List of nearest stars and brown dwarfs to Earth
File:Flying among the closest stars to the Solar System.ogv
There are 52 stellar systems beyond our own Solar system that currently lie within 5.0 parsecs (16.3 light-years) of the Sun. These systems contain a total of 63 stars, of which 50 are red dwarfs, by far the most common type of star in the Milky Way. Much more massive stars, such as our own, make up the remaining 13. In addition to these "true" stars, there are 11 brown dwarfs (objects not quite massive enough to fuse hydrogen), and 4 white dwarfs (extremely dense objects that remain after stars such as our Sun exhaust all fusable hydrogen in their core and slowly shed their outer layers while only the collapsed core remains). Despite the relative proximity of these objects to Earth, only nine (not including the Sun) are brighter than 6.5 apparent magnitude, the dimmest magnitude visible to the naked eye from Earth.[1] All of these objects are located in the Local Bubble, a region within the Orion–Cygnus Arm of the Milky Way.
Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will possibly approach the Solar system to less than 5.0 parsecs (16 light-years) over the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec (3.3 light-years) and another 7 within 0.5 parsecs (1.6 light-years).[2] This number is likely much higher, due to the sheer number of stars needed to be surveyed; a star approaching the Solar System 10 million years ago, moving at a typical Sun-relative 20–200 kilometers per second, would be 600–6,000 light years from the Sun at present day, with millions of stars closer to the Sun. The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun.[3] It is currently predicted to pass 19,300 ± 3,200 astronomical units (0.305 ± 0.051 light-years) from the Sun in +0.041
−0.039 million years from the present, close enough to significantly disturb our Solar System's 1.280Oort cloud.[2][3]
The easiest way to determine stellar distance to the Sun for objects at these distances is parallax, which measures how much stars appear to move against background objects over the course of Earth's orbit around the Sun. As a parsec (parallax-second) is defined by the distance of an object that would appear to move exactly one second of arc against background objects, stars less than 5 parsecs away will have measured parallaxes of over 0.2 arcseconds, or 200 milliarcseconds. Determining past and future positions relies on accurate astrometric measurements of their parallax and total proper motions (how far they move across the sky due to their actual velocity relative to the Sun), along with spectroscopically determined radial velocities (their speed directly towards or away from us, which combined with proper motion defines their true movement through the sky relative to the Sun). Both of these measurements are subject to increasing and significant errors over very long time spans, especially over the several thousand-year time spans it takes for stars to noticeably move relative to each other.[4]
List[edit | edit source]
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Visible to the unaided eye |
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Brown dwarf |
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White dwarf |
The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible colors. Some of the parallax and distance results are preliminary measurements.[5]
Designation | Distance[6] (light-years (±err)) |
Stellar class | Apparent magnitude (mV[5] or mJ) |
Absolute magnitude (MV[5] or MJ) |
Epoch J2000.0 | Parallax (mas (±err)) [5][note 1] |
Discovery date [note 2] |
Notes and additional references | ||
---|---|---|---|---|---|---|---|---|---|---|
System | Star | Right ascension[5] | Declination[5] | |||||||
Solar System | Sun | 0 | G2V[5] | −26.74![]() |
4.85 | N/A | N/A | N/A | N/A | eight planets |
Alpha Centauri (Rigil Kentaurus) |
Proxima Centauri (V645 Centauri) | ±0.0011 4.2441 | M5.5Ve | 11.09 | 15.53 | 14h 29m 43.0s | −62° 40′ 46″ | ±0.20 768.50[7] | 1915 | flare star, one planet (b) (2016) |
α Centauri A (HD 128620) | ±0.0068 4.3650 | G2V[5] | 0.01![]() |
4.38 | 14h 39m 36.5s | −60° 50′ 02″ | ±1.17 747.23 [8][9][10] |
N/A | ||
α Centauri B (HD 128621) | K1V[5] | 1.34![]() |
5.71 | 14h 39m 35.1s | −60° 50′ 14″ | 1689 | one suspected planet (c) (2013) (planet b refuted in 2015) | |||
Barnard's Star (BD+04°3561a) | ±0.0032 5.9577 | M4.0Ve | 9.53 | 13.22 | 17h 57m 48.5s | +04° 41′ 36″ | ±0.29 547.45[7] | 1916 | flare star, largest known proper motion[11] | |
Luhman 16 (WISE 1049−5319) ![]() |
Luhman 16A![]() |
±0.0011 6.5029 | L8±1[12] | 10.7 J | 14.2 J | 10h 49m 15.57s | −53° 19′ 06″ | ±0.082 501.557[13] | 2013 | one refuted planet (Ab[14] in 2017[15]) |
Luhman 16B![]() |
T1±2[12] | |||||||||
WISE 0855−0714![]() |
±0.13 7.26[16] | Y2 | 25.0 J | 08h 55m 10.83s | −07° 14′ 42.5″ | ±8 449[17] | 2014 | sub-brown dwarf | ||
Wolf 359 (CN Leonis) | ±0.031 7.856 | M6.0V[5] | 13.44 | 16.55 | 10h 56m 29.2s | +07° 00′ 53″ | ±1.62 415.16[18] | 1919 | flare star | |
Lalande 21185 (BD+36°2147) | ±0.014 8.307 | M2.0V[5] | 7.47 | 10.44 | 11h 03m 20.2s | +35° 58′ 12″ | ±0.67 392.64[19] | 1801 | one suspected planet (2017)[20] | |
Sirius (α Canis Majoris) |
Sirius A | ±0.010 8.659 | A1V[5] | −1.46![]() |
1.42 | 06h 45m 08.9s | −16° 42′ 58″ | ±0.45 376.68[7] | N/A | brightest star in the night sky |
Sirius B![]() |
DA2[5] | 8.44 | 11.34 | 1844 | ||||||
Luyten 726-8 | Luyten 726-8 A (BL Ceti) | ±0.012 8.791 | M5.5Ve | 12.54 | 15.40 | 01h 39m 01.3s | −17° 57′ 01″ | ±0.5 371.0[7] | 1949 | flare star (Archetypal member) |
Luyten 726-8 B (UV Ceti) | M6.0Ve | 12.99 | 15.85 | |||||||
Ross 154 (V1216 Sagittarii) | ±0.0019 9.7035 | M3.5Ve | 10.43 | 13.07 | 18h 49m 49.4s | −23° 50′ 10″ | ±0.064 336.123[7] | 1925 | flare star | |
Ross 248 (HH Andromedae) | ±0.0041 10.2903 | M5.5Ve | 12.29 | 14.79 | 23h 41m 54.7s | +44° 10′ 30″ | ±0.13 316.96[7] | 1925 | flare star | |
Epsilon Eridani (BD−09°697) | ±0.016 10.446 | K2V[5] | 3.73![]() |
6.19 | 03h 32m 55.8s | −09° 27′ 30″ | ±0.47 312.22[7] | 150 | three circumstellar disks, two suspected planets (AEgir (debated) and c) (2000 & 2002)[21] | |
Lacaille 9352 (CD−36°15693) | ±0.0016 10.7211 | M0.5V | 7.34 | 9.75 | 23h 05m 52.0s | −35° 51′ 11″ | ±0.045 304.219[7] | 1753 | ||
Ross 128 (FI Virginis) | ±0.0026 11.0074 | M4.0Vn | 11.13 | 13.51 | 11h 47m 44.4s | +00° 48′ 16″ | ±0.070 296.307[7] | 1925 | flare star, one planet (b) (2017)[22] | |
EZ Aquarii (Gliese 866, Luyten 789-6) |
EZ Aquarii A | ±0.034 11.109 | M5.0Ve | 13.33 | 15.64 | 22h 38m 33.4s | −15° 17′ 57″ | ±0.9 293.60[23] | 1937 | A & B flare stars |
EZ Aquarii B | M? | 13.27 | 15.58 | 1937 | ||||||
EZ Aquarii C | M? | 14.03 | 16.34 | 1995 | ||||||
61 Cygni | 61 Cygni A (BD+38°4343) | ±0.0012 11.4008 | K5.0V[5] | 5.21![]() |
7.49 | 21h 06m 53.9s | +38° 44′ 58″ | ±0.03 286.08[7] | N/A | B flare star, first star (besides Sun) to have measured distance[24] possible circumstellar disk. |
61 Cygni B (BD+38°4344) | K7.0V[5] | 6.03![]() |
8.31 | 21h 06m 55.3s | +38° 44′ 31″ | 1725 | ||||
Procyon (α Canis Minoris) |
Procyon A | ±0.032 11.402 | F5V–IV[5] | 0.38![]() |
2.66 | 07h 39m 18.1s | +05° 13′ 30″ | ±0.81 286.05 [8][9] |
N/A | |
Procyon B![]() |
DQZ[5] | 10.70 | 12.98 | 1844 | ||||||
Struve 2398 (Gliese 725, BD+59°1915) |
Struve 2398 A (HD 173739) | ±0.0012 11.4880 | M3.0V[5] | 8.90 | 11.16 | 18h 42m 46.7s | +59° 37′ 49″ | ±0.03 283.91[7] | 1835 | flare stars |
Struve 2398 B (HD 173740) | M3.5V[5] | 9.69 | 11.95 | 18h 42m 46.9s | +59° 37′ 37″ | 1835 | ||||
Groombridge 34 (Gliese 15) |
Groombridge 34 A (GX Andromedae) | ±0.0008 11.6182 | M1.5V[5] | 8.08 | 10.32 | 0h 18m 22.9s | +44° 01′ 23″ | ±0.02 280.73[7] | 1813 | flare star, two suspected planets (Ac, 2017) and Ab, 2014)[25] |
Groombridge 34 B (GQ Andromedae) | M3.5V[5] | 11.06 | 13.30 | 1813 | flare star | |||||
DX Cancri (G 51-15) | ±0.0056 11.6780 | M6.5Ve | 14.78 | 16.98 | 08h 29m 49.5s | +26° 46′ 37″ | ±0.13 279.29[7] | 1972 | flare star | |
Tau Ceti (BD−16°295) | ±0.022 11.753 | G8Vp[5] | 3.49![]() |
5.68 | 01h 44m 04.1s | −15° 56′ 15″ | ±0.52 277.52[7] | N/A | one debris disk two planets (e and f) (2012), three suspected planets (d, g and h) (2012, 2017), two refuted planets (b and c in 2017) | |
Epsilon Indi (CPD−57°10015) |
Epsilon Indi A | ±0.011 11.869 | K5Ve[5] | 4.69![]() |
6.89 | 22h 03m 21.7s | −56° 47′ 10″ | ±0.25 274.80[7] | N/A | one planet (b) (2018)[26] |
Epsilon Indi Ba![]() |
T1.0V | 12.3 J[27] | 22h 04m 10.5s | −56° 46′ 58″ | 2003 | |||||
Epsilon Indi Bb![]() |
T6.0V | 13.2 J[27] | 2003 | |||||||
GJ 1061 (LHS 1565) | ±0.0029 11.9803 | M5.5V[5] | 13.09 | 15.26 | 03h 35m 59.7s | −44° 30′ 45″ | ±0.066 272.245[7] | 1995 | [28][29] | |
YZ Ceti (LHS 138) | ±0.0035 12.1084 | M4.5V[5] | 12.02 | 14.17 | 01h 12m 30.6s | −16° 59′ 56″ | ±0.078 269.363[7] | 1961 | flare star, three planets (b, c, and d) (2017),[30] one suspected planet (e) | |
Luyten's Star (BD+05°1668) | ±0.036 12.199 | M3.5Vn | 9.86 | 11.97 | 07h 27m 24.5s | +05° 13′ 33″ | ±0.79 267.36[31] | 1935 | two planets (b, c) (2017)[32] | |
Teegarden's Star (SO025300.5+165258) | ±0.013 12.496 | M6.5V | 15.14 | 17.22 | 02h 53m 00.9sg | +16° 52′ 53″ | ±0.27 261.01[7] | 2003 | tentative radial velocity variation (2010)[29][33] | |
SCR 1845-6357 | SCR 1845-6357 A | ±0.054 12.571 | M8.5V[5] | 17.39 | 19.41 | 18h 45m 05.3s | −63° 57′ 48″ | ±1.11 259.45 [note 3] |
2004 | [29] |
SCR 1845-6357 B![]() |
T6[34] | 13.3 J[27] | 18h 45m 02.6s | −63° 57′ 52″ | 2006 | |||||
Kapteyn's Star (CD−45°1841) | ±0.0013 12.8294 | M1.5V[5] | 8.84 | 10.87 | 05h 11m 40.6s | −45° 01′ 06″ | ±0.026 254.226[7] | 1898 | two suspected planets (b and c) (2014)[35] | |
Lacaille 8760 (AX Microscopii) | ±0.0029 12.9515 | M0.0V[5] | 6.67 | 8.69 | 21h 17m 15.3s | −38° 52′ 03″ | ±0.056 251.829[7] | 1753 | flare star | |
Kruger 60 (BD+56°2783) |
Kruger 60 A | ±0.0052 13.0724 | M3.0V[5] | 9.79 | 11.76 | 22h 27m 59.5s | +57° 41′ 45″ | ±0.1 249.5[7] | 1880 | B flare star |
Kruger 60 B (DO Cephei) | M4.0V[5] | 11.41 | 13.38 | 1890? | ||||||
DEN 1048-3956![]() |
±0.0066 13.1932 | M8.5V[5] | 17.39 | 19.37 | 10h 48m 14.7s | −39° 56′ 06″ | ±0.12 247.22[7] | 2001 | [36][37] | |
Ross 614 (V577 Monocerotis, Gliese 234) |
Ross 614A (LHS 1849) | ±0.049 13.424 | M4.5V[5] | 11.15 | 13.09 | 06h 29m 23.4s | −02° 48′ 50″ | ±0.88 242.97[7] | 1927 | A flare star |
Ross 614B (LHS 1850) | M5.5V | 14.23 | 16.17 | 1936 | ||||||
UGPS J0722-0540![]() |
±0.13 13.43 | T9[5] | 16.52 J[38] | 07h 22m 27.3s | –05° 40′ 30″ | ±2.4 242.8[39] | 2010 | [40] | ||
Wolf 1061 (Gliese 628, BD−12°4523) | ±0.0038 14.0458 | M3.0V[5] | 10.07 | 11.93 | 16h 30m 18.1s | −12° 39′ 45″ | ±0.063 232.210[7] | 1919 | three planets (b, c, and d) (2015)[41] | |
Wolf 424 (FL Virginis, LHS 333, Gliese 473) |
Wolf 424 A | ±0.26 14.05 | M5.5Ve | 13.18 | 14.97 | 12h 33m 17.2s | +09° 01′ 15″ | ±4.3 232.2[42] | 1919 | flare stars |
Wolf 424 B | M7Ve | 13.17 | 14.96 | 1941 | ||||||
Van Maanen's star (Gliese 35, LHS 7)![]() |
±0.0023 14.0744 | DZ7[5] | 12.38 | 14.21 | 00h 49m 09.9s | +05° 23′ 19″ | ±0.038 231.737[7] | 1896 | closest known free-floating white dwarf, third known white dwarf possible debris disk (1917), possible planet (b) (2004) (debated) | |
Gliese 1 (CD−37°15492) | ±0.0037 14.1725 | M1.5 V [5] | 8.55 | 10.35 | 00h 05m 24.4s | −37° 21′ 27″ | ±0.060 230.133[7] | 1884 | ||
WISE 1639-6847![]() |
±0.56 14.30[note 4] | Y0.5 | 20.57 J | 22.10 J | 16h 39m 40.9s | −68° 47′ 46″ | ±8.9 228.1[43] | 2012 | ||
L 1159-16 (TZ Arietis, Gliese 83.1) | ±0.0070 14.5843 | M4.5V[5] | 12.27 | 14.03 | 02h 00m 13.2s | +13° 03′ 08″ | ±0.11 223.63[7] | unknown | flare star | |
Gliese 674 (LHS 449) | ±0.0033 14.8387 | M3.0V[5] | 9.38 | 11.09 | 17h 28m 39.9s | −46° 53′ 43″ | ±0.049 219.801[7] | unknown | one planet (b) (2007)[44] | |
Gliese 687 (LHS 450, BD+68°946) | ±0.0022 14.8401 | M3.0V[5] | 9.17 | 10.89 | 17h 36m 25.9s | +68° 20′ 21″ | ±0.032 219.781[7] | unknown | possible flare star, one planet (b) (2014)[45] | |
LHS 292 (LP 731-58) | ±0.011 14.885 | M6.5V[5] | 15.60 | 17.32 | 10h 48m 12.6s | −11° 20′ 14″ | ±0.16 219.12[7] | unknown | flare star | |
WISE J0521+1025![]() |
±3 15[note 4] | T7.5[46] | 15.26 J | 16.95 J | 05h 21m 26.3s | +10° 25′ 28″ | ±40 217.5 | 2012 | distance highly uncertain | |
LP 145-141 (WD 1142-645, Gliese 440)![]() |
±0.0023 15.1182 | DQ6[5] | 11.50 | 13.18 | 11h 45m 42.9s | −64° 50′ 29″ | ±0.032 215.737[7] | 1917 | ||
G 208-44 G 208-45 (GJ 1245) |
G 208-44 A (V1581 Cyg) | ±0.0050 15.2090 | M5.5V[5] | 13.46 | 15.17 | 19h 53m 54.2s | +44° 24′ 55″ | ±0.07 214.45[7] | unknown | flare stars |
G 208-45 | M6.0V[5] | 14.01 | 15.72 | 19h 53m 55.2s | +44° 24′ 56″ | unknown | ||||
G 208-44 B | M5.5 | 16.75 | 18.46 | 19h 53m 54.2s | +44° 24′ 55″ | unknown | ||||
Gliese 876 (Ross 780) | ±0.0054 15.2504 | M3.5V[5] | 10.17 | 11.81 | 22h 53m 16.7s | −14° 15′ 49″ | ±0.076 213.867[7] | unknown | four planets (d (2005), c (2001), b (1998), and e (2010))[47] two possible planets (f and g) (2014) (debated) | |
LHS 288 (Luyten 143-23) | ±0.0056 15.7703 | M5.5V[5] | 13.90 | 15.51 | 10h 44m 21.2s | −61° 12′ 36″ | ±0.074 206.817[7] | unknown | one tentative planet (b) (2007)[29] | |
GJ 1002 | ±0.0098 15.8164 | M5.5V[5] | 13.76 | 15.40 | 00h 06m 43.8s | −07° 32′ 22″ | ±0.13 206.21[7] | unknown | ||
Groombridge 1618 (Gliese 380) | ±0.0026 15.8797 | K7.0V[5] | 6.59 | 8.16 | 10h 11m 22.1s | +49° 27′ 15″ | ±0.034 205.392[7] | 1838 | flare star, one suspected debris disk, one suspected planet (b) (1989) (tentative) | |
DEN 0255-4700![]() |
±0.020 15.885 | L7.5V[5] | 22.92 | 24.44 | 02h 55m 03.7s | −47° 00′ 52″ | ±0.25 205.33[7] | 1999 | [37] | |
Gliese 412 | Gliese 412 A | ±0.013 15.983 | M1.0V[5] | 8.77 | 10.34 | 11h 05m 28.6s | +43° 31′ 36″ | ±0.17 204.06[7] | 1850s? | |
Gliese 412 B (WX Ursae Majoris) | M5.5V[5] | 14.48 | 16.05 | 11h 05m 30.4s | +43° 31′ 18″ | 1850s? | flare star | |||
Gliese 832 | ±0.0034 16.1939 | M1.5 V[5] | 8.66 | 10.20 | 21h 33m 34.0s | −49° 00′ 32″ | ±0.043 201.407[7] | 1910s? | possible flare star, two planets (b (2008) and c (2014))[48][49] | |
AD Leonis | ±0.0055 16.1970 | M3.0V[5] | 9.32 | 10.87 | 10h 19m 36.4s | +19° 52′ 10″ | ±0.068 201.368[7] | 1850s? | flare star | |
GJ 1005 | GJ 1005 A | ±0.76 16.26[note 4] | M4V[50] | 11.48[50] | 00h 15m 28.11s | −16° 08′ 01.6″ | ±9.4 200.5[50] | unknown | ||
GJ 1005 B | M7V | ? | ? | unknown | ||||||
System | Star | Distance[6] (Light-years (±err)) |
Stellar class | Apparent magnitude (mV[5] or mJ) |
Absolute magnitude (MV[5] or MJ) |
Right ascension[5] | Declination[5] | Parallax (mas (±err)) [5][note 1] |
Discovery date [note 2] |
Notes and Additional references |
Designation | Epoch J2000.0 |
Maps of nearby stars[edit | edit source]
Distant future and past encounters[edit | edit source]
Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astrometric measurements of parallax and total proper motions, along with spectroscopically determined radial velocities. Although predictions can be extrapolated back into the past or forward into the future, they are subject to increasing significant cumulative errors over very long periods.[4] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[51]
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.[52] 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.[53]
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.
Star name | HIP number |
Minimum distance (light-years) |
Date of approach in 1000s of years |
Current distance (light-years) |
Stellar classification |
Mass in M☉ | Current apparent magnitude |
Current Constellation | Current Right ascension |
Current Declination |
---|---|---|---|---|---|---|---|---|---|---|
Gliese 710 | 89825 | +0.043 −0.036 0.178 |
+41 −39 1280 |
±0.057 62.103 | K7V | 0.4–0.6 | 9.6 | Serpens | 18h 19m 50.843s | −01° 56′ 18.98″ |
2MASS J0610-4246 | N/A | +0.084 −0.090 0.755 |
164.4+8.8 −8.9 −1 |
±0.60 319.75 | early K | ~0.8 | 11.79 | Puppis | 06h 10m 55.448s | −42° 46′ 03.39″ |
Scholz's star and companion brown dwarf | N/A | +0.37 −0.22 0.82 |
+10 −14 −69 |
±3.4 19.6 | M9+T5 | 0.15 | 18.3 | Monoceros | 07h 20m 03.20s | −08° 46′ 51.2″ |
HD 283856 | N/A | +0.75 −0.55 1.13 |
+40 −34 374 |
±17 290 | K0V (binary?) | ~0.8 | 10.46 | Taurus | 04h 48m 28.124s | +27° 00′ 39.06″ |
TYC 1662-1962-1 | N/A | +0.22 −0.21 1.84 |
+18 −19 −1513 |
±1.0 284.5 | Early K | ~0.8 | 10.95 | Vulpecula | 21h 14m 32.911s | +21° 53′ 32.76″ |
HD 7977 | N/A | +0.18 −0.16 1.88 |
+44 −46 −2798 |
±0.70 247.03 | G0V | ~1.2 | 9.04 | Cassiopeia | 01h 20m 31.597s | +61° 52′ 57.08″ |
2MASS J2146+3813 | N/A | +0.18 −0.15 1.89 |
+8.0 −6.8 84.4 |
±0.0083 22.9603 | M5V | ~0.15 | 10.82 | Cygnus | 21h 46m 22.285s | +38° 13′ 03.12″ |
2MASS J0634-7449 | N/A | +0.083 −0.080 2.169 |
+12 −13 −898 |
±0.29 213.28 | mid K | ~0.6 | 12.69 | Mensa | 06h 34m 29.385s | −74° 49′ 47.12″ |
TYC 2730-1701-1 | N/A | +0.31 −0.29 2.31 |
+21 −22 −714 |
±9.1 829.1 | G? | ~1 | 9.44 | Pegasus | 21h 50m 41.029s | +36h 20m 46.73s |
2MASS J0409+0245 | N/A | +0.088 −0.091 2.684 |
±13 912 | ±0.18 101.40 | Early M | ~0.4 | 11.73 | Taurus | 04h 09m 02.050s | +02° 45′ 38.32″ |
Gliese 3649 | N/A | +0.093 −0.089 2.975 |
±12 −509 | ±0.048 54.415 | M1 | 0.49 | 10.85 | Leo | 11h 12m 38.97s | +18° 56′ 05.4″ |
2MASS J0605+4020 | N/A | +4.5 −2.1 2.9 |
+210 −350 −860 |
±20 248 | K | ~0.5 | 12.07 | Auriga | 06h 05m 05.077s | +40° 20′ 37.72″ |
2MASS J1818-4038 | N/A | +1.3 −1.1 3.0 |
+54 −50 1049 |
±5.6 191.4 | K/M | ~0.5 | 11.97 | Corona Australis | 18h 18m 17.213s | −40° 38′ 39.48″ |
BD-21 1529 | N/A | +0.29 −0.28 3.01 |
+14 −15 −1685 |
±1.8 374.1 | G5V | ~0.95 | 9.67 | Canis Major | 06h 37m 48.004s | −21° 22′ 21.94″ |
Ross 248 | N/A | +0.15 −0.14 3.11 |
+1.9 −1.8 39.2 |
±0.0041 10.2903 | M6V | 0.136 | 12.29 | Andromeda | 23h 41m 54.99s | +44° 10′ 40.8″ |
Proxima Centauri | 70890 | ±0.0033 3.1034 | ±0.054 28.677 | ±0.0011 4.2441 | M5Ve | 0.15 | 11.05 | Centaurus | 14h 29m 42.949s | −62° 40′ 46.14″ |
Alpha Centauri AB | A: 71683 B: 71685 |
±0.060 3.242 | +1.00 −0.98 29.63 |
±0.024 4.321 | A: G2V B: K1V |
A: 1.100 B: 0.907[56] |
A: -0.01 B: +1.33 |
Centaurus | 14h 39m 36.495s | −60° 50′ 02.31″ |
Gliese 445 | 57544 | ±0.0050 3.3365 | ±0.052 46.301 | ±0.0043 17.1424 | M4 | 0.15? | 10.8 | Camelopardalis | 11h 47m 41.377s | +78° 41′ 28.18″ |
HIP 117795 | 117795 | ±0.013 3.433 | ±0.21 93.46 | ±0.075 87.336 | K8V | ~0.5 | 10.6 | Cassiopeia | 23h 53m 20.014s | +59° 56′ 42.95″ |
2MASS J0625-2408 | N/A | +0.25 −0.27 3.59 |
+30 −31 −1849 |
±2.7 537.1 | K/M | ~0.5 | 12.91 | Canis Major | 06h 25m 42.744s | −24° 08′ 35.02″ |
Barnard's Star | 87937 | ±0.0074 3.7604 | ±0.027 11.731 | ±0.0032 5.9577 | sdM4 | 0.144 | 9.54 | Ophiuchus | 17h 57m 48.498s | +04° 41′ 36.25″ |
2MASS J2241-2759 | N/A | +0.67 −0.62 3.79 |
+53 −55 −2809 |
±2.6 414.7 | K7V | ~0.5 | 12.28 | Piscis Austrinus | 22h 41m 50.996s | −27° 59′ 47.04″ |
Gliese 3379 | N/A | ±0.016 4.194 | ±0.52 −156.13 | ±0.0063 16.9813 | M3.5V | 0.19 | 11.31 | Orion | 06h 00m 03.824s | +02° 42′ 22.97″ |
Zeta Leporis | 27288 | +0.59 −0.51 4.70 |
+45 −49 −860 |
±0.65 71.34 | A2Vann | 2.0 | 3.55 | Lepus | 05h 46m 57.341s | −14° 49′ 19.02″ |
Lalande 21185 | 54035 | ±0.018 4.692 | +0.082 −0.081 22.039 |
±0.014 8.307 | M2V | 0.39 | 7.52 | Ursa Major | 11h 03m 20.194s | +35° 58′ 11.55″ |
2MASS J1941-4602 | N/A | +0.087 −0.085 4.854 |
+6.5 −6.7 −463.7 |
±0.066 66.996 | M4-M6 | ~0.15 | 12.4 | Telescopium | 19h 41m 53.18s | −46° 02′ 31.4″ |
See also[edit | edit source]
![]() |
- Interstellar travel
- List of brightest stars
- list of star systems within 15–20 light years
- List of star systems within 20–25 light-years
- List of star systems within 25–30 light-years
- List of nearest bright stars
- List of nearest exoplanets
- List of nearest galaxies
- Lists of stars
- Nearby Stars Database
- Stars and planetary systems in fiction
- The Magnificent Seven
- List of Solar System objects by greatest aphelion
- List of trans-Neptunian objects
Notes[edit | edit source]
- ↑ a b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
- ↑ a b Before 1900: earliest certain recorded observation. 1900–1930: first catalogued. After 1930: earliest trigonometric or spectroscopic parallax.
- ↑ Systems with their first accurate trigonometric parallaxes measured by RECONS
- ↑ a b c Might not be within 5 parsecs of the Sun.
References[edit | edit source]
- ↑ Weaver, Harold F. (1947). "The Visibility of Stars Without Optical Aid". Publications of the Astronomical Society of the Pacific. 59 (350): 232–243. Bibcode:1947PASP...59..232W. doi:10.1086/125956.
- ↑ a b Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616 (37): A37. arXiv:1805.07581
. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456.
- ↑ a b Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
- ↑ a b Matthews, R. A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. 35: 1. Bibcode:1994QJRAS..35....1M.
- ↑ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap aq ar as at au av aw ax ay az ba bb bc bd be bf "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). September 17, 2007. Retrieved 2007-11-06.
- ↑ a b From parallax.
- ↑ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an Gaia Collaboration. "Gaia DR2". gea.esac.esa.int. Retrieved 10 May 2018.
- ↑ a b General Catalogue of Trigonometric Parallaxes.
- ↑ a b Hipparcos Catalogue.
- ↑ Söderhjelm, Staffan (1999). "Visual binary orbits and masses POST HIPPARCOS". Astronomy and Astrophysics. 341: 121. Bibcode:1999A&A...341..121S.
- ↑ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
- ↑ a b Luhman, K. L. (2013). "Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun". The Astrophysical Journal Letters. 767 (1): L1. arXiv:1303.2401
. Bibcode:2013ApJ...767L...1L. doi:10.1088/2041-8205/767/1/L1.
- ↑ Lazorenko, P. F.; Sahlmann, J. (23 August 2018). "Updated astrometry and masses of the LUH 16 brown dwarf binary". arXiv:1808.07835
[astro-ph.SR].
- ↑ Boffin, H. M. J.; et al. (2013). "Possible astrometric discovery of a substellar companion to the closest binary brown dwarf system WISE J104915.57-531906.1". Astronomy & Astrophysics. 561: L4. arXiv:1312.1303
. Bibcode:2014A&A...561L...4B. doi:10.1051/0004-6361/201322975.
- ↑ Bedin L. R.; et al. (27 June 2017). "Hubble Space Telescope astrometry of the closest brown dwarf binary system - I. Overview and improved orbit". Monthly Notices of the Royal Astronomical Society. 470 (1): 1140–1155. arXiv:1706.00657
. Bibcode:2017MNRAS.470.1140B. doi:10.1093/mnras/stx1177. Retrieved 27 June 2017.
- ↑ Luhman, K. L. (April 21, 2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal Letters. 786 (2): L18. arXiv:1404.6501
. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18.
- ↑ Luhman, K. L.; Esplin, T. L. (6 September 2016). "The Spectral Energy Distribution of the Coldest Known Brown Dwarf". The Astronomical Journal. 152 (3): 78. arXiv:1605.06655
. Bibcode:2016AJ....152...78L. doi:10.3847/0004-6256/152/3/78. ISSN 1538-3881.
- ↑ Davison, Cassy L.; et al. (19 February 2015). "A 3D Search for Companions to 12 Nearby M-Dwarfs". The Astronomical Journal. 149 (3): 106. arXiv:1501.05012
. Bibcode:2015AJ....149..106D. doi:10.1088/0004-6256/149/3/106. ISSN 1538-3881.
- ↑ van Leeuwen, F. (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv:0708.1752
. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. ISSN 0004-6361.
- ↑ Bailer-Jones, C. A. L.; et al. (2017). "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey". The Astronomical Journal. 153 (5): 208. arXiv:1702.03571
. doi:10.3847/1538-3881/aa66ca.
- ↑ Janson, M.; et al. (September 2008), "A comprehensive examination of the ε Eridani system. Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches", Astronomy and Astrophysics, 488 (2): 771–780, arXiv:0807.0301
, Bibcode:2008A&A...488..771J, doi:10.1051/0004-6361:200809984
- ↑ 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 and Astrophysics Review. 18 (1–2): 67–126. arXiv:0908.2624
. Bibcode:2010A&ARv..18...67T. doi:10.1007/s00159-009-0025-1.
- ↑ 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 - ↑ Bailer-Jones, C. A. L.; et al. (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: 51. arXiv:1408.5645
. doi:10.1088/0004-637X/794/1/51.
- ↑ 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].
- ↑ a b c Chris Gelino, Davy Kirkpatrick, Adam Burgasser. "DwarfArchives.org: Photometry, spectroscopy, and astrometry of M, L, and T dwarfs". caltech.edu. Retrieved 2012-06-10. (main page)
- ↑ 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 c d Henry, Todd J.; Jao, Wei-Chun; Subasavage, John P.; Beaulieu, Thomas D.; Ianna, Philip A.; Costa, Edgardo; Méndez, René A. (December 2006). "The Solar Neighborhood. XVII. Parallax Results from the CTIOPI 0.9 m Program: 20 New Members of the RECONS 10 Parsec Sample". The Astronomical Journal. 132 (6): 2360–2371. arXiv:astro-ph/0608230
. Bibcode:2006AJ....132.2360H. doi:10.1086/508233.
- ↑ Bailer-Jones, C. A. L.; et al. (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
. doi:10.1051/0004-6361/201731581.
- ↑ Gatewood, George (1 July 2008). "Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions". The Astronomical Journal. 136 (1): 452–460. Bibcode:2008AJ....136..452G. doi:10.1088/0004-6256/136/1/452.
- ↑ Bailer-Jones, C. A. L.; 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 & Astrophysics. 602: A88. arXiv:1703.05386
. doi:10.1051/0004-6361/201630153.
- ↑ Barnes, J. R.; et al. (2012). "ROPS: A New Search for Habitable Earths in the Southern Sky". Monthly Notices of the Royal Astronomical Society. 424 (1): 591–604. arXiv:1204.6283
. Bibcode:2012MNRAS.424..591B. doi:10.1111/j.1365-2966.2012.21236.x.
- ↑ 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 and Astrophysics. 471 (2): 655. arXiv:0706.3824
. Bibcode:2007A&A...471..655K. doi:10.1051/0004-6361:20077881.
- ↑ 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.
- ↑ 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. Bibcode:2005AJ....129.1954J. doi:10.1086/428489.
- ↑ 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.
- ↑ 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". arXiv:1004.0317v2
[astro-ph.SR].
- ↑ Leggett, S. K.; et al. (1 April 2012). "The Properties of the 500 K Dwarf UGPS J072227.51-054031.2, and a Study of the Far-Red Flux of Cold Brown Dwarfs". The Astrophysical Journal. 748 (2): 74. arXiv:1201.2973
. Bibcode:2012ApJ...748...74L. doi:10.1088/0004-637X/748/2/74. ISSN 0004-637X.
- ↑ 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. 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.
- ↑ Gliese, W. and Jahreiß, H. (1991). "Gl 473". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 10 May 2018.
- ↑ Martin, Emily C.; et al. (17 September 2018). "Y dwarf Trigonometric Parallaxes from the Spitzer Space Telescope". arXiv:1809.06479
[astro-ph.SR].
- ↑ "The Extrasolar Planet Encyclopaedia — Catalog Listing".
- ↑ 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.
- ↑ Bihain, G.; Scholz, R.-D.; Storm, J.; Schnurr, O. (26 August 2013). "An overlooked brown dwarf neighbour (T7.5 at ~ 5 pc) of the Sun and two additional T dwarfs at about 10 pc". Astronomy & Astrophysics. 557 (43): A43. arXiv:1307.2722
. Bibcode:2013A&A...557A..43B. doi:10.1051/0004-6361/201322141.
- ↑ 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.
- ↑ 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.
- ↑ 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.
- ↑ a b c "G 158-50 - SIMBAD". SIMBAD. Retrieved 2015-09-12.
- ↑ 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 [ITAL]Hipparcos[/ITAL] Data". The Astronomical Journal. 117 (2): 1042–1055. doi:10.1086/300723.
- ↑ 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
. doi:10.1051/0004-6361/201833456.
- ↑ 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.
- ↑ 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.
- ↑ "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 | edit source]
- List of nearest stars and brown dwarfs at Wikipedia, the free Terran encyclopedia that anyone can 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. (March 18, 2001). "Map of the 25 nearest star systems". Astronomy Picture of the Day. NASA. Retrieved 2005-10-24.
- "Notable Nearby Stars". SolStation. Retrieved 2005-10-24.
- "Cool stars in the solar Neighbourhood". D. Montes, UCM. Retrieved 2005-11-14.
- The dynamics of the closest stars
- Takeda, G.; E. B. Ford; A. Sills; F. A. Rasio; D. A. Fischer; J. A. Valenti (2006). "Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~ 1000 Cool Stars from the SPOCS Catalog". California & Carnegie Planet Search. Retrieved 2006-10-13.
- Nearest Stars 3D View
- Table 4 "The Census of Stars and Brown Dwarfs within 8 Parsecs of the Sun" in Bailer-Jones, C. A. L.; et al. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 156. arXiv:1205.2122
. doi:10.1088/0004-637X/753/2/156.
- http://phl.upr.edu/projects/nearby-stars-catalog