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WD 0810–353

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Coordinates: Sky map 08h 12m 27.07s, −35° 29′ 43.3″
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WD 0810-353[1][2][3]
Location of WD 0810-353 (circled)
Observation data
Epoch J2000.0[1]      Equinox J2000.0[1]
Constellation Puppis
Right ascension 08h 12m 27.06600s[4]
Declination −35° 29′ 43.3241″[4]
Apparent magnitude (V) 14.469[5]
Characteristics
Evolutionary stage white dwarf
Spectral type DAH[2]
Astrometry
Radial velocity (Rv)−373.74±8.18[4] km/s
Proper motion (μ) RA: −365.479[4] mas/yr
Dec.: −329.204[4] mas/yr
Parallax (π)89.5064 ± 0.0155 mas[4]
Distance36.439 ± 0.006 ly
(11.172 ± 0.002 pc)
Absolute magnitude (MV)14.228[citation needed]
Details
Mass0.63[2] M☉
Radius0.01[6] R☉
Luminosity0.00017[7] L☉
Surface gravity (log g)8.09[2] cgs
Temperature6,093[2] K
Age2.7[2][a] Gyr
Database references
SIMBADdata

WD 0810-353 (UPM J0812-3529) is a white dwarf currently located 36 light-years (11 parsecs) from the Solar System. This stellar remnant may approach the Solar System 29,000 years from now at about 0.15 parsecs or 31,000 AU from the Sun, crossing well inside the Oort cloud.[3]

Observations

WD 0810-353 is a dim object with an apparent magnitude of 14.5[2] in the southern constellation of Puppis. Its motion perpendicular to the line of sight is considerable; it is consistently listed as a high proper motion star.[8]

Physical properties

WD 1810-353 is a white dwarf of spectral type DAH[2] with a very strong magnetic field, perhaps as strong as 30 MG.[2] It has a mass of 0.63 M☉ and an age of 2.7 billion years;[2] its effective temperature is 6,093 K[2] or 6,273 K[9]. Gaia Data Release 3 (Gaia DR3) gives a value of its radial velocity of −373.74±8.18 km/s which could be incorrect because the Gaia software pipeline does not include any template for white dwarfs.[10] Alternate analyses suggest a radial velocity as high as 4,248 km/s.[11]

Flyby

Considering the values from Gaia DR3, WD 1810-353 will traverse the Oort cloud, disturbing the population of comets there.[3] Both the minimum approach distance and the timing of this flyby depend strongly on the value of the radial velocity.[10] The Gaia DR3 mean BP/RP low-resolution spectrum suggests that WD 0810-353 could be a hypervelocity runaway white dwarf ejected during a type Ia supernova explosion.[11] Extensive analyses show that the relative velocity during the flyby could be high enough, or the minimum approach distance large enough, to prevent any significant perturbation on the Oort cloud.

Notes

  1. ^ This is the "cooling age", the length of time since the object became a white dwarf

References

  1. ^ a b c "UPM J0812-3529". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-10-12.
  2. ^ a b c d e f g h i j k Bagnulo, Stefano; Landstreet, John D. (2020). "Discovery of six new strongly magnetic white dwarfs in the 20 pc local population". Astronomy & Astrophysics. 643. EDP Sciences: A134. arXiv:2010.05795. Bibcode:2020A&A...643A.134B. doi:10.1051/0004-6361/202038565. ISSN 0004-6361.
  3. ^ a b c Bobylev, Vadim; Bajkova, Anisa (2022). "Search for close encounters of stars with the Solar System using Gaia DR3 catalog". arXiv:2206.14443.
  4. ^ a b c d e f 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. ^ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. "UCAC4 Catalogue". VizieR On-line Data Catalog: I/322A/out. Bibcode:2012yCat.1322....0Z.
  6. ^ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics. 657: A7. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. S2CID 237605138.
  7. ^ Jiménez-Esteban, F. M.; Torres, S.; Rebassa-Mansergas, A.; Skorobogatov, G.; Solano, E.; Cantero, C.; Rodrigo, C. (2018). "A white dwarf catalogue from Gaia-DR2 and the Virtual Observatory". Monthly Notices of the Royal Astronomical Society. 480 (4): 4505. arXiv:1807.02559. Bibcode:2018MNRAS.480.4505J. doi:10.1093/mnras/sty2120.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  8. ^ Finch, Charlie T.; Zacharias, Norbert; Jao, Wei-Chun (2018-03-29). "URAT South Parallax Results". The Astronomical Journal. 155 (4). American Astronomical Society: 176. Bibcode:2018AJ....155..176F. doi:10.3847/1538-3881/aab2b1. ISSN 1538-3881.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  9. ^ Holberg, J. B.; Oswalt, T. D.; Sion, E. M.; McCook, G. P. (2016-06-30). "The 25 parsec local white dwarf population". Monthly Notices of the Royal Astronomical Society. 462 (3). Oxford University Press (OUP): 2295–2318. Bibcode:2016MNRAS.462.2295H. doi:10.1093/mnras/stw1357. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  10. ^ a b Bailer-Jones, C. A. L. (2022-08-01). "Stars That Approach within One Parsec of the Sun: New and More Accurate Encounters Identified in Gaia Data Release 3". The Astrophysical Journal Letters. 935 (1). American Astronomical Society: L9. arXiv:2207.06258. Bibcode:2022ApJ...935L...9B. doi:10.3847/2041-8213/ac816a}. ISSN 1538-4357.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  11. ^ a b de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (2022). "Deep and fast Solar System flybys: The controversial case of WD 0810-353". arXiv:2210.04863.
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