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SDSS J1228+1040

SDSS J1228+1040 (SDSS J122859.93+104032.9, WD 1226+110) is a white dwarf with a debris disk around it. The disk formed when a planetary body was tidally disrupted around the white dwarf. It is the first gaseous disk discovered around a white dwarf.[2]

SDSS J1228+1040

Doppler imaging of the calcium gas around SDSS J1228+1040. The map is "inside-out", with the outer part being closer to the white dwarf
Credit: University of Warwick/C. Manser/ESO
Observation data
Epoch J2000      Equinox J2000
Constellation Virgo
Right ascension 12h 28m 59.93s
Declination +10° 40′ 33.05″
Characteristics
Evolutionary stage white dwarf
Spectral type DAZ[1][2]
Apparent magnitude (G) 16.4[3]
Astrometry
Proper motion (μ) RA: -50.254 ±0.069 mas/yr[3]
Dec.: -24.729 ±0.049 mas/yr[3]
Parallax (π)7.7634 ± 0.0662 mas[3]
Distance420 ± 4 ly
(129 ± 1 pc)
Details[4][2]
Mass0.705 ±0.051 M☉
Radius0.01169 ±0.00078 R☉
Surface gravity (log g)8.150 ±0.089 cgs
Temperature20,713 ±281 K
Agecooling age: 100 ±5 Myr
total age: 170 Myr
Other designations
GALEX J122859.9+104032, WD 1226+110, WD 1226+109, LAMOST J122859.93+104032.9, SDSS J122859.93+104032.9, WIRED J122859.93+104032.9, WISE J122859.87+104032.8
Database references
SIMBADdata

SDSS J1228+1040 was first identified as a white dwarf in 2006 from SDSS spectroscopic data. These observations identified it as a DA white dwarf, which indicates the detection of hydrogen.[1]

The gaseous disk was discovered in 2006, using data from the William Herschel Telescope. This gaseous disk was discovered by the emission of the calcium triplet at 850-866 nm and weaker emission due to iron at 502 nm and 517 nm. The double peak of the calcium triplet is seen as evidence of a rotating disk. The authors constrain the outer radius of the gaseous disk to 1.2 R☉. The authors also find absorption due to magnesium.[2] Additional elements in emission were detected in 2016.[5] Hubble far-ultraviolet observations did not detect any emission-lines, which constrained the gaseous disk temperature to around 5000 K. The researchers modelled the disk to have a spiral shape.[6]

In 2010 it was found that the calcium emission line changed between two epochs. The red side of the emission line complex switched to the blue side. This was first interpreted as a clumpy disk and the change in emission lines was seen as possible evidence of these clumps moving.[7] Spectroscopic data from 2003 to 2015 were used for doppler imaging, which resolved the gaseous disk. The changes in calcium emission were interpreted as precession of the disk, with a period of 24-30 years. These timescales are in agreement with precession under the influence of general relativity.[5] Modelling of the gaseous disk were carried out in 2021, finding an eccentricity of 0.188 ±0.004 and semi-major axis of 0.879 ±0.005 R☉ for the gas ring.[8] The gaseous disk was modelled in detail in 2024, finding an inner disk radius of 0.57 R☉, an outer radius of 1.7 R☉ and a peak emission at 1 R☉. The disk shows eccentricity with the eccentricity of the inner edge being 0.44 and at the outer edge being nearly zero. The inclination is unconstrained in this work. The precession period was found to be 20.5 years. The researchers point out that the progenitor had a very eccentric orbit around the white dwarf, before it was disrupted. The precession should dissipate within around 200 years, meaning the disk is very young and should contain most of the mass of the progenitor, which they estimate to be 1021 g, equivalent to a body with a size of about 50 km.[9]

In 2009 a dusty component was discovered, thanks to the detection of infrared excess. This discovery was made with observations from the Very Large Telescope, the United Kingdom Infrared Telescope and the Spitzer Space Telescope. The modelled dusty disk has an inner radius of 18 white dwarf radii and the outer radius is 107 white dwarf radii. The outer radius is similar to the gaseous disk radius of 108 white dwarf radii. The inner disk has a temperature of 1670 K and the outer disk has a temperature of 450 K. According to this work the disk has an inclination of around 70°.[10] Later modelling found that the dusty disk has an inner temperature of 1300±50 K, an outer temperature of 500±70 K.[7] It was found that the disk is variable in infrared light. The 3.6 and 4.5 μm flux decreased by 20% from 2007 to 2014 and remained at this level until 2018.[11]

Absorption and emission lines found around SDSS J1228+1040
Element Absoption Emission Reference
calcium yes yes [2][12]
iron yes [2]
magnesium yes yes [2][5]
oxygen yes yes [5][12]
silicon yes [12]
carbon yes [12]
aluminium yes [12]
chromium yes [12]
nickel yes [12]

A candidate planetesimal

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Main article: SDSS J1228+1040 b

The planetesimal, called SDSS 1228+1040 b, was suggested as an explanation of a 123.4 minute variation of the calcium emission line. The researchers found that this planetesimal must be orbiting within the disk.[13] The body was modelled to have a size of around 72 km.[14] Another study does however blame precession for the variability of the calcium emission line.[9]

Other gaseous white dwarf disks

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Other gaseous disks were discovered. Especially Gaia helped in increasing this sample and these systems often also show variable emission lines,[15][16] which could be a sign of precession in these disks.[9]

See also

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References

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  1. ^ a b Eisenstein, Daniel J.; Liebert, James; Harris, Hugh C.; Kleinman, S. J.; Nitta, Atsuko; Silvestri, Nicole; Anderson, Scott A.; Barentine, J. C.; Brewington, Howard J.; Brinkmann, J.; Harvanek, Michael; Krzesiński, Jurek; Neilsen, Eric H., Jr.; Long, Dan; Schneider, Donald P. (2006-11-01). "A Catalog of Spectroscopically Confirmed White Dwarfs from the Sloan Digital Sky Survey Data Release 4". The Astrophysical Journal Supplement Series. 167 (1): 40–58. arXiv:astro-ph/0606700. Bibcode:2006ApJS..167...40E. doi:10.1086/507110. ISSN 0067-0049.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  2. ^ a b c d e f g Gänsicke, B. T.; Marsh, T. R.; Southworth, J.; Rebassa-Mansergas, A. (2006-12-01). "A Gaseous Metal Disk Around a White Dwarf". Science. 314 (5807): 1908–1910. arXiv:astro-ph/0612697. Bibcode:2006Sci...314.1908G. doi:10.1126/science.1135033. ISSN 0036-8075. PMID 17185598.
  3. ^ a b c 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.
  4. ^ Koester, D.; Gänsicke, B. T.; Farihi, J. (2014-06-01). "The frequency of planetary debris around young white dwarfs". Astronomy and Astrophysics. 566: A34. arXiv:1404.2617. Bibcode:2014A&A...566A..34K. doi:10.1051/0004-6361/201423691. ISSN 0004-6361.
  5. ^ a b c d Manser, Christopher J.; Gänsicke, Boris T.; Marsh, Thomas R.; Veras, Dimitri; Koester, Detlev; Breedt, Elmé; Pala, Anna F.; Parsons, Steven G.; Southworth, John (2016-02-01). "Doppler imaging of the planetary debris disc at the white dwarf SDSS J122859.93+104032.9". Monthly Notices of the Royal Astronomical Society. 455 (4): 4467–4478. arXiv:1511.02230. Bibcode:2016MNRAS.455.4467M. doi:10.1093/mnras/stv2603. ISSN 0035-8711.
  6. ^ Hartmann, S.; Nagel, T.; Rauch, T.; Werner, K. (2016-09-01). "The gaseous debris disk of the white dwarf SDSS J1228+1040. HST/COS search for far-ultraviolet signatures". Astronomy and Astrophysics. 593: A67. arXiv:1607.08158. Bibcode:2016A&A...593A..67H. doi:10.1051/0004-6361/201628403. ISSN 0004-6361.
  7. ^ a b Melis, C.; Jura, M.; Albert, L.; Klein, B.; Zuckerman, B. (2010-10-01). "Echoes of a Decaying Planetary System: The Gaseous and Dusty Disks Surrounding Three White Dwarfs". The Astrophysical Journal. 722 (2): 1078–1091. arXiv:1007.2023. Bibcode:2010ApJ...722.1078M. doi:10.1088/0004-637X/722/2/1078. ISSN 0004-637X.
  8. ^ Trevascus, David; Price, Daniel J.; Nealon, Rebecca; Liptai, David; Manser, Christopher J.; Veras, Dimitri (2021-07-01). "Formation of eccentric gas discs from sublimating or partially disrupted asteroids orbiting white dwarfs". Monthly Notices of the Royal Astronomical Society. 505 (1): L21–L25. arXiv:2105.00626. Bibcode:2021MNRAS.505L..21T. doi:10.1093/mnrasl/slab043. ISSN 0035-8711.
  9. ^ a b c Goksu, Olcay Ates; Kutra, Taylor; Wu, Yanqin (2024-05-01). "On the Rigidly Precessing, Eccentric Gas Disk Orbiting the White Dwarf SDSS J1228+1040". The Astronomical Journal. 167 (5): 236. arXiv:2308.01234. Bibcode:2024AJ....167..236G. doi:10.3847/1538-3881/ad3216. ISSN 0004-6256.
  10. ^ Brinkworth, C. S.; Gänsicke, B. T.; Marsh, T. R.; Hoard, D. W.; Tappert, C. (2009-05-01). "A Dusty Component to the Gaseous Debris Disk Around the White Dwarf SDSS J1228+1040". The Astrophysical Journal. 696 (2): 1402–1406. arXiv:0902.4044. Bibcode:2009ApJ...696.1402B. doi:10.1088/0004-637X/696/2/1402. ISSN 0004-637X.
  11. ^ Xu, Siyi; Su, Kate Y. L.; Rogers, L. K.; Bonsor, Amy; Olofsson, Johan; Veras, Dimitri; van Lieshout, Rik; Dufour, Patrick; Green, Elizabeth M.; Schlawin, Everett; Farihi, Jay; Wilson, Thomas G.; Wilson, David J.; Gänsicke, Boris T. (2018-10-01). "Infrared Variability of Two Dusty White Dwarfs". The Astrophysical Journal. 866 (2): 108. arXiv:1808.09426. Bibcode:2018ApJ...866..108X. doi:10.3847/1538-4357/aadcfe. ISSN 0004-637X.
  12. ^ a b c d e f g Gänsicke, B. T.; Koester, D.; Farihi, J.; Girven, J.; Parsons, S. G.; Breedt, E. (2012-07-01). "The chemical diversity of exo-terrestrial planetary debris around white dwarfs". Monthly Notices of the Royal Astronomical Society. 424 (1): 333–347. arXiv:1205.0167. Bibcode:2012MNRAS.424..333G. doi:10.1111/j.1365-2966.2012.21201.x. ISSN 0035-8711.
  13. ^ Manser, Christopher J.; et al. (April 2019). "A planetesimal orbiting within the debris disc around a white dwarf star". Science. 364 (6435): 66–69. arXiv:1904.02163. Bibcode:2019Sci...364...66M. doi:10.1126/science.aat5330. PMID 30948547. S2CID 96434522.
  14. ^ Dwomoh, Arianna M.; Bauer, Evan B. (2023-08-01). "Reinterpreting the Polluted White Dwarf SDSS J122859.93+104032.9 in Light of Thermohaline Mixing Models: More Polluting Material from a Larger Orbiting Solid Body". The Astrophysical Journal. 952 (2): 95. arXiv:2306.03864. Bibcode:2023ApJ...952...95D. doi:10.3847/1538-4357/acdb69. ISSN 0004-637X.
  15. ^ Manser, Christopher J.; Gänsicke, Boris T.; Gentile Fusillo, Nicola Pietro; Ashley, Richard; Breedt, Elmé; Hollands, Mark; Izquierdo, Paula; Pelisoli, Ingrid (2020-04-01). "The frequency of gaseous debris discs around white dwarfs". Monthly Notices of the Royal Astronomical Society. 493 (2): 2127–2139. arXiv:2002.01936. Bibcode:2020MNRAS.493.2127M. doi:10.1093/mnras/staa359. ISSN 0035-8711.
  16. ^ 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. arXiv:2010.03695. Bibcode:2020ApJ...905...56M. doi:10.3847/1538-4357/abbdfa. ISSN 0004-637X.
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