{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:YU4OEKFBEGC5VVKEY7AR6WJQRX","short_pith_number":"pith:YU4OEKFB","schema_version":"1.0","canonical_sha256":"c538e228a12185dad544c7c11f59308ded2f8e5968ac08473bb423c1f66fa4ff","source":{"kind":"arxiv","id":"2504.15955","version":1},"attestation_state":"computed","paper":{"title":"Temperature anisotropy instabilities of solar wind electrons with regularized Kappa-halos resolved with ALPS","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"physics.plasm-ph","authors_text":"(2) Centre for mathematical Plasma-Astrophysics, 3001 Leuven, (3) Mullard Space Science Laboratory, (4) Department of Planetary Science, Belgium, D-44780 Bochum, Daniel Verscharen (3), Dorking RH5 6NT, Dustin L. Schr\\\"oder (1), Germany, Horst Fichtner (1), Kristopher G. Klein (4) ((1) Institut f\\\"ur Theoretische Physik, KU Leuven, Lehrstuhl IV: Plasma-Astroteilchenphysik, Marian Lazar (2), Ruhr-Universit\\\"at Bochum, Tucson, UK, University College London, University of Arizona, USA)","submitted_at":"2025-04-22T14:50:39Z","abstract_excerpt":"Space plasmas in various astrophysical setups can often be both very hot and dilute, making them highly susceptible to waves and fluctuations, which are generally self-generated and maintained by kinetic instabilities. In this sense, we have in-situ observational evidence from the solar wind and planetary environments, which reveal not only wave fluctuations at kinetic scales of electrons and protons, but also non-equilibrium distributions of particle velocities. This paper reports on the progress made in achieving a consistent modeling of the instabilities generated by temperature anisotropy,"},"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":"2504.15955","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"physics.plasm-ph","submitted_at":"2025-04-22T14:50:39Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"032dbeeda7b88d8ed21f4874ef242c5096dfa1dd9ce6eb1ce85d8190a86d5765","abstract_canon_sha256":"ea5456c399cbb9b3f094170823200ced5fe57be9ebe94b0240c2a8cac0ba1012"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:52:32.592540Z","signature_b64":"W+GSmlOP+7k1z+k0cXAebJrnJORQ+YQOtfakqQZuGhFI1KeorNQ6XuNUWBsdt+NXDWOVXVqlMavEZoDxi206Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c538e228a12185dad544c7c11f59308ded2f8e5968ac08473bb423c1f66fa4ff","last_reissued_at":"2026-07-05T10:52:32.592064Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:52:32.592064Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Temperature anisotropy instabilities of solar wind electrons with regularized Kappa-halos resolved with ALPS","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"physics.plasm-ph","authors_text":"(2) Centre for mathematical Plasma-Astrophysics, 3001 Leuven, (3) Mullard Space Science Laboratory, (4) Department of Planetary Science, Belgium, D-44780 Bochum, Daniel Verscharen (3), Dorking RH5 6NT, Dustin L. Schr\\\"oder (1), Germany, Horst Fichtner (1), Kristopher G. Klein (4) ((1) Institut f\\\"ur Theoretische Physik, KU Leuven, Lehrstuhl IV: Plasma-Astroteilchenphysik, Marian Lazar (2), Ruhr-Universit\\\"at Bochum, Tucson, UK, University College London, University of Arizona, USA)","submitted_at":"2025-04-22T14:50:39Z","abstract_excerpt":"Space plasmas in various astrophysical setups can often be both very hot and dilute, making them highly susceptible to waves and fluctuations, which are generally self-generated and maintained by kinetic instabilities. In this sense, we have in-situ observational evidence from the solar wind and planetary environments, which reveal not only wave fluctuations at kinetic scales of electrons and protons, but also non-equilibrium distributions of particle velocities. This paper reports on the progress made in achieving a consistent modeling of the instabilities generated by temperature anisotropy,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2504.15955","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2504.15955/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2504.15955","created_at":"2026-07-05T10:52:32.592120+00:00"},{"alias_kind":"arxiv_version","alias_value":"2504.15955v1","created_at":"2026-07-05T10:52:32.592120+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2504.15955","created_at":"2026-07-05T10:52:32.592120+00:00"},{"alias_kind":"pith_short_12","alias_value":"YU4OEKFBEGC5","created_at":"2026-07-05T10:52:32.592120+00:00"},{"alias_kind":"pith_short_16","alias_value":"YU4OEKFBEGC5VVKE","created_at":"2026-07-05T10:52:32.592120+00:00"},{"alias_kind":"pith_short_8","alias_value":"YU4OEKFB","created_at":"2026-07-05T10:52:32.592120+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX","json":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX.json","graph_json":"https://pith.science/api/pith-number/YU4OEKFBEGC5VVKEY7AR6WJQRX/graph.json","events_json":"https://pith.science/api/pith-number/YU4OEKFBEGC5VVKEY7AR6WJQRX/events.json","paper":"https://pith.science/paper/YU4OEKFB"},"agent_actions":{"view_html":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX","download_json":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX.json","view_paper":"https://pith.science/paper/YU4OEKFB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2504.15955&json=true","fetch_graph":"https://pith.science/api/pith-number/YU4OEKFBEGC5VVKEY7AR6WJQRX/graph.json","fetch_events":"https://pith.science/api/pith-number/YU4OEKFBEGC5VVKEY7AR6WJQRX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX/action/storage_attestation","attest_author":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX/action/author_attestation","sign_citation":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX/action/citation_signature","submit_replication":"https://pith.science/pith/YU4OEKFBEGC5VVKEY7AR6WJQRX/action/replication_record"}},"created_at":"2026-07-05T10:52:32.592120+00:00","updated_at":"2026-07-05T10:52:32.592120+00:00"}