Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line
This is the second paper in a series dedicated to studies of the X-ray binary Cyg X-1 in the HeII λ 4686 Å line using 3D Doppler tomography. A detailed analysis of the tomogram constructed has made it possible for the first time to obtain information about the motions of gaseous flows including all...
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| Veröffentlicht in: | Astronomy reports 2018-03, Vol.62 (3), p.225-237 |
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| creator | Agafonov, M. I. Karitskaya, E. A. Sharova, O. I. Bochkarev, N. G. Zharikov, S. V. Butenko, G. Z. Bondar’, A. V. Bubukin, I. T. |
| description | This is the second paper in a series dedicated to studies of the X-ray binary Cyg X-1 in the HeII λ 4686 Å line using 3D Doppler tomography. A detailed analysis of the tomogram constructed has made it possible for the first time to obtain information about the motions of gaseous flows including all three velocity components. The observations were obtained in June 2007 at the Terskol Branch of the Institute of Astronomy (Russia) and the National Astronomical Observatory of Mexico. The correctness of the tomographic results and their discussion is analyzed. The results are compared with a 2D Doppler tomogram reconstruction. Model-atmosphere computations of HeII λ 4686 Å line profiles are used to estimate the influence of absorption features of the Osupergiant on the emission structure in the tomogram. The correctness of the 3D solutions is confirmed by the good agreement between the original sequence of spectral data and a control data set computed using the constructed 3D Doppler tomogram. Tomograms constructed using the data of each of the two observatories are compared. The results of the reconstruction for inclinations of the system of 40° and 45° essentially coincide. The maximum absorption (corresponding to the O supergiant) and emission structural features in the 3D tomogram are located in its central (
V
x
,
V
y
) section, where the velocity component perpendicular to the orbital plane
V
z
is zero. The emission is generated mainly in the outer part of the accretion structure, close to the supergiant. A gaseous stream from the Lagrangian point L1 with its motion close to the orbital plane can be distinguished. Its maximum velocity reaches 800 km/s. The identification of an emission structure with
V
z
~ 300 km/s and with
V
x
,
V
y
in the velocity interval corresponding to the donor star was unexpected. Its presence may indicate, for example, an outflow of matter from a magnetic pole of the supergiant. |
| doi_str_mv | 10.1134/S1063772918030010 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_journals_2015582904</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2015582904</sourcerecordid><originalsourceid>FETCH-LOGICAL-c268t-b3360b582bd255b1ecb282644cd32284963d3a37d9f55b5774ab77f238a48fe53</originalsourceid><addsrcrecordid>eNp1kM1Kw0AUhQdRsFYfwN0F19H5y2SyrK3aQsFFK7gLk2TSpiSZOJMKeQB9KZfufSYnVHAhrs6F75wD9yB0SfA1IYzfrAgWLIpoTCRmGBN8hEYkFDQQUpJjf3scDPwUnTm38w4imRih90mjqt6VDkwBbAYz07aVtrA2tdlY1W77AXRbDc-BVT3clo2yPax61-kapv2m2TuPCBTW1LBqddZZVcFj6rR9VV1pGgdlAxTjaNChaK4XC_j6AC6kgM83WJaNPkcnhaqcvvjRMXq6v1tP58Hy8WExnSyDjArZBSljAqehpGlOwzAlOkuppILzLGeUSh4LljPFojwuPA6jiKs0igrKpOKy0CEbo6tDb2vNy167LtmZvfUTuIRiEvrmGHPvIgdXZo1zVhdJa8va_50QnAxzJ3_m9hl6yDjvbTba_jb_H_oGxYN_NA</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2015582904</pqid></control><display><type>article</type><title>Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line</title><source>SpringerLink Journals</source><creator>Agafonov, M. I. ; Karitskaya, E. A. ; Sharova, O. I. ; Bochkarev, N. G. ; Zharikov, S. V. ; Butenko, G. Z. ; Bondar’, A. V. ; Bubukin, I. T.</creator><creatorcontrib>Agafonov, M. I. ; Karitskaya, E. A. ; Sharova, O. I. ; Bochkarev, N. G. ; Zharikov, S. V. ; Butenko, G. Z. ; Bondar’, A. V. ; Bubukin, I. T.</creatorcontrib><description>This is the second paper in a series dedicated to studies of the X-ray binary Cyg X-1 in the HeII λ 4686 Å line using 3D Doppler tomography. A detailed analysis of the tomogram constructed has made it possible for the first time to obtain information about the motions of gaseous flows including all three velocity components. The observations were obtained in June 2007 at the Terskol Branch of the Institute of Astronomy (Russia) and the National Astronomical Observatory of Mexico. The correctness of the tomographic results and their discussion is analyzed. The results are compared with a 2D Doppler tomogram reconstruction. Model-atmosphere computations of HeII λ 4686 Å line profiles are used to estimate the influence of absorption features of the Osupergiant on the emission structure in the tomogram. The correctness of the 3D solutions is confirmed by the good agreement between the original sequence of spectral data and a control data set computed using the constructed 3D Doppler tomogram. Tomograms constructed using the data of each of the two observatories are compared. The results of the reconstruction for inclinations of the system of 40° and 45° essentially coincide. The maximum absorption (corresponding to the O supergiant) and emission structural features in the 3D tomogram are located in its central (
V
x
,
V
y
) section, where the velocity component perpendicular to the orbital plane
V
z
is zero. The emission is generated mainly in the outer part of the accretion structure, close to the supergiant. A gaseous stream from the Lagrangian point L1 with its motion close to the orbital plane can be distinguished. Its maximum velocity reaches 800 km/s. The identification of an emission structure with
V
z
~ 300 km/s and with
V
x
,
V
y
in the velocity interval corresponding to the donor star was unexpected. Its presence may indicate, for example, an outflow of matter from a magnetic pole of the supergiant.</description><identifier>ISSN: 1063-7729</identifier><identifier>EISSN: 1562-6881</identifier><identifier>DOI: 10.1134/S1063772918030010</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Absorption ; Astronomy ; Binary stars ; Celestial bodies ; Construction ; Control data (computers) ; Deposition ; Emission ; Emissions ; Lagrangian equilibrium points ; Magnetic poles ; Observations and Techniques ; Observatories ; Outflow ; Physics ; Physics and Astronomy ; Reconstruction ; Tomography ; Two dimensional models ; Velocity ; X ray binaries ; X ray stars ; X-ray astronomy</subject><ispartof>Astronomy reports, 2018-03, Vol.62 (3), p.225-237</ispartof><rights>Pleiades Publishing, Ltd. 2018</rights><rights>Astronomy Reports is a copyright of Springer, (2018). All Rights Reserved.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c268t-b3360b582bd255b1ecb282644cd32284963d3a37d9f55b5774ab77f238a48fe53</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S1063772918030010$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S1063772918030010$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,780,784,27924,27925,41488,42557,51319</link.rule.ids></links><search><creatorcontrib>Agafonov, M. I.</creatorcontrib><creatorcontrib>Karitskaya, E. A.</creatorcontrib><creatorcontrib>Sharova, O. I.</creatorcontrib><creatorcontrib>Bochkarev, N. G.</creatorcontrib><creatorcontrib>Zharikov, S. V.</creatorcontrib><creatorcontrib>Butenko, G. Z.</creatorcontrib><creatorcontrib>Bondar’, A. V.</creatorcontrib><creatorcontrib>Bubukin, I. T.</creatorcontrib><title>Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line</title><title>Astronomy reports</title><addtitle>Astron. Rep</addtitle><description>This is the second paper in a series dedicated to studies of the X-ray binary Cyg X-1 in the HeII λ 4686 Å line using 3D Doppler tomography. A detailed analysis of the tomogram constructed has made it possible for the first time to obtain information about the motions of gaseous flows including all three velocity components. The observations were obtained in June 2007 at the Terskol Branch of the Institute of Astronomy (Russia) and the National Astronomical Observatory of Mexico. The correctness of the tomographic results and their discussion is analyzed. The results are compared with a 2D Doppler tomogram reconstruction. Model-atmosphere computations of HeII λ 4686 Å line profiles are used to estimate the influence of absorption features of the Osupergiant on the emission structure in the tomogram. The correctness of the 3D solutions is confirmed by the good agreement between the original sequence of spectral data and a control data set computed using the constructed 3D Doppler tomogram. Tomograms constructed using the data of each of the two observatories are compared. The results of the reconstruction for inclinations of the system of 40° and 45° essentially coincide. The maximum absorption (corresponding to the O supergiant) and emission structural features in the 3D tomogram are located in its central (
V
x
,
V
y
) section, where the velocity component perpendicular to the orbital plane
V
z
is zero. The emission is generated mainly in the outer part of the accretion structure, close to the supergiant. A gaseous stream from the Lagrangian point L1 with its motion close to the orbital plane can be distinguished. Its maximum velocity reaches 800 km/s. The identification of an emission structure with
V
z
~ 300 km/s and with
V
x
,
V
y
in the velocity interval corresponding to the donor star was unexpected. Its presence may indicate, for example, an outflow of matter from a magnetic pole of the supergiant.</description><subject>Absorption</subject><subject>Astronomy</subject><subject>Binary stars</subject><subject>Celestial bodies</subject><subject>Construction</subject><subject>Control data (computers)</subject><subject>Deposition</subject><subject>Emission</subject><subject>Emissions</subject><subject>Lagrangian equilibrium points</subject><subject>Magnetic poles</subject><subject>Observations and Techniques</subject><subject>Observatories</subject><subject>Outflow</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Reconstruction</subject><subject>Tomography</subject><subject>Two dimensional models</subject><subject>Velocity</subject><subject>X ray binaries</subject><subject>X ray stars</subject><subject>X-ray astronomy</subject><issn>1063-7729</issn><issn>1562-6881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNp1kM1Kw0AUhQdRsFYfwN0F19H5y2SyrK3aQsFFK7gLk2TSpiSZOJMKeQB9KZfufSYnVHAhrs6F75wD9yB0SfA1IYzfrAgWLIpoTCRmGBN8hEYkFDQQUpJjf3scDPwUnTm38w4imRih90mjqt6VDkwBbAYz07aVtrA2tdlY1W77AXRbDc-BVT3clo2yPax61-kapv2m2TuPCBTW1LBqddZZVcFj6rR9VV1pGgdlAxTjaNChaK4XC_j6AC6kgM83WJaNPkcnhaqcvvjRMXq6v1tP58Hy8WExnSyDjArZBSljAqehpGlOwzAlOkuppILzLGeUSh4LljPFojwuPA6jiKs0igrKpOKy0CEbo6tDb2vNy167LtmZvfUTuIRiEvrmGHPvIgdXZo1zVhdJa8va_50QnAxzJ3_m9hl6yDjvbTba_jb_H_oGxYN_NA</recordid><startdate>20180301</startdate><enddate>20180301</enddate><creator>Agafonov, M. I.</creator><creator>Karitskaya, E. A.</creator><creator>Sharova, O. I.</creator><creator>Bochkarev, N. G.</creator><creator>Zharikov, S. V.</creator><creator>Butenko, G. Z.</creator><creator>Bondar’, A. V.</creator><creator>Bubukin, I. T.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</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>KL.</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></search><sort><creationdate>20180301</creationdate><title>Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line</title><author>Agafonov, M. I. ; Karitskaya, E. A. ; Sharova, O. I. ; Bochkarev, N. G. ; Zharikov, S. V. ; Butenko, G. Z. ; Bondar’, A. V. ; Bubukin, I. T.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c268t-b3360b582bd255b1ecb282644cd32284963d3a37d9f55b5774ab77f238a48fe53</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Absorption</topic><topic>Astronomy</topic><topic>Binary stars</topic><topic>Celestial bodies</topic><topic>Construction</topic><topic>Control data (computers)</topic><topic>Deposition</topic><topic>Emission</topic><topic>Emissions</topic><topic>Lagrangian equilibrium points</topic><topic>Magnetic poles</topic><topic>Observations and Techniques</topic><topic>Observatories</topic><topic>Outflow</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Reconstruction</topic><topic>Tomography</topic><topic>Two dimensional models</topic><topic>Velocity</topic><topic>X ray binaries</topic><topic>X ray stars</topic><topic>X-ray astronomy</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Agafonov, M. I.</creatorcontrib><creatorcontrib>Karitskaya, E. A.</creatorcontrib><creatorcontrib>Sharova, O. I.</creatorcontrib><creatorcontrib>Bochkarev, N. G.</creatorcontrib><creatorcontrib>Zharikov, S. V.</creatorcontrib><creatorcontrib>Butenko, G. Z.</creatorcontrib><creatorcontrib>Bondar’, A. V.</creatorcontrib><creatorcontrib>Bubukin, I. T.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</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 Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>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>Astronomy reports</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Agafonov, M. I.</au><au>Karitskaya, E. A.</au><au>Sharova, O. I.</au><au>Bochkarev, N. G.</au><au>Zharikov, S. V.</au><au>Butenko, G. Z.</au><au>Bondar’, A. V.</au><au>Bubukin, I. T.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line</atitle><jtitle>Astronomy reports</jtitle><stitle>Astron. Rep</stitle><date>2018-03-01</date><risdate>2018</risdate><volume>62</volume><issue>3</issue><spage>225</spage><epage>237</epage><pages>225-237</pages><issn>1063-7729</issn><eissn>1562-6881</eissn><abstract>This is the second paper in a series dedicated to studies of the X-ray binary Cyg X-1 in the HeII λ 4686 Å line using 3D Doppler tomography. A detailed analysis of the tomogram constructed has made it possible for the first time to obtain information about the motions of gaseous flows including all three velocity components. The observations were obtained in June 2007 at the Terskol Branch of the Institute of Astronomy (Russia) and the National Astronomical Observatory of Mexico. The correctness of the tomographic results and their discussion is analyzed. The results are compared with a 2D Doppler tomogram reconstruction. Model-atmosphere computations of HeII λ 4686 Å line profiles are used to estimate the influence of absorption features of the Osupergiant on the emission structure in the tomogram. The correctness of the 3D solutions is confirmed by the good agreement between the original sequence of spectral data and a control data set computed using the constructed 3D Doppler tomogram. Tomograms constructed using the data of each of the two observatories are compared. The results of the reconstruction for inclinations of the system of 40° and 45° essentially coincide. The maximum absorption (corresponding to the O supergiant) and emission structural features in the 3D tomogram are located in its central (
V
x
,
V
y
) section, where the velocity component perpendicular to the orbital plane
V
z
is zero. The emission is generated mainly in the outer part of the accretion structure, close to the supergiant. A gaseous stream from the Lagrangian point L1 with its motion close to the orbital plane can be distinguished. Its maximum velocity reaches 800 km/s. The identification of an emission structure with
V
z
~ 300 km/s and with
V
x
,
V
y
in the velocity interval corresponding to the donor star was unexpected. Its presence may indicate, for example, an outflow of matter from a magnetic pole of the supergiant.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.1134/S1063772918030010</doi><tpages>13</tpages></addata></record> |
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| source | SpringerLink Journals |
| subjects | Absorption Astronomy Binary stars Celestial bodies Construction Control data (computers) Deposition Emission Emissions Lagrangian equilibrium points Magnetic poles Observations and Techniques Observatories Outflow Physics Physics and Astronomy Reconstruction Tomography Two dimensional models Velocity X ray binaries X ray stars X-ray astronomy |
| title | Analysis of 3D Doppler Tomography of the X-ray Binary System Cygnus X-1 from Spectral Observations in 2007 in the HeII λ 4686 Å Line |
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