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When a planet or brown dwarf enters a star’s outer atmosphere, drag and gravitational forces can strip away orbital energy and send the companion spiraling inward. The encounter can heat and disturb the star’s gas, eject material that later cools into dust, and destroy or partially vaporize the companion. But engulfment does not always mean the companion is destroyed: the outcome depends on the companion, its orbit, and the star’s stage of evolution.

What “swallowing” means

In astronomy, a star swallows a companion when it expands around it or when the companion’s orbit decays until it enters the star’s atmosphere or envelope. Once inside, the companion moves through dense gas. Drag and gravitational interactions transfer orbital energy and angular momentum to the star and surrounding material, often causing the companion to spiral farther inward.

The result is not necessarily a dramatic stellar explosion. An engulfment can produce a comparatively faint transient, and the companion’s fate may range from disruption or vaporization to partial survival. Some stellar gas may be expelled; as it cools, it can form dust and glow in infrared light.

How a planet-engulfment event can unfold

  1. The orbit changes. A companion can be engulfed as its star expands late in life, or it can gradually lose orbital energy and move inward while the star is still relatively compact.
  2. The companion reaches the atmosphere. As it grazes or enters the star’s outer layers, drag and gravitational interaction accelerate the inward spiral.
  3. Energy is deposited in the star and gas. The encounter heats and rearranges nearby material. Some of the star’s outer gas may be thrown outward, while the companion may be disrupted or partly vaporized.
  4. The aftermath emits light. Hot gas and expanding, cooling dust can produce optical and infrared signals. Those emissions allow astronomers to reconstruct what may have happened, but they are not a direct recording of the companion’s final moments.

What astronomers inferred from ZTF SLRN-2020

ZTF SLRN-2020, about 12,000 light-years away in the Milky Way, is a prominent observed candidate for planetary engulfment. The Zwicky Transient Facility detected an optical flash, while NEOWISE data showed infrared brightening about a year earlier, consistent with dust. The 2023 discovery paper interpreted the faint optical outburst and long-lasting infrared emission as a planet-engulfment event. Its estimated optical luminosity was about 1035 erg s−1, and its estimated radiated energy was about 6.5 × 1041 erg. Those study-specific estimates led the authors to infer a companion below roughly ten Jupiter masses; they are not universal values for engulfment events. The discovery paper.

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Webb’s 2025 follow-up changed the favored explanation for how the planet reached the star. MIRI found that the star was not bright enough to be the swollen red giant initially proposed as the cause. Instead, the observations support an interpretation in which a close-in planet’s orbit decayed over millions of years until it grazed the stellar atmosphere and plunged inward. NIRSpec detected a hot circumstellar disk of molecular gas, including carbon monoxide, closer to the star, with cooler dust expanding farther out. This sequence is a reconstruction from observations and models, not direct footage of the event. Webb’s follow-up report.

Can a brown dwarf survive being engulfed?

It is possible, though one reported case cannot establish how often it happens. A 2006 Nature paper described WD 0137–349, a white dwarf with a brown dwarf in a close orbit. The authors concluded that the brown dwarf had been engulfed by the star’s red-giant progenitor and that the interaction had little effect on it. This is evidence that a brown dwarf can survive engulfment, not proof that all brown dwarfs do. The 2006 study.

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Surviving a red giant is not the same as surviving engulfment

NASA’s 2026 Webb report on WD 1856 b describes a Jupiter-sized planet that likely remained on a wide orbit while its star was a red giant, then migrated inward after the star became a white dwarf. In that proposed history, the planet survived the star’s red-giant phase by staying far away; it was not swallowed and then recovered. NASA’s report on WD 1856 b.

Why outcomes vary

No single case determines what happens in every system. The outcome depends on interacting properties:

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  • Companion mass and structure: a planet and a brown dwarf are not interchangeable, and their ability to withstand heating and disruption differs.
  • Starting orbit: the initial distance and the rate of orbital decay affect how and when the companion enters the star.
  • Stellar evolution: the star’s size and evolutionary stage determine whether it expands around a companion or the companion spirals into its atmosphere.
  • Energy and angular momentum transfer: how much of the companion’s orbital energy and angular momentum reaches the star and nearby gas helps shape the aftermath.

The cases above also rely on different kinds of evidence: transient light and infrared emission for ZTF SLRN-2020, a close brown dwarf orbiting a white dwarf for WD 0137–349, and an inferred history of later migration for WD 1856 b. They are not directly comparable experiments.

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What the published 8% figure does—and does not—mean

A 2024 Nature study identified at least seven instances of planetary ingestion using chemical-abundance evidence in a homogeneous sample of 91 co-natal stellar pairs. That is the study’s sample result, sometimes summarized as 8%; it is not a finding that exactly 8% of all stars have swallowed planets. The 2024 study.

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