X/719/1/890. S2CID 118707953.
- ^ Fontanive, C.; Bedin, L. R.; Bardalez Gagliuffi, D. C. (1 February 2021). "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. arXiv:2011.13873. Bibcode:2021MNRAS.501..911F. doi:10.1093/mnras/staa3732. ISSN 0035-8711.
- ^ Suárez Mascareño, A.; González-Alvarez, E.; et al. (November 2022). "Two temperate Earth-mass planets orbiting the nearby star GJ 1002". Astronomy & Astrophysics. 670: A5. arXiv:2212.07332. Bibcode:2023A&A...670A...5S. doi:10.1051/0004-6361/202244991. S2CID 254353639.
- ^ 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. arXiv:2002.10562. Bibcode:2020A&A...638A...5C. doi:10.1051/0004-6361/201937369. S2CID 211296466.
{{cite journal}}: CS1 maint: numeric names: authors list (link) - ^ Bailey, Jeremy; et al. (2009). "A Jupiter-like Planet Orbiting the Nearby M Dwarf GJ832". The Astrophysical Journal. 690 (1): 743–747. arXiv:0809.0172. Bibcode:2009ApJ...690..743B. doi:10.1088/0004-637X/690/1/743. S2CID 17172233.
- ^ Wittenmyer, R. A.; Tuomi; et al. (2014). "GJ 832c: A super-earth in the habitable zone". The Astrophysical Journal. 791 (2): 114. arXiv:1406.5587. Bibcode:2014ApJ...791..114W. doi:10.1088/0004-637X/791/2/114. S2CID 12157837.
- ^ Gorrini, P.; Astudillo-Defru, N.; Dreizler, S.; et al. (2022). "Detailed stellar activity analysis and modelling of GJ 832". Astronomy & Astrophysics. 664. EDP Sciences: A64. arXiv:2206.07552. Bibcode:2022A&A...664A..64G. doi:10.1051/0004-6361/202243063. ISSN 0004-6361.
- ^ van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
- ^ Burgasser, Adam J.; Tinney, C. G.; Cushing, Michael C.; Saumon, Didier; Marley, Mark S.; Bennett, Clara S.; Kirkpatrick, J. Davy (2008). "2MASS J09393548-2448279: The Coldest and Least Luminous Brown Dwarf Binary Known?" (PDF). The Astrophysical Journal. 689 (1): L53–L56. Bibcode:2008ApJ...689L..53B. doi:10.1086/595747.
- ^ a b Dupuy, Trent J.; Liu, Michael C. (2012). "The Hawaii Infrared Parallax Program. I. Ultracool Binaries and the L/T Transition". The Astrophysical Journal Supplement. 201 (2): 19. arXiv:1201.2465. Bibcode:2012ApJS..201...19D. doi:10.1088/0067-0049/201/2/19. S2CID 119256363.
- ^ Benedict, G. F.; Henry, T. J.; Franz, O. G.; McArthur, B. E.; Wasserman, L. H.; Jao, Wei-Chun; Cargile, P. A.; Dieterich, S. B.; Bradley, A. J.; Nelan, E. P.; Whipple, A. L. (2016). "The Solar Neighborhood. XXXVII. The Mass–Luminosity Relation for Main-Sequence M Dwarfs". The Astronomical Journal. 152 (5): 141. arXiv:1608.04775. Bibcode:2016AJ....152..141B. doi:10.3847/0004-6256/152/5/141. S2CID 54029447.
- ^ Schilbach, E.; Röser, S.; Scholz, R.-D. (2009). "Trigonometric parallaxes of ten ultracool subdwarfs". Astronomy and Astrophysics. 493 (2): L27–L30. arXiv:0811.4136. Bibcode:2009A&A...493L..27S. doi:10.1051/0004-6361:200811281. S2CID 17774863.
- ^ "Milky Way Past Was More Turbulent Than Previously Known". ESO News. European Southern Observatory. 6 April 2004.
After more than 1,000 nights of observations spread over 15 years, they have determined the spatial motions of more than 14,000 solar-like stars residing in the neighbourhood of the Sun.
- ^ See also: Stellar kinematics.
- ^ 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. Bibcode:1999AJ....117.1042G. doi:10.1086/300723. S2CID 122929693.
- ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (13 August 2018). "New stellar encounters discovered in the second data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
- ^ Bailer-Jones, C. A. L. (13 July 2022). "Stars that approach within one parsec of the Sun: New and more accurate encounters identified in Gaia Data Release 3". The Astrophysical Journal Letters. 935 (1): 152. arXiv:2207.06258. Bibcode:2022ApJ...935L...9B. doi:10.3847/2515-5172/ac842b. S2CID 251154282.
- ^ Bobylev, Vadim; Bajkova, Anisa (14 July 2022). "Search for Close Stellar Encounters with the Solar System Based on Data from the Gaia DR3 Catalogue". Astronomy Letters. 48 (9): 542–549. arXiv:2206.14443. Bibcode:2022AstL...48..542B. doi:10.1134/S1063773722080011. S2CID 256832377.
- ^ de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (28 June 2022). "An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced". Research Notes of the AAS. 6 (6): 136. Bibcode:2022RNAAS...6..136D. doi:10.3847/2515-5172/ac7b95.
- ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (28 July 2022). "The Closest Past Flyby of a Known Star to the Solar System: HD 7977, UCAC4 237-008148 or WISE J072003.20-084651.2?". Research Notes of the AAS. 6 (7): 152. Bibcode:2022RNAAS...6..152D. doi:10.3847/2515-5172/ac842b. S2CID 251154282.
- ^ Table 3, Bobylev, Vadim V. (March 2010). "Searching for Stars Closely Encountering with the Solar System". Astronomy Letters. 36 (3): 220–226. arXiv:1003.2160. Bibcode:2010AstL...36..220B. doi:10.1134/S1063773710030060. S2CID 118374161.
- ^ 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. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
- ^ Bobylev, Vadim; Bajkova, Anisa (29 June 2022). "Search for Close Stellar Encounters with the Solar System Based on Data from the Gaia DR3 Catalogue". Astronomy Letters. 48 (9): 542–549. arXiv:2206.14443. Bibcode:2022AstL...48..542B. doi:10.1134/S1063773722080011. S2CID 256832377.
- ^ "A Family Portrait of the Alpha Centauri System - VLT Interferometer Studies the Nearest Stars". European Southern Observatory. 15 March 2003. Retrieved 24 January 2011.
External links
edit- "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.
- Nemiroff, R.; Bonnell, J., eds. (18 March 2001). "Map of the 25 nearest star systems". Astronomy Picture of the Day. NASA. Retrieved 24 October 2005.
- "Notable Nearby Stars". SolStation. Retrieved 24 October 2005.
- "Cool stars in the solar Neighbourhood". D. Montes, UCM. Retrieved 14 November 2005.
- 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 13 October 2006.
- 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. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. S2CID 119279752.
.png){kind=link}