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Detailed Study of IU Per: An Eclipsing Semi-Detached Binary with Pulsating Component

This paper presents a comprehensive analysis of the binary star system IU Per, characterized as an eclipsing semi-detached binary with a pulsating component. Using CCD photometric observations in B and V filters, we explore the long-term behavior of the system, determine geometric and physical parameters, and analyze short-term light curve variations attributed to the pulsation activity of the primary component, typical of Delta Scuti stars. Our findings include orbital characteristics, period analysis, and connections to AG Dra, offering insights into the nature of this unique stellar system.

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Detailed Study of IU Per: An Eclipsing Semi-Detached Binary with Pulsating Component

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  1. Preliminarydiscussion on IU Per L. Hric, E. Kundra Astronomical Institute of the Slovak Academy of Sciences, 059 60TatranskáLomnica, Slovak Republic KOLOS 2011

  2. Abstract IU Perseiisaneclipsingsemi - detachedbinarywithpulsatingcomponent. Usingourphotometric CCD observations in B and V filtersweintroducethe model ofthissystem in detail. Wedeterminedthe (O - C) diagram behaviour and geometricandphysicalparametersofsemi – detachedsystem. Wedetectedtheshort – term variations on thelightcurve. What's more, weobtainedtheresidua, by comparisonofobservational and syntheticlightcurves, ofwhichthedetailedperiodanalysisenabled to characterize and localizetheirsource. WeexplainthesevariationsasthepulsationactivityoftheprimarycomponenttypicalfortheDelta ScutiStars.

  3. Outline • IU Per – overview of the system • Long-term photometric behaviour (activity, BV photometry, period analysis, discovery of 0.3 – 0.65 hours period) • Period analysis of IU Per and pulsation periods • Monitoring of (O – C) diagram • Conection with AG Dra

  4. IU Per – overview of the system • eclipsingsemi - detachedbinarywithpulsatingcomponent • a new memberoftheoscillating EA (oEA) stars, a groupofmass-accretingpulsatingcomponents in Algol-typesemi-detachedeclipsingbinarysystemsBuddinget al. (2004) • orbitalperiodof 0.8570257 day and MinI = HJD 2452500.214 • Kreiner (2004) • primarycomponent A4, secondary G6 IV • primarydelta Scuti type withpulsationperiodof 34 min and multi-periodicity • Kimet al. (1996) • 101 visual and photographicandonephotoelectrictimesof minima • Qian (2001) • MinI = HJD 2445611. 4370(10)+0. 85702955(32) x E – 4.82(78) x 10−10x E2 • (O – C) diagram onlyfrom 23 photoelectric and CCD data • Zhanget al. (2009)

  5. IU Per – overview of the system • (O – C) diagram onlyfrom 23 photoelectric and CCD data • Zhanget al. (2009) • linear and andquadraticephemeris • MinI = HJD 2454413. 0933(5)+0. 8685702543(20) x E • MinI = HJD 2454413. 0920(7)+0. 85702357(70) x E – 2.53(92) x 10-10 x E2 • on the base ofthelightcurveshapetheyproposed to reclassify IU Per to thegroupof EB and type ofBeta LyraeinsteadofAlgol type • To observethechangesof (O-C) diagram in thelongesttime intervalwetried to obtainallpossibledatapublished in theliterature • Nelson 2002, • Zejda, Mikulášek, Wolf, 2006 • Brátet al.2007, 2008, 2009 • Zhanget al. 2009) • By thesewereobtained 163 timesofprimary minima and 4 timesofsecondary minima.

  6. Observations

  7. (O – C) Qian et al. (2001)

  8. By Fitsch (1981) we calculated for the average density of the primary of IU Per and selected periods of pulsations ((0.0125 d, 0.0167 d, 0.0208 d, 0.025 d) we calculated the following values of pulsation constant 0.00635, 0.00846, 0.01058, 0.01270 Fitch (1981) From published models of pulsations of the stars of type sigma scuti (Fitch 1981) we identified for the pulsation constants 0.01058 and 0.01270 the following modes of pulsations: The fifth harmonic radial mode of pulsations 5H The sixth harmonic non-radial mode of pulsations p7

  9. Resonance in AG Dra • We discovered the resonance 14/9 between orbital and pulsation periods. • P orbital = (549.8 ± 0.8) days x 9 = 4948.2 ± 7.2 P pulsation = (352.8 ± 1.1) days x 14 = 4939.2 ± 15.4

  10. Thank you for your attention

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