Misplaced Pages

Wolf 1346

Article snapshot taken from[REDACTED] with creative commons attribution-sharealike license. Give it a read and then ask your questions in the chat. We can research this topic together.

Star in the constellation Vulpecula
Wolf 1346
Location of Wolf 1346 (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Vulpecula
Right ascension 20 34 21.88470
Declination +25° 03′ 49.7504″
Apparent magnitude (V) 11.546
Characteristics
Evolutionary stage White dwarf
Spectral type DA2.4
U−B color index −0.784
B−V color index −0.075
J−H color index −0.033
J−K color index −0.147
Astrometry
Radial velocity (Rv)71.0±7.4 km/s
Proper motion (μ) RA: −403.387 mas/yr
Dec.: −563.404 mas/yr
Parallax (π)67.4085 ± 0.0367 mas
Distance48.39 ± 0.03 ly
(14.835 ± 0.008 pc)
Details
Mass0.636±0.005 M☉
Radius0.0139±0.0006 R☉
Luminosity0.0332+0.0056
−0.0048 L☉
Surface gravity (log g)8.015±0.006 cgs
Temperature21608±153 K
Age60 Myr
Other designations
Gaia DR2 1831553382794173824, GJ 794, HD 340611, HIP 101516, AC +25°68981, G 186-31, LAWD 82, LFT 1554, LHS 3562, LSPM J2034+2503, LTT 16005, NLTT 49494, PLX 4895.00, PM 20322+2454, PM J20343+2503, WD 2032+248, Wolf 1346, TIC 298186852, TYC 2161-1038-1, GCRV 12872, 2MASS J20342188+2503498, WISEA J203421.56+250343.8
Database references
SIMBADdata

Wolf 1346, otherwise known as HD 340611 and WD 2032+248, is a star in the northern constellation of Vulpecula. With an apparent magnitude of 11.546, it is too faint to be seen by the naked eye but can be observed using a telescope with an aperture of 51 mm (2.0 in) or larger. It is located at a distance of approximately 48.4 light-years (14.8 pc) according to Gaia EDR3 parallax measurements, and is receding away from the Sun at a heliocentric radial velocity of +71.0 km/s.

Properties

This is a young, non-magnetic white dwarf with an age of 60 million years. It is a little less than two-thirds the mass of the Sun and just 1.4% the radius, that is 1.5 times the size of Earth or 9,670 km (6,010 mi). With an effective temperature of 21,608 K (21,335 °C; 38,435 °F), it shines with 3.3% of the Sun's luminosity. It belongs to the thin disk of the Milky Way. There is marginal indication that the star is orbited by a binary companion.

It has the spectral type DA2.4, indicating that the atmosphere is dominated by hydrogen, which is the only element whose spectral lines show up in the star's visible spectrum. It has been subject to multiple ultraviolet spectroscopic observations. Silicon lines were discovered in 1984 from spectra obtained by the International Ultraviolet Explorer. The abundance of silicon in the photosphere has been measured at log(Si/H)=−7.5 ± 0.2, which, compared to the solar value of log(Si/H)=−4.5, is approximately one thousand times less. This amount is comparable to what is expected from radiative levitation. Carbon, nitrogen, and oxygen are absent in the spectra, consistent with theories of element diffusion. Observations by the Hopkins Ultraviolet Telescope revealed that the Lyman-beta line shows signs of the dihydrogen cation (H2), which, in cooler DA white dwarfs, causes similar signatures in the Lyman-alpha line.

Notes

  1. This is just the cooling age.

References

  1. ^ 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.
  2. ^ Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (21 April 2010). "UBV ( RI ) C JHK observations of Hipparcos -selected nearby stars" (PDF). Monthly Notices of the Royal Astronomical Society. 403 (4): 1949–1968. doi:10.1111/j.1365-2966.2009.16182.x. Retrieved 31 January 2025.
  3. ^ Gianninas, A.; Bergeron, P.; Ruiz, M. T. (20 December 2011). "A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS". The Astrophysical Journal. 743 (2): 138. doi:10.1088/0004-637X/743/2/138. ISSN 0004-637X. Retrieved 30 January 2025.
  4. ^ Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  5. Kharchenko, N.V.; Scholz, R.‐D.; Piskunov, A.E.; Röser, S.; Schilbach, E. (2007). "Astrophysical supplements to the ASCC‐2.5: Ia. Radial velocities of ∼55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889–896. doi:10.1002/asna.200710776. ISSN 0004-6337. Retrieved 31 January 2025.
  6. Vincent, O.; Barstow, M. A.; Jordan, S.; Mander, C.; Bergeron, P.; Dufour, P. (2024). "Classification and parameterization of a large Gaia sample of white dwarfs using XP spectra". Astronomy & Astrophysics. 682: A5. doi:10.1051/0004-6361/202347694. ISSN 0004-6361. Record for this source at VizieR.
  7. Bédard, A.; Bergeron, P.; Fontaine, G. (10 October 2017). "Measurements of Physical Parameters of White Dwarfs: A Test of the Mass–Radius Relation". The Astrophysical Journal. 848 (1): 11. doi:10.3847/1538-4357/aa8bb6. ISSN 0004-637X. Record for this source at VizieR.
  8. ^ Berdyugin, Andrei V.; Piirola, Vilppu; Bagnulo, Stefano; Landstreet, John D.; Berdyugina, Svetlana V. (2022). "Highly sensitive search for magnetic fields in white dwarfs using broad-band circular polarimetry" (PDF). Astronomy & Astrophysics. 657: A105. doi:10.1051/0004-6361/202142173. ISSN 0004-6361. Retrieved 23 January 2025.
  9. "Wolf 1346". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 January 2025.
  10. North, Gerald; James, Nick (2014). Observing Variable Stars, Novae and Supernovae. Cambridge University Press. p. 24. ISBN 978-1-107-63612-5.
  11. Torres, S; Cantero, C; Rebassa-Mansergas, A; Skorobogatov, G; Jiménez-Esteban, F M; Solano, E (1 June 2019). "Random Forest identification of the thin disc, thick disc, and halo Gaia -DR2 white dwarf population". Monthly Notices of the Royal Astronomical Society. 485 (4): 5573–5589. doi:10.1093/mnras/stz814. ISSN 0035-8711. Retrieved 31 January 2025. Record for this source at VizieR.
  12. Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019). "Stellar and substellar companions of nearby stars from Gaia DR2: Binarity from proper motion anomaly" (PDF). Astronomy & Astrophysics. 623: A72. doi:10.1051/0004-6361/201834371. ISSN 0004-6361. Retrieved 23 January 2025.
  13. ^ Holberg, J. B.; Barstow, M. A.; Bruhweiler, F. C.; Collins, J. (1996). "Photospheric Silicon in the DA White Dwarf Wolf 1346". The Astronomical Journal. 111: 2361. doi:10.1086/117969.
  14. ^ Wesemael, F.; Henry, R. B. C.; Shipman, H. L. (1984). "Metal abundances in the hot DA white dwarfs Wolf 1346 and Feige 24". The Astrophysical Journal. 287: 868. doi:10.1086/162745. ISSN 0004-637X.
  15. Morvan, E.; Vauclair, G.; Vauclair, S. (July 1986). "Silicon abundances in Feige 24 and Wolf 1346 : results of the diffusion theory". Astronomy & Astrophysics. 163: 145–150. Bibcode:1986A&A...163..145M.
  16. Koester, D.; Finley, D. S.; Allard, N. F.; Kruk, J. W.; Kimble, R. A. (1 June 1996). "Quasi-Molecular Satellites of Lyβ in the Spectrum of the DA White Dwarf Wolf 1346". The Astrophysical Journal. 463 (2): L93 – L99. doi:10.1086/310062. Retrieved 23 January 2025.
Constellation of Vulpecula
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Star clusters
Nebulae
Galaxies
NGC
Other
Astronomical events
Category
Categories:
Wolf 1346 Add topic