{
  "annotation_id": "153c0bf4-d0de-4dd7-ba42-6f5788f61af5",
  "date_created": "2026-02-17T05:53:16.176000Z",
  "date_modified": "2026-02-17T05:53:16.176000Z",
  "file_hash": "957bb8bc44200331a3c904ee4f5cb882a9d03b14c0d4e99ff82b49bb29307a1c",
  "private": false,
  "record": {
    "abstract": "The small number of impact craters found on Titan suggests that its surface is relatively young. Previous work estimated its surface age to be between 200 and 1000 Myr. This estimate, however, is based on crater scaling laws for water and sand, which are not representative of the composition of Titan\u0027s icy surface. Titan\u0027s surface is likely composed of water ice, methane clathrates, or a combination of both. Here, we perform impact simulations for impactors of various sizes that strike an icy target with a 0-15 km thick methane clathrate cap layer. We derive new crater scaling laws based on our numerical results, and find that Titan\u0027s surface age is 300-340 Myr, assuming heliocentric impactors and surface clathrates. This age, which represents the crater retention age, indicates a relatively youthful surface, suggesting that active endogenic and/or exogenic processes have recently reshaped Titan\u0027s surface.",
    "arxiv_id": "2601.08306",
    "authors": [
      "Shigeru Wakita",
      "Brandon C. Johnson",
      "Jason M. Soderblom",
      "Catherine D. Neish"
    ],
    "categories": [
      "astro-ph.EP"
    ],
    "license": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
    "title": "A youthful Titan implied by improved impact simulations",
    "url": "https://arxiv.org/abs/2601.08306",
    "version": "v1"
  },
  "schema_id": "dorsal/arxiv",
  "source": {
    "execution_id": "49718860-614b-495a-a20d-a9cd078b5367",
    "id": "arXiv Dataset",
    "type": "Model",
    "variant": "snapshot-2026-01-17",
    "version": "0.1.0"
  },
  "user_id": 1000002
}