WD 0816–310

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WD 0816–310
Artist's impression of WD 0816-310, a magnetic white dwarf with a metal scar (eso2403a).jpg
Artist's impression of WD 0816–310, its disk, its magnetic field and the metal scars near one of the magnetic poles
Credit: ESO/L. Calçada
Observation data
Epoch J2000       Equinox J2000
Constellation Puppis
Right ascension 08h 18m 40.26s
Declination −31° 10′ 20.33″
Characteristics
Evolutionary stage white dwarf
Spectral type DBAZ [1]
Apparent magnitude  (G)15.39 [2]
Variable type magnetic and spectroscopic variable [1]
Astrometry
Proper motion (μ)RA: 237.736 ±0.020  mas/yr [2]
Dec.: -786.034 ±0.024  mas/yr [2]
Parallax (π)51.6508 ± 0.0240  mas [2]
Distance 63.15 ± 0.03  ly
(19.361 ± 0.009  pc)
Details [1]
Mass 0.72  M☉
Surface gravity (log g)8.25  cgs
Temperature 6250  K
Rotation 10.89426 days [3]
Age cooling age: 4.2 Gyr
total age: 4.8  Gyr
Other designations
CNS5 2061, SCR J0818-3110, 2MASS  J08184024-3110196, PM J08186-3110, TIC  147018085, Gaia  DR2 5548080118369905408
Database references
SIMBAD data

WD 0816–310 (PM J08186–3110) is a magnetic white dwarf with metal pollution, originating from the tidal disruption of a planetary body. The metals are guided by the magnetic field onto the surface of the white dwarf, creating a "scar" on the surface of the white dwarf. This scar is rich in the accreted planetary material. [4] [3]

The object was first identified as a possible white dwarf in 2005, from data of the Digitized Sky Survey. [5] It was confirmed as a white dwarf in 2008 with spectroscopic data from CTIO and the same team found that the white dwarf is polluted with calcium, magnesium and iron. [6] In 2019 a variable magnetic field was discovered thanks to Zeeman splitting. This observation was made with archived spectropolarimetric data from FORS1 at the Very Large Telescope (VLT). [7] In 2021 the white dwarf was studied in detail with the 4 m telescope at CTIO, and with the VLT (FORS1 and X-shooter). The elements sodium, magnesium, calcium, chromium, manganese, iron and nickel were detected in the atmosphere of the white dwarf. The atmosphere is enriched in magnesium, relative to other elements, which is predicted for old stellar systems. The researchers also found hydrogen in this otherwise helium-dominated atmosphere of WD 0816–310. The presence of hydrogen could be explained with the pollution of an asteroid containing water ice. These researchers found that the abundance of metals changed between two spectra 10 years apart. They suggested that spots enriched in metals are present on the surface of the white dwarfs, a process controlled by the magnetic field of the white dwarfs. [1] In 2024 this was confirmed with circular spectropolarimetric observations with FORS2 on the VLT. The observations measured a dipolar field strength at the pole of about 140 Kilogauss. Around 310,000 years ago WD 0816–310 accreted a Vesta-sized object with a composition similar to chondritic meteorites. [3]

The observations showed that the variation metal line strength and magnetic field intensity are synchronized. This is seen as evidence that the magnetic field determines the local density of metals on the surface. These patches are likely present near one of the magnetic poles of the white dwarf. The material from an accreted asteroid will first form a disk around the white dwarf. Closer to the white dwarf the dusty material will sublimate into a metal-gas. The researchers claim that white dwarf will ionize at least a part of the gas. These ions will follow the magnetic field of the white dwarf and as a result of the Lorentz force it will follow a spiral orbit around the local field line. On their way to the poles of the white dwarf, the ions will collide with neutral atoms in the gas disk, ionizing them in the process. This leads to a substantial level of ionization of the gas disk. [3]

A study in 2024 that discovered the second metal scar around WD 2138-332, suggests that metal scars are common around magnetic white dwarfs with metal pollution. [8]

See also

Related Research Articles

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WD 0806−661, formally named Maru, is a DQ white dwarf with an extremely cold Y-type substellar companion, located in the constellation Volans at 62.7 light-years from Earth. The companion was discovered in 2011, and is the only known Y-type companion to a star or stellar remnant. At the time of its discovery WD 0806-661 B had the largest actual and apparent separation of any known planetary-mass object, as well as being the coldest directly imaged substellar object then known.

<span class="mw-page-title-main">GL Virginis</span> Star in the constellation Virgo

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<span class="mw-page-title-main">WD 1337+705</span> Star in the constellation Ursa Minor

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References

  1. 1 2 3 4 Kawka, Adela; Vennes, Stéphane; Allard, Nicole F.; Leininger, T.; Gadéa, F. X. (2021-01-01). "The nearby magnetic cool DZ white dwarf PM J08186-3110". Monthly Notices of the Royal Astronomical Society. 500: 2732–2740. arXiv: 2010.15319 . Bibcode:2021MNRAS.500.2732K. doi: 10.1093/mnras/staa3421 . ISSN   0035-8711.
  2. 1 2 3 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.
  3. 1 2 3 4 Bagnulo, Stefano; Farihi, Jay; Landstreet, John D.; Folsom, Colin P. (2024-03-01). "Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf". The Astrophysical Journal. 963 (1): L22. arXiv: 2402.16526 . Bibcode:2024ApJ...963L..22B. doi: 10.3847/2041-8213/ad2619 . ISSN   0004-637X.
  4. ↑ information@eso.org. "Metal scar found on cannibal star". www.eso.org. Retrieved 2024-09-15.
  5. ↑ Lépine, Sébastien (2005-09-01). "New High Proper Motion Stars from the Digitized Sky Survey. III. Stars with Proper Motions 0.45" < μ < 2.0" yr-1 South of Declination -30°". The Astronomical Journal. 130 (3): 1247–1260. arXiv: astro-ph/0501266 . Bibcode:2005AJ....130.1247L. doi:10.1086/432161. ISSN   0004-6256.
  6. ↑ Subasavage, John P.; Henry, Todd J.; Bergeron, P.; Dufour, P.; Hambly, Nigel C. (2008-09-01). "The Solar Neighborhood. Xx. Discovery and Characterization of 21 New Nearby White Dwarf Systems". The Astronomical Journal. 136: 899–908. arXiv: 0805.2515 . Bibcode:2008AJ....136..899S. doi:10.1088/0004-6256/136/3/899. ISSN   0004-6256.
  7. ↑ Bagnulo, S.; Landstreet, J. D. (2019-10-01). "Discovery of weak magnetic fields in four DZ white dwarfs in the local 20 pc volume. Implications for the frequency of magnetic fields with cooling age". Astronomy and Astrophysics. 630: A65. arXiv: 1908.08418 . Bibcode:2019A&A...630A..65B. doi:10.1051/0004-6361/201936068. ISSN   0004-6361.
  8. ↑ Bagnulo, S.; Landstreet, J. D.; Farihi, J.; Folsom, C. P.; Hollands, M. A.; Fossati, L. (2024-08-01). "Metal accretion scars may be common on magnetic, polluted white dwarfs". Astronomy and Astrophysics. 688: L14. arXiv: 2407.17196 . Bibcode:2024A&A...688L..14B. doi:10.1051/0004-6361/202451215. ISSN   0004-6361.
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