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 (MJ)	Semi-major axis (au)	Discovery method	Discovery year	Note	Reference
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.	[1][2]
WD J0914+1914	metal-polluted single		0.070 to 0.074	detection of accreted planet material via spectroscopy	2019	likely ice giant	[3]
WD 1856+534	single	>0.84[4]	0.019	transiting	2020	the white dwarf co-moves with G 229-20 A/B	[5][6][7]
MOA-2010-BLG-477L	single	1.4±0.3	2.8±0.5	microlensing	2012/2021	a Jupiter-analogue	[8]
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	[9][10]
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.	[11][12]

List of candidate exoplanets

System name	Host star	Status	Mass of planet (MJ)	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,[13] no orbiting body was detected, rejecting the idea of an unipolar inductor model[14]	[13]
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[15]	[16][17]
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[15]	[16][17]
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[18]	[18]
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[19] 33.65 ± 0.05 day period. ESPRESSO radial velocity observations however possibly detects a planet with a 16 day period[20]	[21]
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	[22]
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	[22]
GALEX J071816.4+373139	massive single	candidate	3.6		infrared excess	2024	planet candidate has a temperature of about 400 K	[23]
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	[24]
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	[25]
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]
WD 2226-210	single	candidate		0.034	transiting	2024	orbits the central white dwarf of the Helix Nebula, has a radius of 1 RJ or 2.3 R🜨	[28]
		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.	[29]

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.^[30] 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 (MJ)	Semi-major axis (au)	Discovery method	Discovery year	Note	Reference
PSR B1620-26	white dwarf+pulsar	2.5±1	23	pulsar timing	1993		[31]
DP Leonis	white dwarf+donor star	6.28	8.19	eclipse timing variations	2009	has a size of 1.14 RJ	[32]
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,[33] might be only one planet[34]	[35]
		2.28±0.38	3.39±0.10
UZ Fornacis	white dwarf+red dwarf	6.3	5.9	eclipse timing variations	2011	planet b & c	[36][37]
		7.7	2.8
HU Aquarii	white dwarf+M4.5V star	5.9	3.6	eclipse timing variations	2011	planet b & c	[38][39]
		4.5	5.4
RR Caeli (AB)	white dwarf+dM star	3.0	5.2	eclipse timing variations	2021	planet b	[40]
		2.7	9.7			planet c
SDSS J1208+3550	single	9.5	0.00213	timing	2013	orbits its star in slightly less than an hour	[41]
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 RJ	[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	[49]
GK Virginis	white dwarf+red dwarf	0.95	7.38	timing	2020	eclipsing binary	[50]
KPD 0005+5106	X-ray single	1		timing	2021	Jupiter-analogue, has the same exact size and mass of Jupiter.	[51]
PSR J0337+1715 (AB) b	pulsar+2 white dwarfs	0.03		pulsar timing	2022	probably similar to Neptune or Uranus.	[52]

List of transiting debris or minor planets

System name	Metal pollution	Type of transiting object	Semi-major axis (R☉)	Discovery method	Discovery Year	Note	Ref.
WD 1145+017	yes	minor planet	1.16[53]	transiting	2015		[54]
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	[55]
WD 0145+234	yes	no transiting object	1.29[56]	tidal disruption event	2019	one asteroid disrupted in 2018	[57]
ZTF J0139+5245	yes	debris cloud	77.4	transiting	2020	highly eccentric orbit (e>0.97)[58]	[59][60]
ZTF J0328-1219	yes	2 debris clumps	b: 2.11 c: 2.28	transiting	2021		[61][62]
SDSS J0107+2107	yes	debris		transiting	2021		[61]
ZTF J0347−1802		debris		transiting	2021	transit duration of about 70 days	[61]
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	[61][63]
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	[61][64]
WD 1054-226	yes	many debris clouds	3.69	transiting	2022	disk detected in transit, variable with a period of 25.02 hours	[65]
WD J0923+7326	yes	debris		transiting	2025	Long and short-term variability with the strongest variability in the sample.	[66]
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.	[66]
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.	[66]
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.	[66]
WD J1650+1443	yes	debris		transiting	2025	Low-amplitude variability.	[66]
WD J1944+4557	yes	debris		transiting	2025	Sporadic, but prominent dips. Will be studied in an upcoming paper.	[66]

List of planetary debris around white dwarfs

About 6% of white dwarfs show infrared excess due to a disk around a white dwarf.^[67] In the past only a relative small sample of white dwarf disks was known.^[68] 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.^[69][70][67] 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	[71] first metal absorption line (calcium) discovered[72] in a white dwarf
G 29-38	11,600	chondritic object	yes	C, O, Mg, Si, Ca, Ti, Cr, Fe, silicates	1987/2005	[68][73][74][75] 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	[68][76][77][78] second confirmed disk
WD 1425+540	14,490	exo-Kuiper Belt Object	no	C, N, O, Mg, Si, S, Ca, Fe, Ni	2017	[79] 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	[80] 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	[81][82] strong and broad sodium feature
WD J1644–0449	3,830	meteoritic composition, except for Lithium	no	Li, Na, K, Ca	2021	[83] 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[84]	yes	Li, Na, Ca	2021	[85] 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[86] finds higher temperature and lower age (6.4 Gyrs).
LSPM J0207+3331	6,120	2 minor planets	yes		2021	[87] 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	[72][88] 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	[89] 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	[90] 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	[65] disk detected in transit
WD J2147–4035	3,048		no	Na, K, Li, C?	2022	[91] 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	[92] 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	[93] First observation of metals being guided by magnetic fields towards the magnetic poles
SBSS 1612+554 (J1613+5521)	12,000	3x1019 g of material (about the mass of 243 Ida)	yes	silicates	2019/2025	[94][95] 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	[96][95] 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	[95] 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	[97][98][99][68] has minor planet
WD 1041+091	17,912	18	38	yes	C, O, Mg, Al, Si, P, S, Ca, Fe, Ni	Ca	2007	[100][68][101] possibly differentiated carbonate-rich body
WD 0738+1835	13,600	12	21	yes	O, Na, Mg, Si, Ca, Fe	Ca	2010	[102][103][68] 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	[104][105][68] 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	[106][68]
WD 1349-230	17,000	13	35	yes	Ca	Ca	2012	[107][108][103][68]
WD 1617+1620	13,432	9	20	yes		Ca	2012	[109][103][68]
WD 1344+0324	26,071	90	105	yes		Ca	2017	[110] coldest debris disk discovered at the time
WD 0145+234	13,000	13?	24?	yes		Ca, carbonates?	2019	[111][57][112] 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	[111][113][114]
WD 0347+1624	20,620			yes	Ca, Mg, Al	Ca, O, Fe	2020	[115][113]
WD 0510+2315	21,700			yes	O, S, Mg, Al, Si, Ca	O, Mg, Ca, Fe	2020	[111][113]
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	[115][111][113]
WD 0644-0352	20,850			yes	Ca, H, O, Mg, Al, Si, Ti, Cr, Fe	Ca	2020	[115][113][111] 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	[115][111][113]
WD 2100+2122	25,320	33	57	yes	Ca, Mg, Al, Si, Fe	Ca, Fe, O, Mg, Si	2020	[115][113][114]
WD 0846+5703	17,803			yes	Si, Mg	Ca, Mg, Fe	2021	[116] exceptionally strong infrared excess
WD 0234-0406	12,454			yes	Mg, O, Ca, Al, Ti, Fe	Ca, Mg/Fe	2021	[116] possibly water containing object accreted
WD 0529-3401	23,197			yes	Mg, Si, Ca	H, Ca, Mg, O, Fe	2021	[116] strong suggestion of water-containing body due to emission of H, O
WD 1930-5028	13,306			yes	Mg, Ca	Ca, Mg, Fe	2021	[116]
WD 2133+2428	29,282			yes		Ca, O	2021	[116] hottest white dwarf with a gaseous disk
WD 2212-1352	13,454			yes	Mg, Si, C, Ca, Al, Fe	Ca, Mg, Fe	2021	[116]
WD J1013−0427	21,900	18.2	47.9	no	H, Ca, Si, Mg	Ca	2025	[66] Also shows transiting debris.

See also

• Confirmed brown dwarf orbiting stellar remnants
• List of white dwarfs
• Timeline of white dwarfs, neutron stars, and supernovae
• List of exoplanet extremes
• List of exoplanet firsts