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WD J1953−1019

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WD J1953−1019

Pan-STARRS color composite image of the WD J1953−1019 system, with the three components annotated.[a]
Observation data
Epoch 2015.5      Equinox 2015.5
Constellation Aquila[3]
Right ascension A: 19h 53m 33.12s[4]
B: 19h 53m 36.00s[5]
C: 19h 53m 36.04s[6]
Declination A: −10° 19′ 54.8″[4]
B: −10° 19′ 31.5″[5]
C: −10° 19′ 29.2″[6]
Characteristics
Evolutionary stage White dwarf
Spectral type DA
Apparent magnitude (V) 17.27 (A)
16.05 (B)
16.29 (C)
Apparent magnitude (G) 17.28 (A)
16.35 (B)
16.44 (C)
Apparent magnitude (B) 17.27 (A)
16.05 (B)
16.29 (C)
Apparent magnitude (R) 17.30 (A)
16.30 (B)
16.44 (C)
Apparent magnitude (g) 17.18 (A)
16.15 (B)
16.24 (C)
Astrometry
A
Proper motion (μ) RA: −10.958 mas/yr[4]
Dec.: −16.137 mas/yr[4]
Parallax (π)7.7645±0.0965 mas[4]
Distance420 ± 5 ly
(129 ± 2 pc)
B
Proper motion (μ) RA: −11.482 mas/yr[5]
Dec.: −16.518 mas/yr[5]
Parallax (π)7.7517±0.0613 mas[5]
Distance421 ± 3 ly
(129 ± 1 pc)
C
Proper motion (μ) RA: −10.922 mas/yr[6]
Dec.: −15.783 mas/yr[6]
Parallax (π)7.6628±0.0612 mas[6]
Distance426 ± 3 ly
(131 ± 1 pc)
Details[1]
MassA: 0.63±0.03
B: 0.62±0.03
C: 0.60±0.03 M☉
TemperatureA: 13715±310
B: 22223±360
C: 22104±350 K
Other designations
A: Gaia DR2 4190500054845023488
B: Gaia DR2 4190499986125543168
C: Gaia DR2 4190499986125543296
Database references
SIMBADA
B
C

WD J1953−1019 is a hierarchical triple system of white dwarfs located at about 130 parsecs (about 420 light years) from the Earth. This is the first triple system of white dwarfs to be resolved.[7][1] The three white dwarfs have an atmosphere of pure hydrogen and a mass of about 0.6 times that of the Sun.

The system consists of a central pair, WD J1953−1019 BC, and a distant companion, WD J1953−1019 A. WD J1953−1019 B and C correspond to the sources Gaia DR2 4190499986125543168[8] and 4190499986125543296[9] respectively. The white dwarfs of the central pair, WD J1953−1019 B and C, are separated 303.25±0.01 AU from each other while the distant companion, WD J1953−1019 A, orbits the barycenter, or center of mass, of the central binary at a distance of 6398.97±0.09 AU.[1]

The cooling age found by M. Perpinyà-Vallès and collaborators for the three white dwarfs is consistent, with an estimated value between 40 and 290 million years.[1] The three stars would each come from a star that had a mass between 1.6 and 2.6 times that of the Sun. A collision of the central pair due to Lidov-Kozai oscillations is unlikely as the system is dynamically stable.[1] However, if this collision occurred, it could produce a type Ia supernova below the Chandrasekhar mass.[1]

See also

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Notes

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  1. ^ The color composite consists of Pan-STARRS images taken in g, i, and y passband filters.[1] These filters correspond to specific wavelengths of 481 nm, 752 nm, and 962 nm, respectively.[2]

References

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  1. ^ a b c d e f g Perpinyà-Vallès, M.; Rebassa-Mansergas, A.; Gänsicke, B. T.; Toonen, S.; Hermes, J. J.; Gentile Fusillo, N. P.; Tremblay, P.-E. (February 2019). "Discovery of the first resolved triple white dwarf". Monthly Notices of the Royal Astronomical Society. 483 (1): 901–907. arXiv:1811.07752. Bibcode:2019MNRAS.483..901P. doi:10.1093/mnras/sty3149.
  2. ^ Tonry, J. L.; Stubbs, C. W.; Lykke, K. R.; Doherty, P.; Shiivers, I. S.; Gentile Fusillo, N. P.; et al. (May 2012). "The Pan-STARRS1 Photometric System". The Astrophysical Journal. 750 (2): 14. arXiv:1203.0297. Bibcode:2012ApJ...750...99T. doi:10.1088/0004-637X/750/2/99. S2CID 119266289. 99.
  3. ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
  4. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  5. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  6. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  7. ^ "A student at the UPC's Barcelona School of Telecommunications has discovered the first resolved triple white dwarf system ever reported". BarcelonaTech. Universitat Politècnica de Catalunya. 13 February 2019. Retrieved 7 May 2019.
  8. ^ "Gaia DR2 4190499986125543168 -- White Dwarf". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 7 May 2019.
  9. ^ "Gaia DR2 4190499986125543296 -- White Dwarf". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 7 May 2019.
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