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#redirect [[List of brown dwarfs]]
{{Short description|WISE 1019+6529 is a pair of brown dwarfs}}
{{Starbox begin
| name = WISE 1019+6529
}}
{{Starbox image
| image = [[File:Aa44965-22-fig3.jpg|250px]]
| caption = The binary WISE 1019+6529 with Keck AO
| credit = <!--credit for image if the image's use requires them (optional)-->
}}
{{Starbox observe
| epoch = J2000
| equinox = J2000
| constell = [[Ursa Major]]
| ra = {{RA|10|19|05.75}}
| dec = {{Dec|+65|29|52.70}}
}}
{{Starbox character
| type = binary brown dwarf
| class = T5.5 ±0.5 & T7.0 ±0.5<ref name="Vedantham2023"/>
}}
{{Starbox astrometry
| parallax = 41.25
| p_error = 1.75
| parallax_footnote = <ref name="Kirkpatrick2019"/>
}}
{{Starbox detail
| source = <ref name="Vedantham2023"/>
| component1 = WISE 1019+6529A
| mass_mj = 41 ±18
| temperature = 1000
| gravity = 5.5
| rotation = {{val|3.13|0.32|0.27}} hours
| luminosity_bolometric = 10<sup>-4.994 ± 0.063</sup>
| component2 = WISE 1019+6529B
| mass_mj2 = 32 ±16
}}
{{Starbox orbit
| reference = <ref name="Vedantham2023"/>
| primary = WISE 1019+6529A
| name = WISE 1019+6529B
| period = >30
| axis_unitless = >5.2 [[astronomical unit|AU]]
| eccentricity = <0.96
| inclination = <86
}}
{{Starbox relpos
| reference = <ref name="Vedantham2023"/>
| epoch = 15 January 2015
| primary = WISE 1019+6529A
| component = WISE 1019+6529B
| angdistmas = 423.0 ± 1.6
| posang = 161.71 ± 0.23
| projsep = 9.9 ± 0.4
}}
{{Starbox catalog
| names =[[2MASS]]&nbsp;J10190575+6529526, CNS5&nbsp;2530, [[Transiting Exoplanet Survey Satellite|TIC]]&nbsp;287254768, WISEA&nbsp;J101905.61+652954.0, WISEP&nbsp;J101905.63+652954.2, WISE&nbsp;J101905.62+652954.2, EQ&nbsp;J1019+6529
}}
{{Starbox reference
| Simbad =WISEP+J101905.63%2B652954.2
}}
{{starbox end}}
'''WISEPA J101905.63+652954.2''' (also called '''WISE 1019+6529''') is a binary made up of two cold [[brown dwarf|brown dwarfs]]. Both brown dwarfs have a late [[T dwarf|spectral type T]]. The pair was detected in [[radio astronomy|radio emission]], which is pulsed and periodic. The radio emission could, in principle, be powered by the interaction of the binary.<ref name="Vedantham2023"/>

WISE 1019+6529 was discovered in 2011 with the [[Wide-field Infrared Survey Explorer]] and spectroscopy from the [[NASA Infrared Telescope Facility]], [[Palomar Observatory|Palomar]] and [[W. M. Keck Observatory|Keck Observatory]] confirmed it as a T6 or T7-dwarf.<ref name="Kirkpatrick2011"/> A preliminary [[parallax]] is published, placing it 24 parsec distant from the [[solar system]], and it has a [[proper motion]] of 150.6 ±1.1 mas/yr.<ref name="Kirkpatrick2019"/> In 2023 a study was published, describing the 144 [[Hertz|MHz]] radio emission detected with the [[Low Frequency Array]]. The same paper describes observations with Keck [[adaptive optics]], which showed that the brown dwarf is a binary. The researchers find a polar dipole [[magnetic field]] strength of 660 ± 300 [[Gauss]] for the T5.5 dwarf and 460 ± 210 Gauss for the T5.5 dwarf. The surface magnetic field strength is constrained between 51.4–10<sup>3</sup> Gauss, which was constrained with cyclotron maser emission and the upper limit of [[Hydrogen alpha|H-alpha]] luminosity. The radio emission could, in principle, be powered by a binary interaction, if the mass loss rate is ≥25 [[tonne|tonnes]] per second. The researchers also find that the radio emission is consistent with a Jupiter-like [[aurora]].<ref name="Vedantham2023"/>

== See also ==
Other T-dwarfs with detected radio emission<ref name="Rose2023"/>

* [[SIMP J013656.5+093347.3]] T2.5, planetary-mass object
* [[2MASS J10475385+2124234]] T6.5
* [[WISEPA J062309.94-045624.6]] T8

== References ==
{{reflist |refs=

<ref name="Vedantham2023">{{Cite journal |last=Vedantham |first=H. K. |last2=Dupuy |first2=T. J. |last3=Evans |first3=E. L. |last4=Sanghi |first4=A. |last5=Callingham |first5=J. R. |last6=Shimwell |first6=T. W. |last7=Best |first7=W. M. J. |last8=Liu |first8=M. C. |last9=Zarka |first9=P. |date=2023-07-01 |title=Polarised radio pulsations from a new T-dwarf binary |url=https://ui.adsabs.harvard.edu/abs/2023A&A...675L...6V/abstract |journal=Astronomy and Astrophysics |volume=675 |pages=L6 |arxiv=2301.01003 |bibcode=2023A&A...675L...6V |doi=10.1051/0004-6361/202244965 |issn=0004-6361}}</ref>

<ref name="Kirkpatrick2011">{{Cite journal |last=Kirkpatrick |first=J. Davy |last2=Cushing |first2=Michael C. |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Marsh |first6=Kenneth A. |last7=Wright |first7=Edward L. |last8=Mainzer |first8=A. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Thompson |first11=Maggie A. |last12=Bauer |first12=James M. |last13=Benford |first13=Dominic J. |last14=Bridge |first14=Carrie R. |last15=Lake |first15=Sean E. |date=2011-12-01 |title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) |url=https://ui.adsabs.harvard.edu/abs/2011ApJS..197...19K/abstract |journal=The Astrophysical Journal Supplement Series |volume=197 |pages=19 |arxiv=1108.4677 |bibcode=2011ApJS..197...19K |doi=10.1088/0067-0049/197/2/19 |issn=0067-0049}}</ref>

<ref name="Kirkpatrick2019">{{Cite journal |last=Kirkpatrick |first=J. Davy |last2=Martin |first2=Emily C. |last3=Smart |first3=Richard L. |last4=Cayago |first4=Alfred J. |last5=Beichman |first5=Charles A. |last6=Marocco |first6=Federico |last7=Gelino |first7=Christopher R. |last8=Faherty |first8=Jacqueline K. |last9=Cushing |first9=Michael C. |last10=Schneider |first10=Adam C. |last11=Mace |first11=Gregory N. |last12=Tinney |first12=Christopher G. |last13=Wright |first13=Edward L. |last14=Lowrance |first14=Patrick J. |last15=Ingalls |first15=James G. |date=2019-02-01 |title=Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the “Planetary” Mass Regime |url=https://ui.adsabs.harvard.edu/abs/2019ApJS..240...19K/abstract |journal=The Astrophysical Journal Supplement Series |volume=240 |pages=19 |arxiv=1812.01208 |bibcode=2019ApJS..240...19K |doi=10.3847/1538-4365/aaf6af |issn=0067-0049}}</ref>

<ref name="Rose2023">{{Cite journal |last1=Rose |first1=Kovi |last2=Pritchard |first2=Joshua |last3=Murphy |first3=Tara |last4=Caleb |first4=Manisha |last5=Dobie |first5=Dougal |last6=Driessen |first6=Laura |last7=Duchesne |first7=Stefan W. |last8=Kaplan |first8=David L. |last9=Lenc |first9=Emil |last10=Wang |first10=Ziteng |date=2023-07-01 |title=Periodic Radio Emission from the T8 Dwarf WISE J062309.94-045624.6 |journal=The Astrophysical Journal |volume=951 |issue=2 |pages=L43 |arxiv=2306.15219 |bibcode=2023ApJ...951L..43R |doi=10.3847/2041-8213/ace188 |doi-access=free |issn=0004-637X}}</ref>
}}
[[Category:T-type brown dwarfs]]
[[Category:Astronomical radio sources]]
[[Category:Ursa Major]]

Revision as of 14:09, 6 October 2024

WISE 1019+6529

The binary WISE 1019+6529 with Keck AO
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
Right ascension 10h 19m 05.75s
Declination +65° 29′ 52.70″
Characteristics
Evolutionary stage binary brown dwarf
Spectral type T5.5 ±0.5 & T7.0 ±0.5[1]
Astrometry
Parallax (π)41.25 ± 1.75 mas[2]
Distance79 ± 3 ly
(24 ± 1 pc)
Details[1]
WISE 1019+6529A
Mass41 ±18 MJup
Luminosity (bolometric)10-4.994 ± 0.063 L☉
Surface gravity (log g)5.5 cgs
Temperature1000 K
Rotation3.13+0.32
−0.27 hours
WISE 1019+6529B
Mass32 ±16 MJup
Orbit[1]
PrimaryWISE 1019+6529A
CompanionWISE 1019+6529B
Period (P)>30 yr
Semi-major axis (a)>5.2 AU
Eccentricity (e)<0.96
Inclination (i)<86°
Position (relative to WISE 1019+6529A)[1]
ComponentWISE 1019+6529B
Epoch of observation15 January 2015
Angular distance423.0 ± 1.6 mas
Position angle161.71 ± 0.23°
Projected separation9.9 ± 0.4 AU
Other designations
2MASS J10190575+6529526, CNS5 2530, TIC 287254768, WISEA J101905.61+652954.0, WISEP J101905.63+652954.2, WISE J101905.62+652954.2, EQ J1019+6529
Database references
SIMBADdata

WISEPA J101905.63+652954.2 (also called WISE 1019+6529) is a binary made up of two cold brown dwarfs. Both brown dwarfs have a late spectral type T. The pair was detected in radio emission, which is pulsed and periodic. The radio emission could, in principle, be powered by the interaction of the binary.[1]

WISE 1019+6529 was discovered in 2011 with the Wide-field Infrared Survey Explorer and spectroscopy from the NASA Infrared Telescope Facility, Palomar and Keck Observatory confirmed it as a T6 or T7-dwarf.[3] A preliminary parallax is published, placing it 24 parsec distant from the solar system, and it has a proper motion of 150.6 ±1.1 mas/yr.[2] In 2023 a study was published, describing the 144 MHz radio emission detected with the Low Frequency Array. The same paper describes observations with Keck adaptive optics, which showed that the brown dwarf is a binary. The researchers find a polar dipole magnetic field strength of 660 ± 300 Gauss for the T5.5 dwarf and 460 ± 210 Gauss for the T5.5 dwarf. The surface magnetic field strength is constrained between 51.4–103 Gauss, which was constrained with cyclotron maser emission and the upper limit of H-alpha luminosity. The radio emission could, in principle, be powered by a binary interaction, if the mass loss rate is ≥25 tonnes per second. The researchers also find that the radio emission is consistent with a Jupiter-like aurora.[1]

See also

Other T-dwarfs with detected radio emission[4]

References

  1. ^ a b c d e f Vedantham, H. K.; Dupuy, T. J.; Evans, E. L.; Sanghi, A.; Callingham, J. R.; Shimwell, T. W.; Best, W. M. J.; Liu, M. C.; Zarka, P. (2023-07-01). "Polarised radio pulsations from a new T-dwarf binary". Astronomy and Astrophysics. 675: L6. arXiv:2301.01003. Bibcode:2023A&A...675L...6V. doi:10.1051/0004-6361/202244965. ISSN 0004-6361.
  2. ^ a b Kirkpatrick, J. Davy; Martin, Emily C.; Smart, Richard L.; Cayago, Alfred J.; Beichman, Charles A.; Marocco, Federico; Gelino, Christopher R.; Faherty, Jacqueline K.; Cushing, Michael C.; Schneider, Adam C.; Mace, Gregory N.; Tinney, Christopher G.; Wright, Edward L.; Lowrance, Patrick J.; Ingalls, James G. (2019-02-01). "Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime". The Astrophysical Journal Supplement Series. 240: 19. arXiv:1812.01208. Bibcode:2019ApJS..240...19K. doi:10.3847/1538-4365/aaf6af. ISSN 0067-0049.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  3. ^ 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: 19. arXiv:1108.4677. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. ISSN 0067-0049.
  4. ^ 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.
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