Astronomy:WD 2359-434

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Coordinates: Sky map 00h 02m 10.766s, −43° 09′ 56.02″

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
Equinox J2000.0]] (ICRS)
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)122.27 ± 1.13[4] mas
Distance26.7 ± 0.2 ly
(8.18 ± 0.08 pc)
Absolute magnitude (MV)13.20[2][4][note 1]
Details
Mass0.85 ± 0.01[4] M
Radius0.0097[4][note 2] R
Surface gravity (log g)8.39 ± 0.01[4] cgs
Temperature8570 ± 50[2] K
Age1.82 ± 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,[6] EGGR 165,[1] 2MASS J00021076-4309560[1]
Database references
SIMBADdata

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.

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[7] 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
Source Paper Parallax, mas Distance, pc Distance, ly Ref.
Woolley Woolley et al. 1970 122 ± 8 8.2 ± 0.6 26.7 ± 1.9 [8]
GJ, 3rd version Gliese, Jahreiss 1991 128.2 ± 6.4 7.80 ± 0.41 25.44 ± 1.37 [9]
YPC, 4th edition van Altena et al. 1995 127.4 ± 6.8 7.85 ± 0.44 25.60 ± 1.44 [6]
CTIOPI 0.9 m TSN 21 (Subasavage et al. 2009) 122.27 ± 1.13 8.18 ± 0.08 26.68 ± 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.

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,[10] using Wood model D[11] 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),[11] 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,[12] 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).

References

  1. 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "GJ 915 -- White Dwarf". Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gliese+915. Retrieved 2011-11-03. 
  2. 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Holberg, J. B.; Sion; Oswalt; McCook; Foran; Subasavage (2008). "A NEW LOOK AT THE LOCAL WHITE DWARF POPULATION". The Astronomical Journal 135: 1225–1238. doi:10.1088/0004-6256/135/4/1225. Bibcode2008AJ....135.1225H. https://commons.erau.edu/cgi/viewcontent.cgi?article=1948&context=publication. 
  3. 3.0 3.1 3.2 Sion, Edward M.; Holberg; Oswalt; McCook; Wasatonic (2009). "THE WHITE DWARFS WITHIN 20 PARSECS OF THE SUN: KINEMATICS AND STATISTICS". The Astronomical Journal 138: 1681–1689. doi:10.1088/0004-6256/138/6/1681. Bibcode2009AJ....138.1681S. 
  4. 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 4.13 4.14 4.15 4.16 4.17 4.18 4.19 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: 4547–4560. doi:10.1088/0004-6256/137/6/4547. Bibcode2009AJ....134.4547S. 
  5. Pauli, E.-M.; Napiwotzki; Heber; Altmann; Odenkirchen (2006). "3D kinematics of white dwarfs from the SPY project. II". Astronomy and Astrophysics 447: 173–184. doi:10.1051/0004-6361:20052730. Bibcode2006A&A...447..173P.  (see Table 8)
  6. 6.0 6.1 Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)
  7. The Solar Neighborhood (TSN) Series in The Astronomical Journal
  8. Stars within 25 pc of the Sun (Woolley+ 1970)
  9. Nearby Stars, Preliminary 3rd Version (Gliese+ 1991)
  10. Matías Cristóbal Radiszcz Sotomayor, BINARIEDAD ESTELAR Y SUB-ESTELAR EN ENANAS BLANCAS CERCANAS[yes|permanent dead link|dead link}}]
  11. 11.0 11.1 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. doi:10.1086/171038. Bibcode1992ApJ...386..539W. 
  12. Weidemann, V. (2000). "Revision of the initial-to-final mass relation". Astronomy and Astrophysics 363: 647–656. Bibcode2000A&A...363..647W.