{"corpus_id":119814400,"paper_sha":"09334f033c857070ea5b7e650211e9926ffe7e49","doi":"10.1086/190035","arxiv_id":null,"pmid":null,"pmcid":null,"mag_id":1964225025,"dblp_id":null,"acl_id":null,"title":"A Catalog of Magnetic Stars.","year":1958,"publication_date":null,"venue":"","journal":{"name":"Astrophysical Journal Supplement Series","pages":"141","volume":"3"},"journal_issn":null,"journal_title":null,"publication_types":[],"pubmed_pub_types":null,"s2_fields_of_study":["Physics"],"reference_count":0,"citation_count":284,"influential_citation_count":27,"is_open_access":false,"arxiv_categories":null,"arxiv_license":null,"arxiv_journal_ref":null,"mesh_headings":null,"chemicals":null,"comments_corrections":null,"source_flags":1,"s2_open_access_pdf_url":null,"s2_open_access_landing_url":null,"s2_open_access_license":null,"s2_open_access_status":null,"pmc_open_access_pdf_url":null,"pmc_open_access_landing_url":null,"pmc_open_access_license":null,"pmc_open_access_status":null,"unpaywall_open_access_pdf_url":null,"unpaywall_open_access_landing_url":null,"unpaywall_open_access_license":null,"unpaywall_open_access_status":null,"abstract":"This is a catalog of magnetic stars with a compilation of numerous observations. The analysis and discussion of the results will be taken up in a later paper. The observations have been made over a period of 11 years with the 100-inch and 200-inch telescopes, using an analyzer for the Zeeman effect. Table 1 lists repeated observations of 89 sharp-line stars. Ma etic polarity, field strength, and velocity are tabulated. Notes on spectral peculiarities and line widts are given. Table 2 lists 66 stars that probably, but not definitely, show the Zeeman effect. Table 3 consists of 61 sharp-line stars not showing evidence of a coherent magnetic field. Table 4 is a collection of 122 stars with lines too broad to permit measurement. Of the magnetic stars in Table 1, one is a cluster-type variable, 1 is a subdwarf, 2 are of type S, 3 are M giants, 7 are \"metallic4ine\" objects, and 70 are A-type stars with sharp or ultra-sharp lines. Stellar magnetic fields are therefore probably ubiquitous. All stellar magnetic fields appear to be variable. Of the A-type stars sufficiently observed, S are regnlar magnetic variables having periods near 1 week, very large and nearly uniform magnetic amplitude, and nearly symmetrical reversal of polarity; about 22 are irregnlar variables showing reversal of polarity; and about 15 are irregnlar variables showing always the same polarity. The irregnlar variations prove that large-scale intrinsic hydromagnetic fluctuations occur in the photospheric layers.","claims":[{"public_id":"cl_b99575d7eaf21460cd2174206f8eeaab","status":"active","text":"Among the magnetic stars in Table 1, the sample includes a cluster-type variable, a subdwarf, type S stars, M giants, metallic-line objects, and many A-type stars with sharp or ultra-sharp lines.","confidence":0.94,"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/claims/cl_b99575d7eaf21460cd2174206f8eeaab"},{"public_id":"cl_f8b949c34d2aa03e51b74857360a5480","status":"active","text":"Among the sufficiently observed A-type stars, some are regular magnetic variables with periods near 1 week, very large and nearly uniform magnetic amplitude, and nearly symmetrical reversal of polarity.","confidence":0.93,"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/claims/cl_f8b949c34d2aa03e51b74857360a5480"},{"public_id":"cl_47c9dbb0c815dcf31c0cf1daebabde73","status":"active","text":"Irregular variations in magnetic polarity and amplitude indicate large-scale intrinsic hydromagnetic fluctuations in the photospheric layers.","confidence":0.95,"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/claims/cl_47c9dbb0c815dcf31c0cf1daebabde73"},{"public_id":"cl_05ffe7e4399c5f23fbf48a055f1436dd","status":"active","text":"Stellar magnetic fields are probably ubiquitous and appear to be variable.","confidence":0.91,"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/claims/cl_05ffe7e4399c5f23fbf48a055f1436dd"},{"public_id":"cl_d36ab9ea03f3a0508a3decfc26ba6b0f","status":"active","text":"The catalog compiles repeated observations of 89 sharp-line stars, 66 stars that probably but not definitely show the Zeeman effect, 61 sharp-line stars with no evidence of a coherent magnetic field, and 122 stars with lines too broad to permit measurement.","confidence":0.98,"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/claims/cl_d36ab9ea03f3a0508a3decfc26ba6b0f"}],"concepts":[{"public_id":"co_02fc58363a4afa02fe35b59a2fa90d10","status":"active","name":"magnetic stars","description":"Stars included in the catalog that show evidence of magnetic fields or Zeeman splitting.","types":["astronomical object"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_02fc58363a4afa02fe35b59a2fa90d10"},{"public_id":"co_3d1c5b373c8a471339b2cecdbb2b8de9","status":"active","name":"A-type stars","description":"Stars of spectral class A, some of which are discussed as magnetic variables in the catalog.","types":["astronomical object"],"aliases":["A stars"],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_3d1c5b373c8a471339b2cecdbb2b8de9"},{"public_id":"co_3ddb26494d8ee88f914959d666a7394a","status":"active","name":"metallic-line objects","description":"Stars showing unusually strong metallic spectral lines.","types":["astronomical object"],"aliases":["metallic-line stars"],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_3ddb26494d8ee88f914959d666a7394a"},{"public_id":"co_60ac92b0a8b4a77beca4e29b01b9a692","status":"active","name":"regular magnetic variables","description":"Magnetic stars with periodic and relatively symmetric reversals of polarity and fairly uniform amplitude.","types":["astronomical object","variable star class"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_60ac92b0a8b4a77beca4e29b01b9a692"},{"public_id":"co_880d78313a70ed5eb094da4fa18dfc7a","status":"active","name":"stellar magnetic fields","description":"Magnetic fields associated with stars.","types":["physical property"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_880d78313a70ed5eb094da4fa18dfc7a"},{"public_id":"co_9d0966c4e05607f45bebf580a9002ac5","status":"active","name":"magnetic polarity","description":"The sign or orientation of the observed stellar magnetic field.","types":["measurement"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_9d0966c4e05607f45bebf580a9002ac5"},{"public_id":"co_d49154aab6978547a98c52c0fb9892f3","status":"active","name":"Zeeman effect","description":"The splitting or polarization of spectral lines caused by a magnetic field.","types":["physical effect"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_d49154aab6978547a98c52c0fb9892f3"},{"public_id":"co_e226e0486e08412c5382b2f9366db183","status":"active","name":"variability","description":"Changes over time in observed magnetic properties such as field strength or polarity.","types":["phenomenon"],"aliases":["magnetic variability"],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_e226e0486e08412c5382b2f9366db183"},{"public_id":"co_e52851cca2c9cd157cc138b10f528f5e","status":"active","name":"photospheric layers","description":"The visible surface layers of a star where the observed fluctuations are inferred to occur.","types":["astronomical layer"],"aliases":["photosphere"],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_e52851cca2c9cd157cc138b10f528f5e"},{"public_id":"co_f91d2042ca702a5dd7b530d0bbbb21e8","status":"active","name":"irregular magnetic variables","description":"Magnetic stars whose field behavior changes without a regular periodic pattern.","types":["astronomical object","variable star class"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_f91d2042ca702a5dd7b530d0bbbb21e8"},{"public_id":"co_fd2c397b979adab6201b908719a556ad","status":"active","name":"sharp-line stars","description":"Stars with narrow spectral lines that allow magnetic measurements and classification.","types":["astronomical object"],"aliases":[],"contributors":[{"id":1,"public_id":"12632b8b5f","public_label":"Anonymous (12632b8b5f)","roles":["extraction"],"url":"https://sah.borca.ai/u/12632b8b5f"}],"url":"https://sah.borca.ai/concepts/co_fd2c397b979adab6201b908719a556ad"}],"external_ids":{"DOI":"10.1086/190035","ArXiv":null,"PubMed":null,"PubMedCentral":null,"MAG":1964225025,"DBLP":null,"ACL":null},"open_access":{"is_open_access":false,"pdf_url":null,"landing_url":"https://sah.borca.ai/papers/119814400","source":null,"pdf_url_source":null,"license":null,"reason":"pdf_url_not_indexed"},"reference_availability":{"status":"unknown","references_indexed":false,"full_text_available":false,"full_text_source":null,"count_basis":"semantic_scholar_metadata","extraction_status":"not_applicable","reason":null},"source":{"provider":"episteme2","base_corpus":"semantic_scholar_dump","freshness_mode":"unknown","basis":["semantic_scholar_metadata","postgres_metadata"],"limits":["paper metadata is based on indexed upstream scholarly datasets","claims and concepts are available only for extracted papers","absence of claims or concepts means no extracted graph data is available in this response"],"status":"available","degraded":false,"degraded_reasons":[],"diagnostics":{"status":"available","degraded":false,"degraded_reasons":[],"metadata_status":"available","graph_status":"available","abstract_status":"available"},"source_flags":1},"paper_id":632237,"paper_uid":"84b4382e-2341-4082-9ae8-d4124ecd70d0","canonical_identity":{"paper_id":632237,"paper_uid":"84b4382e-2341-4082-9ae8-d4124ecd70d0","identity_status":"available","lookup_basis":"semantic_scholar_external_id","compatibility_path":"corpus_id"},"url":"https://sah.borca.ai/papers/119814400"}