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Using the Radiometric Bode's Law, we estimate the radio flux produced by the interaction of Proxima Centauri's stellar wind and Proxima b's magnetosphere for different planetary magnetic field strengths. For plausible planetary masses, Proxima b produces 6-83 mJy of auroral radio flux at frequencies of 0.3-"},"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":"1706.07038","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2017-06-21T17:59:47Z","cross_cats_sorted":[],"title_canon_sha256":"0ef2d2c9b389f2c3448a37eefc857a00ad153b02c97a0338081266426e0cd1f2","abstract_canon_sha256":"6346780c35f62141809e161b134ef6add14b96c8c2291fba49727820388c6b2a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:31:40.756194Z","signature_b64":"DwxZ0mwgMEiF7dgQ+CfLdcq9UN33jaMLaABCsGSYsPZLsucS4Jtb8f6S0MNzGzFVTIAYnEwiKt3ry2Fz5m0vAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5d5e72b2b2a04d064d80e566bf987154771721ec7a481737960371764f3e6b98","last_reissued_at":"2026-05-18T00:31:40.755724Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:31:40.755724Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Detectability of Radio Auroral Emission from Proxima B","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Abraham Loeb, Blakesley Burkhart","submitted_at":"2017-06-21T17:59:47Z","abstract_excerpt":"Magnetically active stars possess stellar winds whose interaction with planetary magnetic fields produces radio auroral emission. 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