Astronomy:WD 0145+234

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Short description: White dwarf in the constellation Aries

Coordinates: Sky map 01h 47m 54.81s, +23° 39′ 43.6″

WD 0145+234
Observation data
Equinox J2000.0]] (ICRS)
Constellation Aries[1]
Right ascension  01h 47m 54.81s[2][3]
Declination +23° 39′ 43.6″[2][3]
Apparent magnitude (V) 11.64[4]
Characteristics
Spectral type DA[2]
Astrometry
Distance98.08 ly
(29.458[3] pc)
Details
Temperature12910[2] K
Other designations
WD 0145+234; 2MASS J01475481+2339437; 1SWASP J014754.80+233943.8; Gaia DR2 291057843317534464; CHSS 3403; Mrk 362; WD 0145+23
Database references
SIMBADdata

WD 0145+234 is a white dwarf star approximately 95 ly (29 pc)[3] from Earth in the constellation of Aries that has been associated with studies suggesting that a very large exoasteroid near the star was substantially disrupted, resulting in a considerable amount of dust and debris around the star.[3][5] Alternatively, the outburst around WD 0145+234 is explained with ongoing collisions between planetesimals inside the dusty debris disk around the white dwarf.[6]

The outburst around WD 0145+234 appeared in 2018 in data by the Wide-Field Infrared Survey Explorer. Outburst around white dwarfs in the infrared are not unusual. Novae and dwarf novae also show outbursts, but they are accompanied by an outburst in the optical and appear around binaries. WD 0145+234 is however a single white dwarf and did not show any brightening in the optical images taken by CRTS and ASASSN. This suggested that the outburst was caused by recent replenishing or redistribution of dust.[3] A follow-up study using the Spitzer Space Telescope found a decrease of the infrared brightness, beginning in late 2019. The decrease is accompanied by small bumps superimposed on the decrease of infrared brightness. The team studying WD 0145+234 with Spitzer concluded that the increase of brightness was not caused by the a tidal disruption of an exoasteroids, but by ongoing collisions in the disk around the white dwarf. A similar decrease in infrared brightness was found around the white dwarf GD 56.[6] WD 0145+234 is also unusual because not only does it show metal pollution in the form of absorption lines, which are found around 25-50% of white dwarfs, but also emission lines caused by calcium gas, which are less common.[7] It is still not clear what causes the metal emission lines around some white dwarfs, but the existence of such lines around WD 0145+234 suggests that metal gas is formed in collisions. There are still some unanswered questions for this hypothesis: Some white dwarfs with metal gas show variable emission lines, while WD 0145+234 does not show any variability in the calcium emission line. It is unclear why some white dwarfs show variable metal emission lines.[6]

Other white dwarfs with planetary pollution also show infrared variability, with the prototype being G29-38, which showed a decrease of infrared flux by about 35% over a period of 300 days.[8] White dwarfs with the highest infrared variations show calcium emission lines, just like WD 0145+234.[9] WD 0145+234 might be the system with one of the highest activity of this class of objects.[6]

Observations with NIRSpec released in a preprint in October 2023 showed that the debris disk is returning to its quiescent state. MIRI spectroscopy showed emission at 9-12 micron, consistent with silicate minerals and a tentative emission feature around 7 microns was interpreted as carbonates. The authors noted that emission of silicate minerals begins at 9 microns and therefore resembles more the emission feature of enstatite than that of fosterite.[10]

Exoasteroid disrupted by star (artist concept)

See also

References

  1. ↑ Staff (2 August 2008). "Finding the constellation which contains given sky coordinates". DJM.cc. http://djm.cc/constellation.html. 
  2. ↑ 2.0 2.1 2.2 2.3 Staff (2019). "WD 0145+234". SIMBAD. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=WD+0145%2B234. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Wang, Ting-gui; et al. (10 October 2019). "An On-going Mid-infrared Outburst in the White Dwarf 0145+234: Catching in Action of Tidal Disruption of an Exoasteroid?". arXiv:1910.04314v1 [astro-ph.SR].
  4. ↑ Staff (2019). "WD0145+234". Villanova University. http://www.astronomy.villanova.edu/WDCatalog/WDhtm/WD0145+234.htm. 
  5. ↑ Letzer, Rafi (17 October 2019). "An Asteroid-Smashing Star Ground a Giant Rock to Bits and Covered Itself in the Remains". LiveScience. https://www.livescience.com/white-dwarf-asteroid-smasher.html. 
  6. ↑ 6.0 6.1 6.2 6.3 Swan, Andrew; Kenyon, Scott J.; Farihi, Jay; Dennihy, Erik; Gänsicke, Boris T.; Hermes, J. J.; Melis, Carl; von Hippel, Ted (2021-09-01). "Collisions in a gas-rich white dwarf planetary debris disc". Monthly Notices of the Royal Astronomical Society 506 (1): 432–440. doi:10.1093/mnras/stab1738. ISSN 0035-8711. PMID 34248393. Bibcode: 2021MNRAS.506..432S. 
  7. ↑ Melis, Carl; Klein, Beth; Doyle, Alexandra E.; Weinberger, Alycia; Zuckerman, B.; Dufour, Patrick (2020-12-01). "Serendipitous Discovery of Nine White Dwarfs with Gaseous Debris Disks". The Astrophysical Journal 905 (1): 56. doi:10.3847/1538-4357/abbdfa. ISSN 0004-637X. Bibcode: 2020ApJ...905...56M. 
  8. ↑ Xu, S.; Jura, M. (2014-09-01). "The Drop during Less than 300 Days of a Dusty White Dwarf's Infrared Luminosity". The Astrophysical Journal 792 (2): L39. doi:10.1088/2041-8205/792/2/L39. ISSN 0004-637X. Bibcode: 2014ApJ...792L..39X. https://ui.adsabs.harvard.edu/abs/2014ApJ...792L..39X. 
  9. ↑ Swan, Andrew; Farihi, Jay; Wilson, Thomas G.; Parsons, Steven G. (2020-08-01). "The dust never settles: collisional production of gas and dust in evolved planetary systems". Monthly Notices of the Royal Astronomical Society 496 (4): 5233–5242. doi:10.1093/mnras/staa1688. ISSN 0035-8711. Bibcode: 2020MNRAS.496.5233S. https://ui.adsabs.harvard.edu/abs/2020MNRAS.496.5233S. 
  10. ↑ Swan, Andrew; Farihi, Jay; Su, Kate Y. L.; Desch, Steven J. (17 October 2023). "The first white dwarf debris disk observed by JWST". MNRAS Letters. Bibcode: 2023arXiv231009355S. https://ui.adsabs.harvard.edu/abs/2023arXiv231009355S/abstract. 



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