WD 2359−434

Last updated
WD 2359−434
Gliese 915 and Earth.png
Size of WD 2359−434 in comparison with Earth. On the left is Earth, on the right is WD 2359-434.
Observation data
Epoch J2000 [1]        Equinox J2000 [1]
Constellation Phoenix
Right ascension 00h 02m 10.766s [1]
Declination −43° 09′ 56.02″ [1]
Apparent magnitude  (V)12.76 [2]
Characteristics
Spectral type DAP5.8 [3]
Apparent magnitude  (B)13.12 [1]
Apparent magnitude  (V)12.76 [2]
Apparent magnitude  (RKC)12.82 [4]
Apparent magnitude  (IKC)12.66 [4]
Apparent magnitude  (J)12.60 ± 0.03 [4]
Apparent magnitude  (H)12.43 ± 0.02 [4]
Apparent magnitude  (KS)12.45 ± 0.02 [4]
Astrometry
Radial velocity (Rv)-58.8 ± 10.8 [5]  km/s
Proper motion (μ)RA: 589 [4]   mas/yr
Dec.: -664 [4]   mas/yr
Parallax (π)120.0143 ± 0.0215  mas [6]
Distance 27.176 ± 0.005  ly
(8.332 ± 0.001  pc)
Absolute magnitude  (MV)13.20 [2] [4] [note 1]
Details
Mass 0.85 ± 0.01 [4]   M☉
Radius 0.0097 [4] [note 2]   R☉
Surface gravity (log g)8.39 ± 0.01 [4]   cgs
Temperature 8570 ± 50 [2]   K
Age 1.82 ± 0.06 [4] [note 3]   Gyr
Other designations
Gliese 915, [2] [3] LHS  1005, [2] LFT  1849, [1] LTT  9857, [1] LP  988-88, [1] L  362-81, [7] EGGR 165, [1] LAWD 96, [1] 2MASS  J00021076-4309560 [1]
Database references
SIMBAD data
Phoenix constellation map.svg
Red pog.png
WD 2359−434
Location of WD 2359−434 in the constellation Phoenix

WD 2359-434 (Gliese 915, LHS 1005, L 362-81) is a nearby degenerate star (white dwarf) of spectral class DAP5.8, [3] the single known component of the system, located in the constellation Phoenix, the nearest star in this constellation.

Contents

Distance

WD 2359−434, probably, is the 11th closest white dwarf, or, possibly, 9th, 10th, or 12th (see Gliese 293, GJ 1087 and Gliese 518). Currently, the most accurate distance estimate of WD 2359−434 is trigonometric parallax from CTIOPI (Cerro Tololo Inter-American Observatory Parallax Investigation) 0.9 m telescope program, published in 2009 in the 21st paper of RECONS's The Solar Neighborhood (TSN) series [8] Subasavage et al. 2009: [4] 122.27 ± 1.13 mas, corresponding to a distance 8.18 ± 0.08 pc, or 26.68 ± 0.25 ly.

WD 2359−434 distance estimates
SourcePaperParallax, mas Distance, pc Distance, ly Ref.
Woolley Woolley et al. 1970 122 ± 88.2 ± 0.626.7 ± 1.9 [9]
GJ, 3rd version Gliese, Jahreiss 1991 128.2 ± 6.47.80 ± 0.4125.44 ± 1.37 [10]
YPC, 4th edition van Altena et al. 1995 127.4 ± 6.87.85 ± 0.4425.60 ± 1.44 [7]
CTIOPI 0.9 mTSN 21 (Subasavage et al. 2009)122.27 ± 1.138.18 ± 0.0826.68 ± 0.25 [4]

The most accurate estimate is marked in bold.

Physical parameters

WD 2359−434's mass is 0.85 ± 0.01 Solar masses, [4] its surface gravity is 108.39 ± 0.01 (2.45 · 108) cm·s −2, [4] or approximately 250,000 of Earth's, corresponding to a radius 6780 km, or 1.06 of Earth's.

WD 2359−434 is relatively hot and young white dwarf, its temperature is 8570 ± 50 K; [2] its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 1.82 ± 0.06 Gyr. [4] Gliese 518 should appear bluish-white, due temperature, comparable with that of A-type main sequence stars.

As all white dwarfs, WD 2359−434 is composed of very dense degenerate matter, its mean density is 1,300,000 g·cm −3, [4] [note 4] i.e. mass of one cubic millimetre of WD 2359−434 matter is 1.3 kg.

Unusually for a white dwarf star, WD 2359-434 has a weak, non-dipole magnetic field of 50,000 - 100,000 Gauss. [11]

Main sequence progenitor properties

As all degenerate stars, WD 2359−434 previously existed initially as main-sequence star and then as giant star, until all the thermonuclear fuel was exhausted, after which WD 2359−434 lost most of its mass. According to the 2010 thesis for the degree of Doctor of Science, [12] using Wood model D [13] initial–final mass relation and WD 2359−434's white dwarf mass value 0.97 ± 0.03  M☉ from Holberg et al. 2008, [2] its main sequence progenitor mass was 7.09 M☉. Using expression for pre-white dwarf lifetime 10 · (MMS/M☉)2.5 (Gyr), [13] was found WD 2359−434 main sequence age 0.07 Gyr.

White dwarf mass value 0.85 ± 0.01 M☉ from Subasavage et al. 2009, [4] in Wood model D yields MS (main sequence) mass 6.03 M☉, and MS lifetime 0.11 Gyr, corresponding to B-type main sequence star.

According to initial-final mass relation from Weidemann 2000 paper, [14] WD 2359−434's main sequence progenitor should have mass about 4.6 M☉ and lifespan 0.22 Gyr, and, again, should be of B spectral type. There are also other models.

See also

Notes

  1. ↑ From apparent magnitude and parallax.
  2. ↑ From surface gravity and mass.
  3. ↑ White dwarf cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star).
  4. ↑ From mass and surface gravity (assuming spherical shape).

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References

  1. 1 2 3 4 5 6 7 8 9 10 11 "GJ 915 -- White Dwarf". Centre de Données astronomiques de Strasbourg . Retrieved 2011-11-03.
  2. 1 2 3 4 5 6 7 8 Holberg, J. B.; Sion; Oswalt; McCook; Foran; Subasavage (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. S2CID   122855486.
  3. 1 2 3 Sion, Edward M.; Holberg; Oswalt; McCook; Wasatonic (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.
  4. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 Subasavage, John P.; Jao; Henry; Bergeron; Dufour; Ianna; Costa; Mendez (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....134.4547S. doi:10.1088/0004-6256/137/6/4547. S2CID   14696597.
  5. ↑ Pauli, E.-M.; Napiwotzki; Heber; Altmann & Odenkirchen (2006). "3D kinematics of white dwarfs from the SPY project. II". Astronomy and Astrophysics . 447 (1): 173–184. arXiv: astro-ph/0510494 . Bibcode:2006A&A...447..173P. doi:10.1051/0004-6361:20052730. S2CID   14250519. (see Table 8)
  6. ↑ 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.
  7. 1 2 Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)
  8. ↑ The Solar Neighborhood (TSN) Series in The Astronomical Journal
  9. ↑ Stars within 25 pc of the Sun (Woolley+ 1970)
  10. ↑ Nearby Stars, Preliminary 3rd Version (Gliese+ 1991)
  11. ↑ Landstreet, J. D.; Bagnulo, S.; Valyavin, G.; Valeev, A. F. (2017), "Monitoring and modelling of white dwarfs with extremely weak magnetic fields", Astronomy & Astrophysics, 607: A92, arXiv: 1709.04099 , doi:10.1051/0004-6361/201731432, S2CID   119502643
  12. ↑ Matías Cristóbal Radiszcz Sotomayor, BINARIEDAD ESTELAR Y SUB-ESTELAR EN ENANAS BLANCAS CERCANAS [ permanent dead link ]
  13. 1 2 Wood, M. A. (1992). "Constraints on the age and evolution of the Galaxy from the white dwarf luminosity function". The Astrophysical Journal . 386: 539–561. Bibcode:1992ApJ...386..539W. doi: 10.1086/171038 .
  14. ↑ Weidemann, V. (2000). "Revision of the initial-to-final mass relation". Astronomy and Astrophysics . 363: 647–656. Bibcode:2000A&A...363..647W.
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