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LP 658-2 is a degenerate (white dwarf) star in the constellation of Orion,[1] the single known object in its system. It has an apparent visual magnitude of approximately 14.488.[2]

LP 658-2
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Orion
Right ascension 05h 55m 09.53s[1]
Declination −04° 10′ 07.1″[1]
Apparent magnitude (V) 14.488[2]
Characteristics
Spectral type DZ11.8[2]
Apparent magnitude (B) 15.49[1]
Apparent magnitude (V) 14.488[2]
Apparent magnitude (RKC) 13.99[3]
Apparent magnitude (IKC) 13.51[3]
Apparent magnitude (J) 13.05 ± 0.03[3]
Apparent magnitude (H) 12.86 ± 0.03[3]
Apparent magnitude (KS) 12.78 ± 0.03[3]
B−V color index 1.0[1][2]
Astrometry
Proper motion (μ) RA: 535.249±0.017[4] mas/yr
Dec.: −2317.011±0.015[4] mas/yr
Parallax (π)155.2373 ± 0.0175 mas[4]
Distance21.010 ± 0.002 ly
(6.4418 ± 0.0007 pc)
Absolute magnitude (MV)15.44 ± 0.03[3]
Details[2]
From Holberg etal. (2008)
Mass0.45±0.01 M☉
Radius0.014[2][note 1] R☉
Surface gravity (log g)7.80±0.02[2] cgs
Temperature4,270±70,[2] K
Age6.42[5][note 2] Gyr
Details[3]
From Subasavage etal. (2009)
Mass0.80±0.01 M☉
Radius0.010 R☉
Surface gravity (log g)8.35±0.01 cgs
Temperature5,180±70 K
Age6.82±0.02[note 2] Gyr
Other designations
GJ 223.2, GJ 9193, HL 4, LHS 32, LP 658-2, NLTT 15811, G 099-044[6] , G 99-44, G 106-12, WD 0552–041, EGGR 45.[1]
Database references
SIMBADdata

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,[3] 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[6]
CTIOPI 1.5 mTSN-14 (Costa et al., 2005)156.93 ± 2.676.37 ± 0.1120.78 ± 0.35[8]
CTIOPI 0.9 mTSN-21 (Subasavage et al., 2009)156.13 ± 0.846.40 ± 0.0320.89 ± 0.11[3]

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. White dwarf cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star)

References


  1. "GJ 223.2". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2011-01-17.
  2. 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.
  3. 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.
  4. Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  5. 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.
  6. 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.
  7. Table 1 in Sion et al. 2009
  8. 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.

На других языках

- [en] LP 658-2

[es] Gliese 223.2

Gliese 223.2 (GJ 223.2 / LHS 32 / G 99-44 / WD 0552-041)[1] es una enana blanca de magnitud aparente +14,45 situada en la constelación de Orión. De acuerdo a su paralaje —0,155 segundos de arco—, Gliese 223.2 se encuentra a 21,0 años luz de distancia, siendo una de las 100 estrellas más próximas al sistema solar.[2] Las estrellas más cercanas a Gliese 223.2 son Gliese 205 y G 99-49, respectivamente a 3,11 y 4,25 años luz. La brillante Tabit (π3 Orionis) se encuentra a 9,3 años luz de distancia.[3]


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