A perspective from extinct radionuclides on a Young Stellar Object: The Sun and its accretion disk
arXiv:1105.5172 · doi:10.1146/annurev-earth-040610-133428
Abstract
Meteorites, which are remnants of solar system formation, provide a direct glimpse into the dynamics and evolution of a young stellar object (YSO), namely our Sun. Much of our knowledge about the astrophysical context of the birth of the Sun, the chronology of planetary growth from micrometer-sized dust to terrestrial planets, and the activity of the young Sun comes from the study of extinct radionuclides such as 26Al (t1/2 = 0.717 Myr). Here we review how the signatures of extinct radionuclides (short-lived isotopes that were present when the solar system formed and that have now decayed below detection level) in planetary materials influence the current paradigm of solar system formation. Particular attention is given to tying meteorite measurements to remote astronomical observations of YSOs and modeling efforts. Some extinct radionuclides were inherited from the long-term chemical evolution of the Galaxy, others were injected into the solar system by a nearby supernova, and some were produced by particle irradiation from the T-Tauri Sun. The chronology inferred from extinct radionuclides reveals that dust agglomeration to form centimeter-sized particles in the inner part of the disk was very rapid (<50 kyr), planetesimal formation started early and spanned several million years, planetary embryos (possibly like Mars) were formed in a few million years, and terrestrial planets (like Earth) completed their growths several tens of million years after the birth of the Sun.
49 pages, 9 figures, 1 table. Uncorrected preprint
References in corpus (11)
- Towards planetesimals: dense chondrule clumps in the protoplanetary nebula
- Equilibration in the Aftermath of the Lunar-Forming Giant Impact
- Short-lived Nuclei in the Early Solar System: Possible AGB Sources
- Abundant Circumstellar Silica Dust and SiO Gas Created by a Giant Hypervelocity Collision in the ~12 Myr HD172555 System
- Interaction of Supernova Ejecta with Nearby Protoplanetary Disks
- Simultaneous Triggered Collapse of the Presolar Dense Cloud Core and Injection of Short-Lived Radioisotopes by a Supernova Shock Wave
- Growth of Dust as the Initial Step Toward Planet Formation
- Injection of Short-Lived Radionuclides into the Early Solar System from a Faint Supernova with Mixing-Fallback
- Supernova Propagation And Cloud Enrichment: A new model for the origin of Fe in the early solar system
- From discs to planetesimals I: evolution of gas and dust discs
- Dispersal of protoplanetary disks by central wind stripping