View source for Astronomy:SIMP J013656.5+093347

{{short description|Possible exoplanet in the constellation Pisces}}
{{Starbox begin
| name= SIMP J013656.5+093347}}
{{Starbox image
| image=[[File:NewBrownDawf5(1).jpg|300px]]
| caption=Artist's impression of SIMP&nbsp;J013656.5+093347 and its auroras.
| credit=Chuck Carter, Caltech, NRAO/AUI/[[Organization:National Science Foundation|NSF]]
}}
{{Starbox observe
| epoch=J2000
| ra={{RA|01|36|57}}
| dec={{DEC|+09|33|47.3}}
| constell=[[Astronomy:Pisces (constellation)|Pisces]]}}
{{Starbox character
| class=T2.5<ref name="artigau2006" />
| appmag_1=13.455 ± 0.030
| appmag_1_passband=J
| appmag_2=12.771 ± 0.032
| appmag_2_passband=H
| appmag_3=12.562 ± 0.024
| appmag_3_passband=K
}}
{{Starbox astrometry
| radial_v=
| prop_mo_ra= 1238.982 ± 1.189<ref name="Gaia">{{Cite journal|last=Gaia Collaboration|date=2018-08-01|title=Gaia Data Release 2 - Summary of the contents and survey properties|journal=Astronomy & Astrophysics|language=en|volume=616|pages=A1|arxiv=1804.09365|doi=10.1051/0004-6361/201833051|bibcode=2018A&A...616A...1G|s2cid=49211658|issn=0004-6361}}</ref>
| prop_mo_dec= -17.353 ± 0.841<ref name="Gaia"/>
| parallax= 163.4478
| p_error= 0.4629
| parallax_footnote=<ref name="GaiaEDR3">{{Cite Gaia EDR3|2572901021957789568}}</ref>
| absmag_v=
}}
{{Starbox detail
| mass_mj= 12.7 ± 1.0<ref name="Gagné et al"/>
| radius_rj= 1.22 ± 0.01<ref name="Gagné et al"/>
| luminosity=
| temperature= 1098 ± 6<ref name="Gagné et al"/>
| metal=
| rotation= 2.406 ± 0.008<ref name="Croll et al"/> hours
| rotational_velocity=
| gravity= 4.31 ± 0.03<ref name="Gagné et al"/>
| age_myr= 200 ± 50<ref name="Gagné et al"/>
}}
{{Starbox catalog
| names=2MASS J01365662+0933473;<br>IPMS J013656.57+093347.3;<br> IBIS J013656.57+093347.3}}
{{Starbox reference
| Simbad=2MASS+J01365662%2B0933473
}}
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Pisces_constellation_map.svg
|alt=SIMP0136 is located in the constellation Pisces
|caption=Location of SIMP0136 in the constellation [[Astronomy:Pisces (constellation)|Pisces]]|border=infobox|mark=Red_pog.png|width=300
|label=SIMP0136
|position=bottom
|lat=42.8
|long=19.5
}}|caption=
}}
{{Starbox end}}'''SIMP J013656.5+093347''' (abbreviated '''SIMP0136''') is a [[Astronomy:Brown dwarf|brown dwarf]] or [[Astronomy:Sub-brown dwarf|planetary mass object]]<ref name="Gagné et al"/> at 19.9 light-years from Earth in the constellation [[Astronomy:Pisces (constellation)|Pisces]]. It belongs to the spectral class T2.5<ref name="artigau2006" /> and its position shifts due to its [[Astronomy:Proper motion|proper motion]] annually by about 1.24 arcsec in the [[Right ascension|right ascension]].<ref name="Gaia">{{Cite journal|last=Gaia Collaboration|date=2018-08-01|title=Gaia Data Release 2 - Summary of the contents and survey properties|journal=Astronomy & Astrophysics|language=en|volume=616|pages=A1|arxiv=1804.09365|doi=10.1051/0004-6361/201833051|bibcode=2018A&A...616A...1G|s2cid=49211658|issn=0004-6361}}</ref>

This brown dwarf provided the first evidence for periodic variability flux variations among T dwarfs. This has been interpreted as a signature of weather patterns coming in and out of view over the object's 2.4h rotation period. The shape of this lightcurve evolves over timescales of days, which has been interpreted as a sign of evolution of the cloud patterns in its atmosphere.<ref name="Croll et al">{{cite arXiv|last1=Croll|first1=Bryce|last2=Muirhead|first2=Philip S.|last3=Lichtman|first3=Jack|last4=Han|first4=Eunkyu|last5=Dalba|first5=Paul A.|last6=Radigan|first6=Jacqueline|date=September 2016|title=Long-term, Multiwavelength Light Curves of Ultra-Cool Dwarfs: II. The evolving Light Curves of the T2.5 SIMP 0136 & the Uncorrelated Light Curves of the M9 TVLM 513|language=en|eprint=1609.03587|class=astro-ph.SR}}</ref>

In 2017, it was announced that the object's mass may be as low as 12.7 [[Astronomy:Jupiter mass|Jupiter mass]]es and might be considered a [[Astronomy:Rogue planet|rogue planet]] rather than a brown dwarf as it seems to be a member of the relatively young, 200 million-year-old Carina-Near stellar [[Astronomy:Moving group|moving group]].<ref name="Gagné et al">{{Cite journal|last1=Gagné|first1=Jonathan|last2=Faherty|first2=Jacqueline K.|last3=Burgasser|first3=Adam J.|last4=Artigau|first4=Étienne|last5=Bouchard|first5=Sandie|last6=Albert|first6=Loïc|last7=Lafrenière|first7=David|last8=Doyon|first8=René|last9=Bardalez-Gagliuffi|first9=Daniella C.|date=2017-05-15|title=SIMP J013656.5+093347 is Likely a Planetary-Mass Object in the Carina-Near Moving Group|journal=The Astrophysical Journal|volume=841|issue=1|pages=L1|doi=10.3847/2041-8213/aa70e2|issn=2041-8213|arxiv=1705.01625|bibcode=2017ApJ...841L...1G|s2cid=119024210 |doi-access=free }}</ref><ref>{{Cite web|url=http://newatlas.com/brown-dwarf-is-a-planet/49445/|title=Presto change-o! Brown dwarf star is now a planet|website=newatlas.com|language=en|access-date=2018-08-07|date=2017-05-11}}</ref><ref name="SA-20180803">{{cite web |last=Starr |first=Michelle |title=There Is an Absolutely Gigantic Rogue Planet Wandering Our Galactic Neighbourhood |url=https://www.sciencealert.com/giant-rogue-exoplanet-simp-j01365663-0933473-magnetic-field-aurora-brown-dwarf |date=3 August 2018 |work=ScienceAlert.com |access-date=3 August 2018 }}</ref>

In 2018, astronomers noted, "Detecting SIMP J01365663+0933473 with the [[Astronomy:Very Large Array|VLA]] through its [[Astronomy:Aurora|aurora]]l radio emission, also means that we may have a new way of detecting exoplanets, including the elusive rogue ones not orbiting a parent star ... This particular object is exciting because studying its magnetic dynamo mechanisms can give us new insights on how the same type of mechanisms can operate in extrasolar planets - planets beyond our Solar System ... We think these mechanisms can work not only in brown dwarfs, but also in both gas giant and terrestrial planets."<ref name="SA-20180803" /> During the observation with the VLA only one pulse was detected for SIMP0136.The [[Physics:Magnetic flux|magnetic flux]] of SIMP0136 was estimated to be 3.2 [[Physics:Gauss (unit)|kG]].<ref>{{Cite journal|last1=Kao|first1=Melodie M.|last2=Hallinan|first2=Gregg|last3=Pineda|first3=J. Sebastian|last4=Stevenson|first4=David|last5=Burgasser|first5=Adam|date=August 2018|title=The Strongest Magnetic Fields on the Coolest Brown Dwarfs|journal=Astrophysical Journal Supplement Series|language=en|volume=237|issue=2|pages=25|doi=10.3847/1538-4365/aac2d5|arxiv=1808.02485 |issn=0067-0049|bibcode=2018ApJS..237...25K|doi-access=free}}</ref>

==References==
{{reflist|refs=

<ref name="artigau2006">{{cite journal|author=Artigau |display-authors=0 |bibcode=2009ApJ...701.1534A |title=Photometric Variability of the T2.5 Brown Dwarf SIMP&nbsp;J013656.5+093347: Evidence for Evolving Weather Patterns|journal=The Astrophysical Journal |volume=701 |pages=1534–1539 |year=2009|issue=2 |arxiv = 0906.3514 |doi = 10.1088/0004-637X/701/2/1534 |s2cid=3123957 }}</ref>

}}

{{Sky|01|36|57|+|09|33|47|19.95}}
{{Stars of Pisces}}

{{DEFAULTSORT:SIMP J013656.5+093347}}
[[Category:Brown dwarfs]]
[[Category:Rogue planets]]
[[Category:Pisces (constellation)]]

{{Sourceattribution|SIMP J013656.5+093347}}