### Abstract

Among the calcium-aluminum-rich inclusions (CAIs), excess ^{41}K (^{41}K*), which was produced by the decay of the short-lived radionuclide ^{41}Ca (t_{1/2} = 0.1 Myr, has so far been detected in fassaite and in two grains of melilites. These observations could be used to provide important constraints on the thermal history and size of the planetesimals into which the CAIs were incorporated, provided the diffusion kinetic properties of K in these minerals are known. Thus, we have experimentally determined K diffusion kinetics in the melilite end-members, åkermanite and gehlenite, as a function of temperature (900-1200 °C) and crystallographic orientation at 1 bar pressure. The closure temperature of K diffusion in melilite, T_{c}(K:mel), for the observed grain size of melilite in the CAIs and cooling rate of 10-100 °C/Myr, as calculated from our diffusion data, is much higher than that of Mg in anorthite. The latter was calculated from the available Mg diffusion data in anorthite. Assuming that the planetesimals were heated by the decay of ^{26}Al and ^{60}Fe, we have calculated the size of a planetesimal as a function of the accretion time t_{f} such that the peak temperature at a specified radial distance r_{c} equals T_{c}(K:mel). The ratio (r_{c}/R)^{3} defines the planetesimal volume fraction within which ^{41} K* in melilite grains would be at least partly disturbed, if these were randomly distributed within a planetesimal. A similar calculation was also carried out to define R versus t_{f} relation such that ^{26}Mg* was lost from ∼50% of randomly distributed anorthite grains, as seems to be suggested by the observational data. These calculations suggest that ∼60% of melilite grains should retain ^{41}K* if ∼50% of anorthite grains had retained ^{26}Mg*. Assuming that t_{f} was not smaller than the time of chondrule formation, our calculations yield minimum planetesimal radius of ∼20-30 km, depending on the choice of planetesimal surface temperature and initial abundance of the heat producing isotope ^{60}Fe.

Original language | English (US) |
---|---|

Pages (from-to) | 1911-1919 |

Number of pages | 9 |

Journal | Meteoritics and Planetary Science |

Volume | 39 |

Issue number | 12 |

State | Published - Dec 2004 |

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### ASJC Scopus subject areas

- Geophysics

### Cite this

**Potassium diffusion in melilite : Experimental studies and constraints on the thermal history and size of planetesimals hosting CAIs.** / Ito, Motoo; Ganguly, Jibamitra.

Research output: Contribution to journal › Article

*Meteoritics and Planetary Science*, vol. 39, no. 12, pp. 1911-1919.

}

TY - JOUR

T1 - Potassium diffusion in melilite

T2 - Experimental studies and constraints on the thermal history and size of planetesimals hosting CAIs

AU - Ito, Motoo

AU - Ganguly, Jibamitra

PY - 2004/12

Y1 - 2004/12

N2 - Among the calcium-aluminum-rich inclusions (CAIs), excess 41K (41K*), which was produced by the decay of the short-lived radionuclide 41Ca (t1/2 = 0.1 Myr, has so far been detected in fassaite and in two grains of melilites. These observations could be used to provide important constraints on the thermal history and size of the planetesimals into which the CAIs were incorporated, provided the diffusion kinetic properties of K in these minerals are known. Thus, we have experimentally determined K diffusion kinetics in the melilite end-members, åkermanite and gehlenite, as a function of temperature (900-1200 °C) and crystallographic orientation at 1 bar pressure. The closure temperature of K diffusion in melilite, Tc(K:mel), for the observed grain size of melilite in the CAIs and cooling rate of 10-100 °C/Myr, as calculated from our diffusion data, is much higher than that of Mg in anorthite. The latter was calculated from the available Mg diffusion data in anorthite. Assuming that the planetesimals were heated by the decay of 26Al and 60Fe, we have calculated the size of a planetesimal as a function of the accretion time tf such that the peak temperature at a specified radial distance rc equals Tc(K:mel). The ratio (rc/R)3 defines the planetesimal volume fraction within which 41 K* in melilite grains would be at least partly disturbed, if these were randomly distributed within a planetesimal. A similar calculation was also carried out to define R versus tf relation such that 26Mg* was lost from ∼50% of randomly distributed anorthite grains, as seems to be suggested by the observational data. These calculations suggest that ∼60% of melilite grains should retain 41K* if ∼50% of anorthite grains had retained 26Mg*. Assuming that tf was not smaller than the time of chondrule formation, our calculations yield minimum planetesimal radius of ∼20-30 km, depending on the choice of planetesimal surface temperature and initial abundance of the heat producing isotope 60Fe.

AB - Among the calcium-aluminum-rich inclusions (CAIs), excess 41K (41K*), which was produced by the decay of the short-lived radionuclide 41Ca (t1/2 = 0.1 Myr, has so far been detected in fassaite and in two grains of melilites. These observations could be used to provide important constraints on the thermal history and size of the planetesimals into which the CAIs were incorporated, provided the diffusion kinetic properties of K in these minerals are known. Thus, we have experimentally determined K diffusion kinetics in the melilite end-members, åkermanite and gehlenite, as a function of temperature (900-1200 °C) and crystallographic orientation at 1 bar pressure. The closure temperature of K diffusion in melilite, Tc(K:mel), for the observed grain size of melilite in the CAIs and cooling rate of 10-100 °C/Myr, as calculated from our diffusion data, is much higher than that of Mg in anorthite. The latter was calculated from the available Mg diffusion data in anorthite. Assuming that the planetesimals were heated by the decay of 26Al and 60Fe, we have calculated the size of a planetesimal as a function of the accretion time tf such that the peak temperature at a specified radial distance rc equals Tc(K:mel). The ratio (rc/R)3 defines the planetesimal volume fraction within which 41 K* in melilite grains would be at least partly disturbed, if these were randomly distributed within a planetesimal. A similar calculation was also carried out to define R versus tf relation such that 26Mg* was lost from ∼50% of randomly distributed anorthite grains, as seems to be suggested by the observational data. These calculations suggest that ∼60% of melilite grains should retain 41K* if ∼50% of anorthite grains had retained 26Mg*. Assuming that tf was not smaller than the time of chondrule formation, our calculations yield minimum planetesimal radius of ∼20-30 km, depending on the choice of planetesimal surface temperature and initial abundance of the heat producing isotope 60Fe.

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M3 - Article

AN - SCOPUS:14844364325

VL - 39

SP - 1911

EP - 1919

JO - Meteoritics and Planetary Science

JF - Meteoritics and Planetary Science

SN - 1086-9379

IS - 12

ER -