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Recently, the S-star binary, called D9, was found to be orbited by a circumbinary disk. Due to the gravitational interaction between Sgr A* and the binary, the disk could be short-lived. We investigate the evolution of the disk around a stellar binary while orbiting Sgr A*. We use the \\texttt{AMUSE} framework for coupling a gravity solver (for the binary and Sgr. A*) with a hydrodynamics solver (for the disk). We find that, the disk eventually settles b"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":true,"formal_links_present":false},"canonical_record":{"source":{"id":"2604.09856","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2026-04-10T19:35:46Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"1d892b18475e6a3ffb15b364c3602364410df0d173406c5b3847e4a01e066d0c","abstract_canon_sha256":"8f91244ee7784566dec8309ad2b82a95ec63fcbcc35a34e4597223cc0ada5b5a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-06-19T16:10:37.258254Z","signature_b64":"TudU+ihHowv6g85irqn3pbsO5sKdPuTVwB9M5Lm/3hALaOL0EkKZQdMecyhinUQ2ZQDxsJGFHGc812ticlwKBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6d4585e1fca46a6f11c175ec5505109927fc9c0f5d672da9dc636ac908b98d22","last_reissued_at":"2026-06-19T16:10:37.257854Z","signature_status":"signed_v1","first_computed_at":"2026-06-19T16:10:37.257854Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Kozai-driven mass loss of the circumbinary disk in D9 in orbit around the supermassive black hole Sgr A*","license":"http://creativecommons.org/licenses/by/4.0/","headline":"The circumbinary disk around D9 loses about 7 percent of its mass every von Zeipel-Lidov-Kozai cycle induced by Sgr A*.","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Lucas Pouw, Simon Portegies Zwart, Tim van der Vuurst, Yannick Badoux","submitted_at":"2026-04-10T19:35:46Z","abstract_excerpt":"The supermassive black hole (Sgr A*) in the Galactic center is surrounded by the S-star cluster consisting of young stars on eccentric orbits. Recently, the S-star binary, called D9, was found to be orbited by a circumbinary disk. Due to the gravitational interaction between Sgr A* and the binary, the disk could be short-lived. We investigate the evolution of the disk around a stellar binary while orbiting Sgr A*. We use the \\texttt{AMUSE} framework for coupling a gravity solver (for the binary and Sgr. A*) with a hydrodynamics solver (for the disk). We find that, the disk eventually settles b"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We find the disk loses ∼7% ± 2% of its mass every vZLK cycle. If we extrapolate this mass loss, the disk will have 1% of its current mass left after another ∼4 Myr. D9 will then be ∼6.7 Myr old, which is on the same order as the current average age of S cluster members. The vZLK-driven mass loss could, therefore, explain the absence of Brγ emission from other S cluster members.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The mass loss rate of ~7% per cycle remains constant over multiple Myr without significant changes from unmodeled physics such as stellar winds, radiation, or variations in initial disk conditions.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Numerical simulations find that vZLK oscillations induce periodic mass loss from D9's circumbinary disk at a rate of ~7% per 62.5 kyr cycle, leading to near-total depletion after ~4 Myr.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"The circumbinary disk around D9 loses about 7 percent of its mass every von Zeipel-Lidov-Kozai cycle induced by Sgr A*.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"eb0421b692ddbf509a542cc10cc1c48d8f07051f5e6e8138f48ae2cf0998734b"},"source":{"id":"2604.09856","kind":"arxiv","version":2},"verdict":{"id":"e648bf3b-c637-494f-9de2-d16d3868ed8e","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T16:56:42.133778Z","strongest_claim":"We find the disk loses ∼7% ± 2% of its mass every vZLK cycle. If we extrapolate this mass loss, the disk will have 1% of its current mass left after another ∼4 Myr. D9 will then be ∼6.7 Myr old, which is on the same order as the current average age of S cluster members. The vZLK-driven mass loss could, therefore, explain the absence of Brγ emission from other S cluster members.","one_line_summary":"Numerical simulations find that vZLK oscillations induce periodic mass loss from D9's circumbinary disk at a rate of ~7% per 62.5 kyr cycle, leading to near-total depletion after ~4 Myr.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The mass loss rate of ~7% per cycle remains constant over multiple Myr without significant changes from unmodeled physics such as stellar winds, radiation, or variations in initial disk conditions.","pith_extraction_headline":"The circumbinary disk around D9 loses about 7 percent of its mass every von Zeipel-Lidov-Kozai cycle induced by Sgr A*."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.09856/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":27,"sample":[{"doi":"","year":2012,"title":"2012, ApJ, 757, L29","work_id":"33d295ac-ea0c-460a-931f-87b8d814d7a6","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2019,"title":"Cheng, S. 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