UBVRI Photometric Study of the Totally Eclipsing Very Short Period W Ursae Majoris Binary GSC 2765-0348
ABSTRACT GSC 2765-0348 is a very short period ( P = 0.2835 d), solar type, G4V contact binary. Complete BVRI and partial U light curves covering the secondary eclipse are presented, along with a period study, surface temperature determination, and a simultaneous UBVRI light-curve solution. Our light...
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Veröffentlicht in: | Publications of the Astronomical Society of the Pacific 2012-10, Vol.124 (920), p.1025-1034 |
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creator | Samec, Ronald G. Flaaten, Daniel Jaso, Adam Oliver, Bruce Rehn, Travis Faulkner, Danny R. Van Hamme, W. |
description | ABSTRACT GSC 2765-0348 is a very short period ( P = 0.2835 d), solar type, G4V contact binary. Complete BVRI and partial U light curves covering the secondary eclipse are presented, along with a period study, surface temperature determination, and a simultaneous UBVRI light-curve solution. Our light curves show low-level ripples, surface activity, and asymmetries due to magnetic activity. Light curve amplitudes vary from 0.4-0.6 mag ( V) in the primary and secondary eclipses. The difference in adjacent maxima varies from ∼3-5%. Modeled results include two spot regions, one hot and one cool, both at equatorial positions of the primary, more massive component. A firm 34% fill-out and a small mass ratio of 0.31 is also determined. A total eclipse of 33 minutes is found to occur in the secondary eclipse, making GSC 2765-0348 a W-type (less massive star is hotter), W UMa variable. |
doi_str_mv | 10.1086/668126 |
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Complete BVRI and partial U light curves covering the secondary eclipse are presented, along with a period study, surface temperature determination, and a simultaneous UBVRI light-curve solution. Our light curves show low-level ripples, surface activity, and asymmetries due to magnetic activity. Light curve amplitudes vary from 0.4-0.6 mag ( V) in the primary and secondary eclipses. The difference in adjacent maxima varies from ∼3-5%. Modeled results include two spot regions, one hot and one cool, both at equatorial positions of the primary, more massive component. A firm 34% fill-out and a small mass ratio of 0.31 is also determined. A total eclipse of 33 minutes is found to occur in the secondary eclipse, making GSC 2765-0348 a W-type (less massive star is hotter), W UMa variable.</description><identifier>ISSN: 0004-6280</identifier><identifier>EISSN: 1538-3873</identifier><identifier>DOI: 10.1086/668126</identifier><identifier>CODEN: PASPAU</identifier><language>eng</language><publisher>Chicago, IL: University of Chicago Press</publisher><subject>Astronomy ; Earth, ocean, space ; Exact sciences and technology</subject><ispartof>Publications of the Astronomical Society of the Pacific, 2012-10, Vol.124 (920), p.1025-1034</ispartof><rights>2012. The Astronomical Society of the Pacific. All rights reserved. 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Complete BVRI and partial U light curves covering the secondary eclipse are presented, along with a period study, surface temperature determination, and a simultaneous UBVRI light-curve solution. Our light curves show low-level ripples, surface activity, and asymmetries due to magnetic activity. Light curve amplitudes vary from 0.4-0.6 mag ( V) in the primary and secondary eclipses. The difference in adjacent maxima varies from ∼3-5%. Modeled results include two spot regions, one hot and one cool, both at equatorial positions of the primary, more massive component. A firm 34% fill-out and a small mass ratio of 0.31 is also determined. 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Complete BVRI and partial U light curves covering the secondary eclipse are presented, along with a period study, surface temperature determination, and a simultaneous UBVRI light-curve solution. Our light curves show low-level ripples, surface activity, and asymmetries due to magnetic activity. Light curve amplitudes vary from 0.4-0.6 mag ( V) in the primary and secondary eclipses. The difference in adjacent maxima varies from ∼3-5%. Modeled results include two spot regions, one hot and one cool, both at equatorial positions of the primary, more massive component. A firm 34% fill-out and a small mass ratio of 0.31 is also determined. A total eclipse of 33 minutes is found to occur in the secondary eclipse, making GSC 2765-0348 a W-type (less massive star is hotter), W UMa variable.</abstract><cop>Chicago, IL</cop><pub>University of Chicago Press</pub><doi>10.1086/668126</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
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subjects | Astronomy Earth, ocean, space Exact sciences and technology |
title | UBVRI Photometric Study of the Totally Eclipsing Very Short Period W Ursae Majoris Binary GSC 2765-0348 |
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