A model for planetesimal meltdown by 26Al and its implications for meteorite parent bodies

By P. J. Hevey, I. Sanders. 2006

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View Paper: https://www.semanticscholar.org/paper/f42d86466711271533c9a5b7f165e808672866c7

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In Astronomy and Astrophysics

Citations in the corpus

Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula (2014, methodology): “Chronological studies (Nyquist et al. 2009) and consideration of thermal history (Hevey and Sanders 2006) could provide constraints on the accretion times of meteorite parent bodies.”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “We consider a body that has differentiated into a core, mantle and crust (Hevey and Sanders 2006) and determine whether its core is susceptible to dynamo action.”
The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, methodology): “The performance of the thermal code was validated in the case of constant ψ by reproducing temperature profiles from Miyamoto et al. (1981), while profiles from Hevey & Sanders (2006) were used for validation when ψ = ψ(r).”
The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, background): “…formation within a few Ma after CAI formation is consistent with decay of 26Al as the dominant heat source facilitating melting and differentiation (Hevey and Sanders 2006), and thermal modeling of planetesimals heated internally by 26Al decay to obtain inferred core formation ages indicates that…”
Chondrules and the Protoplanetary Disk (2011, background): “Given the inferred early solar abundances of these nuclides (Table 2), any asteroid with a chondritic bulk composition larger than 20–30 km in diameter would have been melted by radiogenic heat provided that the asteroid formed <1–1.5 Myr after CAIs (Hevey & Sanders 2006, Bizzarro et al. 2005).”
Chronology of the angrite parent body and implications for core formation in protoplanets (2012, background): “Hevey and Sanders (2006) argued that in bodies heated by 26Al decay convection in the magma ocean began at 50% silicate melting, which was reached about 0.8 Myr after (instantaneous) accretion.”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, background): “For instance, a 5-km-diameter planetesimal (with 26Al/27Al = 5 × 10−5 and initial temperature T at 100 K) would reach 1,500 K in its core within ~4 × 105 years, whereas its surface would remain at T < 400 K (e.g., Ghosh et al. 2006, Hevey & Sanders 2006, LaTourette & Wasserburg 1998).”
EVIDENCE FOR MAGNESIUM ISOTOPE HETEROGENEITY IN THE SOLAR PROTOPLANETARY DISK (2011, background): “…CAI formation, the amount of energy resulting from the decay of 26Al in a body with a (26Al/27Al)0 ratio of 1 × 10−5 is ∼1.2 kJ g−1, which is 75% of the energy required to completely melt a chondritic body (Hevey & Sanders 2006); this would lead to the formation of an asteroid-wide magma ocean.”
Magma oceans in the inner solar system (2012, background): “Although it is likely that some heating planetesimals did not melt, models indicate that bodies larger than ∼20 km in radius that accreted within ∼2 Ma of the first solids in the solar system would have melted to some extent (Hevey & Sanders 2006).”
Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, background): “Hevey and Sanders (2006) found that for an initial 60Fe/56Fe of 1.8 10 6, the contribution of 60Fe heating would have been only one-eights of that due to 26Al decay and, hence, has no significant influence on the thermal models for early-formed planetesimals.”
Chondrites as samples of differentiated planetesimals (2009, methodology): “To calculate heat fluxes, the possibility of a core dynamo, and temperature gradients in the unmelted crust, we assume instantaneous accretion and solve the heat conduction in a sphere with initial (26)Al evenly distributed (Hevey and Sanders, 2006).”
Ceres’ evolution and present state constrained by shape data (2010, methodology): “For the pressures in Ceres, the silicate solidus is between 1210 and 1425 K depending on composition (Senshu et al., 2002; Senshu and Matsui, 2006; Hevey and Sanders, 2006; Médard and Grove, 2006).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, background): “These planitesimals in turn were partially dried through radiogenic heating, primarily by the short-lived isotope 26Al (Moskovitz & Gaidos 2011; Hevey & Sanders 2006).”
Toward Planetesimals: Dense Chondrule Clumps in the Protoplanetary Nebula (2008, background): “…together, 3 because objects larger than only 10km or so, which accreted at the same time that refractory inclusions formed (4.567 Byr ago), would have incorporated their full complement of 26Al and would have melted (LaTourette and Wasserburg 1998; Woolum and Cassen 1999, Hevey and Sanders 2006).”
Chondrule formation during planetesimal accretion (2011, background): “Al, with half-life τ 1/2 = 0.72 Ma, led to the meltdown of planetesimals ≳30 km diameter that accreted in the first ~1 Ma (Hevey and Sanders, 2006; Sahijpal et al., 2007).”
Towards initial mass functions for asteroids and Kuiper Belt Objects (2010, background): “5 Myr after CAIs, because of radiogenic heating by live (26)Al (LaTourrette and Wasserburg, 1998; Woolum and Cassen, 1999; McSween et al., 2002; Hevey and Sanders, 2006).”