G 99-47

Last updated
G 99-47
V1201OriLightCurve.png
A visual band light curve for V1201 Orionis, adapted from Brinkworth et al. (2013) [1]
Observation data
Epoch J2000 [2]        Equinox J2000 [2]
Constellation Orion
Right ascension 05h 56m 25.47s [2]
Declination +05° 21′ 48.6″ [2]
Apparent magnitude  (V)14.105 [3]
Characteristics
Spectral type DAP8.9 [4]
Apparent magnitude  (B)14.69 [2]
Apparent magnitude  (V)14.10 [2]
Apparent magnitude  (R)14.0 [2]
Apparent magnitude  (I)13.6 [2]
Apparent magnitude  (J)12.930 ± 0.022 [2]
Apparent magnitude  (H)12.720 ± 0.025 [2]
Apparent magnitude  (K)12.653 ± 0.024 [2]
Astrometry
Proper motion (μ)RA: -444.685 [5]   mas/yr
Dec.: -925.140 [5]   mas/yr
Parallax (π)123.1989 ± 0.0170  mas [5]
Distance 26.474 ± 0.004  ly
(8.117 ± 0.001  pc)
Absolute magnitude  (MV)14.59 [3] [6] [note 1]
Details
Mass 0.71 ± 0.03 [3]   M☉
Radius 0.011 [3] [note 2]   R☉
Surface gravity (log g)8.20 ± 0.05 [3]   cgs
Temperature 5790 ± 110 [3]   K
Age 3.97 [4] [note 3]   Gyr
Other designations
WD 0553+053, [3] [4] V1201 Ori, [2] LHS  212, [3] LTT  17891, [2] NLTT  15834, [2] G  099-047, [6] GJ  1087, [2] G  102-40, [2] G  106-15, [2] EGGR 290, [2] 2MASS  J05562547+0521486, [2] USNO-B1.0 0953-00073703, Gaia DR2 3320184202856027776 [2]
Database references
SIMBAD data

G 99-47 (V1201 Orionis) is a nearby degenerate star (white dwarf) of spectral class DAP8 (DAP8.9, [4] or DAP8.7 [3] ), the single known component of the system, located in the constellation Orion. G 99-47 is probably the tenth closest white dwarf, followed by Gliese 293, Gliese 518 and Gliese 915.

Contents

The mass of G 99-47 is 0.71±0.03 Solar masses; [3] its surface gravity is 108.20 ± 0.05 (1.58 · 108) cm·s−2, [3] or approximately 162 000 of Earth's, corresponding to a radius 7711 km, or 121% of Earth's. Its temperature is 5790 ± 110 K, [3] almost like the Sun's; its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 3.97 Gyr. [4] Due almost equal to the Sun's temperature, GJ 1087 should appear almost the same white color as the Sun. The white dwarf has a strong magnetic field, with measured vertical component near surface equal to 560 T. [7]

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)

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References

  1. ↑ Brinkworth, Carolyn S.; Burleigh, Matthew R.; Lawrie, Katherine; Marsh, Thomas R.; Knigge, Christian (August 2013). "Measuring the Rotational Periods of Isolated Magnetic White Dwarfs". The Astrophysical Journal. 773 (1): 47. Bibcode:2013ApJ...773...47B. doi: 10.1088/0004-637X/773/1/47 . hdl: 2381/37593 . S2CID   56285149.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 "V* V1201 Ori -- White Dwarf". Centre de Données astronomiques de Strasbourg . Retrieved 2011-11-01.
  3. 1 2 3 4 5 6 7 8 9 10 11 12 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.
  4. 1 2 3 4 5 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.
  5. 1 2 3 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.
  6. 1 2 Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)
  7. ↑ Bagnulo, Stefano; Landstreet, John D. (2020), "Discovery of six new strongly magnetic white dwarfs in the 20 pc local population", Astronomy & Astrophysics, 643: A134, arXiv: 2010.05795 , Bibcode:2020A&A...643A.134B, doi:10.1051/0004-6361/202038565, S2CID   222290583
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