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Peer-reviewedCC BY-NC-NDAnnual Review of Astronomy and Astrophysics

Carbon from Interstellar Clouds to Habitable Worlds

  • Edwin A. Bergin1
  • M. M. Hirschmann2
  • André Izidoro3
  1. 11Department of Astronomy, University of Michigan, Ann Arbor, Michigan, USA; email: [email protected]
  2. 22Department of Earth and Environmental Sciences, University of Minnesota, Minneapolis, Minnesota, USA
  3. 33Department of Earth, Environmental and Planetary Sciences, Rice University, Houston, Texas, USA
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Abstract

Carbon is an essential element for a habitable world. Inner disk ( r < 3 au) planetary carbon compositions are strongly influenced by the supply and survival of carbonaceous solids. Here we trace the journey of carbon from the interstellar medium (ISM) to the processes leading to planet formation. The review highlights the following central aspects: ▪ Organics forming in evolved star envelopes are supplemented by aromatic molecules forming in the dense ISM to represent the seeds of (hydro)carbon supply through pervasive pebble drift to rocky planets and sub-Neptune cores. ▪ Within the protoplanetary disk, the sharp gradient in the C/Si content of Solar System bodies and mineral geochemistry outlines a tale of carbon loss from pebbles to within planetesimals and planets, as well as from planetary atmospheres. ▪ Within two planet formation paradigms (pebble and planetesimal accretion), there is a range of possible planetary carbon content that is strongly influenced by early (<0.5-Myr) formation of a pressure bump that titrates drift. Overall, it is unlikely that the carbon architecture of our Solar System applies to all systems. In the absence of giant planets, carbon-rich rocky worlds and sub-Neptunes may be common. We outline observations that support the presence of such carbon-rich worlds and discuss habitability of terrestrial worlds.

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Cite

BibTeXRIS
BibTeX
@article{bergin2026carbon,
  title = {{Carbon from Interstellar Clouds to Habitable Worlds}},
  author = {Edwin A. Bergin and M. M. Hirschmann and André Izidoro},
  journal = {Annual Review of Astronomy and Astrophysics},
  year = {2026},
  month = jun,
  doi = {10.1146/annurev-astro-043024-121518},
  url = {https://doi.org/10.1146/annurev-astro-043024-121518},
  note = {CC BY-NC-ND},
}
RIS
TY  - JOUR
TI  - Carbon from Interstellar Clouds to Habitable Worlds
AU  - Edwin A. Bergin
AU  - M. M. Hirschmann
AU  - André Izidoro
PY  - 2026
DA  - 2026/06/15
JO  - Annual Review of Astronomy and Astrophysics
DO  - 10.1146/annurev-astro-043024-121518
UR  - https://doi.org/10.1146/annurev-astro-043024-121518
AB  - Carbon is an essential element for a habitable world. Inner disk ( r < 3 au) planetary carbon compositions are strongly influenced by the supply and survival of carbonaceous solids. Here we trace the journey of carbon from the interstellar medium (ISM) to the processes leading to planet formation. The review highlights the following central aspects: ▪ Organics forming in evolved star envelopes are supplemented by aromatic molecules forming in the dense ISM to represent the seeds of (hydro)carbon supply through pervasive pebble drift to rocky planets and sub-Neptune cores. ▪ Within the protoplanetary disk, the sharp gradient in the C/Si content of Solar System bodies and mineral geochemistry outlines a tale of carbon loss from pebbles to within planetesimals and planets, as well as from planetary atmospheres. ▪ Within two planet formation paradigms (pebble and planetesimal accretion), there is a range of possible planetary carbon content that is strongly influenced by early (<0.5-Myr) formation of a pressure bump that titrates drift. Overall, it is unlikely that the carbon architecture of our Solar System applies to all systems. In the absence of giant planets, carbon-rich rocky worlds and sub-Neptunes may be common. We outline observations that support the presence of such carbon-rich worlds and discuss habitability of terrestrial worlds.
SN  - 0066-4146
SN  - 1545-4282
ER  -