View source for Luhman 16

{{Short description|Binary brown dwarf system in the constellation Vela}}
{{Use dmy dates|date=April 2022}}
{{Starbox begin
|name=Luhman 16
}}
{{Starbox image
| image = [[File:Two Brown Dwarfs in Our Backyard.jpg|330px|alt=Luhman 16]]
| caption = WISE image of Luhman 16. In the {{abbr|GMOS|Gemini Multi-Object Spectrograph}} image in the inset, it is resolved into a pair.
}}
{{Starbox observe
|epoch=[[J2000]]{{r|Mamajek2013}}
|equinox=[[J2000]]{{r|Mamajek2013}}
|constell=[[Vela (constellation)|Vela]]
|ra={{RA|10|49|18.771}}<ref name="Bedin2024"/>
|dec={{DEC|−53|19|09.8779}}<ref name="Bedin2024"/>
|appmag_v=16.20<ref name=ucac4/>
}}
{{Starbox character
|class=A: L7.5{{r|Burgasser2013}} <br /> B: T0.5 ± 1{{r|Burgasser2013}}
|appmag_1_passband=i <small>([[Deep Near Infrared Survey of the Southern Sky|DENIS]] filter system)</small>
|appmag_1={{val|14.94|0.03}}{{r|Luhman2013}}
|appmag_2_passband=J <small>([[2MASS]] filter system)</small>
|appmag_2={{val|10.73|0.03}}{{r|Luhman2013}}
|appmag_3_passband=J <small>([[Deep Near Infrared Survey of the Southern Sky|DENIS]] filter system)</small>
|appmag_3={{val|10.68|0.05}}{{r|Luhman2013}}
|appmag_4_passband=H <small>([[2MASS]] filter system)</small>
|appmag_4={{val|9.56|0.03}}{{r|Luhman2013}}
|appmag_5_passband=K<sub>S</sub> <small>([[2MASS]] filter system)</small>
|appmag_5={{val|8.84|0.02}}{{r|Luhman2013}}
|appmag_6_passband=K<sub>S</sub> <small>([[Deep Near Infrared Survey of the Southern Sky|DENIS]] filter system)</small>
|appmag_6={{val|8.87|0.08}}{{r|Luhman2013}}
}}
{{Starbox astrometry
|prop_mo_ra={{val|-2768.511|0.056|0.030}}
|prop_mo_dec={{val|358.472|0.027|0.047}}
|pm_footnote=<ref name="Bedin2024"/>
|parallax=500.993
|p_error=0.050
|parallax_footnote=<ref name="Bedin2024"/>
}}
{{Starbox orbit
| reference = <ref name="Bedin2024"/>
| period = {{val|26.55|0.08}}
| axis_unitless = 3.52 [[astronomical unit|AU]]
| eccentricity = {{val|0.344|0.001}}
| inclination = {{val|79.92|0.008}}
| node = {{val|130.02|0.01}}
| periarg = {{val|136.67|0.09}}
| periastron = {{val|2018.060|0.003}}
}}
{{Starbox detail
|source={{r|Boffin2014|Kniazev2013|Garcia2017}}
|component1=Luhman 16A
|mass_mj={{val|35.4|0.2}}<ref name="Bedin2024"/>
|mass=0.034
|radius_rj=~0.85{{#tag:ref|From : {{resize|75%|<math>R = \sqrt \frac{L}{ 4 \pi  \sigma {T_e}^4} </math>}}, where {{small|<math>L</math>}}  is the luminosity, {{small|<math>R</math>}}  is the radius, {{small|<math>T_e</math>}} is the effective surface temperature and {{small|<math>\sigma </math>}} is the [[Stefan–Boltzmann constant]].|group="note"|name="RadiusCalculationFromLuminosityandTemperature"}}
|luminosity={{val|0.0000219}}{{r|Garcia2017}}
|temperature=1350
|rotation=6.94 hours<ref name=Apai2021/>
|component2=Luhman 16B
|mass_mj2={{val|29.4|0.2}}<ref name="Bedin2024"/>
|mass2=0.028
|radius_rj2=~1.04<ref group="note" name="RadiusCalculationFromLuminosityandTemperature"/>
|luminosity2={{val|0.0000209}}{{r|Garcia2017}}
|temperature2=1210
|rotation2=5.28 hours<ref name=Apai2021/>
}}
{{Starbox relpos
|reference={{r|Luhman2013}}
|primary=A
|component=B
|angdistsec=1.5
|projsep=3
|projsepref=
}}
{{Starbox catalog
| names = LUH 16,{{r|Mamajek2013}} Luhman–WISE 1,{{r|Mamajek2013}} [[Wide-field Infrared Survey Explorer|WISE]] J104915.57−531906.1,{{r|Luhman2013}} [[Deep Near-Infrared Survey of the Southern Sky|DENIS]]-P J104919.0−531910,<ref name="simbad"/> [[2MASS]] J10491891−5319100,{{r|simbad}} [[IRAS]] Z10473-5303,{{r|Mamajek2013}} [[Akari (satellite)|AKARI]] J1049166−531907,{{r|Mamajek2013}} [[Guide Star Catalog|GSC]]2.2 S11132026703,{{r|Mamajek2013}} [[Guide Star Catalog|GSC]]2.3 S4BM006703,{{r|Mamajek2013}} [[TESS Input Catalog|TIC]] 119862115,<ref name="simbad"/> [[Gliese Catalogue of Nearby Stars|GJ]] 11551<ref name="CNS5"/>
}}
{{Starbox reference
|Simbad=WISE+J104915.57-531906.1|sn=The system
|Simbad2=NAME+WISE+J1049-5319A|sn2=A
|Simbad3=NAME+WISE+J1049-5319B|sn3=B
}}
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Vela_constellation_map.svg
|alt=Luhman 16 is located in the constellation Vela.
|caption=Location of Luhman 16 in the constellation [[Vela (constellation)|Vela]]|border=infobox|mark=Red_pog.png|marksize=9|width=330
|label=&nbsp;&nbsp;&nbsp;Luhman&nbsp;16
|position=top
|lat=29.3
|long=20
}}|caption=
}}
{{Starbox end}}

'''Luhman 16''' (also designated '''WISE 1049−5319''' or '''WISE J104915.57−531906.1''') is a [[Binary system|binary]] [[brown dwarf|brown-dwarf]] system in the southern [[constellation]] [[Vela (constellation)|Vela]] at a distance of {{convert|6.51|ly|pc|lk=on|abbr=off}} from the [[Sun]]. These are the [[List of nearest stars and brown dwarfs|closest-known brown dwarfs and the closest system]] found since the measurement of the [[proper motion]] of [[Barnard's Star]] in 1916,{{r|PennState|Plait}} and the third-closest-known system to the Sun (after the [[Alpha Centauri]] system and Barnard's Star). The primary is of [[stellar classification|spectral type]] L7.5 and the secondary of type {{nowrap|T0.5 ± 1}} (and is hence near the L–T transition).{{r|Sahlmann2015}} The masses of Luhman&nbsp;16&nbsp;A and B are 35.4 and 29.4 Jupiter masses, respectively, and their ages are estimated to be 400–800 million years.<ref name="Bedin2024"/> Luhman&nbsp;16&nbsp;A and B orbit each other at a distance of about 3.5 [[astronomical unit]]s{{r|Luhman2013}} with an [[orbital period]] of approximately 26.6 years.<ref name="Bedin2024"/>

==Discovery==
This system was discovered by [[Kevin Luhman]], astronomer from [[Pennsylvania State University]] and a researcher at Penn State's Center for [[Exoplanet]]s and Habitable Worlds,{{r|PennState}} from images made by the [[Wide-field Infrared Survey Explorer]] (WISE) [[Geocentric orbit|Earth-orbiting]] [[satellite]]—[[NASA]] [[infrared|infrared-wavelength]] {{convert|40|cm|abbr=on}} [[space telescope]], a mission that lasted from December 2009 to February 2011; the discovery images were taken from January 2010 to January 2011, and the discovery was announced in 2013 (the pair are the only two objects announced in the discovery paper). The system was found by comparing WISE images at different [[Epoch (astronomy)|epoch]]s to reveal objects that have high [[proper motion]]s.{{r|PennState|Luhman2013}}

Luhman 16 appears in the sky close to the [[galactic plane]], which is densely populated by stars; the abundance of light sources makes it difficult to spot faint objects. This explains why an object so near to the Sun was not discovered in earlier searches.{{r|Luhman2013}}

===Discovery of companion===
[[File:Wise1049-5319 Multi-Color (No Marker, crop).png|thumb|left|Luhman 16 is the yellow disc at the center of this [[Wide-field Infrared Survey Explorer|WISE]] image. The individual brown dwarfs are not resolved.]]
The second component of the system was also discovered by Luhman in 2013, and was announced in the same article as the primary. Its discovery image in the ''i''-band was taken on the night of 23 February 2013 with the [[Gemini Multi-Object Spectrograph]] (GMOS) at the [[Gemini Observatory|Gemini South telescope]], [[Chile]]. The components of the system were resolved with an angular distance of 1.5 [[Minute and second of arc|arcseconds]], corresponding to a projected separation of 3 [[astronomical unit|AU]], and a magnitude difference of 0.45 mag.{{r|Luhman2013}}

===Precovery===
Although the system was first found on images taken by WISE in 2010–2011, afterwards it was [[precovery|precovered]] from the [[Digitized Sky Survey]] (DSS, 1978 ([[infrared|IR]]) & 1992 (red)),{{r|Luhman2013}} Infrared Astronomical Satellite ([[IRAS]], 1983),{{r|Mamajek2013}} [[La Silla Observatory|ESO Schmidt telescope]] (1984 (red)),{{r|Mamajek2013}} [[Guide Star Catalog]] (GSC, 1995),{{r|Mamajek2013}} [[Deep Near Infrared Survey of the Southern Sky]] (DENIS, 1999),{{r|Luhman2013}} Two Micron All-Sky Survey ([[2MASS]], 1999),{{r|Luhman2013}} and the [[Akari (satellite)|AKARI]] satellite (2007).{{r|Mamajek2013}}

On the ESO Schmidt telescope image, taken in 1984, the source looks elongated with a [[position angle]] of 138[[degree (angle)|°]].{{r|Mamajek2013}} The similarity of this position angle with that of the resolved pair in the GMOS image (epoch 2013) in Fig. 1 of Luhman (2013) suggests that the time period between 1984 and 2013 may be close to the orbital period of the system (not far from original orbital period estimate by Luhman (2013){{r|Luhman2013}}).{{r|Mamajek2013}}

==Name==
Eric E. Mamajek proposed the name Luhman 16 for the system, with the components called Luhman 16A and Luhman 16B. The name originates from the frequently updated [[Washington Double Star Catalog]] (WDS). [[Kevin Luhman]] had already published several new discoveries of binary stars that have been compiled in the WDS with discovery identifier "LUH". The WDS catalog now lists this system with the identifier 10493−5319 and discoverer designation LUH 16.<ref name="WashDSCat"/>

The rationale is that Luhman 16 is easier to remember than WISE J104915.57−531906.1 and that "it seems silly to call this object by a 24-character name (space included)".{{r|Mamajek2013}}{{r|Mamajek2013v1}}<ref name="note 1" group="note">In the first e-print version of the article the designation WISE J104915.57−531906 was used, which is an incorrect format for WISE identifiers because the last two characters ".1" were omitted, so it was mentioned that it is a "22-character name". In the second (and last) version of the e-print the correct 24-character designation was used.</ref> The "phone number names" also include WISE J1049−5319 and WISE 1049−5319. Luhman–WISE 1 was proposed as another alternative.{{r|Mamajek2013}}

As a binary object it is also called Luhman 16AB.

==Astrometry==

===Position in the sky===
Luhman 16 is located in the southern celestial hemisphere in the constellation [[Vela (constellation)|Vela]]. As of July 2015, its components are the nearest-known celestial objects in this constellation outside the Solar System. Its celestial coordinates: [[Right ascension|RA]] = {{RA|10|49|18.723}}, [[Declination|Dec]] = {{DEC|−53|19|09.86}}.{{r|Mamajek2013}}

===Distance===
[[File:PIA18003-NASA-WISE-StarsNearSun-20140425-2 correction.png|thumb|upright=2|left|Diagram of the [[List of nearest stars|closest stars]] to the Sun within 7.5 ly (Luhman 16 is labeled as WISE 1049-5319)|alt=Series of partial circles centred on a small yellow disk labelled "Sun", each circle labelled with a distance, and several other small disks labelled with the names of stars.]]
[[File:Angular map of fusors around Sol within 9ly (large).png|thumb|upright=1.5|The position of Luhman 16 on a [[Plan position indicator|radar]] map among all stellar objects or [[star system|stellar systems]] within 9 light years (ly) from the map's center, the Sun (Sol). The diamond-shapes are their positions entered according to [[right ascension]] in [[hour angle|hours angle]] (indicated at the edge of the map's reference disc), and according to their [[declination]]. The second mark shows each's distance from Sol, with the [[Concentric objects|concentric]] circles indicating the distance in steps of one ly.]]

The trigonometric [[parallax]] of Luhman 16 as published by Sahlmann & Lazorenko (2015) is {{val|0.50051|0.00011}} [[arcsecond|arcsec]], corresponding to a distance of {{convert|1.998|±|0.0004|pc|ly|4|order=flip|abbr=off|lk=on}}.{{r|Sahlmann2015}} Subsequent observations with Hubble and Gaia improved the parallax to {{val|500.993|0.059|0.048}} ±0.050 mas, corresponding to a distance of {{val|1.996036|0.00019|0.00024}} ±0.0002 parsec, which is accurate to about 50 astronomical units.<ref name="Bedin2024"/>

===Proximity to the Solar System===
Currently Luhman 16 is the third-closest-known star/brown-dwarf system to the Sun after the triple [[Alpha Centauri]] system (4.37 [[light-year|ly]]) and [[Barnard's Star]] (5.98 ly), pushing [[Wolf 359]] (7.78 ly) to the fifth place, along with the discovery of [[WISE 0855−0714]]. It also holds several records: the nearest [[brown dwarf]], the nearest L-type dwarf, and possibly the nearest T-type dwarf (if component B is of T-type).

===Proximity to Alpha Centauri===
Luhman 16 is the nearest-known star/brown-dwarf system to [[Alpha Centauri]], located {{convert|3.577|ly|pc|abbr=on}} from Alpha Centauri AB, and {{convert|3.520|ly|pc|abbr=on}} from [[Proxima Centauri]].<ref name="note 2" group="note">Assuming parallax of Luhman 16 from Sahlmann & Lazorenko (2015): 500.51 [[milliarcsecond|mas]], parallax of Alpha Centauri AB from Söderhjelm (1999): 747.1 [[milliarcsecond|mas]], and parallax of Proxima Centauri from Benedict ''et al.'' (1999): 768.7 [[milliarcsecond|mas]].</ref> Both systems are located in neighboring constellations, in the same part of the sky as seen from Earth, but Luhman 16 is a bit farther away. Before the discovery of Luhman 16, the Solar System was the nearest-known system to Alpha Centauri.

Luhman 16 is closer to Proxima Centauri than to Alpha Centauri AB, just like Earth, even though Luhman 16 is farther from Earth than is the Alpha Centauri system.  Therefore Luhman 16 has smaller angular distance to Proxima Centauri than to Alpha Centauri AB in Earth's sky, and this makes more contribution{{clarify|date=November 2023}} to the distance difference from Luhman 16 to Alpha Centauri than to the distance difference between them and Earth.

===Proper motion===
[[File:Luhman16AB (cropped).gif|thumb|upright=1.2|Luhman 16A and B orbit each other at a distance of only 3.5 [[astronomical unit|AU]].<ref name="SpaceTel20170605"/>]]

The [[proper motion]] of Luhman 16 as published by Garcia ''et al.'' (2017), is about 2.79″/year, which is relatively large due to the proximity of Luhman 16.{{r|Garcia2017}}

===Radial velocity===
The [[radial velocity]] of {{nowrap|component A}} is {{convert|23.1|±|1.1|km/s|abbr=on}}, and the radial velocity of {{nowrap|component B}} is {{convert|19.5|±|1.2|km/s|abbr=on}}.{{r|Kniazev2013}} Since values of the radial velocity are positive, the system currently is moving away from the Solar System.

Assuming these values for the components, and a mass ratio of {{nowrap|Luhman 16}} from Sahlmann & Lazorenko (2015) of 0.78,{{r|Sahlmann2015}} the system's barycentre radial velocity is about {{convert|21.5|km/s|abbr=on}}.<ref name="note 3" group="note">(23.1 + 19.5 * 0.78) / (1 + 0.78) ≈ 21.5.</ref> This implies that {{nowrap|Luhman 16}} passed by the Solar System around 36,000 years ago at a minimal distance of about {{convert|5.05|ly|pc|abbr=on}}.

==Orbit and masses==
In Luhman 16's original discovery paper, Luhman ''et al.'' (2013) estimated the [[orbital period]] of its components to be about 25 years.{{r|Luhman2013}}

Garcia ''et al.'' (2017), using archival observations extending over 31 years, found an orbital period of 27.4 years with a semi-major axis of 3.54 AU. This orbit has an eccentricity of 0.35 and an inclination of 79.5°. The masses of the components were found to be {{Jupiter mass| {{val|34.2|1.3|1.2}} |link=y|jup=y}} and {{Jupiter mass| {{val|27.9|1.1|1.0}} |jup=y}}, respectively, with their mass ratio being about 0.82.{{r|Garcia2017}}

With the data from [[Gaia (spacecraft)|''Gaia'' DR2]] in 2018, their orbit was refined to a period of {{val|27.5|0.4}} years, with a semi-major axis of {{val|3.56|0.025|u=AU}}, an eccentricity of {{val|0.343|0.005}}, and an inclination of {{val|100.26|0.05|u=°}} (facing the opposite direction as the 2017 study found). Their masses were additionally refined to {{Jupiter mass| {{val|33.51|0.31|0.29}} |jup=y}} and {{Jupiter mass| {{val|28.55|0.26|0.25}} |jup=y}}.{{r|Lazorenko2018}} In 2024 the distance and orbit was further refined, resulting in a semi-major axis of 3.52 AU (assuming a parallax of 500.993 mas), an eccentricity of {{val|0.344|0.001}} and an inclination of {{val|79.92|0.001|u=°}}, bringing the inclination in line with previous measurements. The secondary has a mass which is {{val|83.05|0.06|u=%}} that of the primary. The individual masses were  measured to be 35.2±0.2 and 29.4±0.2 Jupiter masses.<ref name="Bedin2024"/>

These results are consistent with all previous estimates of the orbit and component masses.{{r|Garcia2017}}{{r|Mamajek2013}}{{r|Burgasser2013}}{{r|Sahlmann2015}}

By comparing the rotation periods of the brown dwarfs with the [[projected rotational velocities]], it appears that both brown dwarfs are viewed roughly equator-on, and they are aligned well to their orbits.{{r|Apai2021}}

== Age ==
A 2013 paper, published shortly after Luhman 16 was discovered, concluded that the brown dwarf belongs to the [[thin disk]] of the [[Milky Way]] with 96% probability, and therefore does not belong to a young [[moving group]].<ref name="Mamajek2013"/> Based on [[lithium]] absorption lines the system has a maximum age of about 3–4.5 [[Gigayear|Gyr]].<ref>{{Cite journal|last1=Faherty|first1=Jacqueline K.|author1-link=Jackie Faherty|last2=Beletsky|first2=Yuri|last3=Burgasser|first3=Adam J.|last4=Tinney|first4=Chris|last5=Osip|first5=David J.|last6=Filippazzo|first6=Joseph C.|last7=Simcoe|first7=Robert A.|date=August 2014|title=Signatures of Cloud, Temperature, and Gravity from Spectra of the Closest Brown Dwarfs|journal=The Astrophysical Journal|language=en|volume=790|issue=2|pages=90|doi=10.1088/0004-637X/790/2/90|arxiv=1406.1518|bibcode=2014ApJ...790...90F|issn=0004-637X|doi-access=free}}</ref><ref>{{Cite journal|last1=Burgasser|first1=Adam J.|last2=Sheppard|first2=Scott S.|last3=Luhman|first3=K. L.|date=August 2013|title=Resolved Near-infrared Spectroscopy of WISE J104915.57-531906.1AB: A Flux-reversal Binary at the L dwarf/T Dwarf Transition|journal=The Astrophysical Journal|language=en|volume=772|issue=2|pages=129|doi=10.1088/0004-637X/772/2/129|arxiv=1303.7283|bibcode=2013ApJ...772..129B|issn=0004-637X|doi-access=free}}</ref> Observations with the [[Very Large Telescope|VLT]] showed that the system is older than 120 [[Myr]].<ref>{{Cite journal|last1=Lodieu|first1=N.|last2=Zapatero Osorio|first2=M. R.|last3=Rebolo|first3=R.|last4=Béjar|first4=V. J. S.|last5=Pavlenko|first5=Y.|last6=Pérez-Garrido|first6=A.|date=September 2015|title=VLT X-Shooter spectroscopy of the nearest brown dwarf binary|journal=Astronomy & Astrophysics|language=en|volume=581|pages=A73|doi=10.1051/0004-6361/201424933|arxiv=1506.08848|bibcode=2015A&A...581A..73L|issn=0004-6361|doi-access=free}}</ref>

However, in 2022, Luhman 16 was found to be a member of the newly discovered [[Oceanus moving group]], which has an age of {{val|510|95}} [[Myr]].<ref name="Gagné2022"/> Age estimates of 400–800 Myr in 2024 is in line with the membership with this group. The age estimates are mismatched for both components, which could be due to different cloud coverage resulting in different cooling efficiency. Alternatively this could be due to inaccurate luminosities or errors in the evolutionary models.<ref name="Bedin2024"/>

==Search for planets==
In December 2013, perturbations of the orbital motions in the system were reported, suggesting a third body in the system. The period of this possible companion was a few months, suggesting an orbit around one of the brown dwarfs. Any companion would necessarily be below the brown-dwarf mass limit, as otherwise it would have been detected through direct imaging. Researchers estimated the odds of a false positive as 0.002%, assuming the measurements had not been made in error. If confirmed, this would have been the first exoplanet discovered astrometrically. They estimate the planet to likely have a mass between "a few" and {{Jupiter mass|30|jup=y}}, although they mention that a more massive planet would be brighter and therefore would affect the "photocenter" or measured position of the star. This would make it difficult to measure the astrometric movement of an exoplanet around it.{{r|Boffin2014}}

Subsequent astrometric monitoring of Luhman 16 with the [[Very Large Telescope]] has excluded the presence of any third object with a mass greater than {{Jupiter mass|2|jup=y|link=y}} orbiting around either brown dwarf with a period between 20 and 300 days. Luhman 16 does not contain any close-in giant planets.<ref name="Sahlmann2015"/>

Observations with the ''Hubble Space Telescope'' in 2014–2016 confirmed the nonexistence of any additional brown dwarfs in the system. It additionally ruled out any Neptune mass ({{Earth mass|17|link=yes}}) objects with an orbital period of one to two years.<ref name="Bedin2017"/> This makes the existence of the previously found exoplanet candidate highly unlikely.

Additional observations with Hubble rules out the existence of a planet with >1.5 Neptune masses at an orbit of 400 to 5000 days. This study did however not rule out planets with a mass of less than 3 Neptune masses and a shorter period of 2 to 400 days.<ref name="Bedin2024"/>

==Atmosphere==
A study by Gillon ''et al.'' (2013) found that Luhman 16B exhibited uneven surface illumination during its rotation.<ref name="Gillon2013" /> On 5 May 2013, Crossfield ''et al.'' (2014) used the [[European Southern Observatory]]{{'s}} [[Very Large Telescope]] (VLT) to directly observe the Luhman 16 system for five hours, the equivalent of a full rotation of Luhman 16B.<ref name="eso1404a" /><ref name="Crossfield2014" /> Their research confirmed the observation of Gillon ''et al.'', finding a large, dark region at the middle latitudes, a bright area near its upper pole, and mottled illumination elsewhere. They suggest this variant illumination indicates "patchy global clouds", where darker areas represent thick clouds and brighter areas are holes in the cloud layer permitting light from the interior.<ref name="eso1404a" /><ref name="Crossfield2014" /> Luhman 16B's illumination patterns change rapidly, on a day-to-day basis.<ref name="Gillon2013" /><ref name=Apai2021/> Luhman 16B is one of the most photometrically variable brown dwarfs known, sometimes varying with an amplitude of over 20%.<ref name=Heinze>{{cite journal|doi=10.3847/1538-4357/ac178b|title=Weather on Other Worlds. VI. Optical Spectrophotometry of Luhman 16B Reveals Large-amplitude Variations in the Alkali Lines|year=2021|last1=Heinze|first1=A. N.|last2=Metchev|first2=Stanimir|last3=Kurtev|first3=Radostin|last4=Gillon|first4=Michael|journal=The Astrophysical Journal|volume=920|issue=2|page=108|arxiv=2107.10995|bibcode=2021ApJ...920..108H|s2cid=236318236 |doi-access=free }}</ref> Only [[2MASS J21392676+0220226]] is known to be more variable.<ref name=Heinze/>

Heinze ''et al.'' (2021) observed variability in spectral lines of [[alkali metal]]s such as [[potassium]] and [[sodium]]; they suggested that the variations were caused by changes in cloud cover, which changed the local chemical equilibrium with [[chloride]]s. Lightning or aurorae were deemed possible, but less likely.<ref name=Heinze/>

Luhman 16B's lightcurve shows evidence of [[differential rotation]]. There is evidence of equatorial regions and mid-latitude regions with different rotation periods. The main period is 5.28 hours, corresponding to the rotation period of the equatorial region.<ref name=Apai2021/> Meanwhile, the rotation period of Luhman 16A is likely 6.94 hours.<ref name=Apai2021/>

Biller et al. 2024 observed both components with [[James Webb Space Telescope|JWST]] for 8 hours with [[Mid-Infrared Instrument|MIRI]] LRS and directly followed by an 7 hour observation with [[NIRSpec]]. The observations found [[water vapor]], [[carbon monoxide]] and [[methane]] absorption in both brown dwarfs, which is typical for L/T dwarfs. Luhman 16A shows a flat plateau beyond 8.5 μm, which is indicative of small grain [[Silicate|silicates]]. The lightcurves produced from the observations show that both components are variable, with Luhman 16B being considerable more variable than Luhman 16A. The variability has a complex wavelength dependent trend. The researchers identified changes in behaviour at 2.3 μm and 4.2 μm coincident with the CO band and changes in behaviour at 8.3–8.5 μm coincident with silicate absorption. These changes in behaviour were interpreted as changes of average pressure at three different depths of the atmosphere. The observations also tested if patchy clouds could produce the variability. While small silicate grains corresponding to high-[[altitude]] silicate clouds were found in Luhman 16A, it is unlikely to be a patchy cloud layer. Luhman 16B does not have this small grained silicate feature, but larger grained silicate clouds deeper in the atmosphere are possible. The researchers also tested general circulation models (GCM) and hotspots, but the lightcurves are more complex than these models predict.<ref name="Biller2024"/>

Using data collected by TESS,the research team, [[Daniel Apai|Dániel Apai]], Domenico Nardiello and [[Luigi Rolly Bedin|Luigi R. Bedin]], found that the brown dwarf, between star and gas giant, is more similar to [[Jupiter]] in that its high-speed winds form stripes parallel to the equators of Luhman 16 AB.<ref>{{Cite web |first1=Daniel |last1=Apai |first2=Domenico|last2=Nardiello |first3=Luigi R. |last3=Bedin |date=2021-01-08 |title=Vents et jets découverts sur Luhman 16 AB, la naine brune la plus proche de la Terre |url=https://www.insu.cnrs.fr/fr/cnrsinfo/vents-et-jets-decouverts-sur-luhman-16-ab-la-naine-brune-la-plus-proche-de-la-terre |access-date=2024-08-01 |location=Paris, France |publisher=Institute for Earth Sciences and Astronomy, [[National Centre for Scientific Research]] |language=en}}</ref>

<gallery mode="packed" heights="130">
File:Surface map of Luhman 16B recreated from VLT observations (Vid).ogg|Surface map of Luhman 16B recreated from VLT observations
File:Artist's impression of Luhman 16B recreated from VLT observations.ogg|Artist's impression of Luhman 16B based on the VLT observations
File:Luhman 16 visible light MUSE.jpg|Luhman 16 with VLT's [[Multi-unit spectroscopic explorer|MUSE]] instrument in [[Visible spectrum|visible light]].
File:Luhman16.png|High-speed winds form bands parallel to the equators of Luhman 16 AB.
</gallery>

==Radio and X-ray activity==
In a study by Osten ''et al.'' (2015), Luhman 16 was observed with the [[Australia Telescope Compact Array]] in [[radio wave]]s and with the [[Chandra X-ray Observatory]] in [[X-ray]]s. No radio or X-ray activity was found at Luhman 16 AB, and constraints on radio and X-ray activity were presented, which are "the strongest constraints obtained so far for the radio and X-ray luminosity of any ultracool dwarf".{{r|Osten2015}}

==See also==
*[[Substellar object]]

==Notes==
{{reflist|group=note}}

==References==
{{reflist|33em|refs=
<ref name="simbad">{{cite simbad |title=NAME Luhman 16 |access-date=2 June 2023}}</ref>

<ref name="WashDSCat">{{cite web |url=http://ad.usno.navy.mil/wds/Webtextfiles/wdsnewnotes_main.txt |title=USNO Double Star Catalogs: Notes |work=Washington Double Star Catalog |access-date=20 September 2013 |archive-url=https://web.archive.org/web/20161221060834/http://ad.usno.navy.mil/wds/Webtextfiles/wdsnewnotes_main.txt |archive-date=21 December 2016 |url-status=dead }}</ref>

<!--<ref name="NASA-20140425a">{{cite web |url=http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/ |title=NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun |publisher=[[NASA]] |last1=Clavin |first1=Whitney |last2=Harrington |first2=J. D. |date=25 April 2014 |access-date=25 April 2014 |archive-url=https://web.archive.org/web/20140426004939/http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425 |archive-date=26 April 2014 |url-status=live}}</ref>  -->

<ref name="SpaceTel20170605">{{cite web |url=https://www.spacetelescope.org/images/potw1723a/ |title=Waltzing dwarfs |website=Spacetelescope.org |date=5 June 2017 |access-date=6 June 2017}}</ref>

<ref name="Garcia2017">{{Cite journal|title=Individual, Model-Independent Masses of the Closest Known Brown Dwarf Binary to the Sun |journal=The Astrophysical Journal |volume=846 |issue=2 |pages=97 |arxiv=1708.02714 |first1=E. Victor |last1=Garcia |first2=S. Mark |last2=Ammons |first3=Maissa |last3=Salama |first4=Ian |last4=Crossfield |first5=Eduardo |last5=Bendek |first6=Jeffrey |last6=Chilcote |first7=Vincent |last7=Garrel |first8=James R. |last8=Graham |first9=Paul |last9=Kalas |first10=Quinn |last10=Konopacky |first11=Jessica R. |last11=Lu |first12=Bruce |last12=Macintosh |first13=Eduardo |last13=Marin |first14=Christian |last14=Marois |first15=Eric |last15=Nielsen |first16=Benoît |last16=Neichel |first17=Don |last17=Pham |first18=Robert J. |last18=De Rosa |first19=Dominic M. |last19=Ryan |first20=Maxwell |last20=Service |first21=Gaetano |last21=Sivo |display-authors=5 |year=2017|doi=10.3847/1538-4357/aa844f |bibcode=2017ApJ...846...97G |s2cid=119231762 |doi-access=free }}</ref>

<ref name="Sahlmann2015">{{cite journal |title=Mass ratio of the 2 pc binary brown dwarf LUH 16 and limits on planetary companions from astrometry |journal=Monthly Notices of the Royal Astronomical Society: Letters |first1=Johannes |last1=Sahlmann |first2=Petro F. |last2=Lazorenko |volume=453 |issue=1 |pages=L103–L107 |date=October 2015 |doi=10.1093/mnrasl/slv113 |doi-access=free |bibcode=2015MNRAS.453L.103S |arxiv=1506.07994|s2cid=84178005 }}</ref>

<ref name="Bedin2017">{{cite journal |title=''Hubble Space Telescope'' astrometry of the closest brown dwarf binary system. I. Overview and improved orbit |journal=Monthly Notices of the Royal Astronomical Society |last1=Bedin |first1=L. R. |last2=Pourbaix |first2=D. |last3=Apai |first3=D. |last4=Burgasser |first4=Adam J. |last5=Buenzli |first5=E. |last6=Boffin |first6=H. M. J. |last7=Libralato |first7=M. |display-authors=5 |volume=470 |issue=1 |pages=1140–1155 |date=September 2017 |doi=10.1093/mnras/stx1177 |doi-access=free |bibcode=2017MNRAS.470.1140B |arxiv=1706.00657|s2cid=119385778 }}</ref>

<ref name="Gillon2013">{{cite journal |title=Fast-evolving weather for the coolest of our two new substellar neighbours |journal=[[Astronomy & Astrophysics]] |first1=M. |last1=Gillon |first2=A. H. M. J. |last2=Triaud |first3=E. |last3=Jehin |first4=L. |last4=Delrez |first5=C. |last5=Opitom |first6=P. |last6=Magain |first7=M. |last7=Lendl |first8=D. |last8=Queloz |display-authors=5 |volume=555 |pages=L5 |date=July 2013 |doi=10.1051/0004-6361/201321620 |bibcode=2013A&A...555L...5G |arxiv=1304.0481|s2cid=53347195 }}</ref>

<ref name="eso1404a">{{cite news |url=http://www.eso.org/public/news/eso1404/ |title=First Weather Map of Brown Dwarf |publisher=European Southern Observatory |first1=Ian |last1=Crossfield |first2=Richard |last2=Hook |date=29 January 2014 |access-date=30 January 2014}}</ref>

<ref name="Crossfield2014">{{cite journal |url=http://www.eso.org/public/archives/releases/sciencepapers/eso1404/eso1404a.pdf |title=A Global Cloud Map of the Nearest Known Brown Dwarf |journal=[[Nature (journal)|Nature]] |first1=I. J. M. |last1=Crossfield |first2=B. |last2=Biller |first3=J. E. |last3=Schlieder |first4=N. R. |last4=Deacon |first5=M. |last5=Bonnefoy |first6=D. |last6=Homeier |first7=F. |last7=Allard |first8=E. |last8=Buenzli |first9=Th. |last9=Henning |first10=W. |last10=Brandner |first11=B. |last11=Goldman |first12=T. |last12=Kopytova |display-authors=5 |volume=505 |issue=7485 |pages=654–656 |date=30 January 2014 |doi=10.1038/nature12955 |arxiv=1401.8145 |bibcode=2014Natur.505..654C |pmid=24476888|s2cid=4459375 }}</ref>

<ref name="Mamajek2013v1">{{cite arXiv |title=Comments on the Nearby Binary Brown Dwarf WISE J104915.57-531906 |class=astro-ph.SR |eprint=1303.5345v1 |first=Eric E. |last=Mamajek |date=2013}}</ref>

<ref name="Mamajek2013">{{cite arXiv |title=On the Nearby Binary Brown Dwarf WISE J104915.57-531906.1 (Luhman 16) |class=astro-ph.SR |eprint=1303.5345 |first=Eric E. |last=Mamajek |date=2013}}</ref>

<ref name="Lazorenko2018">{{cite journal |title=Updated astrometry and masses of the LUH 16 brown dwarf binary |journal=Astronomy & Astrophysics |first1=P. F. |last1=Lazorenko |first2=J. |last2=Sahlmann |volume=618 |at=A111 |date=October 2018 |doi=10.1051/0004-6361/201833626 |bibcode=2018A&A...618A.111L |arxiv=1808.07835|s2cid=119540451 }}</ref>

<ref name="Luhman2013">{{cite journal |title=Discovery of a Binary Brown Dwarf at 2 pc from the Sun |journal=[[The Astrophysical Journal Letters]] |last=Luhman |first=K. L. |volume=767 |issue=1 |pages=L1 |date=2013 |arxiv=1303.2401 |doi=10.1088/2041-8205/767/1/L1 |bibcode=2013ApJ...767L...1L|s2cid=8419422 }}</ref>

<ref name="PennState">{{cite news |url=http://science.psu.edu/news-and-events/2013-news/Luhman3-2013 |title=The Closest Star System Found in a Century |publisher=Pennsylvania State University Eberly College of Science |first=Barbara K. |last=Kennedy |date=11 March 2013 |access-date=11 March 2013 |archive-date=17 April 2013 |archive-url=https://web.archive.org/web/20130417184006/http://science.psu.edu/news-and-events/2013-news/Luhman3-2013 |url-status=dead }}</ref>

<ref name="Plait">{{cite web |url=http://www.slate.com/blogs/bad_astronomy/2013/03/11/nearby_stars_astronomers_discover_third_closest_star_system_to_earth.html |title=Howdy, Neighbor! New Twin Stars Are Third Closest to the Sun |work=[[Slate (magazine)|Slate]] |series=Bad Astronomy |first=Phil |last=Plait |author-link=Phil Plait |date=11 March 2013 |access-date=11 March 2013}}</ref>

<ref name="Boffin2014">{{cite journal |title=Possible astrometric discovery of a substellar companion to the closest binary brown dwarf system WISE J104915.57-531906.1 |journal=[[Astronomy & Astrophysics]] |first1=Henri M. J. |last1=Boffin |first2=D. |last2=Pourbaix |first3=K. |last3=Mužić |first4=V.D. |last4=Ivanov |first5=R. |last5=Kurtev |first6=Y. |last6=Beletsky |first7=A. |last7=Mehner |first8=J. P. |last8=Berger |first9=J. H. |last9=Girard |first10=D. |last10=Mawet |display-authors=5 |volume=561 |pages=L4 |date=January 2014 |doi=10.1051/0004-6361/201322975 |bibcode=2014A&A...561L...4B |arxiv=1312.1303|s2cid=33043358 }}</ref>

<ref name="Kniazev2013">{{cite journal |title=Characterization of the Nearby L/T Binary Brown Dwarf WISE J104915.57-531906.1 at 2 Parsecs from the Sun |journal=[[The Astrophysical Journal]] |first1=A. Y. |last1=Kniazev |first2=P. |last2=Vaisanen |first3=K. |last3=Mužić |first4=A. |last4=Mehner |first5=H. M. J. |last5=Boffin |first6=R. |last6=Kurtev |first7=C. |last7=Melo |first8=V. D. |last8=Ivanov |first9=J. |last9=Girard |first10=D. |last10=Mawet |first11=L. |last11=Schmidtobreick |first12=N. |last12=Huelamo |first13=J. |last13=Borissova |first14=D. |last14=Minniti |first15=K. |last15=Ishibashi |first16=S. B. |last16=Potter |first17=Y. |last17=Beletsky |first18=D. A. H. |last18=Buckley |first19=S. |last19=Crawford |first20=A. A. S. |last20=Gulbis |first21=P. |last21=Kotze |first22=B. |last22=Miszalski |first23=T. E. |last23=Pickering |first24=E. |last24=Romero Colmenero |first25=T. B. |last25=Williams |display-authors=5 |volume=770 |issue=2 |page=124 |date=June 2013 |doi=10.1088/0004-637X/770/2/124 |bibcode=2013ApJ...770..124K |arxiv=1303.7171|s2cid=26666665 }}</ref>

<ref name="Burgasser2013">{{cite journal |title=Resolved Near-Infrared Spectroscopy of WISE J104915.57-531906.1AB: A Flux-Reversal Binary at the L dwarf/T dwarf Transition |journal=The Astrophysical Journal |first1=Adam J. |last1=Burgasser |first2=Scott S. |last2=Sheppard |first3=K. L. |last3=Luhman |volume=772 |issue=2 |pages=129 |date=August 2013 |arxiv=1303.7283 |bibcode=2013ApJ...772..129B |doi=10.1088/0004-637X/772/2/129|s2cid=54198323 }}</ref>

<ref name="Osten2015">{{cite journal |title=The Deepest Constraints on Radio and X-Ray Magnetic Activity in Ultracool Dwarfs from WISE J104915.57-531906.1 |journal=[[The Astrophysical Journal Letters]] |first1=Rachel A. |last1=Osten |first2=Carl |last2=Melis |first3=Beate |last3=Stelzer |first4=Keith W. |last4=Bannister |first5=Jackie |last5=Radigan |first6=Adam J. |last6=Burgasser |first7=Alex |last7=Wolszczan |first8=Kevin L. |last8=Luhman |display-authors=5 |volume=805 |issue=1 |pages=L3 |date=May 2015 |doi=10.1088/2041-8205/805/1/L3 |bibcode=2015ApJ...805L...3O |arxiv=1504.06514|s2cid=118152106 }}</ref>

<ref name=Apai2021>{{cite journal |doi= 10.3847/1538-4357/abcb97|title= TESS Observations of the Luhman 16 AB Brown Dwarf System: Rotational Periods, Lightcurve Evolution, and Zonal Circulation|year= 2021|last1= Apai|first1= Dániel|last2= Nardiello|first2= Domenico|last3= Bedin|first3= Luigi R.|journal= The Astrophysical Journal|volume= 906|issue= 1|page= 64|arxiv= 2101.02253|bibcode= 2021ApJ...906...64A|s2cid= 230799537|doi-access= free}}</ref>

<ref name=ucac4>{{cite journal|bibcode=2012yCat.1322....0Z |title=VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012) |journal=VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z |volume=1322 |last1=Zacharias |first1=N. |last2=Finch |first2=C. T. |last3=Girard |first3=T. M. |last4=Henden |first4=A. |last5=Bartlett |first5=J. L.|author5-link=Jennifer Bartlett (astronomer) |last6=Monet |first6=D. G. |last7=Zacharias |first7=M. I. |year=2012 }}</ref>

<ref name="Gagné2022">{{cite journal |arxiv=2208.00070 |last1=Gagné |first1=Jonathan |last2=Moranta |first2=Leslie |last3=Faherty |first3=Jacqueline K. |last4=Kiman |first4=Rocio |last5=Couture |first5=Dominic |author6=Arnaud René Larochelle |last7=Popinchalk |first7=Mark |last8=Morrone |first8=Daniella |title=The Oceanus Moving Group: A New 500 Myr Old Host for the Nearest Brown Dwarf |journal=The Astrophysical Journal |year=2023 |volume=945 |issue=2 |page=119 |doi=10.3847/1538-4357/acb8b7 |bibcode=2023ApJ...945..119G |s2cid=253157990 |doi-access=free }}</ref>

<ref name="CNS5">{{cite journal |arxiv=2211.01449 |last1=Golovin |first1=Alex |last2=Reffert |first2=Sabine |last3=Just |first3=Andreas |last4=Jordan |first4=Stefan |last5=Vani |first5=Akash |last6=Jahreiß |first6=Hartmut |title=The Fifth Catalogue of Nearby Stars (CNS5) |date=November 2022 |journal=[[Astronomy & Astrophysics]] |volume=670 |issue= |pages=A19 |doi=10.1051/0004-6361/202244250 |bibcode=2023A&A...670A..19G|s2cid=253264922 }} Catalogue can be accessed [https://dc.g-vo.org/CNS5 here].</ref>

<ref name="Bedin2024">{{Cite journal |last1=Bedin |first1=L. R. |last2=Dietrich |first2=J. |last3=Burgasser |first3=A. J. |last4=Apai |first4=D. |last5=Libralato |first5=M. |last6=Griggio |first6=M. |last7=Fontanive |first7=C. |last8=Pourbaix |first8=D. |date=8 Mar 2024 |title=HST astrometry of the closest Brown Dwarfs -- II. Improved parameters and constraints on a third body |url=https://onlinelibrary.wiley.com/doi/10.1002/asna.20230158 |journal=Astronomische Nachrichten |volume=345 |issue=1 |arxiv=2403.08865 |doi=10.1002/asna.20230158|bibcode=2024AN....34530158B }}</ref>

<ref name="Biller2024">{{Cite journal |last1=Biller |first1=Beth A. |last2=Vos |first2=Johanna M. |last3=Zhou |first3=Yifan |last4=McCarthy |first4=Allison M. |last5=Tan |first5=Xianyu |last6=Crossfield |first6=Ian J.M. |last7=Whiteford |first7=Niall |last8=Suarez |first8=Genaro |last9=Faherty |first9=Jacqueline |last10=Manjavacas |first10=Elena |last11=Chen |first11=Xueqing |last12=Liu |first12=Pengyu |last13=Sutlieff |first13=Ben J. |last14=Limbach |first14=Mary Anne |last15=Molliere |first15=Paul |first16=Trent J. |last16=Dupuy |first17=Natalia |last17=Oliveros-Gomez |first18=Philip S. |last18=Muirhead |first19=Thomas |last19=Henning |first20=Gregory |last20=Mace |first21=Nicolas |last21=Crouzet |first22=Theodora |last22=Karalidi |first23=Caroline V. |last23=Morley |first24=Pascal |last24=Tremblin |first25=Tiffany |last25=Kataria |date=12 Jul 2024 |title=The JWST Weather Report from the Nearest Brown Dwarfs I: multi-period JWST NIRSpec + MIRI monitoring of the benchmark binary brown dwarf WISE 1049AB |url=https://academic.oup.com/mnras/article/532/2/2207/7712857?login=false |journal=MNRAS |volume=532 |issue=2 |pages=2207–2233 |bibcode=2024MNRAS.532.2207B |arxiv=2407.09194|doi=10.1093/mnras/stae1602|doi-access=free }}</ref>

}}

==Further reading==
*{{cite journal |url=http://www.astronomerstelegram.org/?read=5012 |title=X-ray non-detection of the nearest brown dwarf binary WISE 1049-5319 |journal=The Astronomer's Telegram |first1=P. |last1=Gandhi |first2=C. |last2=Done |first3=V. D. |last3=Ivanov |first4=N. |last4=Huelamo |issue=5012 |date=26 April 2013 |volume=5012 |pages=1 |bibcode=2013ATel.5012....1G}}
*{{cite journal |title=Luhman 16AB: A Remarkable, Variable L/T Transition Binary 2 pc from the Sun |journal=Memorie della Societa Astronomica Italiana |first1=Adam J. |last1=Burgasser |first2=J. |last2=Faherty |first3=Y. |last3=Beletsky |first4=P. |last4=Plavchan |first5=M. |last5=Gillon |first6=J. |last6=Radigan |first7=E. |last7=Jehin |first8=L. |last8=Delrez |first9=C. |last9=Opitom |first10=N. |last10=Morrell |first11=R. |last11=Osten |first12=R. |last12=Street |first13=C. |last13=Melis |first14=A. |last14=Triaud |first15=R. |last15=Simcoe |display-authors=5 |volume=84 |issue=4 |page=1017 |date=2013 |bibcode=2013MmSAI..84.1017B |arxiv=1307.6916}} See related [http://bdofage.tng.iac.es/static/files/slides/1305bdcoa_burgasser.pdf slideshow] {{Webarchive|url=https://web.archive.org/web/20140201173350/http://bdofage.tng.iac.es/static/files/slides/1305bdcoa_burgasser.pdf |date=1 February 2014 }}.
*{{cite journal |title=Weather on the Nearest Brown Dwarfs: Resolved Simultaneous Multi-Wavelength Variability Monitoring of WISE J104915.57-531906.1AB |journal=[[The Astrophysical Journal Letters]] |first1=Beth A. |last1=Biller |first2=Ian J. M. |last2=Crossfield |first3=Luigi |last3=Mancini |first4=Simona |last4=Ciceri |first5=John |last5=Southworth |first6=Taisiya G. |last6=Kopytova |first7=Mickaël |last7=Bonnefoy |first8=Niall R. |last8=Deacon |first9=Joshua E. |last9=Schlieder |first10=Esther |last10=Buenzli |first11=Wolfgang |last11=Brandner |first12=France |last12=Allard |first13=Derek |last13=Homeier |first14=Bernd |last14=Freytag |first15=Coryn A. L. |last15=Bailer-Jones |first16=Jochen |last16=Greiner |first17=Thomas |last17=Henning |first18=Bertrand |last18=Goldman |display-authors=5 |volume=778 |issue=1 |pages=L10 |date=November 2013 |doi=10.1088/2041-8205/778/1/L10 |bibcode=2013ApJ...778L..10B |arxiv=1310.5144|s2cid=56107487 }}
*{{cite journal |title=Rotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoring |journal=[[Astronomy & Astrophysics]] |first1=L. |last1=Mancini |first2=P. |last2=Giacobbe |first3=S. P. |last3=Littlefair |display-authors=etal |volume=584 |pages=A104 |date=November 2015 |doi=10.1051/0004-6361/201526899 |bibcode=2015A&A...584A.104M |arxiv=1510.08099 |s2cid=7331525 }}

==External links==
{{Commons category|Luhman 16}}
*[http://solstation.com/stars/wise1049.htm WISE 1049-5319 AB] {{Webarchive|url=https://web.archive.org/web/20220510124036/http://solstation.com/stars/wise1049.htm |date=10 May 2022 }} at Solstation.com
*[http://www.universetoday.com/100682/wise-nabs-the-closest-brown-dwarfs-yet-discovered/ "WISE Nabs the Closest Brown Dwarfs Yet Discovered"] at ''Universe Today''
*[http://astrobites.org/2013/04/05/checking-out-our-new-neighbors/ "Checking Out Our New Neighbors"] at Astrobites.org
* [http://astrobob.areavoices.com/2020/05/13/nearest-brown-dwarf-might-remind-you-of-jupiter/ Nearest Brown Dwarf Might Remind You Of Jupiter] AstroBob, 5/13/20

{{nearest systems|1}}
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{{DEFAULTSORT:Luhman 16}}
[[Category:Astronomical objects discovered in 2013|20130323]]
[[Category:Binary stars]]
[[Category:Local Bubble]]
[[Category:L-type brown dwarfs]]
[[Category:T-type brown dwarfs]]
[[Category:Vela (constellation)]]
[[Category:WISE objects|J104915.57-531906.1]]
[[Category:Articles containing video clips]]
[[Category:2MASS objects|J10491891-5319100]]
[[Category:TIC objects|119862115]]