List of nearest stars
![Rotating 3D image of the nearest stars](http://upload.wikimedia.org/wikipedia/commons/thumb/5/53/Nearest_stars_rotating_red-green.gif/400px-Nearest_stars_rotating_red-green.gif)
![](http://upload.wikimedia.org/wikipedia/commons/thumb/4/4c/3d_glasses_red_green.svg/37px-3d_glasses_red_green.svg.png)
There are 52 stellar systems beyond our own Solar system that currently lie within 5.0 parsecs (16.3 light-years) of the Sun. These systems contain a total of 63 stars, of which 50 are red dwarfs, by far the most common type of star in the Milky Way. Much more massive stars, such as our own, make up the remaining 13. In addition to these "true" stars, there are 11 brown dwarfs (objects not quite massive enough to fuse hydrogen), and 4 white dwarfs (extremely dense objects that remain after stars such as our Sun exhaust all fusable hydrogen in their core and slowly shed their outer layers while only the collapsed core remains). Despite the relative proximity of these objects to Earth, only nine exceed 6.5 apparent magnitude, the dimmest magnitude visible to the naked eye from Earth.[1] All of these objects are located in the Local Bubble, a region within the Orion–Cygnus Arm of the Milky Way.
Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will possibly approach the Solar system to less than 5.0 parsecs (16 light-years) over the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec (3.3 light-years) and another 7 within 0.5 parsecs (1.6 light-years),[2] although this number is likely, in reality, much higher, due to the sheer number of stars needed to be surveyed. A star approaching the Solar System 10 million years ago, moving at 200 kilometers per second, would be more than 6,000 light years from the Sun at present day, with hundreds of millions of stars closer to the Sun. The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun.[3] It is currently predicted to pass 19,300 ± 3,200 astronomical units (0.305 ± 0.051 light-years) from the Sun in 1.280+0.041
−0.039 million years from the present, close enough to significantly disturb our Solar System's Oort cloud.[2][3]
The easiest way to determine stellar distance to the Sun for objects at these distances is parallax, which measures how much stars appear to move against background objects over the course of Earth's orbit around the Sun. As a parsec (parallax-second) is defined by the distance of an object that would appear to move exactly one second of arc against background objects, stars less than 5 parsecs away will have measured parallaxes of over 0.2 arcseconds, or 200 milliarcseconds. Determining past and future positions relies on accurate astrometric measurements of their parallax and total proper motions (how far they move across the sky due to their actual velocity relative to the Sun), along with spectroscopic determined radial velocities (their speed directly towards or away from us, which combined with proper motion defines their true movement through the sky relative to the Sun). Both of these measurements are subject to increasing and significant errors over very long time spans, especially over the several thousand-year time spans it takes for stars to noticeably move relative to each other.[4]
List
# | Visible to the unaided eye |
§ | Brown dwarf |
‡ | White dwarf |
The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible colors. Some of the parallax and distance results are preliminary measurements.[5]
Designation | Distance[6] (light-years (±err)) |
Stellar class | Apparent magnitude (mV or mJ) | Absolute magnitude (MV or MJ) | Epoch J2000.0 | Parallax (mas (±err)) [5][note 1] |
Discovery date [note 2] |
Notes and additional references | ||
---|---|---|---|---|---|---|---|---|---|---|
System | Star # | Right ascension[5] | Declination[5] | |||||||
Solar System | Sun | 0 | G2V[5] | −26.74[5]# | 4.85[5] | — | — | — | — | eight planets |
Alpha Centauri (Rigil Kentaurus) |
Proxima Centauri (V645 Centauri) | 4.2441±0.0011 | M5.5Ve | 11.09[5] | 15.53[5] | 14h 29m 43.0s | −62° 40′ 46″ | 768.50±0.20[7] | 1915 | flare star, one planet (b) (2016) |
α Centauri A (HD 128620) | 4.3650±0.0068 | G2V[5] | 0.01[5]# | 4.38[5] | 14h 39m 36.5s | −60° 50′ 02″ | 747.23±1.17 [8][9][10] |
— | ||
α Centauri B (HD 128621) | K1V[5] | 1.34[5]# | 5.71[5] | 14h 39m 35.1s | −60° 50′ 14″ | 1689 | one suspected planet (c) (2013) (planet b refuted in 2015) | |||
Barnard's Star (BD+04°3561a) | 5.9577±0.0032 | M4.0Ve | 9.53[5] | 13.22[5] | 17h 57m 48.5s | +04° 41′ 36″ | 547.45±0.29[7] | 1916 | flare star, largest known proper motion[11] | |
Luhman 16 (WISE 1049−5319)§ |
Luhman 16A§ | 6.5049±0.0012 | L8±1[12] | 10.7 J | 14.2 J | 10h 49m 15.57s | −53° 19′ 06″ | 501.398±0.093[13] | 2013 | one refuted planet (Ab[14] in 2017[13]) |
Luhman 16B§ | T1±2[12] | |||||||||
WISE 0855−0714§ | 7.26±0.13[15] | Y2 | 25.0 J | 08h 55m 10.83s | −07° 14′ 42.5″ | 449±8[16] | 2014 | sub-brown dwarf | ||
Wolf 359 (CN Leonis) | 7.856±0.031 | M6.0V[5] | 13.44[5] | 16.55[5] | 10h 56m 29.2s | +07° 00′ 53″ | 415.16±1.62[17] | 1919 | flare star | |
Lalande 21185 (BD+36°2147) | 8.307±0.014 | M2.0V[5] | 7.47[5] | 10.44[5] | 11h 03m 20.2s | +35° 58′ 12″ | 392.64±0.67[18] | 1801 | one suspected planet (2017)[19] | |
Sirius (α Canis Majoris) |
Sirius A | 8.659±0.010 | A1V[5] | −1.46[5]# | 1.42[5] | 06h 45m 08.9s | −16° 42′ 58″ | 376.68±0.45[7] | — | brightest star in the night sky |
Sirius B‡ | DA2[5] | 8.44[5] | 11.34[5] | 1844 | ||||||
Luyten 726-8 | Luyten 726-8 A (BL Ceti) | 8.791±0.012 | M5.5Ve | 12.54[5] | 15.40[5] | 01h 39m 01.3s | −17° 57′ 01″ | 371.0±0.5[7] | 1949 | flare star (Archetypal member) |
Luyten 726-8 B (UV Ceti) | M6.0Ve | 12.99[5] | 15.85[5] | |||||||
Ross 154 (V1216 Sagittarii) | 9.7035±0.0019 | M3.5Ve | 10.43[5] | 13.07[5] | 18h 49m 49.4s | −23° 50′ 10″ | 336.123±0.064[7] | 1925 | flare star | |
Ross 248 (HH Andromedae) | 10.2903±0.0041 | M5.5Ve | 12.29[5] | 14.79[5] | 23h 41m 54.7s | +44° 10′ 30″ | 316.96±0.13[7] | 1925 | flare star | |
Epsilon Eridani (BD−09°697) | 10.446±0.016 | K2V[5] | 3.73[5]# | 6.19[5] | 03h 32m 55.8s | −09° 27′ 30″ | 312.22±0.47[7] | 150 | three circumstellar disks, two suspected planets (AEgir (debated) and c) (2000 & 2002)[20] | |
Lacaille 9352 (CD−36°15693) | 10.7211±0.0016 | M0.5V | 7.34[5] | 9.75[5] | 23h 05m 52.0s | −35° 51′ 11″ | 304.219±0.045[7] | 1753 | ||
Ross 128 (FI Virginis) | 11.0074±0.0026 | M4.0Vn | 11.13[5] | 13.51[5] | 11h 47m 44.4s | +00° 48′ 16″ | 296.307±0.070[7] | 1925 | flare star, one planet (b) (2017)[21] | |
EZ Aquarii (Gliese 866, Luyten 789-6) |
EZ Aquarii A | 11.109±0.034 | M5.0Ve | 13.33[5] | 15.64[5] | 22h 38m 33.4s | −15° 17′ 57″ | 293.60±0.9[22] | 1937 | A & B flare stars |
EZ Aquarii B | M? | 13.27[5] | 15.58[5] | - | ||||||
EZ Aquarii C | M? | 14.03[5] | 16.34[5] | 1995 | ||||||
61 Cygni | 61 Cygni A (BD+38°4343) | 11.4008±0.0012 | K5.0V[5] | 5.21[5]# | 7.49[5] | 21h 06m 53.9s | +38° 44′ 58″ | 286.08±0.03[7] | 1725 | B flare star, first star (besides Sun) to have measured distance[23] possible circumstellar disk. |
61 Cygni B (BD+38°4344) | K7.0V[5] | 6.03[5]# | 8.31[5] | 21h 06m 55.3s | +38° 44′ 31″ | - | ||||
Procyon (α Canis Minoris) |
Procyon A | 11.402±0.032 | F5V–IV[5] | 0.38[5]# | 2.66[5] | 07h 39m 18.1s | +05° 13′ 30″ | 286.05±0.81 [8][9] |
— | |
Procyon B‡ | DQZ[5] | 10.70[5] | 12.98[5] | 1844 | ||||||
Struve 2398 (Gliese 725, BD+59°1915) |
Struve 2398 A (HD 173739) | 11.4880±0.0012 | M3.0V[5] | 8.90[5] | 11.16[5] | 18h 42m 46.7s | +59° 37′ 49″ | 283.91±0.03[7] | 1835 | flare stars |
Struve 2398 B (HD 173740) | M3.5V[5] | 9.69[5] | 11.95[5] | 18h 42m 46.9s | +59° 37′ 37″ | 1835 | ||||
Groombridge 34 (Gliese 15) |
Groombridge 34 A (GX Andromedae) | 11.6182±0.0008 | M1.5V[5] | 8.08[5] | 10.32[5] | 0h 18m 22.9s | +44° 01′ 23″ | 280.73±0.02[7] | 1813 | flare star, two suspected planets (Ac, 2017) and Ab, 2014)[24] |
Groombridge 34 B (GQ Andromedae) | M3.5V[5] | 11.06[5] | 13.30[5] | - | flare star | |||||
DX Cancri (G 51-15) | 11.6780±0.0056 | M6.5Ve | 14.78[5] | 16.98[5] | 08h 29m 49.5s | +26° 46′ 37″ | 279.29±0.13[7] | 1972 | flare star | |
Tau Ceti (BD−16°295) | 11.753±0.022 | G8Vp[5] | 3.49[5]# | 5.68[5] | 01h 44m 04.1s | −15° 56′ 15″ | 277.52±0.52[7] | 150 | one debris disk two planets (e and f) (2012), three suspected planets (d, g and h) (2012, 2017), two refuted planets (b and c in 2017) | |
Epsilon Indi (CPD−57°10015) |
Epsilon Indi A | 11.869±0.011 | K5Ve[5] | 4.69[5]# | 6.89[5] | 22h 03m 21.7s | −56° 47′ 10″ | 274.80±0.25[7] | 1597 | one planet (b) (2018)[25] |
Epsilon Indi Ba§ | T1.0V | 12.3 J[26] | 22h 04m 10.5s | −56° 46′ 58″ | 2003 | |||||
Epsilon Indi Bb§ | T6.0V | 13.2 J[26] | 2003 | |||||||
GJ 1061 (LHS 1565) | 11.9803±0.0029 | M5.5V[5] | 13.09[5] | 15.26[5] | 03h 35m 59.7s | −44° 30′ 45″ | 272.245±0.066[7] | 1995 | [27][28] | |
YZ Ceti (LHS 138) | 12.1084±0.0035 | M4.5V[5] | 12.02[5] | 14.17[5] | 01h 12m 30.6s | −16° 59′ 56″ | 269.363±0.078[7] | 1961 | flare star, three planets (b, c, and d) (2017),[29] one suspected planet (e) | |
Luyten's Star (BD+05°1668) | 12.199±0.036 | M3.5Vn | 9.86[5] | 11.97[5] | 07h 27m 24.5s | +05° 13′ 33″ | 267.36±0.79[30] | 1935 | two planets (b, c) (2017)[31] | |
Teegarden's Star (SO025300.5+165258) | 12.496±0.013 | M6.5V | 15.14[5] | 17.22[5] | 02h 53m 00.9sg | +16° 52′ 53″ | 261.01±0.27[7] | 2003 | tentative radial velocity variation (2010)[28][32] | |
SCR 1845-6357 | SCR 1845-6357 A | 12.571±0.054 | M8.5V[5] | 17.39 | 19.41 | 18h 45m 05.3s | −63° 57′ 48″ | 259.45±1.11 [note 3] |
2004 | [28] |
SCR 1845-6357 B§ | T6[33] | 13.3 J[26] | 18h 45m 02.6s | −63° 57′ 52″ | 2006 | |||||
Kapteyn's Star (CD−45°1841) | 12.8294±0.0013 | M1.5V[5] | 8.84[5] | 10.87[5] | 05h 11m 40.6s | −45° 01′ 06″ | 254.226±0.026[7] | 1898 | two suspected planets (b and c) (2014)[34] | |
Lacaille 8760 (AX Microscopii) | 12.9515±0.0029 | M0.0V[5] | 6.67[5] | 8.69[5] | 21h 17m 15.3s | −38° 52′ 03″ | 251.829±0.056[7] | 1753 | flare star | |
Kruger 60 (BD+56°2783) |
Kruger 60 A | 13.0724±0.0052 | M3.0V[5] | 9.79[5] | 11.76[5] | 22h 27m 59.5s | +57° 41′ 45″ | 249.5±0.1[7] | 1880 | B flare star |
Kruger 60 B (DO Cephei) | M4.0V[5] | 11.41[5] | 13.38[5] | 1890? | ||||||
DEN 1048-3956§ | 13.1932±0.0066 | M8.5V[5] | 17.39[5] | 19.37[5] | 10h 48m 14.7s | −39° 56′ 06″ | 247.22±0.12[7] | 2001 | [35][36] | |
Ross 614 (V577 Monocerotis, Gliese 234) |
Ross 614A (LHS 1849) | 13.424±0.049 | M4.5V[5] | 11.15[5] | 13.09[5] | 06h 29m 23.4s | −02° 48′ 50″ | 242.97±0.88[7] | 1927 | A flare star |
Ross 614B (LHS 1850) | M5.5V | 14.23[5] | 16.17[5] | 1936 | ||||||
UGPS J0722-0540§ | 13.43±0.13 | T9[5] | 16.52 J[37] | 07h 22m 27.3s | –05° 40′ 30″ | 242.8±2.4[38] | 2010 | [39] | ||
Wolf 1061 (Gliese 628, BD−12°4523) | 14.0458±0.0038 | M3.0V[5] | 10.07[5] | 11.93[5] | 16h 30m 18.1s | −12° 39′ 45″ | 232.210±0.063[7] | 1919 | three planets (b, c, and d) (2015)[40] | |
Wolf 424 (FL Virginis, LHS 333, Gliese 473) |
Wolf 424 A | 14.05±0.26 | M5.5Ve | 13.18[5] | 14.97[5] | 12h 33m 17.2s | +09° 01′ 15″ | 232.2±4.3[41] | 1919 | flare stars |
Wolf 424 B | M7Ve | 13.17[5] | 14.96[5] | 1941 | ||||||
Van Maanen's star (Gliese 35, LHS 7)‡ | 14.0744±0.0023 | DZ7[5] | 12.38[5] | 14.21[5] | 00h 49m 09.9s | +05° 23′ 19″ | 231.737±0.038[7] | 1896 | closest known free-floating white dwarf, third known white dwarf possible debris disk (1917), possible planet (b) (2004) (debated) | |
Gliese 1 (CD−37°15492) | 14.1725±0.0037 | M1.5 V [5] | 8.55[5] | 10.35[5] | 00h 05m 24.4s | −37° 21′ 27″ | 230.133±0.060[7] | 1884 | ||
L 1159-16 (TZ Arietis, Gliese 83.1) | 14.5843±0.0070 | M4.5V[5] | 12.27[5] | 14.03[5] | 02h 00m 13.2s | +13° 03′ 08″ | 223.63±0.11[7] | flare star | ||
Gliese 674 (LHS 449) | 14.8387±0.0033 | M3.0V[5] | 9.38[5] | 11.09[5] | 17h 28m 39.9s | −46° 53′ 43″ | 219.801±0.049[7] | one planet (b) (2007)[42] | ||
Gliese 687 (LHS 450, BD+68°946) | 14.8401±0.0022 | M3.0V[5] | 9.17[5] | 10.89[5] | 17h 36m 25.9s | +68° 20′ 21″ | 219.781±0.032[7] | possible flare star, one planet (b) (2014)[43] | ||
LHS 292 (LP 731-58) | 14.885±0.011 | M6.5V[5] | 15.60[5] | 17.32[5] | 10h 48m 12.6s | −11° 20′ 14″ | 219.12±0.16[7] | flare star | ||
WISE J0521+1025§ | 15±3[note 4] | T7.5[44] | 15.26 J | 16.95 J | 05h 21m 26.3s | +10° 25′ 28″ | 217.5±40 | 2012 | distance highly uncertain | |
LP 145-141 (WD 1142-645, Gliese 440)‡ | 15.1182±0.0023 | DQ6[5] | 11.50[5] | 13.18[5] | 11h 45m 42.9s | −64° 50′ 29″ | 215.737±0.032[7] | 1917 | ||
G 208-44 G 208-45 (GJ 1245) |
G 208-44 A (V1581 Cyg) | 15.2090±0.0050 | M5.5V[5] | 13.46[5] | 15.17[5] | 19h 53m 54.2s | +44° 24′ 55″ | 214.45±0.07[7] | flare stars | |
G 208-45 | M6.0V[5] | 14.01[5] | 15.72[5] | 19h 53m 55.2s | +44° 24′ 56″ | |||||
G 208-44 B | M5.5 | 16.75[5] | 18.46[5] | 19h 53m 54.2s | +44° 24′ 55″ | |||||
Gliese 876 (Ross 780) | 15.2504±0.0054 | M3.5V[5] | 10.17[5] | 11.81[5] | 22h 53m 16.7s | −14° 15′ 49″ | 213.867±0.076[7] | four planets (d (2005), c (2001), b (1998), and e (2010))[45] two possible planets (f and g) (2014) (debated) | ||
LHS 288 (Luyten 143-23) | 15.7703±0.0056 | M5.5V[5] | 13.90[5] | 15.51[5] | 10h 44m 21.2s | −61° 12′ 36″ | 206.817±0.074[7] | one tentative planet (b) (2007)[28] | ||
GJ 1002 | 15.8164±0.0098 | M5.5V[5] | 13.76[5] | 15.40[5] | 00h 06m 43.8s | −07° 32′ 22″ | 206.21±0.13[7] | |||
Groombridge 1618 (Gliese 380) | 15.8797±0.0026 | K7.0V[5] | 6.59[5] | 8.16[5] | 10h 11m 22.1s | +49° 27′ 15″ | 205.392±0.034[7] | 1838 | flare star, one suspected debris disk, one suspected planet (b) (1989) (tentative) | |
DEN 0255-4700§ | 15.885±0.020 | L7.5V[5] | 22.92[5] | 24.44[5] | 02h 55m 03.7s | −47° 00′ 52″ | 205.33±0.25[7] | 1999 | [36] | |
Gliese 412 | Gliese 412 A | 15.983±0.013 | M1.0V[5] | 8.77[5] | 10.34[5] | 11h 05m 28.6s | +43° 31′ 36″ | 204.06±0.17[7] | 1850s? | |
Gliese 412 B (WX Ursae Majoris) | M5.5V[5] | 14.48[5] | 16.05[5] | 11h 05m 30.4s | +43° 31′ 18″ | 1850s? | flare star | |||
WISE 1639-6847§ | 16.12±0.25[note 4] | Y0.5 | 20.57 J | 22.10 J | 16h 39m 40.9s | −68° 47′ 46″ | 202.3±3.1[46] | 2012 | ||
Gliese 832 | 16.1939±0.0034 | M1.5 V[5] | 8.66[5] | 10.20[5] | 21h 33m 34.0s | −49° 00′ 32″ | 201.407±0.043[7] | 1910s? | possible flare star, two planets (b (2008) and c (2014))[47][48] | |
AD Leonis | 16.1970±0.0055 | M3.0V[5] | 9.32[5] | 10.87[5] | 10h 19m 36.4s | +19° 52′ 10″ | 201.368±0.068[7] | 1850s? | flare star | |
GJ 1005 | GJ 1005 A | 16.26±0.76[note 4] | M4V[49] | 11.48[49] | 00h 15m 28.11s | −16° 08′ 01.6″ | 200.5±9.4[49] | |||
GJ 1005 B | M7V | ? | ? | |||||||
System | Star # | Distance[6] Light-years (±err) |
Stellar class | Apparent magnitude (mV or mJ) | Absolute magnitude (MV or MJ) | Right ascension[5] | Declination[5] | Parallax[5][note 1] mas (±err) |
Discovery date | Additional references |
Designation | Epoch J2000.0 |
Distant future and past encounters
Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astromertic measurements of parallax and total proper motions, along with spectroscopic determined radial velocities. Although predictions can be extrapolated back into the past or forward into the future, they are subject to increasing significant cumulative errors over very long periods.[4] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[50]
![](http://upload.wikimedia.org/wikipedia/commons/thumb/e/e9/Near-stars-past-future-en.svg/350px-Near-stars-past-future-en.svg.png)
Examples of notable predicted stellar encounters falling within 5 parsecs from the Sun appear in the list below. A summary of the more likely candidates include:
- Scholz's star and its companion brown dwarf is thought to have passed about 52,000 astronomical units (0.25 parsecs; 0.82 light-years) from the Sun about 70,000 years ago.[51]
- Gamma Microscopii approximately 3.8 million years ago has been predicted to approach as close as 6 light-years from the Sun. Maximum apparent magnitude possibly reached −3, being brighter than the current brightest star, Sirius.[citation needed] More recent examination of measurement errors now suggests it may or may not have passed within 5.0 parsecs.
- Gliese 710 / HIP 89825 is the low mass orange K7 spectral type star that currently lies about 63.8 light-years (19.6 parsecs) from the Sun. Based on past and 2007 Hipparcos data,[52] was first estimated to approach just under one light year from the Sun some 1.4 million years from now to appear as a first-magnitude star roughly equal in brightness to Antares. As total proper motion of Gliese 710 is very small and a radial velocity of −119 km/s is fairly high, this suggests it is traveling at a similar and relatively close-approach trajectory to the Solar System. Gaia DR2 in 2018 now predicts the closest known encounter so far known: Minimum perihelion distance is 0.0676±0.0157 parsecs or 13900±3200 AU about 1.281 million years in the future. The Gliese 710 close approach will likely cause the greatest known gravitational perturbation on celestial objects within in the Solar System.[3]
- Ross 248 is presently about 10.3 light-years away from the Sun and in about 31,000 years from now it may be the closest star for several millennia, with a minimum distance of 0.927 parsecs (3.02 light-years) in 36,000 years.[4]
- Gliese 445 present distance is 17.6 light-years but in about 40,000 years it will become the closest star for a period of several thousand years.
- HIP 85605 in 2014 was estimated to approach the Sun between 0.13 to 0.65 light-years (8,200 to 41,100 astronomical units; 0.040 to 0.199 parsecs) within the next 240,000 to 470,000 years.[53][54][55] With the release of Gaia DR2, it was determined that HIP 85605 is actually a much more distant 1790±30 light-years away, and as such will not be passing remotely close to the Sun at any point in time.
See also
- Interstellar travel
- List of brightest stars
- List of star systems within 20–25 light-years
- List of star systems within 25–30 light-years
- List of nearest bright stars
- List of nearest exoplanets
- List of nearest galaxies
- Lists of stars
- Nearby Stars Database
- Stars and planetary systems in fiction
- The Magnificent Seven
- List of Solar System objects by greatest aphelion
- List of trans-Neptunian objects
Notes
- ^ a b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
- ^ 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
- ^ 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. doi:10.1051/0004-6361/201833456.
{{cite journal}}
: CS1 maint: extra punctuation (link) CS1 maint: multiple names: authors list (link) - ^ a b c Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
- ^ a b c Matthews, R.A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. 35: 1. Bibcode:1994QJRAS..35....1M.
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(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist
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ignored (help)CS1 maint: unflagged free DOI (link) - ^ The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr−1 (Motion sample), Wei-Chun Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, Jennifer L. Bartlett, Edgardo Costa, René A. Méndez, The Astronomical Journal 129, #4 (April 2005), pp. 1954–1967. doi:10.1086/428489
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(help)CS1 maint: multiple names: authors list (link) - ^ "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.
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- ^ 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
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- ^ Wittenmyer, R. A.; Tuomi, Mikko; Butler, R. P.; Jones, H. R. A.; Anglada-Escude, Guillem; Horner, Jonathan; Tinney, C. G.; Marshall, J. P.; Carter, B. D.; Bailey, J.; Salter, G. S.; O'Toole, S. J.; Wright, D.; Crane, J. D.; Schectman, S. A.; Arriagada, P.; Thompson, I.; Minniti, D.; Jenkins, J. S.; Diaz, M. (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.
- ^ "Featured Research: Closest known flyby of star to our solar system: Dim star passed through Oort Cloud 70,000 years ago". Science Daily. February 17, 2015. Retrieved 2015-02-21.
- ^ Cite error: The named reference
Bobylev:arXiv1003.2160
was invoked but never defined (see the help page). - ^ Coryn A.L. Bailer-Jones (Dec 11, 2014). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: A35. arXiv:1412.3648. Bibcode:2014yCat..35750035B. doi:10.1051/0004-6361/201425221.
- ^ Mamajek, Eric E.; Barenfeld, Scott A.; Ivanov, Valentin D. (2015). "The Closest Known Flyby of a Star to the Solar System". The Astrophysical Journal. 800 (1): L17. arXiv:1502.04655. Bibcode:2015ApJ...800L..17M. doi:10.1088/2041-8205/800/1/L17.
- ^ Coryn Bailer-Jones (2015-01-01). "The closest encounter is Hip 85605. How reliable is this?". Retrieved 2015-01-05.
External links
- "The 100 nearest star systems", Research Consortium on Nearby Stars
- "NStars database". Northern Arizona University. Archived from the original on October 30, 2005. Retrieved October 24, 2005.
{{cite web}}
: Unknown parameter|deadurl=
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suggested) (help) - Nemiroff, R.; Bonnell, J., eds. (March 18, 2001). "Map of the 25 nearest star systems". Astronomy Picture of the Day. NASA. Retrieved 2005-10-24.
- "Notable Nearby Stars". SolStation. Retrieved 2005-10-24.
- "Cool stars in the solar Neighbourhood". D. Montes, UCM. Retrieved 2005-11-14.
- The dynamics of the closest stars
- Takeda, G.; E. B. Ford; A. Sills; F. A. Rasio; D. A. Fischer; J. A. Valenti (2006). "Structure and Evolution of Nearby Stars with Planets II. Physical Properties of ~ 1000 Cool Stars from the SPOCS Catalog". California & Carnegie Planet Search. Retrieved 2006-10-13.
- Nearest Stars 3D View
- Table 4 "The Census of Stars and Brown Dwarfs within 8 Parsecs of the Sun" in Kirkpatrick et al. (2012) Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function, https://arxiv.org/pdf/1205.2122v1.pdf
- http://phl.upr.edu/projects/nearby-stars-catalog