Solar nebula magnetic fields recorded in the Semarkona meteorite

被引：143

作者：

Fu, Roger R. ^{[1
]}

Weiss, Benjamin P. ^{[1
]}

Lima, Eduardo A. ^{[1
]}

Harrison, Richard J. ^{[2
]}

Bai, Xue-Ning ^{[3
]}

Desch, Steven J. ^{[4
]}

Ebel, Denton S. ^{[5
]}

Suavet, Clement ^{[1
]}

Wang, Huapei ^{[1
]}

Glenn, David ^{[3
]}

Le Sage, David ^{[6
]}

Kasama, Takeshi ^{[7
]}

Walsworth, Ronald L. ^{[3
,6
]}

Kuan, Aaron T. ^{[8
]}

机构：

[1] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA

[2] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[4] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA

[5] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA

[6] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

[7] Tech Univ Denmark, Ctr Electron Nanoscopy, DK-2800 Lyngby, Denmark

[8] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA

来源：

SCIENCE | 2014年 / 346卷 / 6213期

基金：

欧洲研究理事会;

关键词：

PROTOPLANETARY DISKS; ORDINARY CHONDRITES; DUSTY OLIVINES; CHONDRULES; PARTICLES; ACCRETION; ORIGIN; MODEL; STAR;

D O I：

10.1126/science.1258022

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Magnetic fields are proposed to have played a critical role in some of the most enigmatic processes of planetary formation by mediating the rapid accretion of disk material onto the central star and the formation of the first solids. However, there have been no experimental constraints on the intensity of these fields. Here we show that dusty olivine-bearing chondrules from the Semarkona meteorite were magnetized in a nebular field of 54 21 microteslas. This intensity supports chondrule formation by nebular shocks or planetesimal collisions rather than by electric currents, the x-wind, or other mechanisms near the Sun. This implies that background magnetic fields in the terrestrial planet-forming region were likely 5 to 54 microteslas, which is sufficient to account for measured rates of mass and angular momentum transport in protoplanetary disks.

引用

页码：1089 / 1092

页数：4

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