{"work":{"id":"c8e16696-ccfd-4b4f-bb30-400cd8a1ed8c","openalex_id":"https://openalex.org/W2232213006","doi":"10.3847/0004-637x/831/1/64","arxiv_id":"1511.07854","raw_key":null,"title":"and Fortney, Jonathan J","authors":[{"ORCID":"https://orcid.org/0000-0002-5113-8558","given":"Daniel P.","family":"Thorngren","sequence":"first","affiliation":[],"authenticated-orcid":false},{"ORCID":"https://orcid.org/0000-0002-9843-4354","given":"Jonathan J.","family":"Fortney","sequence":"additional","affiliation":[],"authenticated-orcid":false},{"given":"Ruth A.","family":"Murray-Clay","sequence":"additional","affiliation":[]},{"given":"Eric D.","family":"Lopez","sequence":"additional","affiliation":[]}],"authors_text":"Lopez, E","year":2016,"venue":"astro-ph.EP","abstract":"Exoplanet discoveries of recent years have provided a great deal of new data for studying the bulk compositions of giant planets. Here we identify 47 transiting giant planets ($20 M_\\oplus < M < 20 M_{\\mathrm{J}}$) whose stellar insolation is low enough ($F_* < 2\\times10^8\\; \\text{erg}\\; \\text{s}^{-1}\\; \\text{cm}^{-2}$, or roughly $T_\\text{eff} < 1000$) that they are not affected by the hot Jupiter radius inflation mechanism(s). We compute a set of new thermal and structural evolution models and use these models in comparison with properties of the 47 transiting planets (mass, radius, age) to determine their heavy element masses. A clear correlation emerges between the planetary heavy element mass $M_z$ and the total planet mass, approximately of the form $M_z \\propto \\sqrt{M}$. This finding is consistent with the core accretion model of planet formation. We also study how stellar metallicity [Fe/H] affects planetary metal-enrichment and find a weaker correlation than has been previously reported from studies with smaller sample sizes. We confirm a strong relationship between the planetary metal-enrichment relative to the parent star $Z_{\\rm planet}/Z_{\\rm star}$ and the planetary mass, but see no relation in $Z_{\\rm planet}/Z_{\\rm star}$ with planet orbital properties or stellar mass. The large heavy element masses of many planets ($>50$ $M_{\\oplus}$) suggest significant amounts of heavy elements in H/He envelopes, rather than cores, such that metal-enriched giant planet atmospheres should be the rule. We also discuss a model of core-accretion planet formation in a one-dimensional disk and show that it agrees well with our derived relation between mass and $Z_{\\rm planet}/Z_{\\rm star}$.","external_url":"https://doi.org/10.3847/0004-637x/831/1/64","cited_by_count":390,"metadata_source":"doi_reference","metadata_fetched_at":"2026-06-29T06:03:08.293319+00:00","pith_arxiv_id":"1511.07854","created_at":"2026-05-08T18:44:00.409576+00:00","updated_at":"2026-06-29T06:03:08.293319+00:00","title_quality_ok":false,"display_title":"P., Fortney, J","render_title":"P., Fortney, J"},"hub":{"state":{"work_id":"c8e16696-ccfd-4b4f-bb30-400cd8a1ed8c","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":13,"external_cited_by_count":390,"distinct_field_count":2,"first_pith_cited_at":"2025-12-01T15:39:33+00:00","last_pith_cited_at":"2026-06-18T18:00:00+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-29T14:09:00.479049+00:00","tier_text":"hub"},"tier":"hub","role_counts":[],"polarity_counts":[],"runs":{},"summary":{},"graph":{},"authors":[]}}