{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:4N4TCLONRZPGWFJSUBHY7GVKC5","short_pith_number":"pith:4N4TCLON","schema_version":"1.0","canonical_sha256":"e379312dcd8e5e6b1532a04f8f9aaa177e99d270db4dab90dbfd3dbbd5b9e971","source":{"kind":"arxiv","id":"1507.08902","version":2},"attestation_state":"computed","paper":{"title":"Grain size constraints on HL Tau with polarization signature","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Akimasa Kataoka, Cornelis P Dullemond, Munetake Momose, Takashi Tsukagoshi, Takayuki Muto","submitted_at":"2015-07-31T14:51:40Z","abstract_excerpt":"The millimeter-wave polarization of the protoplanetary disk around HL Tau has been interpreted as the emission from elongated dust grains aligned with the magnetic field in the disk. However, the self-scattering of thermal dust emission may also explain the observed millimeter-wave polarization. In this paper, we report a modeling of the millimeter-wave polarization of the HL Tau disk with the self-polarization. Dust grains are assumed to be spherical and to have a power-law size distribution. We change the maximum grain size with a fixed dust composition in a fixed disk model to find the grai"},"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":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1507.08902","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2015-07-31T14:51:40Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"ddbdc12303f90fcb797c33eff4d46a028581fdf2625f8a4af7c1e60972c51dea","abstract_canon_sha256":"ee4fb1f94e9188e7fa6999f06f8942d8240dbf6deefdd029069fd1260c539b35"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:18:43.919787Z","signature_b64":"P/wQpnTUPWaVnoLPMnRmwX3z7mc9Ao+IQZq4lU6xbY78AIvcJGLLM8SyRbzyTViCZXRXuFaZyepZd0ggqi4fBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e379312dcd8e5e6b1532a04f8f9aaa177e99d270db4dab90dbfd3dbbd5b9e971","last_reissued_at":"2026-05-18T01:18:43.918923Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:18:43.918923Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Grain size constraints on HL Tau with polarization signature","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"Akimasa Kataoka, Cornelis P Dullemond, Munetake Momose, Takashi Tsukagoshi, Takayuki Muto","submitted_at":"2015-07-31T14:51:40Z","abstract_excerpt":"The millimeter-wave polarization of the protoplanetary disk around HL Tau has been interpreted as the emission from elongated dust grains aligned with the magnetic field in the disk. However, the self-scattering of thermal dust emission may also explain the observed millimeter-wave polarization. In this paper, we report a modeling of the millimeter-wave polarization of the HL Tau disk with the self-polarization. Dust grains are assumed to be spherical and to have a power-law size distribution. We change the maximum grain size with a fixed dust composition in a fixed disk model to find the grai"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1507.08902","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1507.08902","created_at":"2026-05-18T01:18:43.919069+00:00"},{"alias_kind":"arxiv_version","alias_value":"1507.08902v2","created_at":"2026-05-18T01:18:43.919069+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1507.08902","created_at":"2026-05-18T01:18:43.919069+00:00"},{"alias_kind":"pith_short_12","alias_value":"4N4TCLONRZPG","created_at":"2026-05-18T12:29:05.191682+00:00"},{"alias_kind":"pith_short_16","alias_value":"4N4TCLONRZPGWFJS","created_at":"2026-05-18T12:29:05.191682+00:00"},{"alias_kind":"pith_short_8","alias_value":"4N4TCLON","created_at":"2026-05-18T12:29:05.191682+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15014","citing_title":"Millimeter dust continuum and polarization in protoplanetary disks with scattering: A slab model","ref_index":15,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5","json":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5.json","graph_json":"https://pith.science/api/pith-number/4N4TCLONRZPGWFJSUBHY7GVKC5/graph.json","events_json":"https://pith.science/api/pith-number/4N4TCLONRZPGWFJSUBHY7GVKC5/events.json","paper":"https://pith.science/paper/4N4TCLON"},"agent_actions":{"view_html":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5","download_json":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5.json","view_paper":"https://pith.science/paper/4N4TCLON","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1507.08902&json=true","fetch_graph":"https://pith.science/api/pith-number/4N4TCLONRZPGWFJSUBHY7GVKC5/graph.json","fetch_events":"https://pith.science/api/pith-number/4N4TCLONRZPGWFJSUBHY7GVKC5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5/action/storage_attestation","attest_author":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5/action/author_attestation","sign_citation":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5/action/citation_signature","submit_replication":"https://pith.science/pith/4N4TCLONRZPGWFJSUBHY7GVKC5/action/replication_record"}},"created_at":"2026-05-18T01:18:43.919069+00:00","updated_at":"2026-05-18T01:18:43.919069+00:00"}