The Cradle of the Solar System

  title={The Cradle of the Solar System},
  author={J. Jeff Hester and Steven J. Desch and Kevin Robert Healy and Laurie A. Leshin},
  pages={1116 - 1117}
The recent discovery of decay products of 60Fe in meteorites challenges conventional wisdom about the environment in which the Sun and planets formed. Rather than a region like the well-studied Taurus-Auriga molecular cloud, the solar system must have formed instead in a region more like the Eagle nebula--a region that contained one or more massive stars that went supernova, injecting newly synthesized radionuclides into the nascent solar system. In their Perspective, Hester et al. discuss a… 
The Formation of the Solar System
  • S. Russell
  • Geology, Physics
    Journal of the Geological Society
  • 2007
The study of the origin and evolution of the Solar System is based on laboratory analysis of meteorites and other extraterrestrial materials, and on astronomical observations of star-forming regions
The abundance of 26Al-rich planetary systems in the Galaxy
One of the most puzzling properties of the solar system is the high abundance at its birth of 26Al, a short-lived radionuclide with a mean life of 1 Myr. Now decayed, it has left its imprint in
The radioactive nuclei and in the Cosmos and in the solar system
The cosmic evolution of the chemical elements from the Big Bang to the present time is driven by nuclear fusion reactions inside stars and stellar explosions. A cycle of matter recurrently
The role of massive AGB stars in the early solar system composition
Abstract— We demonstrate that a massive asymptotic giant branch (AGB) star is a good candidate as the main source of short‐lived radionuclides in the early solar system. Recent identification of
26Al and the Formation of the Solar System from a Molecular Cloud Contaminated by Wolf-Rayet Winds
In agreement with previous work, we show that the presence of the short-lived radionuclide (SLR) 26Al in the early solar system was unlikely (less than 2% a priori probability) to be the result of
Short-lived radioisotopes in meteorites from Galactic-scale correlated star formation
Abstract Meteoritic evidence shows that the Solar system at birth contained significant quantities of short-lived radioisotopes (SLRs) such as 60Fe and 26Al produced in supernova explosions and in
Radioactive Probes of the Supernova-contaminated Solar Nebula: Evidence that the Sun Was Born in a Cluster
We construct a simple model for radioisotopic enrichment of the protosolar nebula by injection from a nearby supernova, based on the inverse square law for ejecta dispersion. In this parameter study,
The early solar system contained a number of short-lived radionuclides (SLRs) such as {sup 26}Al with half-lives <15 Myr. The one-time presence of {sup 60}Fe strongly suggests that the source of
The formation of the solar system
The solar system started to form about 4.56 Gyr ago and despite the long intervening time span, there still exist several clues about its formation. The three major sources for this information are
Accretion of Jupiter ’ s Atmosphere from a Supernova-Contaminated Star Cluster Submitted to Icarus 14-Oct-2008
If Jupiter and the Sun both formed directly from the same well-mixed protosolar nebula, then their observed atmospheric compositions should be similar. However, direct sampling of Jupiter’s


Constraints on the Birth Aggregate of the Solar System
Using the observed properties of our Solar System, in particular the isotopic compositions of meteorites and the regularity of the planetary orbits, we constrain the star formation environment of the
Short-Lived Radioactivities and the Birth of the sun
Now extinct short-lived radioactive isotopes were apparently extant in the early solar system. Their abundances can be inferred from isotopic effects in their daughter nuclei in primitive meteorites,
Photoevaporation of Disks and Clumps by Nearby Massive Stars: Application to Disk Destruction in the Orion Nebula
We present a model for the photoevaporation of circumstellar disks or dense clumps of gas by an external source of ultraviolet radiation. Our model includes the thermal and dynamic effects of 6-13.6
The photoevaporation of interstellar clouds. II. Equilibrium cometary clouds
An approximate analytic theory for the evolution of an interstellar cloud which is exposed to the ionizing radiation of a newly formed star is developed. This paper will follow the evolution of a
Near-Infrared Study of M16: Star Formation in the Elephant Trunks
We present combined J, H, and Ks images of M16 that were obtained with SIRIUS (Simultaneous three-color InfraRed Imager for Unbiased Surveys) on the University of Hawaii 2.2 m telescope. In contrast
Disks, Microjets, Windblown Bubbles, and Outflows in the Orion Nebula*
New deep narrowband images of the Orion Nebula obtained with WFPC2 on the Hubble Space Telescope (HST) and spectra taken with the HIRES spectrometer at the Keck Observatory are presented. We report
The Initial Abundance of 60 Fe in the Solar System
60Fe, which decays to radiogenic 60Ni (60Ni*), is a now extinct radionuclide. 60Fe is produced only in stars and thus provides a constraint on the stellar contribution to solar system radionuclides.
Embedded Clusters in Molecular Clouds
The first extensive catalog of galactic embedded clusters is compiled, finding that the embedded cluster birthrate exceeds that of visible open clusters by an order of magnitude or more indicating a high infant mortality rate for protocluster systems.
Disk Mass Limits and Lifetimes of Externally Irradiated Young Stellar Objects Embedded in the Orion Nebula
?????We present 1.3 mm wavelength interferometric observations of externally irradiated young stellar objects (proplyds) embedded within the Orion Nebula, including the three largest circumstellar
Hubble Space Telescope WFPC2 Imaging of M16: Photoevaporation and Emerging Young Stellar Objects
We present Hubble Space Telescope WFPC2 images of elephant trunks in the H II region M16. There are three principle results of this study. First, the morphology and stratified ionization structure of