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 nameHost starMass of planet ()Semi-majoraxis (au)Discovery methodDiscoveryyearNoteReferenceWD 0806-661single1.5-82500direct imaging2011WD 0806-661 B can be interpreted as either a sub-brown dwarf or an exoplanet.WD J0914+1914metal-polluted singledetection of accreted planet material via spectroscopy2019likely ice giantWD 1856+534single>0.840.019transiting2020the white dwarf co-moves with G 229-20 A/BMOA-2010-BLG-477Lsinglemicrolensing2012/2021a Jupiter-analogueKMT-2020-BLG-0414singlemicrolensing2021/20241.9 earth-mass planet, also has a brown dwarf at 22 auQZ Serpentiswhite dwarf+K4 star0.630.019detection via "very long photometric period" (VLPP)2022has an orbital period of 1 day.

List of candidate exoplanets System nameHost starStatusMass of planet ()Semi-major axis (au)Discovery methodDiscovery yearNoteReferenceGD 356singlerejected candidate<12variability and missing IR-excess2010115 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 modelGD 140singlesuspectedanomaly in the Hipparcos-Gaia proper motion2019mass is estimated for separation of 5 AU, to be observed with JWSTLAWD 37singlesuspectedanomaly in the Hipparcos-Gaia proper motion2019mass is estimated for separation of 5 AU, to be observed with JWSTGD 394metal-polluted singlecandidateEUV variability2019either 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 dwarfWD 0141-675metal-polluted singlecandidateGaia DR3 stellar multiples/radial velocity2023rejected due to software error 33.65 ± 0.05 day period. ESPRESSO radial velocity observations however possibly detects a planet with a 16 day periodWD 1202−232 (LP 852-7)metal-polluted singlerejected candidate1–711.47direct imaging2024similar to solar system giant planets in age and separation, no common proper motion and therefore faint background galaxyWD 2105−82 (LAWD 83)metal-polluted singlecandidate<4infrared excess2025first multi-planet system if confirmed, emission by a disk possible, but planet interpretation is seen more likely, confirmed common proper motion of the excessrejected candidate1–234.62direct imaging2024similar to solar system giant planets in age and separation, no common proper motion and therefore faint background galaxyGALEX J071816.4+373139massive singlecandidate3.6infrared excess2024planet candidate has a temperature of about 400 KWD 0310-688 (CPD-69 177)metal-polluted singlecandidate0.1-2infrared excess2024planet candidate has a temperature of KHS 0209+0832metal-polluted singlecandidatedetection of accreted planet material via spectroscopy2024metals in agreement with second-generation giant planet, period of 4.4 days from TESS, enriched in zinc, copper and niobiumSirius Bwhite dwarf+A0V starcandidate1.50.9astrometry2024has a mass range of 0.8-2.4 Jupiter masses.WD 2226-210singlecandidate0.034transiting2024orbits the central white dwarf of the Helix Nebula, has a radius of 1 or 2.3 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. WD 2149+021 (EGGR 150)metal-polluted singlecandidate<8infrared excess2025emission by a disk possible, but planet interpretation is seen more likelyMEAD 62 (2MASS J09424023-4637176)singlecandidate40direct imaging2025cold exoplanet or brown dwarf, would have orbited at 18 AU during the main-sequence, Y dwarf candidateWD 0644+025metal-polluted singlecandidate6.8infrared excess2026around a massive white dwarf with metal pollution, could also be infrared excess from a disk, but disk models produce a poor fit.

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 nameHost starMass of planet ()Semi-majoraxis (au)Discovery methodDiscoveryyearNoteReferencePSR B1620-26white dwarf+pulsar23pulsar timing1993DP Leoniswhite dwarf+donor star6.288.19eclipse timing variations2009has a size of NN SerpentisPCEB: white dwarf+red dwarfeclipse timing variation2010PCEB is surrounded by a dusty disk, might be only one planetUZ Fornaciswhite dwarf+red dwarf6.35.9eclipse timing variations2011planet b & c7.72.8HU Aquariiwhite dwarf+M4.5V star5.93.6eclipse timing variations2011planet b & c4.55.4RR Caeli (AB)white dwarf+dM star3.05.2eclipse timing variations2021planet b2.79.7planet cSDSS J1208+3550single9.50.00213timing2013orbits its star in slightly less than an hourSDSS J1730+5545single60.00139timing2014orbits its star in 35 minutes.DE Canum Venaticorumwhite dwarf+M3V star12.02935.75eclipse timing variations2018has a size of CandidatesLX Serpentis (AB)white dwarf+M3V star7.59.1timing2016also known as Stepanian's StarDW Ursae Majoriswhite dwarf+M3V star10.065.8timing2016accretion disk in the systemGK Virginiswhite dwarf+red dwarf0.957.38timing2020eclipsing binaryKPD 0005+5106X-ray single1timing2021Jupiter-analogue, has the same exact size and mass of Jupiter.PSR J0337+1715 (AB) bpulsar+2 white dwarfs0.03pulsar timing2022Similar in mass to Neptune's moon Triton

List of transiting debris or minor planets System nameMetalpollutionType oftransiting objectSemi-majoraxis ()Discovery methodDiscoveryYearNoteRef.WD 1145+017yesminor planet1.16transiting2015SDSS J1228+1040yesno transiting object0.73variable Calcium absorption line2019planetesimal might orbit within the debris disk of the white dwarfWD 0145+234yesno transiting object1.29tidal disruption event2019one asteroid disrupted in 2018ZTF J0139+5245yesdebris cloud77.4transiting2020highly eccentric orbit (e>0.97)ZTF J0328-1219yes2 debris clumpsb: 2.11c: 2.28transiting2021SDSS J0107+2107yesdebristransiting2021ZTF J0347−1802debristransiting2021transit duration of about 70 daysZTF J0923+4236debristransiting2021period in the order of days, variation in the order of hours, vast long-term variation of transit numbers and depthSBSS 1232+563yesdebristransiting2021deep, 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 hoursWD 1054-226yesmany debris clouds3.69transiting2022disk detected in transit, variable with a period of 25.02 hoursWD J0923+7326yesdebristransiting2025Long and short-term variability with the strongest variability in the sample.WD J1013−0427yesfine grained debristransiting2025Also 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+5937yesdebris from asteroid-fragment collision?transiting2025One 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+1650yesdebristransiting2025One 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+1443yesdebristransiting2025Low-amplitude variability.WD J1944+4557yesdebristransiting2025Sporadic, 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