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Fearless Girl
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Fearless Girl
The statue in March 2017
Fearless Girl
Fearless Girl
Fearless Girl
Fearless Girl
Fearless Girl
Show map of Lower Manhattan Show map of Manhattan Show map of New York City Show map of New York Show map of the US Show all
Artist
Kristen Visbal
Medium
Bronze sculpture
Dimensions
50 inches (130 cm) tall[1]
Weight
250 pounds (110 kg)
Location
New York City, New York, U.S.
Coordinates
40°42′20″N 74°00′48″W / 40.705632°N 74.013392°W / 40.705632; -74.013392Coordinates: 40°42′20″N 74°00′48″W / 40.705632°N 74.013392°W / 40.705632; -74.013392
Fearless Girl is a bronze sculpture by Kristen Visbal, commissioned by State Street Global Advisors via McCann New York, depicting a Latina girl facing the Charging Bull (or "Wall Street bull") statue.[2] It was installed on March 7, 2017, at Bowling Green in the Financial District of Manhattan, New York City. The statue measures approximately 50 inches (130 cm) tall, and weighs about 250 pounds (110 kg).
Fearless Girl was commissioned by investment firm State Street Global Advisors (SSgA) to advertise for an index fund which comprises gender-diverse companies that have a higher percentage of women among their senior leadership. The plaque below the statue states, "Know the power of women in leadership. SHE makes a difference," with "SHE" being both a descriptive pronoun and the fund's NASDAQ ticker symbol.
Contents
[hide]
1 History
2 Reception
3 See also
4 References
History[edit]
The statue was installed on March 7, 2017—the day before International Women's Day—by State Street Global Advisors, in a campaign developed by advertising agency McCann New York.[3] SSgA was celebrating the first anniversary of its "Gender Diversity Index" fund that "invests in U.S. large-capitalization companies that rank among the highest in their sector in achieving gender diversity across senior leadership".[4] The concept for the statue was developed by Senior Art Director Lizzie Wilson and Senior Copywriter Tali Gumbiner. Wilson and Gumbiner established both the idea for the statue as well as the overall look of the girl using countless moodboards and imagery, which Visbal referenced.[5] Fearless Girl, which measures approximately 50 inches (130 cm) tall and weighs about 250 pounds (110 kg),[1] faces Charging Bull, a much larger and heavier bronze statue that is 11 feet (3.4 m) tall and weighs 7,100 pounds (3,200 kg).[6][1] Both are located in Manhattan's Bowling Green, at the intersection of Broadway and Whitehall Street.[7]
Fearless Girl is meant to "send a message" about workplace gender diversity and encourage companies to recruit women to their boards.[8] The plaque below the statue states, "Know the power of women in leadership. SHE makes a difference," with SHE referring to both the gender of the subject and the fund's NASDAQ ticker symbol.[9]
The commission by State Street Global Advisors specified that the statue should depict a girl with hands on her hips and chin up, with a height of 36 inches, which Kristen Visbal and her collaborators then increased to 50 inches, to better match the size of Charging Bull.[1] Still, Visbal commented that "I made sure to keep her features soft; she's not defiant, she's brave, proud, and strong, not belligerent".[1] She modeled the sculpture on two children from Delaware, a friend's daughter who was instructed to pretend she was facing a bull, and a Latina girl, "so everyone could relate to the Fearless Girl."[1]
Fearless Girl was originally given a one-week City Hall permit that was later extended to 30 days.[10] Later, it was announced that the statue would remain in place through February 2018.[11][12] Among those advocating for the statue to stay longer was U.S. Representative Carolyn Maloney of New York's 12th congressional district, who stated, "This statue has touched hearts across the world with its symbolism of the resiliency of women."[13] A petition on Change.org asking for the statue to be made permanent gathered 2,500 signatures in its first 48 hours.[10][14] Efforts to make the statue permanent continued after the statue was granted a one-year permit.[15]
Reception[edit]
Some women criticized the statue as "corporate feminism" that violated their own feminist principles.[16][17] New York Times columnist Gina Bellafante called it "an exercise in corporate imaging" by State Street, which, she wrote, had entered into a deferred prosecution agreement with the United States Department of Justice, agreeing to pay more than $64 million to resolve fraud charges for secretly billing clients for unwarranted commissions. "Corporate feminism", she wrote, "operates with the singular goal of aiding and abetting a universe of mothers who tuck their daughters in at night whispering, 'Someday, honey, you can lead the emerging markets and sovereign debt team at Citigroup, and then become a director at Yahoo.'"[18] Christine Emba, an opinion writer for The Washington Post, wrote that the statue "portrays the empowered woman as a child, reinforcing the idea of femaleness as cute and inoffensive — a child with potential, maybe, but not all the way there."[19]
The Gothamist reported on March 20th 2017 about masked New York activists who took to the streets to deck out the statue in Make America Great Again apparel and an American Flag. They also gifted the statue with a few pro-Trump signs, including one reading, "VETS B4 ILLEGALS" and another with a drawing of Pepe the Frog.[20]
As reported by Bloomberg News, analysts from marketing firm Apex Marketing estimated that the statue resulted in $7.4 million in free advertising for SSGA as of April 2017, broken down into $201,075 worth of free radio advertising, $393,047 worth of free social media advertising, $3,115,751 worth of free TV advertising, and $3,729,926 worth of free online/print news advertising.[21]
Public advocate Letitia James has asked for the statue to be a permanent installation. In a letter to New York City Mayor Bill de Blasio, James states, "Fearless Girl stands as a powerful beacon, showing women—young and old—that no dream is too big and no ceiling is too high".[22]
Arturo Di Modica, who had installed Charging Bull in 1989, has asked that the statue of the girl be removed, arguing that the piece exploits his work for commercial purposes and alters the perception of the bull.[23] He has called Fearless Girl "an advertising trick" that he wants relocated, citing its political messaging.[24][1] On April 12, 2017, Di Modica and his attorney, former New York Civil Liberties Union director Norman Siegel, challenged city officials who let the Fearless Girl statue be installed.[25][26] Di Modica states the statue corrupts Charging Bull's artistic integrity by distorting the intent of his statue from "a symbol of prosperity and for strength" into a villain, and does so for SSgA's commercial gain.[27][28] Siegel said a lawsuit had not been filed as of yet.[25][26] Mayor de Blasio supported keeping the statue, tweeting that "Men who don't like women taking up space are exactly why we need the Fearless Girl."[29]
Artist Alex Gardega added a statue of a small dog, titled Pissing Pug (or Peeing Pug[30] or Sketchy Dog) but it was removed by him after approximately three hours.[31] He describes the Fearless Girl statue as "corporate nonsense" and "disrespect to the artist that made the bull."[32]
At the 2017 Cannes Lions festival, Fearless Girl won three Grand Prix on the first day of the event alone, in the Glass (which deals with marketing addressing gender inequality) and PR categories, and tying for first in the Outdoor category alongside a campaign by Twitter.[33]
See also[edit]
New York City portal
Visual arts portal
2017 in art
Day Without a Woman, a general strike held on March 8, 2017
Women in business
References[edit]
^ Jump up to: a b c d e f g Dobnik, Verena (March 26, 2017). "Will New York invite the 'Fearless Girl' statue to stay on Wall Street?". USA TODAY. Retrieved March 27, 2017.
Jump up ^ "Eight Things You Don't Know About 'Fearless Girl'". Advertising Age.
Jump up ^ Dobnik, Verena (March 9, 2017). "Behind NYC's 'Fearless Girl' statue are 2 corporate giants". ABC News. Archived from the original on March 12, 2017. Retrieved March 13, 2017.
Jump up ^ Mavro, Jill (March 7, 2017). "Driving Gender Diversity with a Bold New Statement". SPDR Blog. Retrieved March 28, 2017.
Jump up ^ Nudd, Tim (March 10, 2017). "The Story of ‘The Fearless Girl,’ From the Women at McCann Who Made Her". Adweek. Retrieved May 4, 2017.
Jump up ^ Schwedel, Heather (March 7, 2017). "A Bronze Little Girl Has Arrived to Face Down the Wall Street Bull. This Should Go Well.". Slate. Retrieved March 7, 2017.
Jump up ^ Wiener-Bronner, Danielle (March 7, 2017). "Why a defiant girl is staring down the Wall Street bull". CNNMoney. Retrieved March 7, 2017.
Jump up ^ Fierberg, Emma; Levy, Rachael (March 7, 2017). "A $2.5 trillion asset manager just put a statue of a defiant girl in front of the Wall Street bull". Business Insider. Retrieved March 7, 2017.
Jump up ^ Dutram, Eric (March 27, 2017). "The 'Fearless Girl' Statue Isn't a Symbol, It Is an Advertisement". NASDAQ.com. Retrieved March 28, 2017.
^ Jump up to: a b Revesz, Rachel (March 9, 2017). "Campaign launches to make 'Fearless Girl' statue on Wall Street permanent". The Independent. Retrieved March 10, 2017.
Jump up ^ "'Fearless Girl' statue will stay through early next year". CNN Money. Retrieved March 27, 2017.
Jump up ^ Silva, Daniella (March 27, 2017). "'Fearless Girl' statue will face off Wall Street bull for another year". NBC News. Retrieved March 27, 2017.
Jump up ^ O'Connor, Roision (March 27, 2017). "The Fearless Girl statue will stay on Wall Street until 2018". The Independent. Retrieved April 11, 2017.
Jump up ^ Bisaria, Anjali (March 10, 2017). "People Have Now Launched A Campaign To Make The 'Fearless Girl' Statue Permanent At Wall Street". IndiaTimes. Retrieved March 10, 2017.
Jump up ^ Stack, Liam (March 27, 2017). "‘Fearless Girl’ Statue to Stay in Financial District (for Now)". The New York Times. Retrieved March 28, 2017.
Jump up ^ The Sculpture of a “Fearless Girl” on Wall Street Is Fake Corporate Feminism. The bronze statue installed by an advertising firm and a financial firm represents basically everything that’s wrong with our society. Jillian Steinhauer, Hyperallergic, March 10, 2017
Jump up ^ The 'Fearless Girl' statue sums up what's wrong with feminism today. Corporate feminism always ends up betraying women’s struggle for justice. That’s why this Wall Street-funded sculpture will never be a symbol to embrace. Cara Marsh Sheffler. The Guardian. March 14, 2017
Jump up ^ Bellafante, Ginia (March 16, 2017). "The False Feminism of ‘Fearless Girl’". The New York Times. ISSN 0362-4331. Retrieved April 13, 2017.
Jump up ^ Emba, Christine (April 14, 2017). "'Fearless Girl' and 'Charging Bull' are more alike than you'd think". The Washington Post. Retrieved April 15, 2017.
Jump up ^ "Men In MAGA Hats Transform 'Fearless Girl' Statue Into Trump Supporter". Gothamist. Retrieved 2017-11-01.
Jump up ^ "The Fearless Girl Is Worth $7.4 Million in Free Publicity for This Company". Bloomberg.com. 2017-04-28. Retrieved 2017-06-01.
Jump up ^ "EXCLUSIVE: Letitia James wants 'Fearless Girl' to be permanent". NY Daily News. Retrieved April 12, 2017.
Jump up ^ Mettler, Katie (April 12, 2017). "Charging Bull sculptor says Fearless Girl distorts his art, so he's fighting back". Chicago Tribune.
Jump up ^ Stack, Liam (March 27, 2017). "‘Fearless Girl’ Statue to Stay in Financial District (for Now)". The New York Times. Retrieved March 28, 2017.
^ Jump up to: a b "'Charging Bull' sculptor says New York's 'Fearless Girl' statue violates his rights". The Guardian. Associated Press. April 11, 2017. ISSN 0261-3077. Retrieved April 13, 2017.
^ Jump up to: a b Barron, James (April 12, 2017). "Wounded by ‘Fearless Girl,’ Creator of ‘Charging Bull’ Wants Her to Move". The New York Times. ISSN 0362-4331. Retrieved April 13, 2017.
Jump up ^ "‘Charging Bull’ sculptor says ‘Fearless Girl’ distorts his art. He’s fighting back.". Washington Post. Retrieved April 12, 2017.
Jump up ^ "Sculptor Of Wall Street Bull Says 'Fearless Girl' Horns In On His Work". NPR. Retrieved April 12, 2017.
Jump up ^ Smith, Aaron (12 April 2017). "NYC mayor to 'Charging Bull' artist: 'Fearless Girl is staying put.'". CNNMoney.
Jump up ^ "'Fearless Girl' joined briefly by 'Peeing Pug' statue". CNNMoney. May 30, 2017.
Jump up ^ "Urinating dog statue placed next to "Fearless Girl" as a critique". NBC News.
Jump up ^ Fugallo, Nick; Jaeger, Max (May 30, 2017). "Pissed-off artist adds statue of urinating dog next to ‘Fearless Girl’". New York Post.
Jump up ^ "Fearless Girl Takes Cannes by Storm, Winning 3 Grand Prix on Her First Day". Adweek. Retrieved 2017-06-22.
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List of nearest stars and brown dwarfs
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Video showing the space around the nearest stars to the Sun.
The following two lists include all the known stars and brown dwarfs that are within 5.0 parsecs (16.3 light-years) of the Sun, or were/will be within 5.0 light-years (1.53 parsecs) in the astronomically near past or future. The easiest way to determine stellar distance to the Sun for these objects 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.
The first table is based on the most accurate observed parallaxes of the stars. The second table additionally lists stars that in the past have come or in the future will come within 1.5 parsecs (4.9 light-years). Determining which stars fall within the stated range 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.[1]
There are 52 stellar systems beyond our own Solar system that currently lie within this 5 parsec distance. 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, meaning only about 12% of these objects can be observed with the naked eye.[2] Besides the Sun, only three are first-magnitude stars: Alpha Centauri, Sirius, and Procyon. All of these objects are located in the Local Bubble, a region within the Orion–Cygnus Arm of the Milky Way.
Based on the latest Gaia DR2 astrometric results released in 2018 of stars brighter than 13.8G apparent magnitude, an estimated 694 solar-like or cooler stars will possibly approach the solar system to less than 5 parsecs over the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec and another 7 within 0.5 parsecs.[3] The closest encounter to the Sun so far predicted is the low mass orange K7 spectral type star Gliese 710 / HIP 89825.[4] Minimum perihelion distance is 0.0676±0.0157 parsecs or 13900±3200 AU about 1.281 million years from now.[3] This is easily within the predicted maximum size of the Oort cloud,[3] whose approach will likely be disruptive enough to affect the orbits of cometary bodies.[4]
Contents
1 List
2 Maps of nearby stars
3 Distant future and past encounters
4 See also
5 Notes
6 References
7 External links
List[edit]
Stars visible to the unaided eye have their magnitude shown in light blue below. Brown dwarfs are shown with their designations in brown. White dwarfs are shown with their designation in beige. The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible colors. Some of the parallax and distance results are preliminary measurements.[5]
Nearest star systems
Designation
Distance[6]
(light-years (±err))
Stellar class
Apparent magnitude (mV or mJ)
Absolute magnitude (MV or MJ)
Epoch J2000.0
Parallax
(mas (±err))
[5][note 1]
Discovery
date
[note 2]
Notes and additional
references
System
Star #
Right ascension[5]
Declination[5]
Solar System Sun 5000000000000000000♠0 G2V[5] −26.74[5] 4.85[5] — — — — eight planets
Alpha Centauri
(Rigil Kentaurus) Proxima Centauri (V645 Centauri) 7000424410000000000♠4.2441±0.0011 M5.5Ve 11.09[5] 15.53[5] 14h 29m 43.0s −62° 40′ 46″ 7002768500000000000♠768.50±0.20[7] 1915 flare star, one planet (b) (2016)
α Centauri A (HD 128620) 7000436500000000000♠4.3650±0.0068 G2V[5] 0.01[5] 4.38[5] 14h 39m 36.5s −60° 50′ 02″ 7002747230000000000♠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) 7000595770000000000♠5.9577±0.0032 M4.0Ve 9.53[5] 13.22[5] 17h 57m 48.5s +04° 41′ 36″ 7002547450000000000♠547.45±0.29[7] 1916 flare star, largest known proper motion[11]
Luhman 16
(WISE 1049−5319) Luhman 16A 7000650490000000000♠6.5049±0.0012 L8±1[12] 10.7 J 14.2 J 10h 49m 15.57s −53° 19′ 06″ 7002501398000000000♠501.398±0.093[13] 2013 one refuted planet (Ab[14] in 2017[13])
Luhman 16B T1±2[12]
WISE 0855−0714 7000726000000000000♠7.26±0.13[15] Y2 25.0 J 08h 55m 10.83s −07° 14′ 42.5″ 7002449000000000000♠449±8[16] 2014 sub-brown dwarf
Wolf 359 (CN Leonis) 7000785600000000000♠7.856±0.031 M6.0V[5] 13.44[5] 16.55[5] 10h 56m 29.2s +07° 00′ 53″ 7002415160000000000♠415.16±1.62[17] 1919 flare star
Lalande 21185 (BD+36°2147) 7000830700000000000♠8.307±0.014 M2.0V[5] 7.47[5] 10.44[5] 11h 03m 20.2s +35° 58′ 12″ 7002392640000000000♠392.64±0.67[18] 1801 one suspected planet (2017)[19]
Sirius
(α Canis Majoris) Sirius A 7000865900000000000♠8.659±0.010 A1V[5] −1.46[5] 1.42[5] 06h 45m 08.9s −16° 42′ 58″ 7002376680000000000♠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) 7000879100000000000♠8.791±0.012 M5.5Ve 12.54[5] 15.40[5] 01h 39m 01.3s −17° 57′ 01″ 7002371000000000000♠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) 7000970350000000000♠9.7035±0.0019 M3.5Ve 10.43[5] 13.07[5] 18h 49m 49.4s −23° 50′ 10″ 7002336123000000000♠336.123±0.064[7] 1925 flare star
Ross 248 (HH Andromedae) 7001102903000000000♠10.2903±0.0041 M5.5Ve 12.29[5] 14.79[5] 23h 41m 54.7s +44° 10′ 30″ 7002316960000000000♠316.96±0.13[7] 1925 flare star
Epsilon Eridani (BD−09°697) 7001104460000000000♠10.446±0.016 K2V[5] 3.73[5] 6.19[5] 03h 32m 55.8s −09° 27′ 30″ 7002312220000000000♠312.22±0.47[7] 150 three circumstellar disks,
two suspected planets (AEgir (debated) and c) (2000 & 2002)[20]
Lacaille 9352 (CD−36°15693) 7001107211000000000♠10.7211±0.0016 M0.5V 7.34[5] 9.75[5] 23h 05m 52.0s −35° 51′ 11″ 7002304219000000000♠304.219±0.045[7] 1753
Ross 128 (FI Virginis) 7001110074000000000♠11.0074±0.0026 M4.0Vn 11.13[5] 13.51[5] 11h 47m 44.4s +00° 48′ 16″ 7002296307000000000♠296.307±0.070[7] 1925 flare star, one planet (b) (2017)[21]
EZ Aquarii
(Gliese 866, Luyten 789-6) EZ Aquarii A 7001111090000000000♠11.109±0.034 M5.0Ve 13.33[5] 15.64[5] 22h 38m 33.4s −15° 17′ 57″ 7002293600000000000♠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) 7001114008000000000♠11.4008±0.0012 K5.0V[5] 5.21[5] 7.49[5] 21h 06m 53.9s +38° 44′ 58″ 7002286080000000000♠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 7001114020000000000♠11.402±0.032 F5V–IV[5] 0.38[5] 2.66[5] 07h 39m 18.1s +05° 13′ 30″ 7002286050000000000♠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) 7001114880000000000♠11.4880±0.0012 M3.0V[5] 8.90[5] 11.16[5] 18h 42m 46.7s +59° 37′ 49″ 7002283910000000000♠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) 7001116182000000000♠11.6182±0.0008 M1.5V[5] 8.08[5] 10.32[5] 0h 18m 22.9s +44° 01′ 23″ 7002280730000000000♠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) 7001116780000000000♠11.6780±0.0056 M6.5Ve 14.78[5] 16.98[5] 08h 29m 49.5s +26° 46′ 37″ 7002279290000000000♠279.29±0.13[7] 1972 flare star
Tau Ceti (BD−16°295) 7001117530000000000♠11.753±0.022 G8Vp[5] 3.49[5] 5.68[5] 01h 44m 04.1s −15° 56′ 15″ 7002277519999999999♠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 7001118690000000000♠11.869±0.011 K5Ve[5] 4.69[5] 6.89[5] 22h 03m 21.7s −56° 47′ 10″ 7002274800000000000♠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) 7001119803000000000♠11.9803±0.0029 M5.5V[5] 13.09[5] 15.26[5] 03h 35m 59.7s −44° 30′ 45″ 7002272245000000000♠272.245±0.066[7] 1995 [27][28]
YZ Ceti (LHS 138) 7001121084000000000♠12.1084±0.0035 M4.5V[5] 12.02[5] 14.17[5] 01h 12m 30.6s −16° 59′ 56″ 7002269363000000000♠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) 7001121990000000000♠12.199±0.036 M3.5Vn 9.86[5] 11.97[5] 07h 27m 24.5s +05° 13′ 33″ 7002267360000000000♠267.36±0.79[30] 1935 two planets (b, c) (2017)[31]
Teegarden's Star (SO025300.5+165258) 7001124960000000000♠12.496±0.013 M6.5V 15.14[5] 17.22[5] 02h 53m 00.9sg +16° 52′ 53″ 7002261010000000000♠261.01±0.27[7] 2003 tentative radial velocity variation (2010)[28][32]
SCR 1845-6357 SCR 1845-6357 A 7001125710000000000♠12.571±0.054 M8.5V[5] 17.39 19.41 18h 45m 05.3s −63° 57′ 48″ 7002259450000000000♠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) 7001128294000000000♠12.8294±0.0013 M1.5V[5] 8.84[5] 10.87[5] 05h 11m 40.6s −45° 01′ 06″ 7002254226000000000♠254.226±0.026[7] 1898 two suspected planets (b and c) (2014)[34]
Lacaille 8760 (AX Microscopii) 7001129515000000000♠12.9515±0.0029 M0.0V[5] 6.67[5] 8.69[5] 21h 17m 15.3s −38° 52′ 03″ 7002251829000000000♠251.829±0.056[7] 1753 flare star
Kruger 60
(BD+56°2783) Kruger 60 A 7001130724000000000♠13.0724±0.0052 M3.0V[5] 9.79[5] 11.76[5] 22h 27m 59.5s +57° 41′ 45″ 7002249500000000000♠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 7001131931999999999♠13.1932±0.0066 M8.5V[5] 17.39[5] 19.37[5] 10h 48m 14.7s −39° 56′ 06″ 7002247220000000000♠247.22±0.12[7] 2001 [35][36]
Ross 614
(V577 Monocerotis, Gliese 234) Ross 614A (LHS 1849) 7001134240000000000♠13.424±0.049 M4.5V[5] 11.15[5] 13.09[5] 06h 29m 23.4s −02° 48′ 50″ 7002242970000000000♠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 7001134300000000000♠13.43±0.13 T9[5] 16.52 J[37] 07h 22m 27.3s –05° 40′ 30″ 7002242800000000000♠242.8±2.4[38] 2010 [39]
Wolf 1061 (Gliese 628, BD−12°4523) 7001140458000000000♠14.0458±0.0038 M3.0V[5] 10.07[5] 11.93[5] 16h 30m 18.1s −12° 39′ 45″ 7002232210000000000♠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 7001140500000000000♠14.05±0.26 M5.5Ve 13.18[5] 14.97[5] 12h 33m 17.2s +09° 01′ 15″ 7002232200000000000♠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) 7001140744000000000♠14.0744±0.0023 DZ7[5] 12.38[5] 14.21[5] 00h 49m 09.9s +05° 23′ 19″ 7002231737000000000♠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) 7001141725000000000♠14.1725±0.0037 M1.5 V [5] 8.55[5] 10.35[5] 00h 05m 24.4s −37° 21′ 27″ 7002230133000000000♠230.133±0.060[7] 1884
L 1159-16 (TZ Arietis, Gliese 83.1) 7001145843000000000♠14.5843±0.0070 M4.5V[5] 12.27[5] 14.03[5] 02h 00m 13.2s +13° 03′ 08″ 7002223630000000000♠223.63±0.11[7] flare star
Gliese 674 (LHS 449) 7001148387000000000♠14.8387±0.0033 M3.0V[5] 9.38[5] 11.09[5] 17h 28m 39.9s −46° 53′ 43″ 7002219801000000000♠219.801±0.049[7] one planet (b) (2007)[42]
Gliese 687 (LHS 450, BD+68°946) 7001148401000000000♠14.8401±0.0022 M3.0V[5] 9.17[5] 10.89[5] 17h 36m 25.9s +68° 20′ 21″ 7002219781000000000♠219.781±0.032[7] possible flare star, one planet (b) (2014)[43]
LHS 292 (LP 731-58) 7001148850000000000♠14.885±0.011 M6.5V[5] 15.60[5] 17.32[5] 10h 48m 12.6s −11° 20′ 14″ 7002219120000000000♠219.12±0.16[7] flare star
WISE J0521+1025 7001150000000000000♠15±3[note 4] T7.5[44] 15.26 J 16.95 J 05h 21m 26.3s +10° 25′ 28″ 7002217500000000000♠217.5±40 2012 distance highly uncertain
LP 145-141 (WD 1142-645, Gliese 440) 7001151182000000000♠15.1182±0.0023 DQ6[5] 11.50[5] 13.18[5] 11h 45m 42.9s −64° 50′ 29″ 7002215737000000000♠215.737±0.032[7] 1917
G 208-44
G 208-45
(GJ 1245) G 208-44 A (V1581 Cyg) 7001152090000000000♠15.2090±0.0050 M5.5V[5] 13.46[5] 15.17[5] 19h 53m 54.2s +44° 24′ 55″ 7002214450000000000♠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) 7001152504000000000♠15.2504±0.0054 M3.5V[5] 10.17[5] 11.81[5] 22h 53m 16.7s −14° 15′ 49″ 7002213867000000000♠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) 7001157703000000000♠15.7703±0.0056 M5.5V[5] 13.90[5] 15.51[5] 10h 44m 21.2s −61° 12′ 36″ 7002206817000000000♠206.817±0.074[7] one tentative planet (b) (2007)[28]
GJ 1002 7001158164000000000♠15.8164±0.0098 M5.5V[5] 13.76[5] 15.40[5] 00h 06m 43.8s −07° 32′ 22″ 7002206210000000000♠206.21±0.13[7]
Groombridge 1618 (Gliese 380) 7001158797000000000♠15.8797±0.0026 K7.0V[5] 6.59[5] 8.16[5] 10h 11m 22.1s +49° 27′ 15″ 7002205392000000000♠205.392±0.034[7] 1838 flare star, one suspected debris disk,
one suspected planet (b) (1989) (tentative)
DEN 0255-4700 7001158850000000000♠15.885±0.020 L7.5V[5] 22.92[5] 24.44[5] 02h 55m 03.7s −47° 00′ 52″ 7002205330000000000♠205.33±0.25[7] 1999 [36]
Gliese 412 Gliese 412 A 7001159830000000000♠15.983±0.013 M1.0V[5] 8.77[5] 10.34[5] 11h 05m 28.6s +43° 31′ 36″ 7002204060000000000♠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 7001161200000000000♠16.12±0.25[note 4] Y0.5 20.57 J 22.10 J 16h 39m 40.9s −68° 47′ 46″ 7002202300000000000♠202.3±3.1[46] 2012
Gliese 832 7001161939000000000♠16.1939±0.0034 M1.5 V[5] 8.66[5] 10.20[5] 21h 33m 34.0s −49° 00′ 32″ 7002201407000000000♠201.407±0.043[7] 1910s? possible flare star, two planets (b (2008) and c (2014))[47][48]
AD Leonis 7001161970000000000♠16.1970±0.0055 M3.0V[5] 9.32[5] 10.87[5] 10h 19m 36.4s +19° 52′ 10″ 7002201368000000000♠201.368±0.068[7] 1850s? flare star
GJ 1005 GJ 1005 A 7001162600000000000♠16.26±0.76[note 4] M4V[49] 11.48[49] 00h 15m 28.11s −16° 08′ 01.6″ 7002200500000000000♠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
Maps of nearby stars[edit]
This map shows all of the star systems within 14 light-years of the Sun (shown as Sol), except for brown dwarfs discovered after 2009. Double and triple stars are shown "stacked", but the true location is the star closest to the central plane. Color corresponds to the table above.
This is a 3D map of the nearest stars using the coordinates listed above. The stars in the front have a right ascension of 18h. An animated version is available here. 3D red green glasses are recommended to view this image correctly.
The locations of the four star systems closest to the Sun. Two, a brown dwarf and a free planet were found by the WISE satellite. The year when the distance to each system was determined is listed after the system's name.
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 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.[1] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.[50]
Distances of the nearest stars from 20,000 years ago until 80,000 years in the future
Examples of notable predicted stellar encounters falling within 5 parsecs from the Sun appear in the list below. A summary of the more likely candidates include:
Scholz's star and its companion brown dwarf is thought to have passed about 52,000 astronomical units (0.25 parsecs; 0.82 light-years) from the Sun about 70,000 years ago.[51]
Gamma Microscopii approximately 3.8 million years ago has been predicted to approach as close as 6 light-years from the Sun. Maximum apparent magnitude possibly reached −3, being brighter than the current brightest star, Sirius.[citation needed] More recent examination of measurement errors now suggests it may or may not have passed within 5.0 parsecs.
Gliese 710 / HIP 89825 is the low mass orange K7 spectral type star that currently lies about 63.8 light-years (19.6 parsecs) from the Sun. Based on past and 2007 Hipparcos data,[52] was first estimated to approach just under one light year from the Sun some 1.4 million years from now to appear as a first-magnitude star roughly equal in brightness to Antares. As total proper motion of Gliese 710 is very small and a radial velocity of −119 km/s is fairly high, this suggests it is traveling at a similar and relatively close-approach trajectory to the Solar System. Gaia DR2 in 2018 now predicts the closest known encounter so far known: Minimum perihelion distance is 0.0676±0.0157 parsecs or 13900±3200 AU about 1.281 million years in the future. The Gliese 710 close approach will likely cause the greatest known gravitational perturbation on celestial objects within in the Solar System.[4]
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.[1]
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.
Known stars that have passed or will pass within 5.1 light-years of the Sun within ±3 million years:[52][56]
Star name
HIP#
Minimum distance
(light-years)
Date of approach
in kiloyears
Current distance
(light-years)
Stellar
classification
Mass in M☉
Current
apparent magnitude
Current Constellation
Current
Right ascension
Current
Declination
Gliese 710 89825 6999178000000000000♠0.178+0.043
−0.036 7003128000000000000♠1280+41
−39 7001621030000000000♠62.103±0.057 K7V 0.4–0.6 9.6 Serpens 18h 19m 50.843s −01° 56′ 18.98″
2MASS J0610-4246 6999755000000000000♠0.755+0.084
−0.090 2996883560000000000♠−1164.4+8.8
−8.9 7002319750000000000♠319.75±0.60 early K ~0.8 11.79 Puppis 06h 10m 55.448s −42° 46′ 03.39″
Scholz's star and companion brown dwarf 6999820000000000000♠0.82+0.37
−0.22 2998310000000000000♠−69+10
−14 7001196000000000000♠19.6±3.4 M9+T5 0.15 18.3 Monoceros 07h 20m 03.20s −08° 46′ 51.2″
HD 283856 7000112999999999999♠1.13+0.75
−0.55 7002374000000000000♠374+40
−34 7002290000000000000♠290±17 K0V (binary?) ~0.8 10.46 Taurus 04h 48m 28.124s +27° 00′ 39.06″
TYC 1662-1962-1 7000184000000000000♠1.84+0.22
−0.21 2996848700000000000♠−1513+18
−19 7002284500000000000♠284.5±1.0 Early K ~0.8 10.95 Vulpecula 21h 14m 32.911s +21° 53′ 32.76″
HD 7977 7000188000000000000♠1.88+0.18
−0.16 2996720200000000000♠−2798+44
−46 7002247030000000000♠247.03±0.70 G0V ~1.2 9.04 Cassiopeia 01h 20m 31.597s +61° 52′ 57.08″
2MASS J2146+3813 7000189000000000000♠1.89+0.18
−0.15 7001844000000000000♠84.4+8.0
−6.8 7001229603000000000♠22.9603±0.0083 M5V ~0.015 10.82 Cygnus 21h 46m 22.285s +38° 13′ 03.12″
2MASS J0634-7449 7000216900000000000♠2.169+0.083
−0.080 2997102000000000000♠−898+12
−13 7002213280000000000♠213.28±0.29 mid K ~0.6 12.69 Mensa 06h 34m 29.385s −74° 49′ 47.12″
TYC 2730-1701-1 7000231000000000000♠2.31+0.31
−0.29 2997286000000000000♠−714+21
−22 7002829100000000000♠829.1±9.1 G? ~1 9.44 Pegasus 21h 50m 41.029s +36h 20m 46.73s
2MASS J0409+0245 7000268400000000000♠2.684+0.088
−0.091 7002912000000000000♠912±13 7002101400000000000♠101.40±0.18 Early M ~0.4 11.73 Taurus 04h 09m 02.050s +02° 45′ 38.32″
Gliese 3649 7000297500000000000♠2.975+0.093
−0.089 2997491000000000000♠−509±12 7001544150000000000♠54.415±0.048 M1 0.49 10.85 Leo 11h 12m 38.97s +18° 56′ 05.4″
2MASS J0605+4020 7000290000000000000♠2.9+4.5
−2.1 2997140000000000000♠−860+210
−350 7002248000000000000♠248±20 K ~0.5 12.07 Auriga 06h 05m 05.077s +40° 20′ 37.72″
2MASS J1818-4038 7000300000000000000♠3.0+1.3
−1.1 7003104900000000000♠1049+54
−50 7002191400000000000♠191.4±5.6 K/M ~0.5 11.97 Corona Australis 18h 18m 17.213s −40° 38′ 39.48″
BD-21 1529 7000301000000000000♠3.01+0.29
−0.28 2996831500000000000♠−1685+14
−15 7002374100000000000♠374.1±1.8 G5V ~0.95 9.67 Canis Major 06h 37m 48.004s −21° 22′ 21.94″
Ross 248 7000311000000000000♠3.11+0.15
−0.14 7001392000000000000♠39.2+1.9
−1.8 7001102903000000000♠10.2903±0.0041 M6V 0.136 12.29 Andromeda 23h 41m 54.99s +44° 10′ 40.8″
Proxima Centauri 70890 7000310340000000000♠3.1034±0.0033 7001286770000000000♠28.677±0.054 7000424410000000000♠4.2441±0.0011 M5Ve 0.15 11.05 Centaurus 14h 29m 42.949s −62° 40′ 46.14″
Alpha Centauri AB 71683
71685 7000324200000000000♠3.242±0.060 7001296300000000000♠29.63+1.00
−0.98 7000432100000000000♠4.321±0.024 G2V+K1V 1.100
0.907[57] -0.01
+1.33 Centaurus 14h 39m 36.495s −60° 50′ 02.31″
Gliese 445 57544 7000333650000000000♠3.3365±0.0050 7001463010000000000♠46.301±0.052 7001171424000000000♠17.1424±0.0043 M4 0.15? 10.8 Camelopardalis 11h 47m 41.377s +78° 41′ 28.18″
HIP 117795 117795 7000343300000000000♠3.433±0.013 7001934599999999999♠93.46±0.21 7001873360000000000♠87.336±0.075 K8V ~0.5 10.6 Cassiopeia 23h 53m 20.014s +59° 56′ 42.95″
2MASS J0625-2408 7000359000000000000♠3.59+0.25
−0.27 2996815100000000000♠−1849+30
−31 7002537100000000000♠537.1±2.7 K/M ~0.5 12.91 Canis Major 06h 25m 42.744s −24° 08′ 35.02″
Barnard's Star 87937 7000376040000000000♠3.7604±0.0074 7001117310000000000♠11.731±0.027 7000595770000000000♠5.9577±0.0032 sdM4 0.144 9.54 Ophiuchus 17h 57m 48.498s +04° 41′ 36.25″
2MASS J2241-2759 7000379000000000000♠3.79+0.67
−0.62 2996719100000000000♠−2809+53
−55 7002414700000000000♠414.7±2.6 K7V ~0.5 12.28 Piscis Austrinus 22h 41m 50.996s −27° 59′ 47.04″
Gliese 3379 7000419400000000000♠4.194±0.016 2997843870000000000♠−156.13±0.52 7001169813000000000♠16.9813±0.0063 M3.5V 0.19 11.31 Orion 06h 00m 03.824s +02° 42′ 22.97″
Zeta Leporis 27288 7000470000000000000♠4.70+0.59
−0.51 2997140000000000000♠−860+45
−49 7001713400000000000♠71.34±0.65 A2Vann 2.0 3.55 Lepus 05h 46m 57.341s −14° 49′ 19.02″
Lalande 21185 54035 7000469200000000000♠4.692±0.018 7001220390000000000♠22.039+0.082
−0.081 7000830700000000000♠8.307±0.014 M2V 0.39 7.52 Ursa Major 11h 03m 20.194s +35° 58′ 11.55″
2MASS J1941-4602 7000485400000000000♠4.854+0.087
−0.085 2997536299999999999♠−463.7+6.5
−6.7 7001669960000000000♠66.996±0.066 M4-M6 ~0.15 12.4 Telescopium 19h 41m 53.18s −46° 02′ 31.4″

See also[edit]
Book: The Nearest Stars
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
Star portal
Astronomy portal
Solar System portal
Space portal
Notes[edit]
^ Jump up to: a b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.
Jump up ^ Before 1900: earliest certain recorded observation. 1900–1930: first catalogued. After 1930: earliest trigonometric or spectroscopic parallax.
Jump up ^ Systems with their first accurate trigonometric parallaxes measured by RECONS
^ Jump up to: a b c Might not be within 5 parsecs of the Sun.
References[edit]
^ Jump up to: a b c Matthews, R.A. (1994). "The Close Approach of Stars in the Solar Neighborhood". Quarterly Journal of the Royal Astronomical Society. Royal Astronomical Society. 35: 1. Bibcode:1994QJRAS..35....1M.
Jump up ^ 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.
^ Jump up to: a b c Bailer-Jones, C.A.L.; Rybizki, J,; Andrae, R.; Fouesnea, M. (2018). "New stellar encounters discovered in the second Gaia data release". arXiv:1805.07581  [astro-ph.SR].
^ Jump up to: a b c Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
^ Jump up to: a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap aq ar as at au av aw ax ay az ba bb bc bd be bf bg bh bi bj bk bl bm bn bo bp bq br bs bt bu bv bw bx by bz ca cb cc cd ce cf cg ch ci cj ck cl cm cn co cp cq cr cs ct cu cv cw cx cy cz da db dc dd de df dg dh di dj dk dl dm dn do dp dq dr ds dt du dv dw dx dy dz ea eb ec ed ee ef eg eh ei ej ek el em en eo ep eq er es et eu ev ew ex ey ez fa fb fc fd fe ff fg fh fi fj fk fl fm fn fo fp fq fr fs ft fu fv fw fx "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars (RECONS). Georgia State University. September 17, 2007. Retrieved 2007-11-06.
^ Jump up to: a b From parallax.
^ Jump up to: 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.
^ Jump up to: a b General Catalogue of Trigonometric Parallaxes.
^ Jump up to: a b Hipparcos Catalogue.
Jump up ^ Visual binary orbits and masses post Hipparcos, Staffan Söderhjelm, Astronomy and Astrophysics 341 (January 1999), pp. 121–140.
Jump up ^ Barnard, E. E. (1916). "A small star with large proper motion". Astronomical Journal. 29 (695): 181. Bibcode:1916AJ.....29..181B. doi:10.1086/104156.
^ Jump up to: a b Luhman, K. L. (2013). "Discovery of a Binary Brown Dwarf at 2 Parsecs from the Sun" (PDF). The Astrophysical Journal Letters. 767: L1. arXiv:1303.2401  . Bibcode:2013ApJ...767L...1L. doi:10.1088/2041-8205/767/1/L1. [permanent dead link]
^ Jump up to: a b 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. CS1 maint: Explicit use of et al. (link)
Jump up ^ Boffin, H. M. J.; Pourbaix, D.; Muzic, K.; Ivanov, V. D.; Kurtev, R.; Beletsky, Y.; Mehner, A.; Berger, J. P.; Girard, J. H.; Mawet, D. (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.
Jump up ^ 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.
Jump up ^ 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.
Jump up ^ Davison, Cassy L.; White, Russel J.; Henry, Todd J.; Riedel, Adric R.; Jao, Wei-Chun; Bailey III, John I.; Quinn, Samuel N.; Cantrell, Justin R.; Subasavage, John P.; Winters, Jen G. (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.
Jump up ^ 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.
Jump up ^ "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey". Butler et al. (2017)
Jump up ^ 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
Jump up ^ ESO. "A temperate exo-Earth around a quiet M dwarf at 3.4 parsecs" (PDF). Retrieved 15 November 2017.
Jump up ^ Torres, G.; Andersen, J.; Giménez, A. (7 October 2009). "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. Retrieved 10 May 2018.
Jump up ^ 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. 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
Jump up ^ "The NASA-UC-UH Eta-Earth Program: IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth". Andrew W. Howard, Geoffrey W. Marcy, Debra A. Fischer, Howard Isaacson, Philip S. Muirhead, Gregory W. Henry, Tabetha S. Boyajian, Kaspar von Braun, Juliette C. Becker, Jason T. Wright, John Asher Johnson. Accessed August 26, 2014.
Jump up ^ "Detection of the closest Jovian exoplanet in the Epsilon Indi triple system". Fabo Feng, Mikko Tuomi, Hugh R. A. Jones. Accessed 21 March 2018.
^ Jump up to: 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. CS1 maint: Multiple names: authors list (link) (main page)
Jump up ^ 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.
^ Jump up to: 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.
Jump up ^ "The HARPS search for southern extra-solar planets XLII. A system of Earth-mass planets around the nearby M dwarf YZ Cet". N. Astudillo-Defru1 , R. F. Díaz, X. Bonfils , J.M. Almenara, J.-B. Delisle, F. Bouchy, X. Delfosse, T. Forveille, C. Lovis, M. Mayor, F. Murgas, F. Pepe, N. C. Santos, D. Ségransan, S. Udry, A. Wünsche (August 10, 2017).
Jump up ^ 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.
Jump up ^ "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". N. Astudillo-Defru, T. Forveille, X. Bonfils, D. Ségransan, F. Bouchy, X. Delfosse, C. Lovis, M. Mayor, F. Murgas, F. Pepe, N. C. Santos, S. Udry, A. Wunsche (March 15, 2017).
Jump up ^ 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.
Jump up ^ The very nearby M/T dwarf binary SCR 1845-6357, Markus Kasper, Beth A. Biller, Adam Burrows, Wolfgang Brandner, Jano Budaj, and Laird M. Close, Astronomy and Astrophysics 471, #2 (August 2007), pp. 655–659. doi:10.1051/0004-6361:20077881
Jump up ^ Guillem Anglada-Escudé; Pamela Arriagada; Mikko Tuomi; Mathias Zechmeister; James S. Jenkins; Aviv Ofir; Stefan Dreizler; Enrico Gerlach; Chris J. Marvin; Ansgar Reiners; Sandra V. Jeffers; R. Paul Butler; Steven S. Vogt; Pedro J. Amado; Cristina Rodríguez-López; Zaira M. Berdiñas; Julian Morin; Jeff D. Crane; Stephen A. Shectman; Ian B. Thompson; Matías Díaz; Eugenio Rivera; Luis F. Sarmiento; Hugh R.A. Jones (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:1406.0818v1  [astro-ph.EP]. Bibcode:2014MNRAS.443L..89A. doi:10.1093/mnrasl/slu076.
Jump up ^ 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
^ Jump up to: a b The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation—First Results from the 1.5 m Telescope Program, Edgardo Costa, René A. Méndez, W.-C. Jao, Todd J. Henry, John P. Subasavage, Misty A. Brown, Philip A. Ianna, and Jennifer Bartlett, The Astronomical Journal 130, #1 (July 2005), pp. 337–349. doi:10.1086/430473
Jump up ^ Lucas; Tinney; Ben Burningham; Leggett; Pinfield; Richard Smart; Jones; Federico Marocco; Barber (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". arXiv:1004.0317v2  [astro-ph.SR].
Jump up ^ Leggett, S. K.; Saumon, D.; Marley, M. S.; Lodders, K.; Canty, J.; Lucas, P.; Smart, R. L.; Tinney, C. G.; Homeier, D.; Allard, F.; Burningham, Ben; Day-Jones, A.; Fegley, B.; Ishii, Miki; Jones, H. R. A.; Marocco, F.; Pinfield, D. J.; Tamura, M. (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.
Jump up ^ Lucas, Philip W.; Tinney; Burningham; Leggett; Pinfield; Smart; et al. (2010). "Discovery of a very cool brown dwarf amongst the ten nearest stars to the Solar System". arXiv:1004.0317v1  [astro-ph.SR]. CS1 maint: Multiple names: authors list (link)
Jump up ^ "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.
Jump up ^ Gliese, W. and Jahreiß, H. (1991). "Gl 473". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 10 May 2018. CS1 maint: Multiple names: authors list (link)
Jump up ^ "The Extrasolar Planet Encyclopaedia — Catalog Listing".
Jump up ^ 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.
Jump up ^ 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: A43. arXiv:1307.2722  . Bibcode:2013A&A...557A..43B. doi:10.1051/0004-6361/201322141.
Jump up ^ 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.
Jump up ^ Tinney, C. G.; Faherty, Jacqueline K.; Kirkpatrick, J. Davy; Cushing, Mike; Morley, Caroline V.; Wright, Edward L. (4 November 2014). "THE LUMINOSITIES OF THE COLDEST BROWN DWARFS". The Astrophysical Journal. 796 (1): 39. arXiv:1410.0746  . Bibcode:2014ApJ...796...39T. doi:10.1088/0004-637X/796/1/39. ISSN 1538-4357.
Jump up ^ Bailey, Jeremy; et al. (2008). "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.
Jump up ^ 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.
^ Jump up to: a b c "G 158-50 - SIMBAD". SIMBAD. Retrieved 2015-09-12.
Jump up ^ See also: Stellar kinematics.
Jump up ^ "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.
^ Jump up to: a b 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.
Jump up ^ 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.
Jump up ^ 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.
Jump up ^ Coryn Bailer-Jones (2015-01-01). "The closest encounter is Hip 85605. How reliable is this?". Retrieved 2015-01-05.
Jump up ^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (19 May 2018). "New stellar encounters discovered in the second Gaia data release". Retrieved 23 May 2018.
Jump up ^ A Family Portrait of the Alpha Centauri System (eso0307), European Southern Observatory. 15 March 2003. Accessed online 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. (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
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0–5 ly →
Main-sequence
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Sun (0 ly)
rest of Solar System
α Cen (4.366±0.007 ly)
K-type main-sequence star B
red dwarf C (Proxima Centauri) (4.2430 ± 0.0017 ly)
planet b
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← 5–10 ly →
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A-type
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white dwarf B
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Wolf 359 (7.856±0.031 ly)
Lalande 21185 (8.307±0.014 ly)
L 726-8 (8.73±0.06 ly)
red dwarf UV Cet
Ross 154 (9.60±0.05 ly)
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Luhman 16 (6.59±0.06 ly)
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WISE 0855−0714 (7.27±0.13 ly)
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← 10–15 ly →
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F-type
Procyon (α CMi) (11.41+0.04
−0.03 ly)
white dwarf B
Main-sequence
stars
G-type
τ Cet (11.905±0.007 ly)
5? planets: b
c
d
e
f
K-type
ε Eri (10.475±0.003 ly)
1 (2?) planets: b
c?
61 Cyg (11.409±0.022 ly)
K-type main-sequence star B
ε Ind (11.815±0.012 ly)
2 T-type brown dwarfs: Ba
Bb
1? planets
M-type
(red dwarfs)
Ross 248 (10.298±0.023 ly)
Lac 9352 (10.685+0.025
−0.024 ly)
Ross 128 (10.94±0.06 ly)
EZ Aqr (11.08±0.13 ly)
2 red dwarfs: B
C
Σ 2398 (11.40±0.07 ly)
red dwarf B
Gmb 34 (11.70±0.03 ly)
red dwarf B
planet Ab
SIPS 1259-4336 (11.8+2.1
−1.5 ly)
DX Cnc (11.83±0.13 ly)
Gliese 1061 (12.04±0.06 ly)
YZ Cet (12.20±0.14 ly)
Luyten's Star (12.20±0.04 ly)
Kapteyn's Star (12.78±0.04 ly)
1 (2?) planets: b
c
Lac 8760 (12.87±0.04 ly)
Kruger 60 (13.18±0.08 ly)
red dwarf B
Ross 614 (13.36±0.04 ly)
red dwarf B
Wolf 1061 (14.0±0.1 ly)
3 planets: b
c
d
Wolf 424 (14.05+0.27
−0.26 ly)
red dwarf B
GJ 1 (14.15±0.06 ly)
TZ Ari (14.51+0.19
−0.18 ly)
LHS 292 (14.76±0.24 ly)
GJ 687 (14.77±0.06 ly)
planet b
GJ 674 (14.81+0.10
−0.09 ly)
planet b
G 208-44 (14.81±0.07 ly)
2 red dwarfs: B
G 208-45
Degenerate
stars
White dwarfs
van Maanen 2 (14.03+0.12
−0.11 ly)
Brown dwarfs
M-type
SCR 1845-6357 (12.57±0.05 ly)
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DEN 1048−3956 (13.15±0.03 ly)
2M1540 (14.3+1.7
−1.4 ly)
T-type
WISE 1506+7027 (11.1+2.3
−1.3 ly)
UGPS J0722-0540 (13.43±0.13 ly)
Y-type
WISE 0350−5658 (12.1+5.2
−1.3 ly)
show
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Subgiant stars
G-type
δ Pav (19.923±0.021 ly)
Main-sequence
stars
A-type
Altair (α Aql) (16.73±0.05 ly)
G-type
σ Dra (18.769±0.019 ly)
η Cas (19.42±0.06 ly)
K-type main-sequence star B
e (82 G.) Eri (19.711±0.023 ly)
3 planets: b
c
d
K-type
Groombridge 1618 (15.89±0.04 ly)
ο² (40) Eri (16.257±0.019 ly)
white dwarf B
red dwarf C
70 Oph (16.58±0.07 ly)
K-type main-sequence star B
GJ 570 (19.05+0.11
−0.10 ly)
2 red dwarfs: B
C
T-type brown dwarf D
36 Oph (19.35±0.06 ly)
2 K-type main-sequence stars: B
C
HR 7703 (19.62±0.03 ly)
red dwarf B
M-type
(red dwarfs)
GJ 876 (15.198±0.014 ly)
4 (6?) planets: d
f?
g?
c
b
e
LHS 288 (15.61+0.21
−0.20 ly)
GJ 1002 (15.74+0.24
−0.23 ly)
GJ 412 (15.81±0.08 ly)
red dwarf B
AD Leo (16.00±0.22 ly)
GJ 832 (16.16±0.08 ly)
2 planets: c
b
EV Lac (16.37±0.08 ly)
GJ 682 (16.56±0.18 ly)
2 planets: b
c
GJ 3379 (16.85±0.16 ly)
G 9-38 (17.05+0.23
−0.22 ly)
red dwarf B
LHS 1723 (17.29±0.07 ly)
GJ 445 (17.58+0.14
−0.13 ly)
GJ 526 (17.73±0.10 ly)
Stein 2051 (18.06±0.08 ly)
white dwarf B
GJ 251 (18.22±0.16 ly)
GJ 205 (18.45±0.12 ly)
LP 816-60 (18.6±0.4 ly)
GJ 229 (18.77±0.11 ly)
T-type brown dwarf B
1? planets: Ab?
GJ 693 (18.95+0.25
−0.24 ly)
Ross 47 (18.99±0.12 ly)
GJ 752 (19.05±0.08 ly)
red dwarf B (vB 10)
GJ 754 (19.30±0.18 ly)
TYC 3980-1081-1 (19.3±4.3 ly)
GJ 588 (19.34±0.15 ly)
YZ CMi (19.43+0.27
−0.26 ly)
GJ 908 (19.50±0.14 ly)
GJ 1005 (19.58±0.09 ly)
red dwarf B
2MASS J05332802-4257205 (~19.6 ly)
Scholz's Star (19.60+0.40
−0.28 ly)
T-type brown dwarf B
GJ 268 (19.74±0.25 ly)
red dwarf B
Degenerate
stars
White dwarfs
LP 145-141 (15.11±0.09 ly)
G 240-72 (19.80+0.29
−0.28 ly)
Brown dwarfs
M-type
2MASS 1835+3259 (18.48±0.05 ly)
L-type
DEN 0255-4700 (16.20+0.32
−0.31 ly)
T-type
DEN 0817-6155 (16.1+1.1
−1.0 ly)
WISE J0521+1025 (16.3±4.2 ly)
2MASS 0939-2448 (17.4±0.4 ly)
T-type brown dwarf B
WISE 1741+2553 (18.1+1.6
−1.4 ly)
2MASS 1114-2618 (18.20±0.14 ly)
2MASS 0415-0935 (18.62±0.18 ly)
WISE J2000+3629 (19.4±6.7 ly)
2MASS 0937+2931 (19.96+0.22
−0.21 ly)
Y-type
WISE 1639-6847 (16.12+0.25
−0.24 ly)
WISE 0359−5401 (19.2+4.2
−2.6 ly)
Sub-brown dwarfs
and rogue planets
Y-type
WISE 1541−2250 (18.6±0.5 ly)
Italic are systems without known trigonometric parallax.
Retrieved from "https://en.wikipedia.org/w/index.php?title=List_of_nearest_stars_and_brown_dwarfs&oldid=849077982"
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