CCD Photometry of the W UMa type star QX Andromeda
We present new B- and V-band photometry of the W UMa-type binary system QX And, which is a member of the open cluster NGC 752. Revised orbital period and new ephemerides were given for the binary system based on the data of times of light minima. The result of a period analysis reveals that the syst...
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| Veröffentlicht in: | New astronomy 2011-04, Vol.16 (3), p.194-198 |
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| creator | Ren, A.B. Zhang, X.B. Luo, C.Q. Luo, Y.P. Deng, L.C. Luo, Z.Q. |
| description | We present new
B- and
V-band photometry of the W UMa-type binary system QX And, which is a member of the open cluster NGC 752. Revised orbital period and new ephemerides were given for the binary system based on the data of times of light minima. The result of a period analysis reveals that the system is undergoing a continuous orbital period increase during the past decades. The rate of period increasing turns out to be about 2.7
×
10
−7
d
yr
−1. With the Wilson–Devinney code, a photometric solution is computed. It yields a contact configuration for the system with a filling factor of 0.361. Combining the results from the photometric solution along with that from the radial-velocity observations, we have determined the absolute parameters for the two components of the system. The masses, radii and luminosity of the primary and secondary stars are calculated as 1.43
±
0.04
M
⊙, 1.45
±
0.09
R
⊙, 2.87
±
0.40
L
⊙ and 0.44
±
0.02
M
⊙, 0.87
±
0.05
R
⊙, 0.99
±
0.13
L
⊙, respectively. The evolutionary status and physical nature of the contact binary system were discussed compared with the theoretical models. |
| doi_str_mv | 10.1016/j.newast.2010.08.007 |
| format | Article |
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B- and
V-band photometry of the W UMa-type binary system QX And, which is a member of the open cluster NGC 752. Revised orbital period and new ephemerides were given for the binary system based on the data of times of light minima. The result of a period analysis reveals that the system is undergoing a continuous orbital period increase during the past decades. The rate of period increasing turns out to be about 2.7
×
10
−7
d
yr
−1. With the Wilson–Devinney code, a photometric solution is computed. It yields a contact configuration for the system with a filling factor of 0.361. Combining the results from the photometric solution along with that from the radial-velocity observations, we have determined the absolute parameters for the two components of the system. The masses, radii and luminosity of the primary and secondary stars are calculated as 1.43
±
0.04
M
⊙, 1.45
±
0.09
R
⊙, 2.87
±
0.40
L
⊙ and 0.44
±
0.02
M
⊙, 0.87
±
0.05
R
⊙, 0.99
±
0.13
L
⊙, respectively. The evolutionary status and physical nature of the contact binary system were discussed compared with the theoretical models.</description><identifier>ISSN: 1384-1076</identifier><identifier>EISSN: 1384-1092</identifier><identifier>DOI: 10.1016/j.newast.2010.08.007</identifier><language>eng</language><publisher>Elsevier B.V</publisher><subject>Binaries: close ; Binaries: eclipsing ; Open cluster and associations: individual (NGC 752) ; Stars individual (QX Andromeda) ; Stars: evolution</subject><ispartof>New astronomy, 2011-04, Vol.16 (3), p.194-198</ispartof><rights>2010 Elsevier B.V.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c338t-6f7ae240974b31d9129ceb6d0ffe8124b9cc16be6d875d17469cb3c9da2ba3a23</citedby><cites>FETCH-LOGICAL-c338t-6f7ae240974b31d9129ceb6d0ffe8124b9cc16be6d875d17469cb3c9da2ba3a23</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://dx.doi.org/10.1016/j.newast.2010.08.007$$EHTML$$P50$$Gelsevier$$H</linktohtml><link.rule.ids>315,781,785,3551,27929,27930,46000</link.rule.ids></links><search><creatorcontrib>Ren, A.B.</creatorcontrib><creatorcontrib>Zhang, X.B.</creatorcontrib><creatorcontrib>Luo, C.Q.</creatorcontrib><creatorcontrib>Luo, Y.P.</creatorcontrib><creatorcontrib>Deng, L.C.</creatorcontrib><creatorcontrib>Luo, Z.Q.</creatorcontrib><title>CCD Photometry of the W UMa type star QX Andromeda</title><title>New astronomy</title><description>We present new
B- and
V-band photometry of the W UMa-type binary system QX And, which is a member of the open cluster NGC 752. Revised orbital period and new ephemerides were given for the binary system based on the data of times of light minima. The result of a period analysis reveals that the system is undergoing a continuous orbital period increase during the past decades. The rate of period increasing turns out to be about 2.7
×
10
−7
d
yr
−1. With the Wilson–Devinney code, a photometric solution is computed. It yields a contact configuration for the system with a filling factor of 0.361. Combining the results from the photometric solution along with that from the radial-velocity observations, we have determined the absolute parameters for the two components of the system. The masses, radii and luminosity of the primary and secondary stars are calculated as 1.43
±
0.04
M
⊙, 1.45
±
0.09
R
⊙, 2.87
±
0.40
L
⊙ and 0.44
±
0.02
M
⊙, 0.87
±
0.05
R
⊙, 0.99
±
0.13
L
⊙, respectively. The evolutionary status and physical nature of the contact binary system were discussed compared with the theoretical models.</description><subject>Binaries: close</subject><subject>Binaries: eclipsing</subject><subject>Open cluster and associations: individual (NGC 752)</subject><subject>Stars individual (QX Andromeda)</subject><subject>Stars: evolution</subject><issn>1384-1076</issn><issn>1384-1092</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNp9kE9LAzEUxIMoWKvfwENunnbNn-1uchHKalWoqGDRW8gmb-mWdlOTVOm3N2XFo6c3PH4zMIPQJSU5JbS8XuU9fOsQc0bSi4ickOoIjSgXRUaJZMd_uipP0VkIK5IIKsUIsbq-xS9LF90Got9j1-K4BPyOF08ax_0WcIja49cPPO2tT5DV5-ik1esAF793jBazu7f6IZs_3z_W03lmOBcxK9tKAyuIrIqGUyspkwaa0pK2BUFZ0UhjaNlAaUU1sbQqSmkabqTVrNFcMz5GV0Pu1rvPHYSoNl0wsF7rHtwuKCE4oRNBZSKLgTTeheChVVvfbbTfK0rUYSG1UsNC6rCQIkKl_sl2M9ggtfjqwKtgOugN2M6Dicq67v-AH9Hhb3M</recordid><startdate>20110401</startdate><enddate>20110401</enddate><creator>Ren, A.B.</creator><creator>Zhang, X.B.</creator><creator>Luo, C.Q.</creator><creator>Luo, Y.P.</creator><creator>Deng, L.C.</creator><creator>Luo, Z.Q.</creator><general>Elsevier B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20110401</creationdate><title>CCD Photometry of the W UMa type star QX Andromeda</title><author>Ren, A.B. ; Zhang, X.B. ; Luo, C.Q. ; Luo, Y.P. ; Deng, L.C. ; Luo, Z.Q.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c338t-6f7ae240974b31d9129ceb6d0ffe8124b9cc16be6d875d17469cb3c9da2ba3a23</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2011</creationdate><topic>Binaries: close</topic><topic>Binaries: eclipsing</topic><topic>Open cluster and associations: individual (NGC 752)</topic><topic>Stars individual (QX Andromeda)</topic><topic>Stars: evolution</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Ren, A.B.</creatorcontrib><creatorcontrib>Zhang, X.B.</creatorcontrib><creatorcontrib>Luo, C.Q.</creatorcontrib><creatorcontrib>Luo, Y.P.</creatorcontrib><creatorcontrib>Deng, L.C.</creatorcontrib><creatorcontrib>Luo, Z.Q.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>New astronomy</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ren, A.B.</au><au>Zhang, X.B.</au><au>Luo, C.Q.</au><au>Luo, Y.P.</au><au>Deng, L.C.</au><au>Luo, Z.Q.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>CCD Photometry of the W UMa type star QX Andromeda</atitle><jtitle>New astronomy</jtitle><date>2011-04-01</date><risdate>2011</risdate><volume>16</volume><issue>3</issue><spage>194</spage><epage>198</epage><pages>194-198</pages><issn>1384-1076</issn><eissn>1384-1092</eissn><abstract>We present new
B- and
V-band photometry of the W UMa-type binary system QX And, which is a member of the open cluster NGC 752. Revised orbital period and new ephemerides were given for the binary system based on the data of times of light minima. The result of a period analysis reveals that the system is undergoing a continuous orbital period increase during the past decades. The rate of period increasing turns out to be about 2.7
×
10
−7
d
yr
−1. With the Wilson–Devinney code, a photometric solution is computed. It yields a contact configuration for the system with a filling factor of 0.361. Combining the results from the photometric solution along with that from the radial-velocity observations, we have determined the absolute parameters for the two components of the system. The masses, radii and luminosity of the primary and secondary stars are calculated as 1.43
±
0.04
M
⊙, 1.45
±
0.09
R
⊙, 2.87
±
0.40
L
⊙ and 0.44
±
0.02
M
⊙, 0.87
±
0.05
R
⊙, 0.99
±
0.13
L
⊙, respectively. The evolutionary status and physical nature of the contact binary system were discussed compared with the theoretical models.</abstract><pub>Elsevier B.V</pub><doi>10.1016/j.newast.2010.08.007</doi><tpages>5</tpages></addata></record> |
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| ispartof | New astronomy, 2011-04, Vol.16 (3), p.194-198 |
| issn | 1384-1076 1384-1092 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_883015819 |
| source | Access via ScienceDirect (Elsevier) |
| subjects | Binaries: close Binaries: eclipsing Open cluster and associations: individual (NGC 752) Stars individual (QX Andromeda) Stars: evolution |
| title | CCD Photometry of the W UMa type star QX Andromeda |
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