Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis
We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti (δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Ast...
Gespeichert in:
| Veröffentlicht in: | The Astronomical journal 2019-01, Vol.157 (1), p.28 |
|---|---|
| Hauptverfasser: | , , , , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext bestellen |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | 1 |
| container_start_page | 28 |
| container_title | The Astronomical journal |
| container_volume | 157 |
| creator | Hong, Kyeongsoo Lee, Jae Woo Koo, Jae-Rim Park, Jang-Ho Kim, Seung-Lee Rittipruk, Pakakaew Kanjanasakul, Chanisa Han, Cheongho |
| description | We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti (δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Astronomy Observatory in Korea and the Thai National Observatory in Thailand during the 2016 and 2017 observing seasons. The radial velocities (RVs) of the primary and the faint secondary components were determined, and the effective temperature and projected rotational velocity of the former star were measured as Teff,1 = 8500 160 K and v1 sin i = 148 13 km s−1, respectively, through a comparison of the observed spectra and stellar atmosphere models. The physical properties of V392 Ori were determined by analysis of our RVs together with the existing multiband light curves. The results are the following: masses of M1 = 2.28 0.30 M and M2 = 0.49 0.10 M , and radii of R1 = 2.08 0.09 R and R2 = 1.15 0.05 R . The primary star located inside the main-sequence band exhibits a δ Sct-type pulsation. On the contrary, the less massive secondary component is significantly oversized and overluminous for its mass and temperature. |
| doi_str_mv | 10.3847/1538-3881/aaf39f |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_O3W</sourceid><recordid>TN_cdi_iop_journals_10_3847_1538_3881_aaf39f</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2365690752</sourcerecordid><originalsourceid>FETCH-LOGICAL-c378t-92ad1df279074a8d04605593d9bab38339d031a76e9a1f9032903c9f28675f93</originalsourceid><addsrcrecordid>eNp1UE1LAzEQDaJgrd49Bry6Nh_7kRxLqVUo7KHFa0izSZuy3axJeui_N8uKPXkYZhjem3nvAfCM0RtleTXDBWUZZQzPpDSUmxsw-VvdgglCKM9KUpT34CGEI0IYM5RPQL21J50F7a0OcNNrFb0LyvUX6AyMBw3roGzbymi7PVyq1vZhmObt3rVwcwlRn-AX5QTW3rrOhkdwZ2Qb9NNvn4Lt-3K7-MjW9epzMV9nilYsZpzIBjeGVBxVuWQNyktUFJw2fCd3lFHKG0SxrErNJTYcUZJKcUNYWRWG0yl4Gc-6EK1IEqNWB-W6LhkQhDBekTy_onrvvs86RHF0Z98lXYLQsijT84IkFBpRKlkPXhvRe3uS_iIwEkO2YghSDEGKMdtEeR0p1vXXm__CfwCG_Xiy</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2365690752</pqid></control><display><type>article</type><title>Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis</title><source>Institute of Physics Open Access Journal Titles</source><creator>Hong, Kyeongsoo ; Lee, Jae Woo ; Koo, Jae-Rim ; Park, Jang-Ho ; Kim, Seung-Lee ; Rittipruk, Pakakaew ; Kanjanasakul, Chanisa ; Han, Cheongho</creator><creatorcontrib>Hong, Kyeongsoo ; Lee, Jae Woo ; Koo, Jae-Rim ; Park, Jang-Ho ; Kim, Seung-Lee ; Rittipruk, Pakakaew ; Kanjanasakul, Chanisa ; Han, Cheongho</creatorcontrib><description>We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti (δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Astronomy Observatory in Korea and the Thai National Observatory in Thailand during the 2016 and 2017 observing seasons. The radial velocities (RVs) of the primary and the faint secondary components were determined, and the effective temperature and projected rotational velocity of the former star were measured as Teff,1 = 8500 160 K and v1 sin i = 148 13 km s−1, respectively, through a comparison of the observed spectra and stellar atmosphere models. The physical properties of V392 Ori were determined by analysis of our RVs together with the existing multiband light curves. The results are the following: masses of M1 = 2.28 0.30 M and M2 = 0.49 0.10 M , and radii of R1 = 2.08 0.09 R and R2 = 1.15 0.05 R . The primary star located inside the main-sequence band exhibits a δ Sct-type pulsation. On the contrary, the less massive secondary component is significantly oversized and overluminous for its mass and temperature.</description><identifier>ISSN: 0004-6256</identifier><identifier>ISSN: 1538-3881</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/aaf39f</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Astronomical models ; ASTRONOMY ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; Atmospheric models ; binaries: eclipsing ; Binary stars ; COMPARATIVE EVALUATIONS ; ECLIPSE ; Eclipsing binary stars ; Light curve ; MASS ; Observatories ; OSCILLATIONS ; Photometric observations ; Physical properties ; PULSATIONS ; RADIAL VELOCITY ; RESOLUTION ; Rotation ; SPECTRA ; SPECTROSCOPY ; Spectrum analysis ; STARS ; stars: fundamental parameters ; stars: individual (V392 Ori) ; stars: oscillations (including pulsations) ; STELLAR ATMOSPHERES ; Stellar models ; Temperature</subject><ispartof>The Astronomical journal, 2019-01, Vol.157 (1), p.28</ispartof><rights>2019. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Jan 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c378t-92ad1df279074a8d04605593d9bab38339d031a76e9a1f9032903c9f28675f93</citedby><cites>FETCH-LOGICAL-c378t-92ad1df279074a8d04605593d9bab38339d031a76e9a1f9032903c9f28675f93</cites><orcidid>0000-0001-9339-4456 ; 0000-0001-8969-0009 ; 0000-0002-5739-9804 ; 0000-0002-8692-2588 ; 0000-0002-2641-9964</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/aaf39f/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,315,782,786,887,27933,27934,38877,38899,53849,53876</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/aaf39f$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/biblio/22897244$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Hong, Kyeongsoo</creatorcontrib><creatorcontrib>Lee, Jae Woo</creatorcontrib><creatorcontrib>Koo, Jae-Rim</creatorcontrib><creatorcontrib>Park, Jang-Ho</creatorcontrib><creatorcontrib>Kim, Seung-Lee</creatorcontrib><creatorcontrib>Rittipruk, Pakakaew</creatorcontrib><creatorcontrib>Kanjanasakul, Chanisa</creatorcontrib><creatorcontrib>Han, Cheongho</creatorcontrib><title>Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti (δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Astronomy Observatory in Korea and the Thai National Observatory in Thailand during the 2016 and 2017 observing seasons. The radial velocities (RVs) of the primary and the faint secondary components were determined, and the effective temperature and projected rotational velocity of the former star were measured as Teff,1 = 8500 160 K and v1 sin i = 148 13 km s−1, respectively, through a comparison of the observed spectra and stellar atmosphere models. The physical properties of V392 Ori were determined by analysis of our RVs together with the existing multiband light curves. The results are the following: masses of M1 = 2.28 0.30 M and M2 = 0.49 0.10 M , and radii of R1 = 2.08 0.09 R and R2 = 1.15 0.05 R . The primary star located inside the main-sequence band exhibits a δ Sct-type pulsation. On the contrary, the less massive secondary component is significantly oversized and overluminous for its mass and temperature.</description><subject>Astronomical models</subject><subject>ASTRONOMY</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>Atmospheric models</subject><subject>binaries: eclipsing</subject><subject>Binary stars</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>ECLIPSE</subject><subject>Eclipsing binary stars</subject><subject>Light curve</subject><subject>MASS</subject><subject>Observatories</subject><subject>OSCILLATIONS</subject><subject>Photometric observations</subject><subject>Physical properties</subject><subject>PULSATIONS</subject><subject>RADIAL VELOCITY</subject><subject>RESOLUTION</subject><subject>Rotation</subject><subject>SPECTRA</subject><subject>SPECTROSCOPY</subject><subject>Spectrum analysis</subject><subject>STARS</subject><subject>stars: fundamental parameters</subject><subject>stars: individual (V392 Ori)</subject><subject>stars: oscillations (including pulsations)</subject><subject>STELLAR ATMOSPHERES</subject><subject>Stellar models</subject><subject>Temperature</subject><issn>0004-6256</issn><issn>1538-3881</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp1UE1LAzEQDaJgrd49Bry6Nh_7kRxLqVUo7KHFa0izSZuy3axJeui_N8uKPXkYZhjem3nvAfCM0RtleTXDBWUZZQzPpDSUmxsw-VvdgglCKM9KUpT34CGEI0IYM5RPQL21J50F7a0OcNNrFb0LyvUX6AyMBw3roGzbymi7PVyq1vZhmObt3rVwcwlRn-AX5QTW3rrOhkdwZ2Qb9NNvn4Lt-3K7-MjW9epzMV9nilYsZpzIBjeGVBxVuWQNyktUFJw2fCd3lFHKG0SxrErNJTYcUZJKcUNYWRWG0yl4Gc-6EK1IEqNWB-W6LhkQhDBekTy_onrvvs86RHF0Z98lXYLQsijT84IkFBpRKlkPXhvRe3uS_iIwEkO2YghSDEGKMdtEeR0p1vXXm__CfwCG_Xiy</recordid><startdate>20190101</startdate><enddate>20190101</enddate><creator>Hong, Kyeongsoo</creator><creator>Lee, Jae Woo</creator><creator>Koo, Jae-Rim</creator><creator>Park, Jang-Ho</creator><creator>Kim, Seung-Lee</creator><creator>Rittipruk, Pakakaew</creator><creator>Kanjanasakul, Chanisa</creator><creator>Han, Cheongho</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0001-9339-4456</orcidid><orcidid>https://orcid.org/0000-0001-8969-0009</orcidid><orcidid>https://orcid.org/0000-0002-5739-9804</orcidid><orcidid>https://orcid.org/0000-0002-8692-2588</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid></search><sort><creationdate>20190101</creationdate><title>Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis</title><author>Hong, Kyeongsoo ; Lee, Jae Woo ; Koo, Jae-Rim ; Park, Jang-Ho ; Kim, Seung-Lee ; Rittipruk, Pakakaew ; Kanjanasakul, Chanisa ; Han, Cheongho</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c378t-92ad1df279074a8d04605593d9bab38339d031a76e9a1f9032903c9f28675f93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astronomical models</topic><topic>ASTRONOMY</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>Atmospheric models</topic><topic>binaries: eclipsing</topic><topic>Binary stars</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>ECLIPSE</topic><topic>Eclipsing binary stars</topic><topic>Light curve</topic><topic>MASS</topic><topic>Observatories</topic><topic>OSCILLATIONS</topic><topic>Photometric observations</topic><topic>Physical properties</topic><topic>PULSATIONS</topic><topic>RADIAL VELOCITY</topic><topic>RESOLUTION</topic><topic>Rotation</topic><topic>SPECTRA</topic><topic>SPECTROSCOPY</topic><topic>Spectrum analysis</topic><topic>STARS</topic><topic>stars: fundamental parameters</topic><topic>stars: individual (V392 Ori)</topic><topic>stars: oscillations (including pulsations)</topic><topic>STELLAR ATMOSPHERES</topic><topic>Stellar models</topic><topic>Temperature</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Hong, Kyeongsoo</creatorcontrib><creatorcontrib>Lee, Jae Woo</creatorcontrib><creatorcontrib>Koo, Jae-Rim</creatorcontrib><creatorcontrib>Park, Jang-Ho</creatorcontrib><creatorcontrib>Kim, Seung-Lee</creatorcontrib><creatorcontrib>Rittipruk, Pakakaew</creatorcontrib><creatorcontrib>Kanjanasakul, Chanisa</creatorcontrib><creatorcontrib>Han, Cheongho</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astronomical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Hong, Kyeongsoo</au><au>Lee, Jae Woo</au><au>Koo, Jae-Rim</au><au>Park, Jang-Ho</au><au>Kim, Seung-Lee</au><au>Rittipruk, Pakakaew</au><au>Kanjanasakul, Chanisa</au><au>Han, Cheongho</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2019-01-01</date><risdate>2019</risdate><volume>157</volume><issue>1</issue><spage>28</spage><pages>28-</pages><issn>0004-6256</issn><issn>1538-3881</issn><eissn>1538-3881</eissn><abstract>We present the results from a detailed analysis of our high-resolution spectra and historical photometric observations of the semidetached eclipsing binary V392 Ori with a δ Scuti (δ Sct) pulsating component. A total of 31 spectroscopic observations were carried out at both the Bohyunsan Optical Astronomy Observatory in Korea and the Thai National Observatory in Thailand during the 2016 and 2017 observing seasons. The radial velocities (RVs) of the primary and the faint secondary components were determined, and the effective temperature and projected rotational velocity of the former star were measured as Teff,1 = 8500 160 K and v1 sin i = 148 13 km s−1, respectively, through a comparison of the observed spectra and stellar atmosphere models. The physical properties of V392 Ori were determined by analysis of our RVs together with the existing multiband light curves. The results are the following: masses of M1 = 2.28 0.30 M and M2 = 0.49 0.10 M , and radii of R1 = 2.08 0.09 R and R2 = 1.15 0.05 R . The primary star located inside the main-sequence band exhibits a δ Sct-type pulsation. On the contrary, the less massive secondary component is significantly oversized and overluminous for its mass and temperature.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/aaf39f</doi><tpages>8</tpages><orcidid>https://orcid.org/0000-0001-9339-4456</orcidid><orcidid>https://orcid.org/0000-0001-8969-0009</orcidid><orcidid>https://orcid.org/0000-0002-5739-9804</orcidid><orcidid>https://orcid.org/0000-0002-8692-2588</orcidid><orcidid>https://orcid.org/0000-0002-2641-9964</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-6256 |
| ispartof | The Astronomical journal, 2019-01, Vol.157 (1), p.28 |
| issn | 0004-6256 1538-3881 1538-3881 |
| language | eng |
| recordid | cdi_iop_journals_10_3847_1538_3881_aaf39f |
| source | Institute of Physics Open Access Journal Titles |
| subjects | Astronomical models ASTRONOMY ASTROPHYSICS, COSMOLOGY AND ASTRONOMY Atmospheric models binaries: eclipsing Binary stars COMPARATIVE EVALUATIONS ECLIPSE Eclipsing binary stars Light curve MASS Observatories OSCILLATIONS Photometric observations Physical properties PULSATIONS RADIAL VELOCITY RESOLUTION Rotation SPECTRA SPECTROSCOPY Spectrum analysis STARS stars: fundamental parameters stars: individual (V392 Ori) stars: oscillations (including pulsations) STELLAR ATMOSPHERES Stellar models Temperature |
| title | Time-series Spectroscopy of the Oscillating Eclipsing Algol System V392 Orionis |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-01T22%3A19%3A11IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_O3W&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Time-series%20Spectroscopy%20of%20the%20Oscillating%20Eclipsing%20Algol%20System%20V392%20Orionis&rft.jtitle=The%20Astronomical%20journal&rft.au=Hong,%20Kyeongsoo&rft.date=2019-01-01&rft.volume=157&rft.issue=1&rft.spage=28&rft.pages=28-&rft.issn=0004-6256&rft.eissn=1538-3881&rft_id=info:doi/10.3847/1538-3881/aaf39f&rft_dat=%3Cproquest_O3W%3E2365690752%3C/proquest_O3W%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2365690752&rft_id=info:pmid/&rfr_iscdi=true |