Astronomy:WD 0810–353

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Short description: White dwarf star in the constellation Puppis

Coordinates: Sky map 08h 12m 27.07s, −35° 29′ 43.3″

WD 0810-353[1][2][3]
Puppis constellation map.svg
Red circle.svg
Location of WD 0810-353 (circled)
Observation data
Equinox J2000.0]] (ICRS)
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[4] mas
Distance36.439 ± 0.006 ly
(11.172 ± 0.002 pc)
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][lower-alpha 1] Gyr
Other designations
UPM J0812-3529, GJ 11192, WD 0810-353, 2MASS J08122707-3529433[1][8]
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 a distance of around 0.15 parsecs, 0.49 light-years or 31,000 astronomical unit|AU from the Sun, crossing well within the proposed boundaries of the Oort cloud.[3] Such close proximity will almost certainly make its flyby the closest in the future, until the flyby of Gliese 710 occurs around 1.14 million years after the dwarf's flyby.

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.[9]

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[10]. 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.[11] Alternate analyses suggest a radial velocity as high as −4,248 km/s.[12]

Flyby

Graph of the distances of various stars from the Sun during the past 20,000 to future 80,000 years.
Distances of the nearest stars from 20,000 years ago until 80,000 years in the future. WD 0810 353 is not shown here, if it were shown here it would be a very curved hyperbola. Because it's much faster than Barnard's star.

Considering the values from Gaia DR3, WD 1810-353 will traverse the Oort cloud, disturbing the population of comets there, Given its mass such an encounter like Gliese 710, would not cause a non-negligible orbital change to the Pluto system and Neptune resonant object.[3] Both the minimum approach distance and the timing of this flyby depend strongly on the value of the radial velocity.[11] 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.[12] 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.

Very strong and complex magnetic field

New observational data confirmed the very strong magnetic field of this white dwarf and provided a new value of the radial velocity,+83±140 km/s[13]. With this value, the future flyby to the Solar System is unremarkable.[12][13]

Notes

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

References

  1. ↑ 1.0 1.1 1.2 "UPM J0812-3529". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=UPM+J0812-3529. 
  2. ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 Bagnulo, Stefano; Landstreet, John D. (2020). "Discovery of six new strongly magnetic white dwarfs in the 20 pc local population". Astronomy & Astrophysics 643: A134. doi:10.1051/0004-6361/202038565. ISSN 0004-6361. Bibcode: 2020A&A...643A.134B. 
  3. ↑ 3.0 3.1 3.2 Bobylev, Vadim; Bajkova, Anisa (2022). "Search for Close Stellar Encounters with the Solar System Based on Data from the Gaia DR3 Catalogue". Astronomy Letters 48 (9): 542–549. doi:10.1134/S1063773722080011. Bibcode: 2022AstL...48..542B. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 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. ↑ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "UCAC4 Catalogue". VizieR On-line Data Catalog: I/322A/Out. Bibcode: 2012yCat.1322....0Z. https://vizier.cds.unistra.fr/viz-bin/VizieR-5?-ref=VIZ62c42b8b2b7fc1&-out.add=.&-source=I/322A/out&UCAC4===273-028648&-out.orig=o. 
  6. ↑ Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3". Astronomy & Astrophysics 657: A7. doi:10.1051/0004-6361/202142146. Bibcode: 2022A&A...657A...7K. 
  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. doi:10.1093/mnras/sty2120. Bibcode: 2018MNRAS.480.4505J. 
  8. ↑ Golovin, Alex; Reffert, Sabine; Just, Andreas; Jordan, Stefan; Vani, Akash; Jahreiß, Hartmut (November 2022). "The Fifth Catalogue of Nearby Stars (CNS5)". Astronomy & Astrophysics 670: A19. doi:10.1051/0004-6361/202244250. Bibcode: 2023A&A...670A..19G.  Catalogue can be accessed here.
  9. ↑ Finch, Charlie T.; Zacharias, Norbert; Jao, Wei-Chun (2018-03-29). "URAT South Parallax Results". The Astronomical Journal (American Astronomical Society) 155 (4): 176. doi:10.3847/1538-3881/aab2b1. ISSN 1538-3881. Bibcode: 2018AJ....155..176F. 
  10. ↑ 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 (Oxford University Press (OUP)) 462 (3): 2295–2318. doi:10.1093/mnras/stw1357. ISSN 0035-8711. Bibcode: 2016MNRAS.462.2295H. 
  11. ↑ 11.0 11.1 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 (American Astronomical Society) 935 (1): L9. doi:10.3847/2041-8213/ac816a. ISSN 1538-4357. Bibcode: 2022ApJ...935L...9B. 
  12. ↑ 12.0 12.1 12.2 de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (2022). "Deep and fast Solar System flybys: The controversial case of WD 0810-353". Astronomy & Astrophysics (EDP Sciences) 668: A14. doi:10.1051/0004-6361/202245020. ISSN 0004-6361. Bibcode: 2022A&A...668A..14D. 
  13. ↑ 13.0 13.1 Landstreet, John D.; Villaver, E.; Bagnulo, Stefano (2023). "Not so fast, not so furious: just magnetic". arXiv:2306.11663 [astro-ph.SR].



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