Proto-Solar Nebula Archives

Water-equivalent content by weight in the Solar System and model predictions. Left upper panel: Midplane temperature of the disk using T1au = 145, 180, 200 and 300 K (from light blue to dark blue respectively) in Eq. 2. Left lower panel: The solid curves show the snowlines calculated using the Tinacci et al. (2023) BE distribution for the different temperature profiles (colours code as above). The data points show the median values of the water-equivalent content by weight for different objects of the Solar System (Sec. 3), where vertical bars represent the minimum and maximum range. Please note that the values reported in Tab. 1 are considered upper limits (see text). The uncertainty of the formation region of the various objects are shown as ellipses, distinguishing NC, CC, and comet populations. Right: Computed snowlines using T1au = 200 K in Eq. 2 and different models (see text): BE distribution (solid line), single BE (dashed) and condensation at 180 K (dotted). The right and left panels share the same vertical axis. -- astro-ph.EP

Astrochemistry, Astrogeology, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Habitable Zones, Interstellar, Status Report, Water/Hycean Worlds & Oceanography

Was Earth’s Water Acquired Locally During The Earliest Phases Of The Solar System Formation?

by Keith CowingJuly 8, 2025July 8, 2025

The origin of the terrestrial water remains debated, as standard Solar System formation models suggest that Earth formed from dry grains, inside the snowline of the Proto-Solar Nebula (PSN).

Proto-Solar Nebula

Was Earth’s Water Acquired Locally During The Earliest Phases Of The Solar System Formation?

Miraflores Butte On Mars

Ocean World Exploration: 2026 American Samoa ROV + Mapping Exploration

Development Of An Adaptive Optics Testbed At MPIA For The ELT/Planetary Camera And Spectrograph (PCS)

Exploring Long-period Architectures: Four New Planet Candidates from Kepler with Periods >342 days

The Selfish Ribosome