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    Scientists Reveal Jupiter Grew in Different, Distinct Phases

    By Julia Venturini, University Of ZurichNo Comments5 Mins Read
    Jupiter Grew in Different, Distinct Phases
    This is Jupiter’s southern hemisphere photographed by NASA’s Juno spacecraft. Credit: NASA/JPL-Caltech/SwRI/MSSS/GeraldEichstaedt/Sean Doran

    With an equator diameter of around 143,000 kilometers (89,000 miles), Jupiter is the largest planet in the solar system and has 300 times the mass of the Earth. The formation mechanism of giant planets like Jupiter has been a hotly debated topic for several decades. Now, astrophysicists of the Swiss National Center of Competence in Research (NCCR) PlanetS of the Universities of Bern and Zürich and ETH Zürich have joined forces to explain previous puzzles about how Jupiter was formed and new measurements. The research results were published in the journal Nature Astronomy.

    “We could show that Jupiter grew in different, distinct phases,” explains Julia Venturini, postdoc at the University of Zürich. “Especially interesting is that it is not the same kind of bodies that bring mass and energy,” adds Yann Alibert, Science Officer of PlanetS and first author of the paper.

    First, the planetary embryo rapidly accreted small, centimeter-sized pebbles and quickly built a core during the initial one million years. The following two million years were dominated by slower accretion of larger, kilometer-sized rocks called planetesimals. They hit the growing planet with great energy, releasing heat.

    “During the first stage the pebbles brought the mass,” Yann Alibert explains: “In the second phase, the planetesimals also added a bit of mass, but what is more important, they brought energy.” After three million years, Jupiter had grown to a body of 50 Earth masses. Then, the third formation phase started dominated by gas runaway accretion leading to today’s gas giant with more than 300 Earth masses.

    Jupiter Grew in Distinct Phases
    Stage 1 (up to 1 Myr): Jupiter (black) grows by pebble accretion (small circles), and planetesimal accretion is negligible. Large primordial planetesimals (large circles) are excited by the growing planet and suffer high collision velocities (large arrows), leading to destructive collisions (yellow), which produce small, second-generation planetesimals (medium circles). Stage 2 (1–3 Myr): Jupiter is massive enough to prevent pebble accretion. The energy associated with the accretion of small planetesimals is large enough to prevent rapid gas accretion (grey arrows). Stage 3 (after 3 Myr): Jupiter is massive enough to accrete large amounts of gas (hydrogen, helium). Nearby pebbles and small planetesimals can be gravitationally captured. Ultimately, a gap (white) is opened in the solar nebula, stopping further gas accretion. Red and blue indicate the two reservoirs of small bodies (inside and outside Jupiter’s orbit, respectively), which are separated by Jupiter’s growth in stage 2 and reconnected in stage 3. The Sun is shown on the left.

    Solar system divided into two parts

    The new model for Jupiter’s birth matches the meteorite data that were presented at a conference in the US last year. At first, Julia Venturini and Yann Alibert were puzzled when they listened to the results. Measurements of the composition of meteorites showed that in the primordial times of the solar system the solar nebula was divided into two regions during two million years. It could therefore be concluded that Jupiter acted as a kind of a barrier when it grew from 20 to 50 Earth masses.

    During this period, the forming planet must have perturbed the dust disk, creating an over-density that trapped the pebbles outside of its orbit. Therefore, material from outward regions could not mix with material of the inner ones until the planet reached enough mass to perturb and scatter rocks inwards.

    “How could it have taken two million years for Jupiter to grow from 20 to 50 Earth masses?” asked Julia Venturini. “That seemed much too long,” she explains: “That was the triggering question that motivated our study.” A discussion by email started among NCCR PlanetS researchers of the Universities of Bern and Zürich and ETH Zürich and the following week the experts in the fields of astrophysics, cosmochemistry and hydrodynamics arranged a meeting in Bern. “In a couple of hours we knew what we had to calculate for our study,” says Yann Alibert: “This was only possible within the framework of the NCCR, which links scientists from various fields.”

    Explanation for delayed growth

    With their calculations, the researchers showed that the time the young planet spent in the mass range of 15 to 50 Earth masses was indeed much longer than previously thought. During this formation phase, the collisions with the kilometer-sized rocks provided enough energy to heat the gaseous atmosphere of the young Jupiter and prevented rapid cooling, contraction and further gas accretion.

    “Pebbles are important in the first stages to build a core quickly, but the heat provided by planetesimals is crucial to delay gas accretion so that it matches the timescale given by the meteorite data,” the astrophysicists summarize.

    They are convinced that their results provide as well key elements for solving long-standing problems of the formation of Uranus and Neptune and exoplanets in this mass regime.

    Reference: “The formation of Jupiter by hybrid pebble–planetesimal accretion” by Yann Alibert, Julia Venturini, Ravit Helled, Sareh Ataiee, Remo Burn, Luc Senecal, Willy Benz, Lucio Mayer, Christoph Mordasini, Sascha P. Quanz and Maria Schönbächler, 27 August 2018, Nature Astronomy.
    DOI: 10.1038/s41550-018-0557-2

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