Tidal downsizing

<p>Tidal downsizing is a hypothetical mechanism for the formation of <a href="/facts/Planets/rbPjE6Bx">planets</a>. The process begins with the formation of large clumps of gas, of roughly 10 <a href="/facts/Jupiter/95m7XjMT">Jupiter</a> masses, via <a href="/facts/Gravitational_instability/nlvV50CI">gravitational instability</a> in the outer parts of the <a href="/facts/Protoplanetary_disk/FtfSbP61">protoplanetary disk</a>. The clumps migrate inward due to gravitational interactions with the gas disk. Solid grains within the clump collide and grow and settle toward the center forming a <a href="/facts/Planetary_core/LyQ7DbAl">massive core</a>. The clump is disrupted due to <a href="/facts/Tide/zNstvWPv">tidal forces</a> or heating from the <a href="/facts/Star/PFbd6ICx">star</a> when it approaches within a few <a href="/facts/Astronomical_unit/gjsbu5xU">AU</a> of the star leaving behind a smaller object. Depending on the extent and timing of the mass loss the remnant may be a <a href="/facts/Terrestrial_planet/jpMC1ULt">terrestrial planet</a>, an <a href="/facts/Ice_giant/mJ4YTuup">ice giant</a> or a <a href="/facts/Gas_giant/pmF6KztG">gas giant</a>.
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Tidal downsizing open-in-new

Tidal downsizing