2MASS J11263991−5003550
{{Short description|Brown dwarf star in the constellation Centaurus 53 light years from Earth}}
{{Starbox begin
|name=2MASS J11263991−5003550
}}
{{Starbox observe
|epoch= J2000.0
|constell=Centaurus
|appmag_v=
}}
{{Starbox character
|type=brown dwarf
|variable = Rotational
}}
{{Starbox astrometry
|parallax=61.6319
|p_error=0.3273
}}
{{Starbox detail
|source=
|mass_mj=
|luminosity=
|temperature= {{val|1270|60|20}}
|age_gyr=
|rotational_velocity={{val|22.8|1.6|2.4}}
}}
{{Starbox catalog
|names=DENIS J112639.9-500355, WISEA J112638.07-500350.1, Gaia DR2 5372923621096443008
}}
{{Starbox reference
|Simbad=2MASS+J11263991-5003550
}}
{{Starbox end}}
2MASS J11263991−5003550 (2MASS J1126−5003) is a brown dwarf about 53 light-years distant from earth. The brown dwarf is notable for an unusual blue near-infrared color.{{Cite journal|last1=Folkes|first1=S. L.|last2=Pinfield|first2=D. J.|last3=Kendall|first3=T. R.|last4=Jones|first4=H. R. A.|date=July 2007|title=Discovery of a nearby L-T transition object in the Southern Galactic plane|journal=MNRAS|language=en|volume=378|issue=3|pages=901–909|doi=10.1111/j.1365-2966.2007.11789.x |arxiv=astro-ph/0703808|bibcode=2007MNRAS.378..901F|issn=0035-8711|doi-access=free}}{{Cite journal|last1=Burgasser|first1=Adam J.|last2=Looper|first2=Dagny L.|last3=Kirkpatrick|first3=J. Davy|last4=Cruz|first4=Kelle L.|last5=Swift|first5=Brandon J.|date=February 2008|title=Clouds, Gravity, and Metallicity in Blue L Dwarfs: The Case of 2MASS J11263991-5003550|journal=Astrophysical Journal|language=en|volume=674|issue=1|pages=451–465|doi=10.1086/524726|arxiv=0710.1123|bibcode=2008ApJ...674..451B|s2cid=6111840|issn=0004-637X}} This brown dwarf does not show subdwarf features and the blue color cannot be explained by an unresolved binary. Instead the blue color is explained by patchy clouds.{{Cite journal|last1=Marley|first1=Mark S.|last2=Saumon|first2=Didier|last3=Goldblatt|first3=Colin|date=November 2010|title=A Patchy Cloud Model for the L to T Dwarf Transition|journal=Astrophysical Journal Letters|language=en|volume=723|issue=1|pages=L117–L121|doi=10.1088/2041-8205/723/1/L117|issn=0004-637X|arxiv=1009.6217|bibcode=2010ApJ...723L.117M|s2cid=56286093}}{{Cite journal |last1=Radigan |first1=Jacqueline |last2=Lafrenière |first2=David |last3=Jayawardhana |first3=Ray |last4=Artigau |first4=Étienne |date=October 2014 |title=Strong Brightness Variations Signal Cloudy-to-clear Transition of Brown Dwarfs |journal=Astrophysical Journal |language=en |volume=793 |issue=2 |pages=75 |doi=10.1088/0004-637X/793/2/75 |issn=0004-637X |arxiv=1404.3247 |bibcode=2014ApJ...793...75R |s2cid=118357522 }} The patchy cloud model allows thick clouds and a cloud coverage of 50% to explain the spectra of 2MASS J1126−5003. Other blue L-dwarfs exist, but are quite rare.{{Cite journal|last1=Kirkpatrick|first1=J. Davy|last2=Looper|first2=Dagny L.|last3=Burgasser|first3=Adam J.|last4=Schurr|first4=Steven D.|last5=Cutri|first5=Roc M.|last6=Cushing|first6=Michael C.|last7=Cruz|first7=Kelle L.|last8=Sweet|first8=Anne C.|last9=Knapp|first9=Gillian R.|last10=Barman|first10=Travis S.|last11=Bochanski|first11=John J.|date=September 2010|title=Discoveries from a Near-infrared Proper Motion Survey Using Multi-epoch Two Micron All-Sky Survey Data|journal=Astrophysical Journal Supplement Series|language=en|volume=190|issue=1|pages=100–146|doi=10.1088/0067-0049/190/1/100|arxiv=1008.3591 |bibcode=2010ApJS..190..100K|issn=0067-0049|doi-access=free}}
2MASS J1126−5003 has a deep water (H2O) absorption feature in its spectra, which is comparable with late L-dwarfs and early T-dwarfs. It also shows weak carbon monoxide (CO) features. It lacks any methane (CH4) feature and is therefore not a T-dwarf. Based on near-infrared spectra this brown dwarf was therefore classified as an L9 spectral type brown dwarf. The optical spectrum is on the other hand more similar to a mid-type L-dwarf. Here a spectral type of L4.5 fits the optical spectrum. This optical spectral type is a more reliable estimate as the near-infrared spectrum does not fit spectra from other L-dwarfs.
Lower metallicity and higher surface gravity might play a role in the formation of the weather on 2MASS J1126−5003. Lower metallicity reduces the available metal species to form cloud condensates. The higher surface gravity might cause an increased sedimentation of cloud condensates, resulting in thinner clouds. Other factors, like rotation, vertical upwelling and magnetic fields might play a role as well.
Previously one suggested scenario were thinner clouds. This brown dwarf shows variations in the J-band and at mid-infrared wavelengths with a period of 3.2 ± 0.3 hours.{{Cite journal|last1=Metchev|first1=Stanimir A.|last2=Heinze|first2=Aren|last3=Apai|first3=Dániel|last4=Flateau|first4=Davin|last5=Radigan|first5=Jacqueline|last6=Burgasser|first6=Adam|last7=Marley|first7=Mark S.|last8=Artigau|first8=Étienne|last9=Plavchan|first9=Peter|last10=Goldman|first10=Bertrand|date=February 2015|title=Weather on Other Worlds. II. Survey Results: Spots are Ubiquitous on L and T Dwarfs|journal=Astrophysical Journal|language=en|volume=799|issue=2|pages=154|doi=10.1088/0004-637X/799/2/154|arxiv=1411.3051 |bibcode=2015ApJ...799..154M|issn=0004-637X|doi-access=free}} This is a clear indication of patchy clouds.
References
{{Reflist}}
{{DEFAULTSORT:2MASS J11263991-5003550}}
{{Centaurus}}