Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars

By S. Kenyon, B. Bromley. 2008

190 citations recorded by the source corpus.

We describe calculations for the formation of icy planets and debris disks at 30-150 AU around 1-3 M☉ stars. Debris disk formation coincides with the formation of planetary systems. As protoplanets grow, they stir leftover planetesimals to large velocities. A cascade of collisions then grinds the leftovers to dust, forming an observable debris disk. Stellar lifetimes and the collisional cascade limit the growth of protoplanets. The maximum radius of icy planets, rmax ≈ 1750 km, is remarkably independent of initial disk mass, stellar mass, and stellar age. These objects contain ≲3%-4% of the initial mass in solid material. Collisional cascades produce debris disks with maximum luminosity ~2 × 10−3 times the stellar luminosity. The peak 24 μm excess varies from ~1% times the stellar photospheric flux for 1 M☉ stars to ~50 times the stellar photospheric flux for 3 M☉ stars. The peak 70-850 μm excesses are ~30-100 times the stellar photospheric flux. For all stars, the 24-160 μm excesses rise at stellar ages of 5-20 Myr, peak at 10-50 Myr, and then decline. The decline is roughly a power law, f ∝ t−n with n ≈ 0.6–1.0. This predicted evolution agrees with published observations of A-type and solar-type stars. The observed far-IR color evolution of A-type stars also matches model predictions.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bf5446c420de4fda46c1500e09aa70a3d8dec0bf

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In Astronomy and Astrophysics

Citations in the corpus

Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “Because of efficient grinding of planetesimals to dust, the planetesimal mass reservoir is reduced with time (Kobayashi et al. 2010; Kenyon & Bromley 2008).”
THE DISK POPULATION OF THE UPPER SCORPIUS ASSOCIATION (2012, background): “For instance, Carpenter et al. (2009) found that the rapid decrease in [24] fraction from A to B stars is expected because of increased ejection of dust grains by radiation pressure (see also Kenyon & Bromley 2008).”
NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, unknown): “Low mass K and M dwarfs could undergo a similar but delayed “rise and fall” of debris disk brightness, peaking at ages of 30–50 Myr (e.g. NGC 2547, Forbrich et al. 2008; Kenyon & Bromley 2008).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, methodology): “We refer the reader to Beauge & Aarseth (1990) and Kenyon & Bromley (2008) and references therein.”
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS (2009, unknown): “The medium-mass nebulae allow us to verify that our calculations of planet formation efficiency are consistent with previous studies of both core accretion and gravitational instability (e.g. Laughlin et al. 2004; Kenyon & Bromley 2008; Kratter et al. 2008; Stamatellos & Whitworth 2009).”
Debris disks as signposts of terrestrial planet formation (2011, methodology): “11 of Löhne et al. 2008; Kenyon & Bromley 2008, 2010; Krivov 2010).”
Debris disc stirring by secular perturbations from giant planets (2009, methodology): “Based on extensive numerical simulations, Kenyon & Bromley (2008) find tPl = 145x −1.15 m “ a 80 AU ”3 „ 2M⊙ m⋆ «3/2 Myr.”