# List of exoplanets and planetary debris around white dwarfs

This is a list of exoplanets and planetary debris disks around white dwarfs.

## List of white dwarf exoplanets
### List of confirmed exoplanets

| System name | Host star | Mass of planet (M$_J$) | Semi-major axis (au) | Discovery method | Discovery year | Note |
| WD 0806-661 | single | 1.5-8 | 2500 | direct imaging | 2011 | WD 0806-661 B can be interpreted as either a sub-brown dwarf or an exoplanet. |
| WD J0914+1914 | metal-polluted single | | 0.070 to 0.074 | detection of accreted planet material via spectroscopy | 2019 | likely ice giant |
| WD 1856+534 | single | >0.84 | 0.019 | transiting | 2020 | the white dwarf co-moves with G 229-20 A/B |
| MOA-2010-BLG-477L | single | 1.4±0.3 | 2.8±0.5 | microlensing | 2012/2021 | a Jupiter-analogue |
| KMT-2020-BLG-0414 | single | 0.0060±0.0006 | 2.1±0.2 | microlensing | 2021/2024 | 1.9 earth-mass planet, also has a brown dwarf at 22 au |
| QZ Serpentis | white dwarf+K5 star | 0.63 | 0.019 | detection via "very long photometric period" (VLPP) | 2022 | has an orbital period of 1 day. |

### List of candidate exoplanets

| System name | Host star | Status | Mass of planet (M$_J$) | Semi-major axis (au) | Discovery method | Discovery year | Note | Reference |
| GD 356 | single | rejected candidate | <12 | | variability and missing IR-excess | 2010 | 115 minute variability, iron-rich terrestrial planet was suspected to electromagnetically interacting with the white dwarf, no orbiting body was detected, rejecting the idea of an unipolar inductor model | |
| GD 140 | single | suspected | 3.74+1.43 −0.90 | | anomaly in the Hipparcos-Gaia proper motion | 2019 | mass is estimated for separation of 5 AU, to be observed with JWST | |
| LAWD 37 | single | suspected | 0.60+0.23 −0.15 | | anomaly in the Hipparcos-Gaia proper motion | 2019 | mass is estimated for separation of 5 AU, to be observed with JWST | |
| GD 394 | metal-polluted single | candidate | | | EUV variability | 2019 | either a metal accretion spot that disappeared or an evaporating planet at a 1.15 day orbit, with a hydrogen-cloud around the planet transiting in front of the white dwarf | |
| WD 0141-675 | metal-polluted single | candidate | 9.26+2.64 −1.15 | | Gaia DR3 stellar multiples/radial velocity | 2023 | rejected due to software error 33.65 ± 0.05 day period. ESPRESSO radial velocity observations however possibly detects a planet with a 16 day period | |
| WD 1202−232 (LP 852-7) | metal-polluted single | candidate | 1–7 | 11.47 | direct imaging | 2024 | similar to solar system giant planets in age and separation | |
| WD 2105−82 (LAWD 83) | metal-polluted single | candidate | 1–2 | 34.62 | direct imaging | 2024 | similar to solar system giant planets in age and separation | |
| GALEX J071816.4+373139 | massive single | candidate | 3.6 | | infrared excess | 2024 | planet candidate has a temperature of about 400 K | |
| WD 0310-688 (CPD-69 177) | metal-polluted single | candidate | 3.0+5.5 −1.9 | 0.1-2 | infrared excess | 2024 | planet candidate has a temperature of 248+84 −61 K | |
| HS 0209+0832 | metal-polluted single | candidate | | | detection of accreted planet material via spectroscopy | 2024 | metals in agreement with giant planet (similar to WD J0914+1914), period of 4.4 days from TESS, first and currently only white dwarf with detection of zinc | |
| Sirius B | white dwarf+A0V star | candidate | 1.5 | 0.9 | astrometry | 2024 | has a mass range of 0.8-2.4 Jupiter masses. | [26] [27] |
| Central star of the Helix Nebula | single | candidate | | 0.034 | transiting | 2024 | orbits the central white dwarf of the Helix Nebula, has a radius of 1 R$_J$ or 2.3 R$_🜨$ | |
| Central star of the Helix Nebula | single | candidate | 1 | 0.004 | accreted material from the planet | 2025 | X-ray signal might have a period of 2.9 hours. Estimated to have been Jupiter-like. Mid-IR excess was interpreted as a disk or cloud formed by disrupted comets in the past. | |

### List of exoplanets detected via timing

Circumbinary exoplanets found with eclipse timing variations are sometimes listed as confirmed planets. The models describing these planets do however often fail to predict eclipse timing and the timing variation could be caused by other effects, such as magnetic effects. Due to the high number of objects detected via timing, this list was separated from the above lists.
| System name | Host star | Mass of planet (M$_J$) | Semi-major axis (au) | Discovery method | Discovery year | Note | Reference |
| PSR B1620-26 | white dwarf+pulsar | 2.5±1 | 23 | pulsar timing | 1993 | | |
| DP Leonis | white dwarf+donor star | 6.28 | 8.19 | eclipse timing variations | 2009 | has a size of 1.14 R$_J$ | |
| NN Serpentis | PCEB: white dwarf+red dwarf | 6.91±0.54 | 5.38±0.20 | eclipse timing variation | 2010 | PCEB is surrounded by a dusty disk, might be only one planet | |
| NN Serpentis | PCEB: white dwarf+red dwarf | 2.28±0.38 | 3.39±0.10 | eclipse timing variation | 2010 | PCEB is surrounded by a dusty disk, might be only one planet | |
| UZ Fornacis | white dwarf+red dwarf | 6.3 | 5.9 | eclipse timing variations | 2011 | planet b & c | |
| UZ Fornacis | white dwarf+red dwarf | 7.7 | 2.8 | eclipse timing variations | 2011 | planet b & c | |
| HU Aquarii | white dwarf+M4.5V star | 5.9 | 3.6 | eclipse timing variations | 2011 | planet b & c | |
| HU Aquarii | white dwarf+M4.5V star | 4.5 | 5.4 | eclipse timing variations | 2011 | planet b & c | |
| RR Caeli (AB) | white dwarf+dM star | 4.2 | 5.3 | eclipse timing variations | 2012 | planet b | |
| SDSS J1208+3550 | single | 9.5 | 0.00213 | timing | 2013 | orbits its star in slightly less than an hour | |
| SDSS J1730+5545 | single | 6 | 0.00139 | timing | 2014 | orbits its star in 35 minutes. | [42] [43] |
| DE Canum Venaticorum | white dwarf+M3V star | 12.0293 | 5.75 | eclipse timing variations | 2018 | has a size of 1.1 R$_J$ | [44] [45] |
| Candidates ||||||||
| LX Serpentis (AB) | white dwarf+M3V star | 7.5 | 9.1 | timing | 2016 | also known as Stepanian's Star | [46][47] [48] |
| DW Ursae Majoris | white dwarf+M3V star | 10.06 | 5.8 | timing | 2016 | accretion disk in the system | |
| GK Virginis | white dwarf+red dwarf | 0.95 | 7.38 | timing | 2020 | eclipsing binary | |
| KPD 0005+5106 | X-ray single | 1 | | timing | 2021 | Jupiter-analogue, has the same exact size and mass of Jupiter. | |
| RR Caeli (AB) | white dwarf+dM star | 2.7 | 9.7 | timing | 2021 | planet c | |
| PSR J0337+1715 (AB) b | pulsar+2 white dwarfs | 0.03 | | pulsar timing | 2022 | probably similar to Neptune or Uranus. | |

### List of transiting debris or minor planets

| System name | Metal pollution | Type of transiting object | Semi-major axis (R$_☉$) | Discovery method | Discovery Year | Note |
| WD 1145+017 | yes | minor planet | 1.16 | transiting | 2015 | |
| SDSS J1228+1040 | yes | no transiting object | 0.73 | variable Calcium absorption line | 2019 | planetesimal might orbit within the debris disk of the white dwarf |
| WD 0145+234 | yes | no transiting object | 1.29 | tidal disruption event | 2019 | one asteroid disrupted in 2018 |
| ZTF J0139+5245 | yes | debris cloud | 77.4 | transiting | 2020 | highly eccentric orbit (e>0.97) |
| ZTF J0328-1219 | yes | 2 debris clumps | b: 2.11 c: 2.28 | transiting | 2021 | |
| SDSS J0107+2107 | yes | debris | | transiting | 2021 | |
| ZTF J0347−1802 | | debris | | transiting | 2021 | transit duration of about 70 days |
| ZTF J0923+4236 | | debris | | transiting | 2021 | period in the order of days, variation in the order of hours, vast long-term variation of transit numbers and depth |
| SBSS 1232+563 | yes | debris | | transiting | 2021 | deep, but sporadic dips, had an about 8-month long nearly 50% deep transit for most of 2023, orbital period of debris might be 14.8 hours |
| WD 1054-226 | yes | many debris clouds | 3.69 | transiting | 2022 | disk detected in transit, variable with a period of 25.02 hours |
| WD J0923+7326 | yes | debris | | transiting | 2025 | Long and short-term variability with the strongest variability in the sample. |
| WD J1013−0427 | yes | fine grained debris | | transiting | 2025 | Also shows calcium emission lines, indicative of a thick eccentric gas disk. Also shows reddening during the dip, indicative of small grain dust grains (radius ≤0.3 μm). One long dip, lasting two years. Recurrence of the transit limited to 20 years. Transit either caused by the collision of two planets at 6 AU or a precessing disk (similar to SDSS J1228+1040). Helium-dominated atmosphere, with H, Ca, Si and Mg. Will be studied in another paper in detail. |
| WD J1237+5937 | yes | debris from asteroid-fragment collision? | | transiting | 2025 | One long-timescale dip, lasting 4 months. No variability in the high-speed follow-up. The researchers suggest that the transit was caused by the collision of two asteroid fragments on an eccentric orbit, producing debris on a long-term orbit. Several metal absorption lines: Ca, Mg, Fe, Al. |
| WD J1302+1650 | yes | debris | | transiting | 2025 | One long-lasting dip feature and nearly continuous and irregular variability in follow-up (similar to WD 1054−226). Shows also hydrogen in a helium-dominated atmosphere. |
| WD J1650+1443 | yes | debris | | transiting | 2025 | Low-amplitude variability. |
| WD J1944+4557 | yes | debris | | transiting | 2025 | Sporadic, but prominent dips. Will be studied in an upcoming paper. |

## List of planetary debris around white dwarfs

About 6% of white dwarfs show infrared excess due to a disk around a white dwarf. In the past only a relative small sample of white dwarf disks was known. Due to advances in white dwarf detection (e.g. with Gaia or LAMOST) and improvement of WISE infrared catalogs with unWISE/CatWISE, the number has increased to hundreds of candidates. Therefore this list will be limited to disks with metal gas emission and notable systems.

### Notable systems with planetary debris

| System name | Host temperature (K) | Likely planetary body accreted | Infrared excess | Metal absorption lines | Discovery year | Notes and References |
| van Maanen 2 | 6,130 | | no | Ca, Fe, Mg | 1917 | first metal absorption line (calcium) discovered in a white dwarf |
| G 29-38 | 11,600 | chondritic object | yes | C, O, Mg, Si, Ca, Ti, Cr, Fe, silicates | 1987/2005 | first confirmed disk |
| GD 362 | 9,740 | asteroid with earth/Moon-like composition | yes | Ca, Na, Mg, Al, Si, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Sr | 2005 | second confirmed disk |
| WD 1425+540 | 14,490 | exo-Kuiper Belt Object | no | C, N, O, Mg, Si, S, Ca, Fe, Ni | 2017 | first nitrogen detected in a white dwarf, likely an exo-KBO |
| SDSS 1557 | 21,800 | object larger than 4 km | yes | Mg, Ca, Si | 2011/2017 | white dwarf with a brown dwarf in a ultra-short orbit (2.27 hrs) and a circumbinary disk around the binary |
| WD J2356−209 | 4,040 | sodium-rich body? | no | Na, Mg, Ca, Fe | 2001/2019 | strong and broad sodium feature |
| WD J1644–0449 | 3,830 | meteoritic composition, except for Lithium | no | Li, Na, K, Ca | 2021 | one of the first detection of lithium and potassium in a white dwarf, similar discoveries at the same time |
| WD 2317+1830 | 4,210 or 4,557 | primitive planetesimal | yes | Li, Na, Ca | 2021 | Coldest and oldest (9.5 Gyrs) white dwarf with a detected disk. Also one of the most massive white dwarfs with a disk. A newer work finds higher temperature and lower age (6.4 Gyrs). |
| LSPM J0207+3331 | 6,120 | 2 minor planets | yes | | 2021 | disk with two components around cold white dwarf |
| GALEX J2339–0424 | 13,735 | exomoon | no | Be, O, Mg, Si, Ca, Ti, Cr, Mn, Fe | 2021 | one of two white dwarfs with the first detection of beryllium, possibly due to exomoon accretion |
| GD 424 | 16,560 | CI crondrite + water-rich body | no | O, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni | 2021 | mainly polluted by a rocky body, but also shows a large amount of trace-hydrogen, which could have come from a past accretion of a water-rich body |
| G238-44 | 20,000 | iron-rich Mercury-like object + Kuiper Belt Object | no | C, N, O, Mg, Al, Si, P, S, Ca, Fe | 2022 | unusual composition, showing that it accreted an iron-rich Mercury-like object and an icy KBO |
| WD 1054–226 | 7,910 | | no | Mg, Al, Ca, Fe | 2022 | disk detected in transit |
| WD J2147–4035 | 3,048 | | no | Na, K, Li, C? | 2022 | coldest white dwarf with metal-pollution, with a cooling age of 10 Gyrs, magnetic white dwarf |
| WD 0956+5912 | 8,720 | Moon-sized object | no | Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni | 2023 | recent accretion of a Moon-sized object |
| PHL 5038 | 7,525 | | no | Ca | 2009/2024 | brown dwarf around the white dwarf is likely responsible for scattering a minor planet towards the white dwarf, first such system discovered |
| WD 0816–310 | 6,250 | Vesta-sized object, likely chrondritic | no | Na, Mg, Ca, Cr, Mn, Fe, Ni | 2024 | First observation of metals being guided by magnetic fields towards the magnetic poles |
| SBSS 1612+554 (J1613+5521) | 12,000 | 3x10$^{19}$ g of material (about the mass of 243 Ida) | yes | silicates | 2019/2025 | Strongest silicate feature around any star or white dwarf detected (as of January 2025). Ongoing collisions must produce sub-micron sized particles to explain the feature. |
| GD 85 (J0719+4021) | 17,000 | | yes | possibly Ca?, glassy silica | 1988/2025 | One of three white dwarfs with glassy or amorphous silica detected. Indicating a high-temperature process and rapid cooling. Proposed formation processes include the formation of obsidian, tektites or processes involving the production and re-condensation of SiO gas. |
| UCAC4 077-007106 (J0707−7438) | 17,000 | | yes | iron?, alloys? | 2025 | Probably dominated by metallic iron and alloys. One of the hottest debris with a temperature of 2040 Kelvin. |

### Gaseous disks

| System name | Host temperature (K) | Disk inner radius (radius white dwarf = Rwd) | Disk outer radius (Rwd) | Infrared excess | Metal absorption lines | Metal emission lines | Disk discovery year | Notes and References |
| WD 1226+110 | 22,020 | 26 | 93 | yes | Mg, Ca, Si, O, C | Ca, Fe | 2006/2009 | has minor planet |
| WD 1041+091 | 17,912 | 18 | 38 | yes | C, O, Mg, Al, Si, P, S, Ca, Fe, Ni | Ca | 2007 | possibly differentiated carbonate-rich body |
| WD 0738+1835 | 13,600 | 12 | 21 | yes | O, Na, Mg, Si, Ca, Fe | Ca | 2010 | Ceres-sized body with bulk-earth composition |
| WD 0842+231 | 18,600 | 13 | 187 | yes | H, C, O, Si, Fe, Mg, Al, Ca, Cr, Mn, Ni | Ca | 2010 | object enhanced in iron, nickel, and maybe carbon, at least 100 km in diameter, eccentric disk, possibly maintained by a planet |
| WD 0959-0200 | 13,280 | 10 | 25 | yes | Mg, Ca | Ca | 2012 | |
| WD 1349-230 | 17,000 | 13 | 35 | yes | Ca | Ca | 2012 | |
| WD 1617+1620 | 13,432 | 9 | 20 | yes | | Ca | 2012 | |
| WD 1344+0324 | 26,071 | 90 | 105 | yes | | Ca | 2017 | coldest debris disk discovered at the time |
| WD 0145+234 | 13,000 | 13? | 24? | yes | | Ca, carbonates? | 2019 | TDE of a minor planet, might had water in the past |
| WD 0006+2858 | 26,000 | 20 | 64 | yes | C, O, S, P, Mg, Al, Si, Ca | Ca, O, Fe, Mg, Fe, Si | 2020 | |
| WD 0347+1624 | 20,620 | | | yes | Ca, Mg, Al | Ca, O, Fe | 2020 | |
| WD 0510+2315 | 21,700 | | | yes | O, S, Mg, Al, Si, Ca | O, Mg, Ca, Fe | 2020 | |
| WD 0611-6931 | 16,550 | 10 | 165 | yes | Ca, C, O, S, P, Mg, Al, Si, Fe, Ni | Ca, O, Fe, Si, Na, Mg | 2020 | |
| WD 0644-0352 | 20,850 | | | yes | Ca, H, O, Mg, Al, Si, Ti, Cr, Fe | Ca | 2020 | possibly some water in the parent body |
| WD 1622+5840 | 19,560 | | | yes | Ca, H, C, O, S, P, Mg, Al, Si, Fe, Ni | Ca, O, Fe | 2020 | |
| WD 2100+2122 | 25,320 | 33 | 57 | yes | Ca, Mg, Al, Si, Fe | Ca, Fe, O, Mg, Si | 2020 | |
| WD 0846+5703 | 17,803 | | | yes | Si, Mg | Ca, Mg, Fe | 2021 | exceptionally strong infrared excess |
| WD 0234-0406 | 12,454 | | | yes | Mg, O, Ca, Al, Ti, Fe | Ca, Mg/Fe | 2021 | possibly water containing object accreted |
| WD 0529-3401 | 23,197 | | | yes | Mg, Si, Ca | H, Ca, Mg, O, Fe | 2021 | strong suggestion of water-containing body due to emission of H, O |
| WD 1930-5028 | 13,306 | | | yes | Mg, Ca | Ca, Mg, Fe | 2021 | |
| WD 2133+2428 | 29,282 | | | yes | | Ca, O | 2021 | hottest white dwarf with a gaseous disk |
| WD 2212-1352 | 13,454 | | | yes | Mg, Si, C, Ca, Al, Fe | Ca, Mg, Fe | 2021 | |
| WD J1013−0427 | 21,900 | 18.2 | 47.9 | no | H, Ca, Si, Mg | Ca | 2025 | Also shows transiting debris. |