WISEPA J062309.94-045624.6

Last updated
WISE J0623-0456
WISE J0623-0456 VLT HAWKI.jpg
Very Large Telescope image of WISE J0623-0456
Observation data
Epoch J2000       Equinox J2000
Constellation Monoceros
Right ascension 06h 23m 09.68s
Declination −04° 56′ 23.52″
Characteristics
Evolutionary stage brown dwarf
Spectral type T8 [1]
Variable type rotational variable [2]
Astrometry
Proper motion (μ)RA: -906.3 ±1.8  mas/yr [3]
Dec.: 168.8 ±1.6  mas/yr [3]
Parallax (π)86.5 ± 1.7  mas [3]
Distance 37.7 ± 0.7  ly
(11.6 ± 0.2  pc)
Details
Mass 13.18+31.26
−9.44 [4] MJ
12.28 ±13.06 [5]   MJup
Radius 0.78+0.17
−0.13 [4] RJ
1.11 ±0.14 [5]   RJup
Luminosity (bolometric)10−5.755+0.060
−0.049 [4]   L☉
Surface gravity (log g)4.70+0.47
−0.42 [4]   cgs
Temperature 743+53
−51 [4] K
624 ±40 [5]   K
Metallicity −0.32+0.18
−0.16 [4]
Rotation 1.912 ± 0.005 hours [2]
Rotational velocity (v sin i)60+70
−55 [4] km/s
>63 [2]  km/s
Age 738+2701
−592 [4]   Myr
Other designations
CNS5 1581, WISEA J062309.92-045624.5, WISEP J062309.94-045624.6, EQ J0623-0456
Database references
SIMBAD data

WISEPA J062309.94-045624.6 (also called WISE J0623-0456) is a brown dwarf of spectral type T8. It is the coldest brown dwarf with a radio emission (as of October 2024). [2]

WISE J0623-0456 was discovered in 2011 with the Wide-field Infrared Survey Explorer and a spectrum with the NASA Infrared Telescope Facility confirmed it as a T8-dwarf. [1] WISE J0623-0456 was identified as a radio source with the Australian SKA Pathfinder. Follow-up observations were carried out with the Australia Telescope Compact Array (ATCA) and MeerKAT. The source showed a double-peaked pulsed emission, with a period of 1.889 ± 0.018 hours in ATCA and 1.912 ± 0.005 hours in MeerKAT. The source has a radio luminousity of 1014.8 erg s−1 Hz −1 and is comparable to other radio bright ultracool dwarfs with a similar spectral type. The radio emission of WISE J0623-0456 is strongly circularly polarized and periodic. The researchers therefore think that the radio emission comes from electron cyclotron maser instability (ECMI), which is connected to aurora in ultracool dwarfs. The researchers find that the magnetic field has a strength of at least B > 0.71 kG. [2] Another work finds that the shape of the lightcurve can be reproduced by active field lines (AFLs). This work also found that the brown dwarf is likely seen pole-on. The rotation and magnetic axes are misaligned significantly (similar to Uranus and Neptune) and the magnetic cycle is likely longer than 6 months. M- and L-dwarfs can produce the observed radio luminosities on their own, but cooler T- and Y-dwarfs don't have the necessary corona to produce the radio emission. The alternative is that the plasma is fed to the magnetosphere from a companion, similar to the role of Io for the aurora on Jupiter. [6]

See also

Other T-dwarfs with detected radio emission [2]

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References

  1. 1 2 Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E. (2011-12-01). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement Series. 197 (2): 19. arXiv: 1108.4677 . Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. ISSN   0067-0049.
  2. 1 2 3 4 5 6 Rose, Kovi; Pritchard, Joshua; Murphy, Tara; Caleb, Manisha; Dobie, Dougal; Driessen, Laura; Duchesne, Stefan W.; Kaplan, David L.; Lenc, Emil; Wang, Ziteng (2023-07-01). "Periodic Radio Emission from the T8 Dwarf WISE J062309.94-045624.6". The Astrophysical Journal. 951 (2): L43. arXiv: 2306.15219 . Bibcode:2023ApJ...951L..43R. doi: 10.3847/2041-8213/ace188 . ISSN   0004-637X.
  3. 1 2 3 Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; Marocco, Federico; Cayago, Alfred J.; Smart, R. L.; Eisenhardt, Peter R.; Kuchner, Marc J.; Wright, Edward L.; Cushing, Michael C.; Allers, Katelyn N.; Bardalez Gagliuffi, Daniella C. (2021-03-01). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 7. arXiv: 2011.11616 . Bibcode:2021ApJS..253....7K. doi: 10.3847/1538-4365/abd107 . ISSN   0067-0049.
  4. 1 2 3 4 5 6 7 8 Zhang, Zhoujian; Liu, Michael C.; Marley, Mark S.; Line, Michael R.; Best, William M. J. (2021-11-01). "Uniform Forward-modeling Analysis of Ultracool Dwarfs. II. Atmospheric Properties of 55 Late-T Dwarfs". The Astrophysical Journal. 921 (1): 95. arXiv: 2105.05256 . Bibcode:2021ApJ...921...95Z. doi: 10.3847/1538-4357/ac0af7 . ISSN   0004-637X.
  5. 1 2 3 Sanghi, Aniket (November 8, 2023). "Table of Ultracool Fundamental Properties". zenodo. doi:10.5281/zenodo.10086810 . Retrieved 2024-10-05.
  6. ↑ Kavanagh, Robert D.; Vedantham, Harish K.; Rose, Kovi; Bloot, Sanne (2024-10-23). "Unravelling sub-stellar magnetospheres". arXiv: 2410.18073 [astro-ph].
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