Astronomy:WD 1856+534

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Short description: White dwarf located in the constellation Draco
WD 1856+534
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Artist's impression of WD 1856+534 and its planet.
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Draco
WD 1856+534
Right ascension  18h 57m 39.344s[1]
Declination +53° 30′ 33.30″[1]
Apparent magnitude (V) 17.244±0.046[2]
G 229-20 A
Right ascension  18h 57m 37.960s[3]
Declination +53° 31′ 15.25″[3]
Apparent magnitude (V) 13.15[2]
G 229-20 B
Right ascension  18h 57m 37.911s[4]
Declination +53° 31′ 12.92″[4]
Apparent magnitude (V) 13.23[2]
Characteristics
WD 1856+534
Evolutionary stage white dwarf
Spectral type DA[5]
Apparent magnitude (J) 15.677±0.055[6]
Apparent magnitude (H) 15.429±0.094[6]
Apparent magnitude (K) 15.548±0.186[6]
G 229-20
Evolutionary stage red dwarf + red dwarf[7]
Spectral type M3.5V[7]
Astrometry
WD 1856+534
Proper motion (μ) RA: +240.749[1] mas/yr
Dec.: −52.470[1] mas/yr
Parallax (π)40.3931 ± 0.0506[1] mas
Distance80.7 ± 0.1 ly
(24.76 ± 0.03 pc)
Absolute magnitude (MV)+14.37[8]
G 229-20 A
Radial velocity (Rv)17.19±0.33[3] km/s
Proper motion (μ) RA: +256.055[3] mas/yr
Dec.: −52.810[3] mas/yr
Parallax (π)40.3480 ± 0.0149[3] mas
Distance80.84 ± 0.03 ly
(24.784 ± 0.009 pc)
G 229-20 B
Radial velocity (Rv)17.38±0.35[4] km/s
Proper motion (μ) RA: +241.527 mas/yr
Dec.: −44.335 mas/yr
Parallax (π)40.3648 ± 0.0147[4] mas
Distance80.80 ± 0.03 ly
(24.774 ± 0.009 pc)
Position (relative to G 229-20)[7]
Angular distance~43″
Observed separation
(projected)		1030+130
−55 AU [7]
Details[9]
WD 1856+534
Mass0.605±0.013 M☉
Radius0.0121±0.0002 R☉
Luminosity0.000077 L☉
Surface gravity (log g)8.05±0.02 cgs
Temperature4,920±50 K
Metallicity [Fe/H]<−8.8[7] dex
AgeCooling age: 5.4±0.7 Gyr
Total age: 7.4 to 10 Gyr
G 229-20 A
Mass0.335±0.024[7] M☉
Radius0.35±0.02[7] R☉
Luminosity0.016[10] L☉
Temperature3,521[7] K
G 229-20 B
Mass0.322±0.023[7] M☉
Radius0.34±0.02[7] R☉
Luminosity0.015[10] L☉
Temperature3,513[7] K
Other designations
WDS J18576+5331
WD 1856+534: LP 141-14, LSPM J1857+5330, NLTT 47263, 2MASS J18573936+5330332[6]
G 229-20: LP 141-13, LSPM J1857+5331, NLTT 47260/47261, 2MASS J18573793+5331140
Database references
SIMBADWD 1856+534
G 229-20
G 229-20 A
G 229-20 B
Exoplanet Archivedata

WD 1856+534 is a white dwarf located in the constellation of Draco. At a distance of about 25 parsecs (80 ly) from Earth, it is the outer component of a visual triple star system consisting of an inner pair of red dwarf stars, named G 229-20. The white dwarf displays a featureless absorption spectrum, lacking strong optical absorption or emission features in its atmosphere. It has an effective temperature of 4,700 K (4,430 °C; 8,000 °F), corresponding to an age of approximately 5.8 billion years.[7] WD 1856+534 is approximately half as massive as the Sun, while its radius is much smaller, being 40% larger than Earth.[11]

Planetary system

The white dwarf is known to host one exoplanet, WD 1856+534 b, in orbit around it. The exoplanet was detected through the transit method by the Transiting Exoplanet Survey Satellite (TESS) between July and August 2019. An analysis of the transit data in 2020 revealed that it is a Jupiter-like giant planet with a radius over ten times that of Earth's, and orbits its host star closely at a distance of 0.02 astronomical units (AU), with an orbital period 60 times shorter than that of Mercury around the Sun.

The unexpectedly close distance of the exoplanet to the white dwarf implies that it must have migrated inward after its host star evolved from a red giant to a white dwarf, otherwise it would have been engulfed by its star.[7] This migration may be related to the fact that WD 1856+534 belongs to a hierarchical triple-star system: the white dwarf and its planet are gravitationally bound to a distant companion, G 229–20, which itself is a binary system of two red dwarf stars.[7] Gravitational interactions with the companion stars may have triggered the planet's migration through the Lidov–Kozai mechanism[12][13][14] in a manner similar to some hot Jupiters. An alternative hypothesis is that the planet instead has survived a common envelope phase.[15] In the latter scenario, other planets engulfed before may have contributed to the expulsion of the stellar envelope.[16] JWST observations seem to disfavour the formation via common envelope and instead favour high eccentricity migration.[17]

The planetary transmission spectrum obtained with GTC OSIRIS is gray and featureless, likely because of the high level of hazes.[18] The transmission spectrum was also obtained with Gemini GMOS. It does not show any features beside a possible dip at 0.55 μm. This feature could be caused be auroral emission at the nightside of the planet. The research find a minimum mass of 0.84 MJ by accounting for the transit geometry of a grazing transit. The researchers also revised the white dwarf parameters and found a total age of 8-10 billion years, in agreement with the system belonging to the thin disk.[5]

Observations with the James Webb Space Telescope published in 2025 show an infrared excess from the star due to thermal emission by the planet, independently confirming its planetary nature. The observations constrain the planet's mass to be less than six times that of Jupiter, and indicate a temperature of 186+6
−7 K, making this the coldest exoplanet directly detected so far, beating out the previous record-holder, Epsilon Indi Ab.[9]

A search with transit timing variations found no additional planets. The search excluded planets with a mass more than 2 MJ with orbital periods as long as 500 days and planets with >10 MJ with orbital periods as long as 1000 days.[19]

The WD 1856+534 planetary system[7][9]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >0.84,[5] ≤5.2+0.7
−0.8 MJ 		0.02085±0.0014 1.407939217(16) ~0 88.778±0.059° 0.946±0.017 RJ

See also

  • WD 1145+017, a white dwarf with a transiting disrupted planetary-mass object
  • WD J0914+1914, a white dwarf with a disk of debris originating from a possible giant planet
  • ZTF J0139+5245, another white dwarf with a disk of debris from a disrupted planetary-mass object
  • CWISEP J1935-1546, a free-floating object with aurora emission in the infrared
  • List of exoplanets and planetary debris around white dwarfs
  • PSR J0337+1715, a trinary compact star system with one pulsar and two white dwarfs. There is also a lunar-mass candidate orbiting all three of them at once

Notes

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 "WD 1856+534 Overview". NASA Exoplanet Archive. https://exoplanetarchive.ipac.caltech.edu/overview/WD%201856%2B534. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ 4.0 4.1 4.2 4.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  5. ↑ 5.0 5.1 5.2 Xu, Siyi; Diamond-Lowe, Hannah; MacDonald, Ryan J.; Vanderburg, Andrew; Blouin, Simon; Dufour, P.; Gao, Peter; Kreidberg, Laura et al. (2021-12-01). "Gemini/GMOS Transmission Spectroscopy of the Grazing Planet Candidate WD 1856+534 b". The Astronomical Journal 162 (6): 296. doi:10.3847/1538-3881/ac2d26. ISSN 0004-6256. Bibcode: 2021AJ....162..296X. 
  6. ↑ 6.0 6.1 6.2 6.3 "LP 141-14 -- White Dwarf". SIMBAD. Université de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=WD+1856%2B534. 
  7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 7.12 7.13 7.14 Vanderburg, AndrewExpression error: Unrecognized word "etal". (September 2020). "A giant planet candidate transiting a white dwarf". Nature 585 (7825): 363–367. doi:10.1038/s41586-020-2713-y. PMID 32939071. Bibcode: 2020Natur.585..363V. 
  8. ↑ Limoges, M. -M.; Bergeron, P.; Lépine, S. (2015). "Physical Properties of the Current Census of Northern White Dwarfs within 40 pc of the Sun". The Astrophysical Journal Supplement Series 219 (2): 19. doi:10.1088/0067-0049/219/2/19. Bibcode: 2015ApJS..219...19L. 
  9. ↑ 9.0 9.1 9.2 Limbach, Mary Anne et al. (April 2025). "Thermal Emission and Confirmation of the Frigid White Dwarf Exoplanet WD 1856+534b". The Astrophysical Journal Letters. 
  10. ↑ 10.0 10.1 Hardegree-Ullman, Kevin K.; Apai, Dániel; Bergsten, Galen J.; Pascucci, Ilaria; López-Morales, Mercedes (2023). "Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets". The Astronomical Journal 165 (6): 267. doi:10.3847/1538-3881/acd1ec. Bibcode: 2023AJ....165..267H. 
  11. ↑ Potter, Steve (16 September 2020). "NASA Missions Spy First Possible 'Survivor' Planet Hugging White Dwarf Star". NASA. 20-086. https://www.nasa.gov/press-release/nasa-missions-spy-first-possible-survivor-planet-hugging-white-dwarf-star. 
  12. ↑ Muñoz, Diego J.; Petrovich, Cristobal (2020-11-19). "Kozai Migration Naturally Explains the White Dwarf Planet WD1856b". The Astrophysical Journal 904 (1): L3. doi:10.3847/2041-8213/abc564. ISSN 2041-8213. Bibcode: 2020ApJ...904L...3M. 
  13. ↑ O'Connor, Christopher E.; Liu, Bin; Lai, Dong (2020-11-30). "Enhanced Lidov-Kozai migration and the formation of the transiting giant planet WD1856+534b". Monthly Notices of the Royal Astronomical Society 501: 507–514. doi:10.1093/mnras/staa3723. ISSN 0035-8711. 
  14. ↑ Stephan, Alexander P.; Naoz, Smadar; Gaudi, B. Scott (2021). "Giant Planets, Tiny Stars: Producing Short-period Planets around White Dwarfs with the Eccentric Kozai–Lidov Mechanism". The Astrophysical Journal 922 (1): 4. doi:10.3847/1538-4357/ac22a9. Bibcode: 2021ApJ...922....4S. 
  15. ↑ Lagos, F.; Schreiber, M. R.; Zorotovic, M.; Gänsicke, B. T.; Ronco, M. P.; Hamers, Adrian S. (2021), "WD 1856 b: a close giant planet around a white dwarf that could have survived a common-envelope phase", Monthly Notices of the Royal Astronomical Society 501 (1): 676–682, doi:10.1093/mnras/staa3703, Bibcode: 2021MNRAS.501..676L 
  16. ↑ Chamandy, Luke; Blackman, Eric G.; Nordhaus, Jason; Wilson, Emily (2021), "Successive common envelope events from multiple planets", Monthly Notices of the Royal Astronomical Society: Letters 502: L110–L114, doi:10.1093/mnrasl/slab017 
  17. ↑ O'Connor, Christopher; Lai, Dong; MacDonald, Ryan; The JWST WD1856b Team (2024-08-01). "The thermal evolution of WD1856b reveals its migration history". AAS Division on Dynamical Astronomy Meeting #55, Id. 401.01 56 (6): 401.01. Bibcode: 2024DDA....5540101O. https://ui.adsabs.harvard.edu/abs/2024DDA....5540101O/abstract. 
  18. ↑ Alonso, R.; Rodríguez-Gil, P.; Izquierdo, P.; Deeg, H. J.; Lodieu, N.; Cabrera-Lavers, A.; Hollands, M. A.; Pérez-Toledo, F. M. et al. (2021), "A transmission spectrum of the planet candidate WD 1856+534 b and a lower limit to its mass", Astronomy & Astrophysics 649: A131, doi:10.1051/0004-6361/202140359, Bibcode: 2021A&A...649A.131A 
  19. ↑ Kubiak, Sarah; Vanderburg, Andrew; Becker, Juliette; Gary, Bruce; Rappaport, Saul A.; Xu, Siyi; de Beurs, Zoe (2023-05-01). "TTV constraints on additional planets in the WD 1856+534 system". Monthly Notices of the Royal Astronomical Society 521 (3): 4679–4694. doi:10.1093/mnras/stad766. ISSN 0035-8711. Bibcode: 2023MNRAS.521.4679K. 




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