Abstract
Our Sun and planetary system were born about 4.5 billion years ago. How did this happen, and what is the nature of our heritage from these early times? This review tries to address these questions from an astrochemical point of view. On the one hand, we have some crucial information from meteorites, comets and other small bodies of the Solar System. On the other hand, we have the results of studies on the formation process of Sun-like stars in our Galaxy. These results tell us that Sun-like stars form in dense regions of molecular clouds and that three major steps are involved before the planet-formation period. They are represented by the prestellar core, protostellar envelope and protoplanetary disk phases. Simultaneously with the evolution from one phase to the other, the chemical composition gains increasing complexity.
In this review, we first present the information on the chemical composition of meteorites, comets and other small bodies of the Solar System, which is potentially linked to the first phases of the Solar System’s formation. Then we describe the observed chemical composition in the prestellar core, protostellar envelope and protoplanetary-disk phases, including the processes that lead to them. Finally, we draw together pieces from the different objects and phases to understand whether and how much we inherited chemically from the time of the Sun’s birth.
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Notes
The famous fossils of cyanobacteria of Australia and for long considered as the first traces of life dated 3.5 Myr (Schopf et al. 2002), are interpreted as inorganic condensations (Skrzypczak et al. 2003; García et al. 2002) and still source of intense debate (Marshall et al. 2011). Conversely, there is consensus on the rise of life about 2 Gyr after the Earth formation, as testified by the rise in the O2 abundance in the atmosphere (Czaja 2010).
Short-lived nuclides are the radionuclides with half-lives shorter than about 10 Myr.
The Atacama Large Millimeter/sub-millimeter Array.
IMHD assumes that the mass to magnetic-flux ratio is constant, which implies that magnetic field lines follow the gas motions, i.e. the magnetic field is “frozen” into the neutral medium.
The Hall effect mainly operates at volume densities between 108 and 1011 cm−3 (Wardle 2004), where the more massive charged particles (ions and charged dust grains) decouple from the magnetic field and collisionally couple with the neutral gas.
The radius at which the gravitational force is balanced by the centrifugal force.
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Acknowledgements
We wish to thank our many colleagues for enlightening discussions over the years: L. Bizzocchi, A. Boley, S. Bottinelli, E. Caux, S. Cazaux, C. Codella, A. Crapsi, L. Dore, T. Douglas, E. Herbst, A. Faure, F. Fontani, J. Henshaw, P. Hily-Blant, J. Ilee, I. Jimenez-Serra, T. Hartquist, C. Kahane, E. Keto, B. Lelfoch, P. Myers, J. Pineda, M. Spaans, M. Tafalla, J. Tan, V. Taquet, C. Vastel, M. Walmsley and L. Wiesenfeld. In addition, C. Ceccarelli acknowledges the stimulating discussions with M. Chaussidon, B. Marty and F. Robert on the meteorites. P. Caselli acknowledges the financial support of successive rolling grants awarded by the UK Science and Technology Funding Council. C. Ceccarelli acknowledges the financial support from the Agence Nationale pour la Recherche (ANR), France (project FORCOMS, contracts ANR-08-BLAN-022, and the CNES (Centre National d’Etudes Spatiales).
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Caselli, P., Ceccarelli, C. Our astrochemical heritage. Astron Astrophys Rev 20, 56 (2012). https://doi.org/10.1007/s00159-012-0056-x
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DOI: https://doi.org/10.1007/s00159-012-0056-x