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Yes. A planet can survive its star’s transformation into a white dwarf if it avoids being engulfed during the star’s red-giant phase. Its orbit may later change, and other bodies in the system can be scattered toward the white dwarf and torn apart. Observed systems show both a planet around a white dwarf and evidence of disrupted planetary material—but those are different kinds of evidence.
How a planet can survive its star’s transformation
A Sun-like star eventually exhausts the hydrogen fuel in its core, expands into a red giant, sheds its outer layers, and leaves behind a hot, compact white dwarf. The expanded star can engulf nearby planets. A planet farther out may avoid the red-giant envelope and remain bound after the star sheds mass. NASA’s overview of white dwarf evolution describes this broader process and the debris that can remain around the remnant: NASA Science’s “Chapter 7: Death and New Life”.
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Avoiding engulfment does not guarantee an unchanged orbit. As the star loses mass and surviving bodies interact gravitationally, orbits can shift. Planets can also redirect asteroids, comets, and other small objects inward. If those objects pass close enough to the white dwarf, tidal forces can break them apart; their material may then be accreted by the star.
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WD 1856 b: a close orbit likely reached later
WD 1856 b is a Jupiter-sized planet orbiting the white dwarf WD 1856+534, about 80 light-years away. NASA’s July 1, 2026 report gives its orbital period as 34 hours and its separation from the star as under 2 million miles (3 million kilometers). The reported mass range is four to eleven Jupiter masses, and its temperature is about 260°F (126°C). Webb transmission observations found signs of small cloud particles and hydrocarbons, most likely methane. See NASA Goddard’s report on Webb’s observations of WD 1856 b.
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Its present closeness does not mean it stayed there while its star expanded. NASA says the planet would have been destroyed at that distance during the red-giant phase. The report interprets its unexpectedly high temperature as residual heat from an earlier inward migration. The proposed timing—3 to 5.5 billion years after the star became a white dwarf—fits a scenario in which it first remained farther away, then moved inward. This is an interpretation of this system, not proof that all planets around white dwarfs migrate the same way.
MOA-2010-BLG-477Lb: a wider planetary companion
A 2022 NASA Technical Reports Server record describes microlensing observations and near-infrared follow-up that did not detect a main-sequence lens star. The authors infer a white dwarf of 0.53 ± 0.11 solar masses and a planet of 1.4 ± 0.3 Jupiter masses. The projected separation is 2.8 ± 0.5 astronomical units, implying a larger semimajor axis. The authors present the system as evidence that a planet can survive its host’s giant and asymptotic giant phases. The reported measurements and interpretation are available in the NASA Technical Reports Server record for “A Jovian analogue orbiting a white dwarf star”.
G238-44: disrupted material, not a surviving-planet detection
NASA’s report on white dwarf G238-44 describes elements in the star’s atmosphere that researchers interpret as material accreted from rocky-metallic and icy bodies. Their account points to small objects scattered inward during chaotic evolution after the star’s main-sequence phase, then torn apart by tides near the white dwarf. The report says G238-44 began capturing material from asteroid-belt-like and Kuiper-belt-like regions within 100 million years after its white dwarf phase began. This is evidence of accreted debris, not a measurement showing that an intact planet in that system survived. See NASA Goddard’s report on G238-44.
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The Sun’s eventual expansion is expected to threaten the inner planets: NASA says Mercury, Venus, and possibly Earth may be destroyed. The fate of the outer planets, especially the gas giants, is unclear. A planet’s outcome depends on its starting orbit, whether it avoids the red-giant envelope, and how the system changes as the star sheds mass and its surviving bodies interact. The white-dwarf examples do not settle the future of Jupiter or Saturn.
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How to read the evidence
- An intact planet around a white dwarf shows that planetary survival is possible, but a present-day close orbit may have been reached only after the star became a white dwarf.
- Pollution or debris around a white dwarf can reveal material from bodies that fell inward and were disrupted; it does not establish that every planet in the system was destroyed.
- System histories are inferred from observations. A planet’s present orbit, the star’s atmosphere, and models of stellar evolution provide different kinds of clues, not a complete record of every event.
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