Может ли Земля пережить фазу красного гиганта Солнца, и как жить, когда Солнце станет белым карликом

Scientific Concepts and Nature/Space Phenomena in the Subtitles

Evolution of the Sun into a Red Giant

• Timeline: The Sun enters the red giant phase in “a few billion years” (described as ~5 billion years in some instances, and “a few billion” in others).
• Fuel/Energy Sources:
  • Hydrogen → helium synthesis capacity is exhausted.
  • The star accumulates helium, then begins energy-producing synthesis of carbon (with emphasis on carbon; other heavier elements like nitrogen and oxygen are also mentioned).
• Expansion and Heating:
  • Greater energy release causes the Sun to expand and heat its outer layers.
  • Outer atmospheric/peripheral regions reach plasma temperatures around ~3,000 K (as stated).
• Mass Loss (“Irruptive”/Irruptive Star):
  • High-speed ejected particles/plasma are described as leaving the stellar surface.
  • Betelgeuse is given as an example of a star undergoing strong mass loss, producing surrounding gas described as “fog” or a nebula-like envelope.
  • This is framed as an irruptive phenomenon: the star sheds mass and forms circumstellar material.

Fate of Earth During and After the Red Giant Stage

• Qualitative model (competing effects):
  • The Sun’s expansion tends to move the “danger zone” outward.
  • Mass loss reduces the Sun’s gravity; if Earth conserves angular momentum, Earth’s orbital radius increases.
• Quantitative claim (theorists’ result):
  • A named group of theorists (from a Belgian Catholic University, mentioned at the institutional level) models the process and concludes Earth is likely to end up in a safer orbital region, potentially outside the Sun’s shrunken surface once it begins contracting.

White Dwarf Formation and Its Properties

• Formation: After the red giant phase, the Sun becomes a white dwarf as nuclear reactions shut down.
• Size scale (as given):
  • Radius ~ 6,000 km, about 100× smaller than the current Sun.
• Composition/State:
  • Described as hot plasma made of carbon nuclei and electrons.
• Cooling:
  • Nuclear reactions stop because the star no longer reaches the pressure and temperature required for fusion beyond carbon.
  • Cooling is extremely slow.
  • The subtitles mention:
    • Initial surface temperatures around ~100,000 K,
    • Cooling that takes up to roughly 10^15 years (stated as “one thousand trillion years”),
    • A long period of illumination lasting for any hypothetical planet.

Habitability Implications for an Earth-Like Planet Around a White Dwarf

• Radiative environment:
  • The subtitles estimate Earth’s equilibrium temperature changes:
    • Current ~ 300 K,
    • Future potentially ~ 1,000 K (about 3× higher), if atmospheric protection is sufficient.
• Long-lived stable illumination:
  • Because white dwarfs cool very slowly, the subtitles argue there could be trillions of years of relatively stable conditions—supportive of long-term civilization timescales.
• Reference to known systems:
  • The subtitles claim white dwarfs with planetary systems have been found.
  • An example described is an ultra-close, ultra-hot “Jupiter” (analogously larger than the white dwarf) with equilibrium temperatures of several thousand Kelvin.

Overall “Story Arc” Described

• Avoiding engulfment: Earth may avoid being swallowed during the Sun’s red giant phase due to orbital expansion driven by the Sun’s reduced gravity as it loses mass.
• A new orbital era: Later, Earth would orbit (or be located relative to) a white dwarf, which emits strongly at first but cools extremely gradually—potentially allowing very long-duration habitable conditions depending on atmosphere and orbital distance.

---

Researchers or Sources Featured (As Named in the Subtitles)

• A group of theorists from the Belgian Catholic University (the institution is named; no individuals are listed).
• Betelgeuse (used as an astrophysical example of a mass-losing star, not as a person).