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  2. Frost line (astrophysics) - Wikipedia

    en.wikipedia.org/wiki/Frost_line_(astrophysics)

    The frost line therefore separates terrestrial planets from giant planets in the Solar System. [12] However, giant planets have been found inside the frost line around several other stars (so-called hot Jupiters). They are thought to have formed outside the frost line, and later migrated inwards to their current positions.

  3. Solar System - Wikipedia

    en.wikipedia.org/wiki/Solar_System

    The boundary in the Solar System beyond which those volatile substances could coalesce is known as the frost line, and it lies at roughly five times the Earth's distance from the Sun. [5] Orbits Animations of the Solar System's inner planets orbiting.

  4. Origin of water on Earth - Wikipedia

    en.wikipedia.org/wiki/Origin_of_water_on_Earth

    The boundary of the region where ice could form in the early Solar System is known as the frost line (or snow line), and is located in the modern asteroid belt, between about 2.7 and 3.1 astronomical units (AU) from the Sun. [23] [24] It is therefore necessary that objects forming beyond the frost line–such as comets, trans-Neptunian objects ...

  5. Formation and evolution of the Solar System - Wikipedia

    en.wikipedia.org/wiki/Formation_and_evolution_of...

    The Solar System travels alone through the Milky Way in a circular orbit approximately 30,000 light years from the Galactic Center. Its speed is about 220 km/s. The period required for the Solar System to complete one revolution around the Galactic Center, the galactic year, is in the range of 220–250 million years. Since its formation, the ...

  6. Accretion (astrophysics) - Wikipedia

    en.wikipedia.org/wiki/Accretion_(astrophysics)

    However, Jovian planets began as large, icy planetesimals, which then captured hydrogen and helium gas from the solar nebula. [32] Differentiation between these two classes of planetesimals arise due to the frost line of the solar nebula. [33]

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  8. Hot Jupiter - Wikipedia

    en.wikipedia.org/wiki/Hot_Jupiter

    In the migration hypothesis, a hot Jupiter forms beyond the frost line, from rock, ice, and gases via the core accretion method of planetary formation. The planet then migrates inwards to the star where it eventually forms a stable orbit. [19] [20] The planet may have migrated inward smoothly via type II orbital migration.

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