Earth’s surface will become uninhabitable long before the Sun finishes its evolution. Whether the planet itself is physically swallowed is less certain. Older calculations found that tides would pull Earth into the expanding Sun, while a 2026 Astronomy & Astrophysics study using updated tidal physics and observations of the near-solar-mass star L2 Pup finds that Earth likely remains outside the Sun through its red-giant and asymptotic-giant phases. That result depends on how much mass the late-stage Sun loses, a quantity that is still poorly constrained.
“Survive” therefore has two meanings: biological habitability and orbital or geological existence. The first ends much earlier; the second may continue into the white-dwarf era.
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What will happen to the Sun?
NASA describes the Sun as roughly halfway through a stellar lifetime of about 10 billion years. It is currently powered by hydrogen fusion in its core. When that core hydrogen is exhausted, the Sun will leave its present stable phase and expand dramatically.
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The red-giant phase
NASA’s educational timelines place the Sun’s transition into a red giant approximately 6 billion years from now. These are rounded evolutionary estimates, not dates that can be assigned to a particular year.
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As the core contracts and the outer layers expand, the Sun will become vastly larger and brighter. Its atmosphere will extend toward the region now occupied by the inner planets. Mercury and Venus are expected to be engulfed. Mars is generally expected to remain outside the expanded photosphere, although its environment will be radically altered.
The asymptotic-giant phase and mass loss
After the red-giant branch, the Sun will enter the asymptotic giant branch (AGB), a later phase of intense expansion and stellar-wind loss. The Sun will shed a substantial fraction of its mass. NASA states that roughly half of the Sun’s mass will eventually be expelled and that surviving outer-planet orbits could settle at about twice their present distances.
The white-dwarf remnant
Once the giant phases end, the remaining core will contract into a white dwarf. NASA describes this remnant as about Earth-sized, extremely hot and faint compared with the swollen giant that preceded it. NASA’s lifecycle pages place this white-dwarf “death” roughly 8 billion years from now, again as an approximate educational timescale.
A white dwarf no longer produces energy through ordinary hydrogen fusion. It gradually cools over immensely long periods. The Sun’s transformation is therefore not an explosion like a supernova; it is a slow sequence of expansion, envelope loss and core contraction.
Why Earth’s habitability ends before its orbit is decided
The first answer to “Will Earth survive?” is straightforward: Earth will not remain habitable at the surface. The Sun’s increasing luminosity will raise the energy received by Earth far beyond the range that supports today’s climate and oceans. During the giant phases, the expanded atmosphere and intense radiation will further disrupt the planet.
NASA states that Earth will not be habitable and that the only chance for survival would be for an advanced civilization to migrate to another planetary home. That statement concerns life and surface conditions, not whether a rocky body remains in an orbit.
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- Biological survival: Earth’s surface loses the conditions required for present-day life well before the Sun reaches maximum size.
- Atmospheric and ocean survival: Heating and interaction with the giant Sun can remove or transform the atmosphere and oceans.
- Physical survival: The rocky planet might remain as an airless, overheated body if it avoids passing through the Sun’s outer layers.
- Orbital survival: The final orbit depends on a competition between tides that remove orbital energy and mass loss that expands the orbit.
A planet can therefore “survive” in an orbital model while no longer being a living Earth.
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The orbital tug of war: tides versus mass loss
Two effects dominate calculations of Earth’s final fate, and they act in opposite directions.
Tidal interaction pulls Earth inward
When the Sun expands, its outer atmosphere becomes much closer to Earth’s orbit and exerts stronger tidal forces. Tides transfer orbital energy into motion and heat within the Sun. That drains energy from Earth’s orbit, reducing its distance from the Sun. Atmospheric drag from the extended solar envelope can add another inward force if Earth enters sufficiently diffuse outer layers.
Mass loss pushes the orbit outward
As the Sun’s wind carries mass into space, its gravitational pull weakens. A planet that is not engulfed responds by moving onto a wider orbit. In a simplified, slow-loss picture, the orbital expansion is related to the ratio of the Sun’s initial and remaining masses. Losing about half the mass can therefore move a surviving outer orbit toward roughly twice its original distance, consistent with NASA’s description.
That simple expansion is not enough to settle Earth’s case. The Sun is changing size at the same time, and the rate of mass loss varies through the red-giant and AGB phases. If tides act strongly before enough mass is removed, Earth can spiral inward. If mass is lost rapidly enough, the outward migration can keep Earth beyond the photosphere.
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|---|---|---|
| Solar mass loss | Weakens the Sun’s gravity and expands a surviving orbit | Red-giant and especially AGB mass-loss episodes |
| Tidal dissipation | Removes orbital energy and draws Earth inward | When the expanded solar envelope approaches Earth’s orbit |
| Drag in the extended envelope | Slows the planet and contributes to inward migration | If Earth enters the Sun’s dense outer atmosphere |
The outcome is sensitive to both the adopted tidal prescription and the assumed history of AGB mass loss. Changing either can change “engulfed” to “survives.”
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What the 2008 calculation predicted
A peer-reviewed calculation by K.-P. Schröder and Robert Connon Smith, published in 2008, used a tested stellar-evolution code to model the Sun’s future expansion and mass loss. Their calculation estimated that the Sun would lose 0.332 solar masses on the red-giant branch about 7.59 billion years from now.
That mass loss expands planetary orbits, but the model also included tides and drag. Its conclusion was that Earth would not escape engulfment. In the same calculation, a hypothetical planet would need to begin at roughly 1.15 astronomical units (AU)—about 15 percent farther from the Sun than Earth is now—to survive.
The 1.15-AU threshold is a result of that model’s assumptions, not a measured boundary in the real future. It illustrates how a modest change in starting distance can decide the result when inward and outward effects nearly balance.
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What the 2026 model changes
Esseldeurs, Mathis and Decin revisited the problem in a 2026 Astronomy & Astrophysics study. Their work changes two important inputs: the treatment of tides and the late-stage mass-loss rates.
Updated tidal physics
The study uses updated, ab initio prescriptions for tidal dissipation rather than relying only on older approximate treatments. With this newer tidal model, the calculations report that Earth survives both the red-giant branch (RGB) and the AGB phase. When older tidal prescriptions are retained, the same broad scenario can still end in engulfment.
An observed stellar proxy
To constrain the uncertain AGB phase, the authors use L2 Pup as an observational proxy. Its inferred initial mass is close to the Sun’s, making its measured mass-loss behavior useful for testing how a near-solar-mass star sheds its envelope late in life.
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When L2 Pup’s observed mass-loss rates are combined with the updated tidal treatment, the model gives Earth a surviving orbit through the AGB phase. The study therefore shifts the best current conditional answer toward survival outside the Sun’s photosphere.
Why the result is not final
The authors explicitly caution that the fate is not robustly determined. Low AGB mass-loss rates still produce engulfment in their calculations. Because the true late-stage solar mass-loss history cannot be observed directly, the result remains dependent on how well L2 Pup represents the future Sun and on how accurately tidal dissipation is described.
In other words, “likely survives” is not the same as “will definitely survive.” The 2026 result is a conditional update based on improved physics and an observed analogue, not a direct forecast verified by experiment.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Comparing the two model generations
| Model or assumption | Main inputs | Reported Earth outcome |
|---|---|---|
| Schröder and Smith, 2008 | Tested stellar-evolution code; 0.332 solar masses lost on the RGB; tides and drag included | Engulfment; a planet starting near 1.15 AU would be required to survive |
| Esseldeurs, Mathis and Decin, 2026, updated tides | Ab initio tidal-dissipation prescription; range of AGB mass-loss rates | Survival in the updated-tide runs, but engulfment remains possible with low AGB mass loss |
| Esseldeurs, Mathis and Decin, 2026, L2 Pup proxy | Observed mass-loss rates from a near-solar-mass evolved star combined with updated tides | Earth likely survives the RGB and AGB phases |
The disagreement is not a simple error-versus-correction story. Both outcomes arise from numerical models of a future that cannot be observed directly. The newer work narrows the plausible range by using updated tidal calculations and an evolved-star observation, while also showing that key uncertainties remain consequential.
What “surviving” Earth would be like
If Earth avoids engulfment, survival would not preserve the present planet. The surface would have undergone extreme heating, and the atmosphere and oceans would not remain in their current state. Any remnant would be a sterilized, geologically altered world orbiting a faint white dwarf.
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1Clear out junk files and repair common Windows errors2Fix the driver behind crashes, sound loss and screen glitches3Repair Windows errors before they cause bigger problemsThe post-AGB orbit would also be much wider than today’s if the planet remained gravitationally bound while the Sun lost a large fraction of its mass. A wider orbit does not restore habitability: a white dwarf supplies far less total light than the main-sequence Sun, and the planet’s atmosphere may already have been stripped or chemically transformed during the giant phases.
For this reason, the phrase “Earth survives the Sun’s death” should be read as “the planet avoids physical engulfment,” not “life continues on Earth.”
Could Earth orbit the Sun’s white dwarf?
Yes, in principle. If Earth is not swallowed and the Sun loses mass gradually enough for the orbit to remain bound, Earth can continue orbiting the compact white-dwarf remnant on an expanded path. Orbital expansion caused by mass loss is the mechanism that makes this possible.
That possibility has strict conditions. Tidal decay and drag must not remove Earth before the envelope is lost, and the mass-loss history must not differ so greatly from the assumed model that the planet crosses into the solar atmosphere. Even a surviving orbit would be the endpoint of a dead, overheated planet rather than a naturally habitable world.
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No direct experiment can test the future Sun–Earth outcome. Researchers must combine stellar-evolution calculations, orbital dynamics and observations of stars that are already in giant phases. Each ingredient carries uncertainty:
- AGB mass loss: The rate can vary sharply and determines how quickly the Sun’s gravity weakens.
- Tidal dissipation: The efficiency with which tides convert orbital energy into heat is difficult to calculate for a distended, convective stellar envelope.
- Proxy selection: L2 Pup is close to solar mass in its inferred initial state, but it is not the Sun, and its history may not match the Sun’s exactly.
- Coupled evolution: Stellar radius, mass loss, tides and orbital distance change together, so a small difference early in the calculation can alter the final outcome.
These uncertainties explain why expert statements have remained cautious. NASA astronomer Dimitri Veras has said that Mercury and Venus will be swallowed and Mars will not, while “the fate of the Earth—which resides in between—is less clear.” The 2026 study makes the survival side more plausible under its preferred assumptions but does not remove that uncertainty.
The best current answer
Earth’s surface habitability ends well before the Sun becomes a white dwarf, regardless of whether the planet is eventually engulfed. Under older tidal prescriptions, Earth is swallowed. Under the updated 2026 treatment, and especially when observed L2 Pup mass-loss rates are used as a proxy, Earth likely remains outside the Sun through the red-giant and AGB phases.
The decisive unknown is the Sun’s late AGB mass-loss history, together with the correct description of tidal dissipation. Until those inputs are better constrained, the scientifically accurate answer is conditional: Earth probably survives physically in the newer proxy-calibrated model, but its definitive fate is not settled—and it will not remain habitable in any case.
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