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HaFLUORESCENCEINUVACTIVEBINARYSTARS By TODDRUSSELLVACCARO ADISSERTATION PRESENTEDTOTHEGRADUATESCHOOL OFTHEUNIVERSITYOFFLORIDAINPARTIALFULFILLMENT OFTHEREQUIREMENTSFORTHEDEGREEOF DOCTOROFPHILOSOPHY UNIVERSITYOFFLORIDA ACKNOWLEDGMENTS Iwouldliketothankmyadvisorforalltheassistanceandguidancehehas givenmeoverthepastfewyears,especiallyforgoingona12nightobservingrunand obtainingthephotometryusedinthiswork. WewouldliketothanktheKittPeak NationalObservatoryandtheSoutheasternAssociationlorResearchinAstronomy forgivingusthetelescopetime. Weareespeciallygratefulfortheobservingsupport ofWalterVanHamme,RolandoBranley,PeterMack,andGerriePeters. Iamgratefultomygraduatecommitteemembersfortakingthetimeoutto performthisduty. I would liketothanktheDepartmentofAstronomyfortheteachingassis- tantshipsthathavemostlysupportedmeduringmytimehereattheUniversityot Floridaandforthefinancialassistanceintravelingtosomeofthemeetings1have attended. Iamespeciallygratefultomywife,Paula,whoselove,patience,support,and devotionhaveallmadethispossible. TABLEOFCONTENTS ACKNOWLEDGMENTS ii LISTOFTABLES iv LISTOFFIGURES v ABSTRACT viii CHAPTERS 1 INTRODUCTION 1 1.1 TheStudyofBinaryStars 1 1.2 UVActiveBinaryStarsandFluorescence 1 2 THESCIENTIFICSTRATEGY 4 2.1 TheModels 4 2.2 TheCandidateSystems 9 3 THEDATA 12 3.1 OurObservations 12 3.2 Photometry 12 3.3 Spectroscopy 14 4 THEANALYSIS 16 4.1 FFAqr 16 4.2 V471Tau 31 5 CONCLUSION 78 REFERENCES 80 BIOGRAPHICALSKETCH 82 iii LISTOFTABLES 3.1 Photometriccoverage 14 3.2 Radialvelocitylines 14 4.1 FFAqrparametersolutions 18 4.2 FFAqrspotsolutions 19 4.3 V471Tauparametersolutions 34 4.4 V471Tauspotparameters 34 IV LISTOFFIGURES 2.1 Modellightcurves: ellipsoidaleffects (top) andellipsoidalcombined withreflectioneffects(bottom) 5 2.2 TheHaprofilemodelofthebacksideofthestar(eclipse) 9 2.3 TheHaprofilemodelshowingthefluorescingregionrotatingintoview (phase=0.30) 9 2.4 TheHaprofilemodelwithfluorescingregioninfullview(phase=0.50). 10 4.1 Themodelradialvelocitycurve(solidline)andourobservedvelocities (points) 19 4.2 Ourmodellightcurve(solidline)andphotometricmeasurements(points) extractedfromthephaseplotintheliterature 20 4.3 SIcmaalgeedspwiecrteurmesadoefwFiFthAqthretWhaDt sprhoogwrathmespots used inourmodels. 22 4.4 LightcurvemodelswithWD(solidline)comparedwithourphotom- etry(dots)ineachcolorobserved 23 4.5 Themodelradialvelocitycurve,whichincludesspots(solidline)and ourobservedvelocities(points) 24 4.6 ObservedspectrumofFFAqrat0=0.52(solidline)andthemodeled Felineat6400A(dashedline) 24 4.7 ObservedspectraofFFAqr(dots)andthemodeledHaprofile(solid line)forphases0.06-0.28 26 4.8 ObservedspectraofFFAqr(dots)andthemodeledHaprofile(solid line)forphases0.30-0.52 27 4.9 ObservedspectraofFFAqr(dots)andthemodeledHaprofile(solid line)forphases0.63-0.95 28 4.10 Themodelradialvelocitycurve(solidline)andourobservedvelocities (points) 33 4.11 IScmaalgeedspwiecrteuremsadofeVw4i7t1htThaeuWtDhatpsrhoogwratmhespotsusedinourmodels. 36 v 4.12 LightcurvemodelswithWD(solidline)comparedwithourphotom- etry(dots)ineachcolorobserved 37 4.13 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.00-0.01 38 4.14 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.03-0.04 40 4.15 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.07-0.08 41 4.16 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.09-0.10 42 4.17 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.12-0.14 43 1.18 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.16-0.17 44 4.19 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.18-0.20 45 4.20 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.21-0.22 46 4.21 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.23-0.24 47 4.22 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.25-0.29 48 4.23 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.30-0.31 49 4.24 ObservedspectraofV471Tau(symbols)andthemodeledHo profile (solidline)forphases0.33-0.35 50 4.25 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.36-0.37 51 4.26 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.39-0.40 52 4.27 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.41-0.42 53 4.28 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.43-0.45 54 4.29 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.46-0.47 55 vi 4.30 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.48-0.49 56 4.31 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.50-0.51 57 4.32 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.52-0.53 61 4.33 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.54-0.58 62 4.34 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.60-0.61 63 4.35 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.62-0.64 64 4.36 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.65-0.67 65 4.37 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.68-0.69 66 4.38 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.71-0.72 67 4.39 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.73-0.75 68 4.40 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.76-0.77 69 4.41 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.78-0.80 70 4.42 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.81-0.82 71 4.43 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.84-0.86 72 4.44 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.89-0.90 73 4.45 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.91-0.92 74 4.46 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.93-0.94 75 4.47 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.95-0.96 76 vii 4.48 ObservedspectraofV471Tau(symbols)andthemodeledHaprofile (solidline)forphases0.97-0.99 77 AbstractofDissertation PresentedtotheGraduateSchool oftheUniversityofFloridainPartialFulfillmentofthe RequirementsfortheDegreeofDoctorofPhilosophy HaFLUORESCENCEINUVACTIVEBINARYSTARS By ToddRussellVaccaro May 2001 Chairman: Dr. RobertE.Wilson MajorDepartment: Astronomy Lightcurves,radialvelocitycurves,andHaspectralprofilemodelsweregen- eratedfortheeclipsingbinariesV471 Tauand FF Aqr. Wemodeled anemission regiononthecoolstarofeachsystemtosimulatefluorescentactivityonthesideof thestarfacingitshotcompanion. Comparisonsofthemodelstoourphotometric andspectroscopicobservationsrevealadditionalcomponentsthatmayarisefromthe intrinsicchromosphericactivityofthecoolerstarandbeassociatedwithdarkspotted regions. Moreemissionswerefoundathighervelocitiesthatplacetheactivitywell abovethestarbutstillbetweenthetwostars. Thesourcesoftheseexcessemissions maybeextendedstructuressuchasprominences,apartiallyionizedwind,orcircum- stellarmaterialsuchasaringordisk. Thecombinedemissionsgreatlycomplicatea formerlysimpleilluminationmodel. IX CHAPTER 1 INTRODUCTION 1.1 TheStudyofBinaryStars The Sun is the only star from which we can measure fundamental stellar propertieswithhighaccuracy. Knowledgeofitsmass,size,andluminosityalongwith itsinternalandexternalphysicalprocessesallowsustotraceitshistory,understand itscurrentstate, andpredictitsfuture. Yetthereareobservationsthatstillelude detailedexplanations,suchasthemagneticactivitycycle,whichhasbeenseenon thephotosphereatleastsincethetimeofGalileo. Abilitytodiscovermoreabout stellarphysicscomesfromthestudyofbinarystarswithsimilaractivities. Shortperiodbinariesofferawealthofinformationabouttheorbitalmotion ofthe starsaswell as anycycle-to-cyclevariations that may exist. Direct visual observationsoftheindividualstarsortheirmotionscannot bemadeinsuchbina- ries;thereforesurfacefeaturesaredeterminedphotometricallywhileradialvelocities mustbemeasuredspectroscopically. Spectroscopycanalsoyieldinformationabout temperature, rotation, chemicalabundances, and physicaldetailsofthesurround- ingenvironment,suchasgasstreams,winds,disks,shells,andextendedstructures (flares,prominences,etc.). Furthersupportingdatacanbeobtainedphotometrically iftheorbitalplaneishighlyinclinedtotheplaneofthesky. Thesesystemsyield accurateorbitalperiodsbyeclipsetimingandprovideinformationonrelativestellar sizesviaeclipsedepthsanddurations. 1.2 UVActiveBinaryStarsandFluorescence Averitablezooofbinarytypesexists. Categoriesarebasedonthetypesof stellarcomponents,onactivities,andonevolutionarystates. Abroadmorphological 1