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Fundamental Properties of O and B Stars with Optical Interferometry
We used interferometric observations made with the CHARA Array of 25 B-type stars and 6 O-type stars to obtain precise measurements of angular size, radius, and effective temperature to test stellar atmospheric models for massive stars. Our measured angular diameters range from 1.09 milli-arcseconds...
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Published in: | Proceedings of the International Astronomical Union 2022-05, Vol.18 (S361), p.382-386 |
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creator | Gordon, Kathryn D. Gies, Douglas R. Schaefer, Gail H. |
description | We used interferometric observations made with the CHARA Array of 25 B-type stars and 6 O-type stars to obtain precise measurements of angular size, radius, and effective temperature to test stellar atmospheric models for massive stars. Our measured angular diameters range from 1.09 milli-arcseconds (mas) for β Tau down to 0.11 mas for 10 Lac, the smallest star yet resolved with the CHARA Array. The rotational oblateness of the rapidly rotating star ζ Oph is directly measured for the first time. We collected ultraviolet to infrared spectrophotometry for all sample stars and derived temperatures, angular diameters, and reddening estimates that best fit the spectra. There is generally good agreement between the observed and spectral fit angular diameters for the O and B stars, indicating that the fluxes predicted from model atmospheres are reliable. The derived and model temperatures for the O stars are also in fair agreement, however the sample size is small and several of the O stars results we consider to be preliminary. On the other hand, the temperatures derived from angular diameters and fluxes tend to be larger (by ≈ 4%) for the B stars than those from published results based on analysis of the line spectrum (Gordon et al. 2018, 2019). |
doi_str_mv | 10.1017/S1743921322002642 |
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Our measured angular diameters range from 1.09 milli-arcseconds (mas) for β Tau down to 0.11 mas for 10 Lac, the smallest star yet resolved with the CHARA Array. The rotational oblateness of the rapidly rotating star ζ Oph is directly measured for the first time. We collected ultraviolet to infrared spectrophotometry for all sample stars and derived temperatures, angular diameters, and reddening estimates that best fit the spectra. There is generally good agreement between the observed and spectral fit angular diameters for the O and B stars, indicating that the fluxes predicted from model atmospheres are reliable. The derived and model temperatures for the O stars are also in fair agreement, however the sample size is small and several of the O stars results we consider to be preliminary. On the other hand, the temperatures derived from angular diameters and fluxes tend to be larger (by ≈ 4%) for the B stars than those from published results based on analysis of the line spectrum (Gordon et al. 2018, 2019).</description><identifier>ISSN: 1743-9213</identifier><identifier>EISSN: 1743-9221</identifier><identifier>DOI: 10.1017/S1743921322002642</identifier><language>eng</language><publisher>Cambridge, UK: Cambridge University Press</publisher><subject>Arrays ; Astronomical models ; B stars ; Contributed Paper ; Diameters ; Fluxes ; Infrared analysis ; Infrared spectra ; Infrared spectrophotometers ; Infrared stars ; Interferometry ; Massive stars ; O stars ; Optical properties ; Rotational spectra ; Spectrophotometry ; Stars & galaxies ; Stellar atmospheres ; Telescopes ; Temperature ; Ultraviolet spectra</subject><ispartof>Proceedings of the International Astronomical Union, 2022-05, Vol.18 (S361), p.382-386</ispartof><rights>The Author(s), 2024. 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IAU</addtitle><description>We used interferometric observations made with the CHARA Array of 25 B-type stars and 6 O-type stars to obtain precise measurements of angular size, radius, and effective temperature to test stellar atmospheric models for massive stars. Our measured angular diameters range from 1.09 milli-arcseconds (mas) for β Tau down to 0.11 mas for 10 Lac, the smallest star yet resolved with the CHARA Array. The rotational oblateness of the rapidly rotating star ζ Oph is directly measured for the first time. We collected ultraviolet to infrared spectrophotometry for all sample stars and derived temperatures, angular diameters, and reddening estimates that best fit the spectra. There is generally good agreement between the observed and spectral fit angular diameters for the O and B stars, indicating that the fluxes predicted from model atmospheres are reliable. The derived and model temperatures for the O stars are also in fair agreement, however the sample size is small and several of the O stars results we consider to be preliminary. On the other hand, the temperatures derived from angular diameters and fluxes tend to be larger (by ≈ 4%) for the B stars than those from published results based on analysis of the line spectrum (Gordon et al. 2018, 2019).</description><subject>Arrays</subject><subject>Astronomical models</subject><subject>B stars</subject><subject>Contributed Paper</subject><subject>Diameters</subject><subject>Fluxes</subject><subject>Infrared analysis</subject><subject>Infrared spectra</subject><subject>Infrared spectrophotometers</subject><subject>Infrared stars</subject><subject>Interferometry</subject><subject>Massive stars</subject><subject>O stars</subject><subject>Optical properties</subject><subject>Rotational spectra</subject><subject>Spectrophotometry</subject><subject>Stars & galaxies</subject><subject>Stellar atmospheres</subject><subject>Telescopes</subject><subject>Temperature</subject><subject>Ultraviolet spectra</subject><issn>1743-9213</issn><issn>1743-9221</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNp1kE1LAzEQhoMoWKs_wFvA8-pMkt1sjlqsFgoVqucl2U10S_fDJIv037ulRQ_iaYbhed6Bl5BrhFsElHdrlIIrhpwxAJYJdkIm-1OiGMPTnx35ObkIYQMgspynEzKbD22lG9tGvaUvvuutj7UNtHN0RXVb0Qe6jtoH-lXHD7rqY12O4KKN1jvru8ZGv7skZ05vg706zil5mz--zp6T5eppMbtfJiWiEInUlRHKOmlSZpxUAGCZ4IJrNBma3CBPsxJKcJVKMXcmVUoyFLIElivh-JTcHHJ7330ONsRi0w2-HV8WHFSOWS4zMVJ4oErfheCtK3pfN9rvCoRi31Xxp6vR4UdHN8bX1bv9jf7f-gZPT2kd</recordid><startdate>202205</startdate><enddate>202205</enddate><creator>Gordon, Kathryn D.</creator><creator>Gies, Douglas R.</creator><creator>Schaefer, Gail H.</creator><general>Cambridge University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>Q9U</scope><orcidid>https://orcid.org/0000-0003-1338-531X</orcidid><orcidid>https://orcid.org/0000-0001-8537-3583</orcidid></search><sort><creationdate>202205</creationdate><title>Fundamental Properties of O and B Stars with Optical Interferometry</title><author>Gordon, Kathryn D. ; Gies, Douglas R. ; Schaefer, Gail H.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c1144-7adb49ef7b52bf79000e24343a1b61b8b1356c0c0fd9518fb59972147c02894f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Arrays</topic><topic>Astronomical models</topic><topic>B stars</topic><topic>Contributed Paper</topic><topic>Diameters</topic><topic>Fluxes</topic><topic>Infrared analysis</topic><topic>Infrared spectra</topic><topic>Infrared spectrophotometers</topic><topic>Infrared stars</topic><topic>Interferometry</topic><topic>Massive stars</topic><topic>O stars</topic><topic>Optical properties</topic><topic>Rotational spectra</topic><topic>Spectrophotometry</topic><topic>Stars & galaxies</topic><topic>Stellar atmospheres</topic><topic>Telescopes</topic><topic>Temperature</topic><topic>Ultraviolet spectra</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Gordon, Kathryn D.</creatorcontrib><creatorcontrib>Gies, Douglas R.</creatorcontrib><creatorcontrib>Schaefer, Gail H.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>Advanced Technologies & Aerospace Database (1962 - current)</collection><collection>ProQuest Central Essentials</collection><collection>AUTh Library subscriptions: ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection (Proquest) (PQ_SDU_P3)</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database (ProQuest)</collection><collection>ProQuest Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>ProQuest Central Basic</collection><jtitle>Proceedings of the International Astronomical Union</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Gordon, Kathryn D.</au><au>Gies, Douglas R.</au><au>Schaefer, Gail H.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Fundamental Properties of O and B Stars with Optical Interferometry</atitle><jtitle>Proceedings of the International Astronomical Union</jtitle><addtitle>Proc. 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There is generally good agreement between the observed and spectral fit angular diameters for the O and B stars, indicating that the fluxes predicted from model atmospheres are reliable. The derived and model temperatures for the O stars are also in fair agreement, however the sample size is small and several of the O stars results we consider to be preliminary. On the other hand, the temperatures derived from angular diameters and fluxes tend to be larger (by ≈ 4%) for the B stars than those from published results based on analysis of the line spectrum (Gordon et al. 2018, 2019).</abstract><cop>Cambridge, UK</cop><pub>Cambridge University Press</pub><doi>10.1017/S1743921322002642</doi><tpages>5</tpages><orcidid>https://orcid.org/0000-0003-1338-531X</orcidid><orcidid>https://orcid.org/0000-0001-8537-3583</orcidid></addata></record> |
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subjects | Arrays Astronomical models B stars Contributed Paper Diameters Fluxes Infrared analysis Infrared spectra Infrared spectrophotometers Infrared stars Interferometry Massive stars O stars Optical properties Rotational spectra Spectrophotometry Stars & galaxies Stellar atmospheres Telescopes Temperature Ultraviolet spectra |
title | Fundamental Properties of O and B Stars with Optical Interferometry |
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