LP 658-2

Last updated
LP 658-2
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Orion [1]
Right ascension 05h 55m 09.53049s [2]
Declination −04° 10′ 07.0653″ [2]
Apparent magnitude  (V)14.488 [3]
Characteristics
Spectral type DZ11.8 [3]
Apparent magnitude  (B)15.49 [4]
Apparent magnitude  (V)14.488 [3]
Apparent magnitude  (RKC)13.99 [5]
Apparent magnitude  (IKC)13.51 [5]
Apparent magnitude  (J)13.05 ± 0.03 [5]
Apparent magnitude  (H)12.86 ± 0.03 [5]
Apparent magnitude  (KS)12.78 ± 0.03 [5]
B−V color index 1.0 [4] [3]
Astrometry
Proper motion (μ)RA: 535.249 mas/yr [2]
Dec.: −2,317.011 mas/yr [2]
Parallax (π)155.2373±0.0175  mas [2]
Distance 21.010 ± 0.002  ly
(6.4418 ± 0.0007  pc)
Absolute magnitude  (MV)15.44 ± 0.03 [5]
Details [3]
From Holberg etal. (2008)
Mass 0.45±0.01  M☉
Radius 0.014 [3] [note 1]   R☉
Surface gravity (log g)7.80±0.02 [3]   cgs
Temperature 4,270±70, [3]   K
Age 6.42 [6] [note 2]   Gyr
Details [5]
From Subasavage etal. (2009)
Mass 0.80±0.01  M☉
Radius 0.010  R☉
Surface gravity (log g)8.35±0.01  cgs
Temperature 5,180±70  K
Age 6.82±0.02 [note 2]   Gyr
Other designations
HL 4, GJ 223.2, GJ 9193, EG GR 45, G 99-44, G 106-12, LHS 32, LP 658-2, NLTT 15811, WD 0552-041 [4]
Database references
SIMBAD data

LP 658-2 is a degenerate (white dwarf) star in the constellation of Orion, [4] the single known object in its system. It has an apparent visual magnitude of approximately 14.488. [3]

Contents

Distance

According to a 2009 paper, it is the eighth closest known white dwarf to the Sun (after Sirius B, Procyon B, van Maanen's star, Gliese 440, 40 Eridani B, Stein 2051 B and GJ 1221). [7] Its trigonometric parallax from the CTIOPI (Cerro Tololo Inter-American Observatory (CTIO) Parallax Investigation) 0.9 m telescope program, published in 2009, is 0.15613 ± 0.00084 arcsec, [5] corresponding to a distance 6.40 ± 0.03 pc, or 20.89 ± 0.11 ly. Also, previous less precise parallax measurements of LP 658-2 present in YPC (Yale Parallax Catalog) and among results of CTIOPI 1.5 m telescope program:

LP 658-2 parallax measurements

SourcePaperParallax, masDistance, pcDistance, lyRef.
YPCvan Altena et al., 1995155.0 ± 2.16.45 ± 0.0921.04 ± 0.29 [8]
CTIOPI 1.5 mTSN-14 (Costa et al., 2005)156.93 ± 2.676.37 ± 0.1120.78 ± 0.35 [9]
CTIOPI 0.9 mTSN-21 (Subasavage et al., 2009)156.13 ± 0.846.40 ± 0.0320.89 ± 0.11 [5]

Physical parameters

There are two sets of published physical parameters of LP 658-2, significantly differing from each other: one from Holberg et al. 2008 and Sion et al. 2009, the other from Subasavage et al. 2009.

Color

Despite it being classified as a "white" dwarf, it appears yellowish white rather than white, due to temperature, cooler than the Sun's and comparable with that of a K-type main sequence star.

Notes

  1. ↑ From surface gravity and mass.
  2. 1 2 White dwarf cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star)

References

  1. ↑ 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.
  2. 1 2 3 4 5 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. 1 2 3 4 5 6 7 8 9 Holberg, J. B.; Sion, E. M.; Oswalt, T.; McCook, G. P.; Foran, S.; Subasavage, John P. (1 April 2008). "A new look at the local white dwarf population". The Astronomical Journal. 135 (4): 1225–1238. Bibcode:2008AJ....135.1225H. doi: 10.1088/0004-6256/135/4/1225 .
  4. 1 2 3 4 "GJ 223.2". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2011-01-17.
  5. 1 2 3 4 5 6 7 8 9 Subasavage, John P.; Jao, Wei-Chun; Henry, Todd J.; Bergeron, P.; Dufour, P.; Ianna, Philip A.; Costa, Edgardo; Méndez, René A. (1 June 2009). "The solar neighborhood. XXI. Parallax results from the CTIOPI 0.9 m program: 20 new members of the 25 parsec white dwarf sample". The Astronomical Journal. 137 (6): 4547–4560. arXiv: 0902.0627 . Bibcode:2009AJ....137.4547S. doi:10.1088/0004-6256/137/6/4547. S2CID   14696597.
  6. ↑ Sion, Edward M.; Holberg, J. B.; Oswalt, Terry D.; McCook, George P.; Wasatonic, Richard (1 December 2009). "The white dwarfs within 20 parsecs of the Sun: kinematics and statistics". The Astronomical Journal. 138 (6): 1681–1689. arXiv: 0910.1288 . Bibcode:2009AJ....138.1681S. doi:10.1088/0004-6256/138/6/1681. S2CID   119284418.
  7. ↑ Table 1 in Sion et al. 2009
  8. ↑ van Altena, W. F.; Lee, J. T.; Hoffleit, E. D. (1995). The General Catalogue of Trigonometric [Stellar] Parallaxes (4th ed.). New Haven, CT: Yale University Observatory. Bibcode:1995gcts.book.....V. VizieR entry.
  9. ↑ Costa, Edgardo; Méndez, René A.; Jao, W.-C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer (July 2005). "The solar neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation—First results from the 1.5 m telescope program". The Astronomical Journal. 130 (1): 337–349. Bibcode:2005AJ....130..337C. doi: 10.1086/430473 . hdl: 10533/176842 .
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