BPM 37093

A light curve for V886 Centauri, adapted from Kanaan et al. (1992)[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Centaurus
Right ascension 12h 38m 49.78112s[2]
Declination −49° 48′ 00.2195″[2]
Apparent magnitude (V) 14.0[3]
Characteristics
Spectral type DAV4.4[4]
Variable type DAV (ZZ Ceti)[4]
Astrometry
Radial velocity (Rv)−12[4] km/s
Proper motion (μ) RA: -557.111 mas/yr[2]
Dec.: -74.036 mas/yr[2]
Parallax (π)67.4058 ± 0.0186 mas[2]
Distance48.39 ± 0.01 ly
(14.836 ± 0.004 pc)
Details
Mass1.10[5] M
Radius0.0057 R
Luminosity0.001[6] L
Surface gravity (log g)8.81 ± 0.05[7] cgs
Temperature11730 ± 350[7] K
Other designations
V886 Cen, BPM 37093, GJ 2095, LFT 931, LHS 2594, LTT 4816, WD 1236-495[3]
Database references
SIMBADdata
ARICNSdata

BPM 37093 (V886 Centauri) is a variable white dwarf star of the DAV, or ZZ Ceti, type, with a hydrogen atmosphere and an unusually high mass of approximately 1.1 times the Sun's. It is 48 light-years (15 parsecs) from Earth in the constellation Centaurus and vibrates; these pulsations cause its luminosity to vary.[3][5] Like other white dwarfs, BPM 37093 is thought to be composed primarily of carbon and oxygen, which are created by thermonuclear fusion of helium nuclei in the triple-alpha process.[8]

Structure

In the 1960s, it was predicted that as a white dwarf cools, its material should crystallize, starting at the center.[9] When a star pulsates, observing its pulsations gives information about its structure. BPM 37093 was first observed to be a pulsating variable in 1992,[1] and in 1995 it was pointed out that this yielded a potential test of the crystallization theory.[10] In 2004, Antonio Kanaan and a team of researchers of the Whole Earth Telescope estimated, on the basis of these asteroseismological observations, that approximately 90% of the mass of BPM 37093 had crystallized.[5][9][11][12] Other work gives a crystallized mass fraction of between 32% and 82%.[7] Any of these estimates would result in a total crystalline mass in excess of 5×1029 kilograms. As the white dwarf has a radius of 4,000 kilometres (2,500 mi), this means that the core of BPM 37093, nicknamed Lucy, is likely one of the largest diamonds in the local region of the universe.[13][14]

Body-centered cubic lattice

Crystallization of the material of a white dwarf of this type is thought to result in a body-centered cubic lattice of carbon and/or oxygen nuclei, which are surrounded by a Fermi sea of electrons.[15]

Nickname and press coverage

In popular culture

See also

References

  1. ^ a b Kanaan, A.; Kepler, S. O.; Giovannini, O.; Diaz, M. (10 March 1992). "The Discovery of a New DAV Star Using IUE Temperature Determination". The Astrophysical Journal. 390: L89–L91. Bibcode:1992ApJ...390L..89K. doi:10.1086/186379. hdl:10183/108720. Archived from the original on 4 December 2021. Retrieved 4 December 2021.
  2. ^ 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.
  3. ^ a b c "WG 22". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved April 1, 2008.
  4. ^ a b c A Catalog of Spectroscopically Identified White Dwarfs Archived 2018-08-08 at the Wayback Machine, George P. McCook and Edward M. Sion, Astrophysical Journal Supplement 121, #1 (March 1999), pp. 1–130. CDS ID III/210 Archived 2013-10-22 at the Wayback Machine.
  5. ^ a b c Whole Earth Telescope observations of BPM 37093: a seismological test of crystallization theory in white dwarfs, A. Kanaan, A. Nitta, D. E. Winget, S. O. Kepler, M. H. Montgomery, T. S. Metcalfe, et al., Astronomy and Astrophysics 432, #1 (March 2005), pp. 219–224. Bibcode:2005A&A...432..219K doi:10.1051/0004-6361:20041125.
  6. ^ Photometric and Spectroscopic Analysis of Cool White Dwarfs with Trigonometric Parallax Measurements, P. Bergeron, S. K. Leggett, María Teresa Ruiz, Astrophysical Journal Supplement 133, #2 (April 2001), pp. 413–449. Bibcode:2001ApJS..133..413B
  7. ^ a b c P. Brassard, G. Fontaine, Asteroseismology of the Crystallized ZZ Ceti Star BPM 37093: A Different View, Astrophysical Journal 622, #1, pp. 572–576. Bibcode:2005ApJ...622..572B
  8. ^ Late stages of evolution for low-mass stars Archived 2020-06-11 at the Wayback Machine, Michael Richmond, lecture notes, Physics 230, Rochester Institute of Technology, accessed online May 3, 2007.
  9. ^ a b Testing White Dwarf Crystallization Theory with Asteroseismology of the Massive Pulsating DA Star BPM 37093, T. S. Metcalfe, M. H. Montgomery, and A. Kanaan, Astrophysical Journal 605, #2 (April 2004), pp. L133–L136. Bibcode:2004ApJ...605L.133M
  10. ^ The Status of White Dwarf Asteroseismology and a Glimpse of the Road Ahead, D. E. Winget, Baltic Astronomy 4 (1995), pp. 129–136. Bibcode:1995BaltA...4..129W
  11. ^ a b "BBC News: Diamond star thrills astronomers". 16 February 2004. Archived from the original on 2007-02-05. Retrieved 2007-02-26.
  12. ^ Press release Archived 2013-12-25 at the Wayback Machine, 2004, Harvard-Smithsonian Center for Astrophysics.
  13. ^ "This Valentine's Day, Give The Woman Who Has Everything The Galaxy's Largest Diamond". Center for Astrophysics. Archived from the original on July 6, 2008. Retrieved May 5, 2009.
  14. ^ "Lucy's in the Sky with Diamonds: Meet the Most Expensive Star Ever Found". Futurism. 12 June 2014. Archived from the original on 11 December 2019. Retrieved 20 May 2019.
  15. ^ Crystallization of carbon-oxygen mixtures in white dwarfs, J. L. Barrat, J. P. Hansen, and R. Mochkovitch, Astronomy and Astrophysics 199, #1–2 (June 1988), pp. L15–L18. Bibcode:1988A&A...199L..15B
  16. ^ "Cosmic Backyard". Abstruse Goose. Archived from the original on 2020-07-02. Retrieved 2020-06-28.