19 90ApJS. . .72. .1913 contract withtheNationalScience Foundation. the AssociationofUniversitiesfor ResearchinAstronomy,Inc.,under © 1990.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. have focusedonsinglemain-sequencestars(Vaughan and The AstrophysicalJournalSupplementSeries,72:191-230,1990January Preston 1980;Duncan1981;Baliunasetal1983;Soderblom 1985; andothers).Onlyafew attemptshavebeenmadetosee discovered brightemissionlinesinthecoresofstrong ena. Burson 1922;Wellmann1940)revealedHandKabsorp- Further observationsbyseveralauthors(e.g.,Deslandres and strengthening theanalogybetweensolarandstellarphenom- tion reversalsontopoftheHandKemissionlines, Ca iiabsorptionfeaturesofaBoo,Tau,andGem. 3 2 1 VisitingAstronomer,KittPeak National Observatory,operatedby Efforts todetectactiveregionsfromrotationalmodulation Over 70yearsago,EberhartandSchwarzschild(1913) CHROMOSPHERIC CanHANDKHaEMISSIONINSINGLEBINARYSTARS -21 McDonald Observatory,UniversityofTexasatAustin;andCenterExcellenceinInformationSystemsEngineering,TennesseeState Dominion AstrophysicalObservatory,HerzbergInstituteofAstrophysics,NationalResearchCouncilCanada;andDepartment identify correlationsbetweenchromosphericactivityatCanHandKHaeffectivesurfacetemperature levels ofactivitythantheirsinglecounterparts.ChromosphericemissionintheCailHandKlinesdependsalso within theevolvedstarsplaysapparentlynorole,whilemain-sequencebinaryshowgenerallyhigher binary starsofspectraltypeF6toM2andluminosityclassIII,IV,V.Thesampleincludesinactivesingle upon surfacetemperatureinthesensethatfluxdeclineswithcoolertemperature.ThetrendHa used ultravioletCrvemission-linefluxestakenfromtheliteratureandcomparedthemwithpresentdata. binary starsoftheRSCVnandBYDraclasswithatotalrangerotationperiodsfrom0.5to310days.A until log^'(K)~5.8ergscmsisreachedandthenfillsinquiterapidly. equivalent width-log^'(CanK)planeisthatwithincreasingKlinefluxtheHaabsorptioncorefirstdeepens evolved starsaregenerallymoreactivethanmain-sequenceofthesamerotationperiod.Binarityperse determine theirrotationalvelocities.Thesedata,supplementedbypublishedobservations,havebeenusedto of 444spectrahavebeenacquiredandareusedtomeasureabsoluteCanHKemission-linesurfacefluxes and rotation.SeveralnewstarswithchromosphericCailHKemissionhavebeendiscovered.Wealso and BalmerHacoreemissionequivalentwidths.Someofthestarsalsohavebeenobservedat6430Áto and binarystarsaswellmoderatelytoextremelyactivesingleincludingtheFKCom Subject headings:Canemission—lineprofilesstars:binarieschromospheres © American Astronomical Society • Provided by theNASA Astrophysics Data System No singleactivity-rotationrelationcanbederivedforallluminosityclasses,andthereisclearevidencethat We haveobtainedhigh-andmedium-resolutionCanHKand/orHalineprofilesfor100single I. INTRODUCTION stars: emission-line—late-typerotation 1 Department ofPhysicsandAstronomy,VanderbiltUniversity Department ofPhysicsandAstronomy,UniversityToledo Klaus G.StrassmeierandFrancisC.Fekel Physics andAstronomy,UniversityofToledo OF SPECTRALTYPESF6-M2 Received 1989April7;acceptedJuly5 1 Gregory W.Henry Robert C.Dempsey Bernard W.Bopp ABSTRACT University AND 191 Absolute CaHandKemission-line fluxesandHacore mainly onultravioletemissionlines. (e.g., Rutten1987)and{b)withasimilarstarinbinary chromospheric behaviorifcomparedwith{a)main-sequence mined. Onereasonforthismight bethecomplicationin system (e.g.,Basri,Laurent,andWalter1985;Basri1987; stars withthesamerotationratesandeffectivetemperatures emission equivalentwidthsfor thesestarsrarelyweredeter- cally activebinarystars(=CABS;Strassmeieretal1988). greater thanthatofourSun.Thestellarparametersthese and theBYDravariablesisatleastoneorderofmagnitude systems havebeensummarizedinacatalogofchromospheri- Simon andFekel1987).Moreover,thelatterstudiesarebased the secondarycomponentor the presenceofacontinuum analysis duetothebinarynature ofthesestars,thatis,e.g., the (presumablyunknown)contamination oftheemissionby if rapidlyrotatingsinglesubgiantsandgiantsdifferintheir The activityinclassesofstarssuchastheRSCVnbinaries 19 90ApJS. . .72. .1913 hot componentwhichdilutestheemissionfromprimary. Worden, Schneeberger,andGiampapa(1981),17stars;Gi- ing CailKemission,thegiantstendedtohavedeeperHa (1984), 14stars;Femândez-Figueroaetal(19866),seven Recent CanHandKobservationsfocusedalmostexclu- While thedwarfstarsinsampleof85spectral hshed bythepresenceofemissionincoreHaline. (1988), 50stars.Amoredetailedinvestigationofsubgiants stars; andmostrecentlyPasquini,Pallavicini,Pakull ampapa etal.(1981),sevenstars;Bopp(1983),19 sively onsinglestars,e.g.,Linskyetal(1979),43stars; (Herbig 1985).Chromosphericactivityisthereforealsoestab- Hyades stars(Cayreletal.1983)andothersolar-typedwarfs Moffett, andHenry1986)aswellinrelativelyyoung Ha inveryactivebinarystars(SmithandBopp1982;Fekel, and giantsinbinarysystemsseemedtobeneeded. instrumentation, andin§IIIwediscusstheanalysistech- most oftheHareferencestars,almostallprogram emission andRossbynumber(theratiobetweentherota- cores. Fromasampleofeightshort-periodRSCVnandW will servetheneedsdescribed.Inadditionwetrytoverify of 100mostlyveryactivestarsbutalsoforweakorinactive UMa stars,Barden(1985)foundapossiblecorrelationofHa same brighteningoftheHacore(increasingR)withincreas- niques applied.Thespectraaredescribedin§IV,andV (0.18-0.3 À)andmedium-resolution(0.5-0.9A)spectrawhich obtained withavarietyoftelescopesbetween1981and1989. stars havebeenobservedatCanandHa.Notethatthe stars whichhadsuspectedactivity.Withtheexceptionof and KHeregionand/ortheBalmerHalineforatotal tional periodandtheconvectivetimescale). type F8andlaterofZarroRogers(1983)showedthe some trendsthatmaybepresent.In§IIwedescribethe Our primarygoalistopresentasetofhigh-resolution and Haobservationswerenotsimultaneous.Thedata c o 192 In thispaperwepresentnewobservationsoftheCanH Several authorsnotedsignificantfillinginofthecores © American Astronomical Society • Provided by theNASA Astrophysics Data System 1986 Apr-1988SepRitter1 m EchelleReticon10242.50.3 Ritter0.3 1985 MarKPNOCF CoudéTI-3CCD150.4 KPNOO.4 1985 Sep,Oct,NovKPNOCF CoudéTI-3CCD7.60.2 KPNOO.2 1988 MayKPNOCF CoudéTI-3CCD7.60.18 KPNO0.18 1989 JanKPNOCFCoudéTI-3 CCD 7.60.21KPNOO.21 1981 Jan,MayMcDonald2.7mCoudéReticon 10244.40.352.7McD0.35 1983 Apr,AugMcDonald2.1mCoudéReticon 17289.50.422.1McD0.42 1986 Feb,MayMcDonald2.1mCoudéReticon 17289.50.282.1McD0.28 1988 MayDAO1.8mCassegrainRCA CCD150.5DAOCCD0.5 1987 DecDAO1.8mCassegrainReticon 1872150.5DAORET0.5 1985 MarKPNOCF CoudéRCACCD7.60.5 KPNO0.5 1988 Mar,AprDAO1.8mCassegrainRCA CCD150.9DAOCCD0.9 1988 Mar,MayKPNOCFCoudéTI-3 CCD 4.70.30KPNO0.30 1987 DecKPNOCFCoudéTEK CCD4.70.24KPNOO.24 -1 Year andMonthTelescopeSpectrographDetector(Amm)(A)Code Telescope-Spectrograph-Detector Combinations STRASSMEIER ETAL Ca ilHandK TABLEI Ha -1 included insomeofthegraphs§V.IndividualCanHand published absoluteHandKfluxesforactivestarswhichwere widths. AppendixAcontainsashortsummaryofpreviously we discusssystematictrendsinthelinefluxesandequivalent K regionplotsforourprogramstarsaregiveninAppendixB. intervals; 1987December,1988March/April,andMay pixel TektronixCCDandhada2-pixelresolutionof0.24A A mm.TheobservationsinDecemberutilizeda512x512 pixel Reticonarrayandhadaspectralresolutionof0.5A. with theCassegrainspectrographfedby1.8mtelescope. grating Aandcamera5atareciprocaldispersionof4.7 May. Thecoudéspectrographwasusedinthirdorderwith observing intervalsin1987December,1988March,and width, aresolutionof0.9Â.Thesamechipwasusedforthe The MarchandAprilobservationsutilizeda512x512pixel The observationsinDecemberwereobtainedwitha1872 data weuseda800XpixelTexasInstruments(TI-3)CCD graph-detector combinations. scope. Table1isasummaryofthedifferenttelescope-spectro- Dominion AstrophysicalObservatory’s(DAO)1.8mtele- Observatory’s (KPNO)0.9mcoudéfeedtelescopeandthe RCA CCDandhad,combinedwiththeslightlylargerslit and aslightlylargerslitwidthresultinginaneffectiveresolu- and awavelengthcoverageof65A.FortheMarchMay signal-to-noise (SNR)ratiosvariedfrom1minuteandSNR tions werecenteredon3950.0A.Theintegrationtimesand tion of0.3Aandawavelengthcoverage56A.Allobserva- SNR «50forHD65195. «150 (attheKlinebottom)forßGem,to90minutesand The DAOdatasetwasobtainedduringthreeobserving The KPNOdatawereobtainedinthecourseofthree Two telescopeshavebeenused;theKittPeakNational Dispersion Resolution II. INSTRUMENTATION a) CalciumHandK Vol. 72 19 90ApJS. . .72. .1913 -1 2 -1 1 Astronomy, Inc.,undercontractwith theNationalScienceFoundation. package forCCDSpectra(PilachowskiandBarnes1987) 0.5 A.Thesignal-to-noiseratiosareinthesamerangeas May observations,butwitheffectivewavelengthresolutionof which isoperatedbytheAssociation ofUniversitiesforResearchin ing the1mreflector. mostly the2.1mtelescope;KPNOusingcoudéfeed vatories: McDonaldObservatory,UniversityofTexas,using KPNO data. A. Forthe1983dataweuseda90¡imslitachievingspectral A mmcoveringawavelengthregionofapproximately265 0.35 Aasearly1981.Thevastmajority,however,was available atKPNOandDAO. the ImageReductionandAnalysisFacility’s(IRAF)sub- intensified 1024pixelReticonarray(Bopp,Dempsey,and resolution of0.28A.TheSNRsforallthreedatasetswerein made witha60jiimwideslitresultinginsomewhatbetter utilized thecoudéspectrographwithgrating2infirstorder A centeredon6570A.TheSNRsfortheseobservationsarein resolution of0.42A,whereasthe1986observationswere reciprocal dispersionof2.5Amm.Thedetectorwasan and the1872pixelReticonhadadispersionof9.5 pass photometryforstarsofvariousspectraltypesandlumi- Willstrop (1964)obtainedabsolutelycalibrated50Aband- runs utilizedcamera5,gratingBorD,andtheTI-3RCA resolution of0.18Awhilecoveringa84fieldcenteredon with theKPNOcoudéfeedtelescopeusingcamera5and taken withthe2.1min1983and1986.Theseobservations telescope anda1024pixelReticonarrayatresolutionof telescope; andRitterObservatory,UniversityofToledo,us- relation toconvertWillstrop’s 3925-3975Afluxesintoabso- color andapparentvisualbrightness.Linskyetalused this nosity classes.BarnesandEvans(1976)haveshownthat the Ha. TheobtainedSNRisapproximately150:1.1985 grating Ainsecondorder.Thedispersionof7mm"and Maniak 1988),whichwhencombinedwitharelativelylarge followed theproceduresoutlinedbyLinskyetal(1979). CCD atresolutionsbetween0.2and0.5A. the rangeof50-150:1. spectral resolutionof0.3A.Thewavelengthcoveragewas60 slit widthinordertodecreaseintegrationtimeresulteda the range50-200:1withmostaround100:1. the TI-3CCDpixelsizeof15ju,mresultedina2-pixelspectral the 1mtelescopeandafiber-fedechellespectrographat angular diameterofastarmaybederivedfromitsV -R No. 1,1990 o 2 -2_ 1 IRAFisdistributedbyNational OpticalAstronomyObservatories, A fewspectrawereobtainedwiththe2.7mMcDonald These observationswereobtainedatthreedifferentobser- The Ritterdatawereobtainedbetween1986and1988with Both datasetswerereducedinthestandardfashionusing Higher resolutionscanswereobtainedin1988,and1989 Our measurementsofthesurfacefluxinergscms III. DESCRIPTIONOFMEASUREDPARAMETERS a) AbsoluteCanHandKSurfaceFlux © American Astronomical Society • Provided by theNASA Astrophysics Data System b) BahnerHa Ca ilHANDKHaEMISSION -2_1 zero-flux level.ThisisdemonstratedinFigure1wherethe where theobservedfluxesarealwaysmeasuredfrom lute surfacefluxesandplottedthemversustheF-Rcolor bottom lineofthegraphshallrepresentzero-fluxlevel. which maybenoted: While thiscalibrationtechniqueplacesallstarsonauniform À bandpass.Thus,allCauHandKspectraforwhichthis color measured relativefluxes,/(AÀ),equaltothecalibratedflux calibration maybeappliedmustcontainthis50Abandpass Knowing theF-Rcolorofastarsonecanderiveitsstellar angstrom, inthe3925-3975ÁbandpassandF-R and foundatightcorrelationwithonly1.4%averagedevia- flux scaleforintercomparisontherearestillseveralproblems centered on3950A. surface continuumfluxinergscmsAthe3925-3975 scribes thentherelationshipbetweenstellarfluxper tion. Apiecewiselinearleast-squaresfittothesedatade- so that calibration ofJ^AA=50A) isderivedfromtheWillstrop A(K)-A(K (Table4)showedinternalerrorsofupto K characteristics. tion (2)includestheHand Kemissionfeaturesbutthe how welltheminimaweredefinedandthereforedepending illustrated inFigure1.Ourmeasurementsof,e.g.,AAiK^= stars whichwereselectedwithout muchregardtotheirHand (CA) starismatchedwiththeappropriatevalueofintrin- lies” ofactiveHyadesstars(Campbell1984)arenotreal but 0.066 mag;Vogt1981).Moreover,severalofourprogram Peg whereabigspotin1977producedF—Rvariationsof on theinstrumentalresolution. ^ indices,aredefinedasthefluxabovezero-fluxlevel colors insteadofobserved. cations listedinKeenan(1983)andFekel,Moffett, and observed F-Rcolor.Tobeonaconsistentscalethroughout for F—Rchangesof<0.03mag(anexceptionmightbeII and Henry1986)whiledarkstarspotsnormallyaccountonly and F-7colorexcessesof0.06-0.10mag(Fekel,Moffett, sic colorinJohnson’s(1966)tables,theCAstarsshowF-R 9%, orapproximately6%intheresultingflux,dependingon and between(e.g.,fortheKline)minima,as due toduplicitywhichmightjustifytheuseoftheoretical Henry (1986).TheseF-RsarelistedinTable2.Recently, catalog or,especiallyforthesinglestars,weusedclassifi- ever possibleweusedthespectraltypesgiveninCABS this paperwedecidedtouseJohnson’s(1966)spectraltype-F stars haveneverbeenobservedinRandtherefore no Soderblom (1989)presentedevidencethatthecolor“anoma- 1Ä1k 1klR — Rcolorrelationforthefluxcalibrationprocedure.When- The HandKemission-linefluxesarederivedbysettingthe 3. Theintegral,/(AX=50Á), inthedenominatorequa- 2. IftheobservedR-Fofachromosphericallyactive 1. Theemission-linesurfacefluxes,alsocalledtheKand x log ^=8.264-3.076(F-R)forF-R<1.3.(1) 50^ <2) 193 19 90ApJS. . .72. .1913 with thosefromotherauthors(Table 7). 194 Usted inTable4.Evenstarswithemissionequivalent widths of>1A,thedifferencesinabsolutelinefluxesare The quantitiesJF(K),W(H)andfF(He)are point (3)mightbesignificant.Toseetowhatextentthis generally lessthan10%butcanreachuptoapproximately namely, measuringactualequivalentwidths(EW)andsub- A resolutionKPNOdataalsoinaslightlydifferentway; would influencetheemission-linefluxeswereduced0.24 boundaries forourfluxintegration(dottedarealabeledW).Thegraphbottomindicatesthezero-fluxlevel.Kand^points,producedby bandpass (dottedarea)includingW(K)andW(H).Rightgraph:DefinitionoftheHa“equivalentwidth”termusedthroughoutthispaper. line reversalintheemissioncenter,markstrengthofabovepseudocontinuum(i.e.dashedlinesshownmiddlegraph). 15% inthecaseofHD106225[JT(K)«2.2À].Aparticular Figure 1,fromtheEWof50Abandpass,labeledWin docontinuum, i.e.,JT(K)andW(Y£)inthemiddlepanelof equivalent widthsoftheKandHemissionfinesmeasuredabovepseudocontinuum(dashedlines),whileWis“equivalentwidth”within50A Figure 1,resultingin tracting theHandKemissionEWmeasuredfrompseu- Middle graph:ShownaretheintegrationboundariesofAX=50Abandpassneededforfluxcalibrationprocedure.W(K)andÍF(H) 02Ä Fig. 2.—Leftpanel:Comparison of theKPNOfluxeswiththosefrom In thecaseofveryactivestars,likeRSCVnbinaries, Fig. 1.—Definitionofmeasuredquantities.Leftgraph:Thered(Æ)andviolet(F)KjpointsthecentralCanKemissiondeterminewavelength © American Astronomical Society • Provided by theNASA Astrophysics Data System 50^ STRASSMEIER ETAL (3) >. Rightpanel:Comparisonofthe KPNO andDAOfluxesfromthispaper problem withthismethodisthedeterminationofcontin- uum. ThisisdemonstratedinthemiddlegraphofFigure1. variable. Weestimatetheinternalprecisionofbothdatasets been obtainedatdifferentepochs,whichisimportantbecause better than«40%takingintoaccountthatthedatahave indices withthoseofotherauthors.Theagreementismostly (KPNO vs.DAO)tobeshghtlybetterthan«20%. most ofourprogramstarsaresupposedtobeintrinsically deviation iswithintheexpectedrangeofexternalerror KPNO andatDAOarecomparedinFigure2a.Theirmean K lineshavebeendetermined,thefluxwhichrisesfrom (KPNO andDAO)tobe«15%,theexternalaccuracy underlying photospheremustbesubtracted.Asdemonstrated approximately 20%.Figure2bcomparesour^andK x The absolutefluxesofstarswhichhavebeenobservedat After theabsolutesurfacefluxesincoresofHand b) HandKLineRadiativeLosses Vol. 72 19 90ApJS. . .72. .1913 _1 by LinskyandAyres(1978),theresultingexcessfluxisnet radiative equilibriummodelatmospheres(i.e.,nochromo- chromospheric radiativelossintheHandKlines,respec- These excessfluxesarelistedinTable3alongwiththe widths andresidualintensitiesofthereferencestars.Inmost uncorrected fluxes. corrected ^andKindices^'(Hx)^'(ICi) sphere), and^reÍKí),whichcanbeusedtoderive tively. Linskyetal(1979)alsopresentHandKindicesfor ing thepreceptsofBopp,Dempsey, andManiak(1988).This the radiativelossesinHandKlinesrepresentedby is schematicallyillustratedin therightsectionofFigure1. cases theprogramstarandreferencewereobserved spectral typeandluminosityclass.ShowninFigure3 are the equivalentwidthofapresumablyinactivestarsame some ofthereferencestarspectra.Table5listsequivalent core bysearchingforthefive to10highestcountsperpixelin First, weestablishedthecontinuum intensityabovetheHa several times.Ifso,weusedtheirmeanvaluesintheanalysis. two relativelyline-free3A windowscenteredat6540and x 1x No. 1,1990CailHANDKHaEMISSION195 coudé feedtelescopeataresolutionof0.18A.Thespectraareshiftedinintensityforbetterdisplay.ordinateispixelswithan arbitrary velocity range of100kms(~2A)indicated.NotetheincreasingHawingswithhotterspectraltype. The Hacoreemissionwasdeterminedbysubtraction of The coreemissionequivalentwidthwasmeasuredfollow- Fig. 3.—Haprofilesfor10referenceabsorption-linestars,(a)Dwarfs;(b)subgiants;(c)giants.Allobservationsweremadewith theKPNO ^'(H^KO =^(H;K)-^(H.(4) 1re c) HaCoreEmissionEquivalentWidths © American Astronomical Society • Provided by theNASA Astrophysics Data System in Table6Awiththeirrespectivestandarddeviations. If The anglebracketsdenotemeanvaluesforthecaseswhere mÁ fortheKittPeakcoudé feeddata,6mAforthe2.1m zero intensitytothefinebottom. more thanonespectrumwasobtained.Thesevaluesarelisted of referencestarstakenonthe samenightisapproximately4 variable HaprofileandfistedtheindividualresultsinTable 6B. Alsofistedaretheresidual intensities,R,measuredfrom G >0.060A,weconsideredthestartohaveanintrinsically = integration fortheequivalentwidth.Thistechniquenearly in astraightlinetothecontinuumlevelresultslimitsof points. Second,extendingthesidesofabsorptionprofile uncertainties ofthesometimesverybroadHawingsand,in With thenomenclatureinFigure1wefollowed rotationally broadenedwiththeappropriatevalueofvsini eliminates thecontaminationbynearbywatervaporlines, 6590 A.Astraightlinewasthendrawnbetweenthesetwo of theprogramstarandthensubtractedfromeachother. v siniofthestar.Therefore,allreferencespectrawerefirst spheric emissionshouldbefirstvisible. addition, concentratesonthecoreoflinewherechromo- c Wa (Hem )((programstar)-(broad.ref.). (5) The internalprecisionofthe “equivalent width”forspectra This artificial“equivalentwidth”howeverdependsonthe 19 90ApJS. . .72. .1913 _1 196 measured, andtheaveragevaluedetermined.TheFWHM of maxima (FWHM)ofseveralfinesinthe6430Àregionwere double-fined. rotational velocities(Table2)for24systems,fiveofwhich are ence stars).Thus,wedeterminedvaluesoftheprojected value. Althoughspectraltypemismatchescancausespurious yses (Vogt1981)todetermine anempiricalrelationshipbe- uncertain upperlimits(particularlyinthecaseofsomerefer- lems (Z>),(c),and(d)makeitalwayssmaller.Thus,wemight program starandreferencestar,(Z>)anunreliablylargevalue for thesefineswasassumedtobetheinstrumentalprofile. comparison-lamp fineswerealsomeasured,andtheaverage a valueofvsiniintheliteratureorexistingvalues are expect someunfortunatecaseswherealloftheseproblemsare core emissionequivalentwidtheithersmallerorlarger,prob- of vsinitheprogramstar,(c)presenceacomposite smaller thanourcutoffvalueof0.04-0.06Â. added togetherresultinginanunrealisticnegativeemission among starswithHandKemission.Table6Acontains11 This maybecausedby(a)spectraltypemismatchesbetween the finebroadeningdetermined frommodelatmosphereanal- Such instrumentallycorrected FWHMwerecomparedwith “emission” equivalentwidths,theirupperlimitshouldbe stars with{W)<-0.1À.Whileproblem{a)makesthe spectrum, and(d)differencesofthechromosphericstructure sion thanthereferencestarused(comparewithHerbig1985). sion equivalentwidths;i.e.,evenweakerchromosphericemis- echelle spectraforfightscatteringinthespectrograph(Bopp, this problemislesssignificant. Dempsey, andManiak1988)butnotthecoudéspectrawhere value exceedsthe0.18ÁKPNOby25%.Therefore, at most,weaklyactive.NotethatwecorrectedtheRitter than +0.04to0.06Àshouldbeconsideredasnonactiveor, cantly broadenedlines(i;sini=11kms),wheretheRitter stars withHacoreemissionequivalentwidths,less exception: r\Boo,theonlyHareferencestarwithsignifi- The 0.42ÁMcDonaldequivalentwidthsareconsistently Ritter Observatoryechelleequivalentwidthsare«10%larger with the0.28ÁMcDonaldspectra—withoneexception, with approximatelythesameresolution.Theexternalaccu- than acorrespondingcoudéobservation.Thereisagainone though, i.e.,ßVir,wheretheMcDonaldvalueis9%larger. coudé feedspectraagreegenerallytowithinafewpercent racy fortheseobservationsisofcoursesomewhatlarger,say of «40mA.SomethestarsinTable6Bhavebeen observed withdifferenttelescope-spectrographconfigurations McDonald data,and10mÂfortheRitterdata.Theexternal cm at differentepochs,however,hasagreaterrangewithmean accuracy forthecoreemissionsestimatedfromspectrataken « 5%largerthanthe0.18ÂKPNOdata,while0.3À « 60mÂ.Theequivalentwidthsfromthe0.18ÁKPNO To determinetherotationalvelocities,fullwidthhalf- For manyofthestarsinoursamplewewereunabletofind A numberofstarswerefoundtohavenegativecoreemis- © American Astronomical Society • Provided by theNASA Astrophysics Data System d) RotationalVelocities STRASSMEIER ETAL n _1 _1 -1 log ^'(Hi),thechromosphericradiativelossnormalizedto fisted aretheuncorrectedHeindices,log^(He),definedas fine widthsatdifferentlocationsintheHandKfines.This nation explainedinTable1. halfway betweenthemeanfluxatKand^ H, The A\andAAwidthsaredefinedasthewavelength in Figure1.TheAAwidthisdefinedasthewavelength pseudocontinuum). Theotherequivalentwidthmeasuresin width abovetheinterpolatedwingofCauHfine(= column acodeforthetelescope-spectrograph-detectorcombi- respectively. Wefisttheseparameterssothattheymay be The lasttwocolumnsfistthefullwidthathalf-maximum for KPNO spectra.Thefirstcolumnfiststheequivalentwidthof corrected Cau^andKindices,log^'(Ki) Ca IIHjandKindices,log^(KJ^(HJ,the for eachofthe83starsfistedinTable3(includingSun)is tween thesetwoquantities: in Figure4alongwiththeirrespectivereferencestars.Tables used intestingdifferentfineformationtheories. defined asthefullwidthmeasuredbetweenfluxlevels table containsonlydatafromthe0.24Àand0.3Áresolution the totalsurfaceluminosityofstar,Rk>ilast the totalsurfacefluxabovezero-fluxlevel,uncorrected tion fistedinLandolt-Bömstein(Schmidt-Kaler1982).Also given inAppendixB(Fig.10).InTable3thestar’seffective of resultswhenvsiniwasdeterminedfrommorethanone of individualwidthsfromfinetofine,onthereproducibility was assumed.Thefactor0.591isfromtheempiricalrelation- reference stars,whileTable 6A fiststhevaluesforactive separations betweenthetwoHandKpoints,respectively. separation betweenKand(Fig.1),similarlyforAA . the Heemissionfeature(ifpresent),definedasequivalent temperature isgivenfromthespectraltype-temperaturerela- spectrum, andonthecalibrationofsystem. tainties of2-3kms,anestimatebasedontheconsistency earlier forwhichamacroturbulenceof5kms(Gray1982) except forthosegiantstarshavingspectraltypesofG5or The valuesofvsiniweredeterminedusingequation(6)with contains theequivalentwidths andresidualintensitiesforthe the KandHfine,FWHM(K)FWH^H), are this table,J^o(K;H)andIF(K;H),areexplainedin§III ship mentionedabove.Therotationalvelocitieshaveuncer- 5, 6A,and6Bsummarizethe Ha-observationresults.Table5 an assumedmacroturbulence,f,of3kms(Gray1982), x2 2 (K2)H2) (K1) x : H 2 lv1R (H1) v sini=0.591 A representativeexampleofoneCanHandKobservation Listed inTable4arethemeasuredequivalentwidthsand Representative Haregionspectraforfivestarsareshown IV. INDIVIDUALRESULTS (fwhmL-fwhmL*) 1/2 Vol. 72 1/2 (6) 19 90ApJS. . .72. .1913 No. 1,1990 © American Astronomical Society • Provided by theNASA Astrophysics Data System 1 1 ß Com 4 UMi ß Vir T Boo HR 5110 £ UMa(B) 77 Boo FK Com BD+36°2368 BM CVn BD+34°2411 BD+57°1417 6 Vir 31 Com 61 UMa DF UMa LR Hya 70 Vir BD-8°3301 HR 4430 LQ Hya 24 UMa ß Cnc ß Gem Ghese 410 Gliese 380 Ghese 378.1 IL Hya o UMa 7T UMa 35 Cnc 28 Mon 54 Cam BD+42°1790 a Gem x Ori BD+40°2197 K Gem BD+47°1117 Gliese 338A OU Gem HR 2081 HR 1908 BD+03°733 BD+64°487 BD+26°730 V492 Per V491 Per V711 Tan CD-26°2085 BD+0°908 HR 1455 El Eri HR 1176 6 Eri VY Ari a Ari AY Get 1 Gem BD+14°690 HR 1362 UX Ari HR 1023 BD+25°497 12 Cam BD+34°363 HR 454 HR 339 HR 166 6 And Star Name 10 Tau 98230 82210 99967 95650 91816 88230 86856 118216 82558 81410 80715 45088 41116 124547 116204 69267 65626 65195 62509 40084 39587 121370 120136 117555 117176 116378 115781 114710 113983 113226 111812 106225 102870 79211 71369 65953 62345 62044 37171 33798 32357 101501 72905 72779 34198 31993 31738 30957 29104 28591 27691 27536 26337 25893 23838 23249 22484 22468 21018 21242 9746 6903 3651 3627 HD 19485 17433 12929 7672 12545 K3III F6IV G0IV F2IV/K2IV G5V K1III F/K0III dMOe G2III G4V GOV G8III G8III G0III K0III F9V K2III dM2e K0V/K0V dK8 dKO G8V G5V K7V G4IV-III K3V/K3V K4in KOin Kim Kim MOVe G0III K4in F9IV/F9rV K3V/K5V K4III K0III K0III GOV G5III G5III G8III GOV K0III K2III dK5e K0+IV [F6-7/1K0III G5III G5IV G8:IV F/G5III-II K1III G8IV G5IV F9V-IV gKl GOV G8IV G2III G5IV/K1IV K2in WD/G5III G5V/K0IV G5III G4V/G6V K3-4IV G5IV K0V K3in Type G0III (hot/cool) Spectral Ca ilHANDKHaEMISSION Properties ofObservedStars 4.82 4.95 4.98 4.26 4.87 6.59 2.68 4.50 8.2 8.87 8.13 4.94 6.35 9.52 9.04 4.56 2.83 8.1 3.61 5.33 7.21 7.58 7.5 7.5 10.12 4.14 4.68 4.16 4.41 5.64 6.58 3.36 3.52 6.52 9.12 6.79 5.89 5.94 3.57 6.25 8.6 4.28 7.4 7.7 7.62 8.42 6.36 6.72 6.27 3.54 5.7 6.5 6.38 7.1 7.0 7.53 7.13 6.95 5.66 8.36 6.87 2.00 5.92 5.47 1.14 7.13 5.55 5.87 3.27 7.0 7.6 (mag) V c 0.84 0.54 0.96 0.50 0.40 0.58 0.54 0.54 0.81 0.50 0.70 0.70 0.51 0.77 0.48 0.58 0.64/0.64 0.64 0.65 /0.79 /0.77 1.28 1.50 1.15 1.20 0.81 0.82/0.82 0.50 0.51 0.69 0.50/0.50 0.69 0.77 0.81 0.82/ 0.50 0.64 0.70 0.69 0.77 0.77 0.77 0.84 0.61 0.99 0.81 0.50 0.64 0.61 0.77 0.48 0.69 0.54/0.55 0.84 1.28 1.06 [/]0.77 /0.69 0.64 /0.60 0.85 0.77 0.81 0.51 1.06 1.06 /0.81 /0.77 0.64 0.96 /0.69 (mag) V-E TABLE 2 a m orb 17.76 orbl8.7 orb2.613 20.66 orbl.033 orb3.980 orb6.8 2.40 2.935 [7] [37] .11] [4.2] [14] 76.6 (0.92?) [160] [10] *80] 10.6 17.1 1.5978 orb37.9 4.5 orb 1.9 3.8 orb219. orb4.00 7.36 5.10 28.4 9.8 84.9 21.3 309.6 2.84 orb6.15 orb23.9 19.410 [20] 6.44 48: 10.163 [300] [150] 7.5 [25] 6.2 Prot 12.69 13.0 [20] [240] 76.0 1.945 [100] 17.4 75.12 [260] (days) 240] 2.6] 87] 150] 180] n] b b b b b b b b b b b b b b b b b b -1 b b b 4 5 6 /10 57 25 3.2 2.8 4 7/35 4.9 ll 14.5 120 l: 15 6/6 25 <3 <15 <15 16 <25 4 20 3.1 22 4 91 2.6 5 2.5 6 25 5.6/S.6 6/6 6 6/6 8 24 8 6 50 6/37 6 29 31 /17 /6 6 2.2 8 91 ÏÔ/IO 10 10/14 12 13/38 10/6 176 /4 (km s) <3 15 15 Chromosphere 197 19 90ApJS. . .72. .1913 198 © American Astronomical Society • Provided by theNASA Astrophysics Data System 2 Star Name ß Oph II Peg ß Aql p Boo HR 9024 HR 8703 61 CygB V1764 Cyg V775 Her p, Her(A) 29 Dra HR 6469 MS Ser \ BooB f BooA a Boo SUN A And 61 CygA BD+15°4057 HR 7275 HR 6806 a CrB 6 CrB a Ser UV CrB HR 5553 HR 5534 e Boo b d c a New measurethispaper. Closevisualbinary. From thespectraltype-colorrelationofJohnson1966. A periodinbracketsisanestimatefromvsini. HD 224085 223460 216489 222107 201092 201091 146361 191262 185151 175742 166469 161797 161096 160538 157482 143313 141714 140573 136901 188512 179094 131511 131156 131156 130948 129989 127665 124897 K1III Type Spectral (hot/cool) KlIV WD/K0-2III G2V K7V G1III K2III-II K5V K1IV-III K0V K2in F6V/G0V K2V/K6V K2III K2V K4V K0III-II K3III G8IV-III KUH K2V G5IV G3.5rV-III K1IH G5V/G5V G8IV [ 1/G5IV G8V G0-2V STRASSMEIER ETAL TABLE 2—Continued (mag) 4.74 2.37 -0.04 0.81 4.63 6.01 6.9 5.85 3.57 5.81 6.40 3.42 2.77 5.51 5.7 8.36 2.64 7.21 V 3.71 7.69 8.04 6.55 5.90 5.60 5.23 7.2 3.7 6.03 7.79 c (mag) 0.81 0.74 0.91 0.58 0.50 0.77 0.96 0.61 0.74/ 0.65 0.84 V-R 0.64 0.80 0.64 0.74 0.84 0.50 0.81 /0.77 0.53 0.54 0.84 [1/0.61 0.81 0.70 0.99 0.54/0.54 1.15 a Prot (days) orbl8.67 6.2 40.25 28.8 81.9 45. 28. 2.898 9.60 [200] [280] [7.7] 11.5 25.38 22.61 24.39 48. 37.9 orb5.43 [13] 1.168 6.718 53.952 [501 '470] 100] h b b b (km s“ v sini A 42 4 6.6 2.4 28 26/25 2.2 2.5 ~0 /8 21 4 15 1.1 1.6 M/6 20 24 6/6 15 <15 ~0 10 Binarity S S S SB1 SB1 S S s s S SB1 SB3 SB2 SB2 S S S SB1 SB1 SB1 SB1 S SB1 SB1 S S SB2 Active Star ? Chromosphere yes yes yes yes yes no no yes yes yes no yes no no no yes yes no no yes yes yes yes no no yes yes yes / Vol. 72 19 90ApJS. . .72. .1913 No. 1,1990 © American Astronomical Society 6 1 d c c b d d d d c d d 1 6 5 6 V492 Per AY Cet HD 19485h 6 And Star NameT/ X Ori HD 31993 HD 27691 HR 1362 V491 PerA V711 Tau UX Ari HR 1023 HD 19485c HD 17433 HD 125454750 HR 454 HR 339 HR 1908 HD 34198 HD 33798 HD 31738 HD 30957 BD+26°730 HR 1455 El Eri HR 1176 HR 2081 10 Tau 12 Cam ß Gern a Gem OU Gem 1 Gem K, Gem HD 651955150 o UMa e 7T UMa6030 28 Mon 54 Cam^ IL Hya HD 80715a 35 Cnc HD 80715b GUese 338A3850 4400 4600 4200 5150 4000 4750 4750 4750 4420 4350 4600 5235 6115 5800 5700 5850 5150 5460 5235 5100 5235 5460 /4840 (K) 6030 6030 /5450 /5000 5150 4730/ 4600 4750 4900 /4750 4000 4730 5850 5150 6060 4730 4600 Balmer HeandCahHKAbsoluteEmission-LineFluxes log ^(Hc)jr (Kl) log (6, 5.79 5.66 (5.79) .27:) Ca ilHANDKHaEMISSION e e 6.61 6.15 6.44 6.45 6.41 6.48 6.55 5.38 5.40 5.42 5.42 4.89 4.79 5.86 6.34 6.29 6.74 6.66 6.72 5.03 6.34 6.41 6.23 6.70 6.81 6.00 6.20 6.48 6.54 6.72 6.54 6.80 6.80 6.38 6.25 6.44 6.64 6.67 6.54 6.37 6.59 6.64 6.54 <5.4 * 6.20 6.17 6.15 5.37 5.36 5.38 6.27 6.26 6.25 6.22 5.29 5.30 5.55 4.88 6.69 6.62 6.70 6.25 6.08 4.86 4.90 6.57 6.45 6.36 6.45 Provided bythe NASA Astrophysics Data System TABLE 3 e e 6.25 6.15 6.67 6.48 6.42 6.38 6.41 5.20 5.22 5.22 5.23 5.81 6.44 6.37 6.56 6.67 6.63 6.44 6.56 4.67 6.42 6.66 6.70 6.70 6.26 6.17 4.80 6.04 6.36 6.58 4.97 6.68 6.72 6.08 6.16 6.37 6.13 6.43 5.29 6.58 6.57 6.21 6.20 6.21 6.04 6.16 6.18 6.57 6.47 5.19 5.22 5.34 6.21 6.24 6.24 6.04 5.21 6.59 <5.4 f 5.44 6.67 6.58 4.83 5.01 4.83 6.46 6.28 6.29 6.32 [erg cm -n-i) log ^’(KOlogJFXHi) 6.14 6.72 6.43 6.40 6.61 6.43 6.54 5.36 6.36 6.26 6.28 6.61 6.72 6.66 6.44 5.37 5.39 5.39 6.79 6.22 5.26 6.43 6.20 6.41 6.52 6.71 6.52 6.79 4.96 6.80 6.33 6.40 6.69 6.57 5.99 6.19 6.59 6.62 6.48 6.48 6.36 6.22 5.27 6.25 6.21 6.16 6.13 5.28 5.25 6.26 6.24 6.06 5.18 5.20 4.78 6.58 6.23 6.66 6.66 5.45 4.88 4.84 6.51 6.45 6.45 6.35 6.14 6.67 6.48 6.43 6.41 6.38 6.40 5.17 5.20 6.23 6.53 6.65 6.63 6.53 5.19 5.20 5.35 6.31 6.69 6.24 6.14 6.43 6.40 6.66 6.58 6.69 4.90 6.27 5.18 6.36 6.67 6.71 6.07 6.02 6.02 6.15 6.17 6.52 6.15 6.12 6.41 5.11 5.21 6.20 6.19 6.23 6.20 6.52 6.53 6.41 6.20 6.01 5.10 5.10 4.95 6.54 6.55 6.22 5.33 6.64 4.81 4.81 6.39 6.28 6.28 6.31 34 L54 L44 4 4 L24 L94 L44 4 4 194 4 134 4 4 4 4 L24 14 134 4 24 4 a 2.3(-5) *(-) 2.3(-4) 2.0(-4) 2.5(-4) 2.l(-5) 2.2(-5) 2.3(-5) 9.0(-5) 5.7(-5) 3.0(-4) 2.2Í-4) 9.2(-5) 2.2(-4) 2.2(-4) 5.1(-6) 9.4(-5) 6.1(-5) 6.0(-5) l-6(-4) (-) (-) L7- LU-) (-) 2.3(-4) (-) 9.6(-5) 8.4(-5) (') 9.5(-6) 7.(-5) 1.0Í-4) 9.5(-6) 1.2(-5) 1.2(-5) UM) iAi-) *(-) 1.5(-) i.iK) 9.6(-5) 8.5(-5) 5.4(-5) 9.5(-6) -() LOf-) i.Oi-) i.Oi-) i.OM) L^-) (-) 1.0Í-5) *(-) *(-) lAM) l.ii-) 7.6(-5 1.0(-5) 1.(-) 1.2(-5) l.l(-5 l.l(-5 1.6(-) 1.6Í-4) L7-4 ^HK (-) KPNOO.24 KPNOO.24 KPNOO.24 KPNOO.24 DAORETO.5 DAORETO.5 DAORETO.5 DAORETO.5 DAORETO.5 DAORETO.5 KPNOO.24 DAORETO.5 KPNOO.24 KPN00.30 DAORETO.5 KPNOO.24 KPNOO.24 KPNOO.24 KPNOO.24 DAORETO.5 DAORETO.5 KPNOO.24 KPNO0.30 DAORETO.5 DAORETO.5 KPNOO.24 KPNOO.24 KPNOO.24 DAOCCDO.9 KPN00.30 KPNOO.24 KPNOO.24 DAOCCDO.9 KPN00.30 KPNOO.24 KPNOO.24 DAOCCDO.9 KPNOO.24 DAORETO.5 DAORETO.5 KPNOO.24 DAOCCDO.9 DAOCCDO.9 DAOCCDO.9 KPNO0.30 DAORETO.5 KPNO0.30 DAOCCDO.9 DAORETO.5 DAOCCDO.9 KPNOO.24 KPNO0.30 KPNOO.24 KPNOO.24 KPN00.30 DAOCCDO.9 DAOCCDO.9 DAORETO.5 DAORETO.5 DAOCCDO.9 DAORETO.5 KPN00.30 DAOCCDO.9 DAORETO.5 KPNO0.30 DAOCCDO.9 KPNO0.30 DAOCCDO.9 KPNOO.24 KPNOO.24 KPNO0.30 Code 199 19 90ApJS. . .72. .1913 American Astronomical Society • Provided by the NASA Astrophysics Data System 6 6 2c e c Star NameT/log^(He)^(Ka)^(Hi)^’(Ki) c e II Peg SUN (Sky)5860 HR 9024 HR 87034420 HD 191262b5770 HD 191262a5770 V1764 Cyg (i Her A And4900 29 Dra HD 175742 HR 6469* a CrB/6030 f BooB4590 4 UMi ß Vir HD 1433134900/ HR 55534900 f BooA r¡ Boo components. 6 CrB UV CrB HR 5534 61 UMa HR 5110* FK Com HD 1163785770 HD 1162044600 HD 115781*4750 HD 1139834900 31 Com HD 1062254750 DF UMa two continua(seeTable2). 70 Vir HR 4430 24 UMa Í UMa(B) LQ Hya5250 Gliese 410 LR Hya Gliese 378.14000 Gliese 3804060 g e c f b a H andKemission tooweaktomeasure(seeFig.10). This measureisapproximatelyour lowerlimitforreliablefluxesfromthe0.24ÂKPNOdata. Both componentsshowHandK emission.Thegivenfluxesarethecombinedfromboth This measureisapproximately ourlowerlimitforreliable fluxesfromthe0.9ÀDAOdata. Both componentsshowHandKemission. Thegivenfluxeshavebeencorrectedforthepresenceof The valueinparenthesesisthepower of10. Fluxes arecontaminatedbythecontinuum ofthe(presumablyhotter)secondarycomponent. 2l (K) {ergcm~s~) 4840 5650 4600 4600 5250 5460 5460 5300 4600 5570 4200 6030 5940 5450 5800 /4660 5850 6115 5570 3850 4420 5200 3580 5250 5770 5.85 TABLE 3—Continued 5.72 5.72 5.56 l-3(-5) KPN00.30 DAORETO.5 DAORETO.5 DAORETO.5 DAORETO.5 DAORETO.5 KPN00.30 DAORETO.5 KPN00.30 Code KPN00.30 DAOCCDO.5 KPN00.30 DAOCCDO.5 DAOCCDO.5 DAOCCDO.9 DAOCCDO.5 DAOCCDO.9 DAOCCDO.5 DAOCCDO.9 DAOCCDO.9 KPNOO.24 DAOCCDO.9 DAOCCDO.9 KPN00.30 DAOCCDO.5 DAOCCDO.9 DAOCCDO.9 DAOCCDO.9 DAOCCDO.5 DAOCCDO.9 KPNO0.30 DAOCCDO.9 KPN00.30 DAOCCDO.9 DAOCCDO.9 KPNO0.30 DAOCCDO.9 DAORETO.5 DAOCCDO.9 KPNOO.24 KPNOO.24 DAOCCDO.5 DAOCCDO.9 DAORET0.5 DAOCCDO.9 DAOCCDO.9 DAOCCDO.5 DAOCCDO.9 DAOCCDO.9 DAOCCDO.5 KPNOO.24 KPN00.30 DAOCCDO.5 DAOCCDO.9 DAOCCDO.9 DAOCCDO.9 KPNO0.30 DAOCCDO.9 DAOCCDO.9 DAOCCDO.5 DAOCCDO.9 KPNOO.24 DAOCCDO.9 DAORETO.5 DAOCCDO.9 KPN00.30 KPNO0.30 DAOCCDO.5 DAORETO.5 DAOCCDO.9 DAOCCDO.5 KPNOO.24 KPNOO.24 DAOCCDO.5 DAOCCDO.9 19 90ApJS. . .72. .1913 b b a a a a a a 1 a 6 6 a a c 6 6 a AY Get Star NameW(He)W(K)W(H)W(K)HAAíkdAAíhdAA(kA(hfwhm(k)fwhmh HR 454 6 And HR 1023 HD 194851i HD 19485c V491 PerB V491 PerA HR 1176 HR 1362 El Eri HR 1455 V492 Per HD 27691 10 Tau ß Gem HD 31993 HD 31738 HD 30957 HD 33798 o UMa HD 34198 SUN (Sky) /a Her 4 UMi /3 Vir IL Hya 7T UMa HD 65195 cr Gem HD 191262b HD 191262a VI764 Cyg 7] Boo 54 Cam* k Gem 022)( 1 Gem UV CrB HR 5110 HR 4430 f UMaB LR Hya HD 80715b HD 80715a 70 Vir HD 113983 HD 106225 61 UMa LQ Hya HD 115781 G1 378.1 Balmer HeandCanHKMeanEquivalentWidthsLineforthe0.24 of 2. nearly identicalabsorptionlinestrengthsandmultipliedthemeasured equivalentwidthsbyafactor component. Nocorrectionhasbeenapplied. similarity ofthespectraltypes,however,nocorrectionsforcontinuum arenecessary. c b a Both componentsshowHandKemissionbutthelinesareblended inourspectra.Duetothe Ca ilHandKemissionfrombothcomponentsresolved.Weassumed equalcontinuaduetothe Equivalentwidthsarecontaminatedbyanunknownamountof continuumofthesecondary © American Astronomical Society (Â) (A) 0.052: blend 0.094 0.025 0.055 0.306 0.182 0.711 2.020 0.148 0.164 0.200 0.320 0.363 0.063 0.060: 0.418 0.620 0.468 0.630 0.058 0.698 0.816 0.038 0.023 0.835 0.096 0.635 0.781 0.042 0.207 0.183 0.133 0.009 0.910 0.184 0.142 0.620 0.160 0.978 0.082 0.316 1.758 1.742 0.179 0.21 1.480 1.328 2*244 0.282 0.043 0.107 1.020 Ca ilHANDKHaEMISSION 0.475 0.066 0.105 0.160 0.258 0.252 0.063 0.040: 1.130 0.283 0.352 0.360 0.040 0*301 0.410 0.551 0.463 0.041 0.368 0.150 0.024 0.021 0.506 0.039 0.090 0.154 0.679 0.142 0.140 0.447 0.080 0.576 0.369 0.21 0.237 0.933 1.076 0.159 0.074 1.116 0.025 0.088 1.011 0.572 1.620 0.30 ÂResolutionKPNOData 0.239 0.475 0.559 2.143 0.453 0.057 0.558 0.240 0.336 1.001 0.580 0.300 0.827 0.025 0.972 1.303 0.142 1.235 0.380 0.090 0.064 1.098 1.323 0.080 0.0600.77 2.027 0.090 1.020 0.365 0.306 0.261 2.028 0.328 0.456 1.026 0.059 0.056 0.485 0.061 0.498 0.213 0.461 0.253 1.722 1.586 1.080 0.122 2.682 0.060 1.182 1.853 1.673 TABLE 4 0.723 0.157 0.396 0.503 0.474 0.050 0.182 0.346 0.280 1.262 0.443 0.019 0.225 0.580 0.658 1.041 0.997 0.115 0.727 0.065 0.696 0.702 0.340 0.058 1.053 0.301 0.297 0.176 0.070 0.356 0.050 0.946 0.056 0.255 0.047 0.614 0.727 0.423 1.489 1.374 1.278 0.337 0.187 0.094 2.185 0.060: 0.174 1.478 1.284 1.104 2.79 blend 2.44 1.57 blend 1.92 2.42 1.27 1.48 2.10 1.92 1.05 2.95 2.10 1.57 2.20 0.62: 0.93: 0.93: 3.10 2.79 1.40 0.77: 0.75: 0.71 blend blend 1.40 1.43 2.48 1.13 1.07 1.57 1.08 0.87 1.27 1.55 1.22 2.63 1.09 0.93: 0.91 2.79 1.24 1.40 1.75 1.05 1.05 2.70 1.57 1.40 1.92 0.62 1.22: 1.40 2.27 1.31 1.40 2.32 1.48 0.77: 1.92 1.26 2.94 blend blend 1.91 1.92 0.74: 2.63 0.92 1.18 1.82 0.60: 0.96 0.70: 2.01 1.24 1.05 0.77 1.00 1.24 1.08: 1.95: 1.48 0.87 2.17 0.80 2*44 0.77: 1.40 1.75 1.28 0.66 0.61 0.46 0.19 Provided bythe NASA Astrophysics Data System 04 1.66 52 0.52 44 0.40 54 70: 65 46 80 73 55 14 57 0.52 0.61 0.64 0.68 0.14 0.47 0.70 0.49 0.56: 0.20 0.70 0.70 0.59 0.49: blend 0.52 0.84 1.13 0.84 0.87 Ö.73 0.52 1.05 1.50 0.46: 1.00 0.53 0.48 0.95 1.34 0.65 0.54 0.67 0.49 0.40 0.31 0.82 0.59 0.42 0.48 0.54 0.54 0.54 0.38 0.38 0.85 Ö.47 0.57 1.19 1.70 1.33 1.22 1.13 0.65 0.79 0.96 0.78: 0.57 0.49 0.79 0.26 0.77 0.96 0.84 0.96 0.47 0.84 1.16 0.62: 0*78: 0.89 1.19 0.70 0.49 0.62 0.70 0.35 0.35 0.38 0.57 0.50 0.54 0.44 0*84 0.73 0.51 0.35 0.40 0.96 1.05 1*49 1.15 201 19 90ApJS. . .72. .1913 -21 u program starsbutdonotintendtogiveafulldiscussionofall profile, i.e.,ifoisgreaterthan60mA. individual observationsforthestarswithvariableHaline was availableforthisearlyGgiant. visible (Fig.10).OuroneHaspectrumshowsastrong ab- of logJS/K)~6.55ergscms.Haisanabsorption Binary Star”(=CABS)catalog(Strässmeieretal.1988)and binary starsinthispaperseetheChromosphericallyActive K fluxlevelasHD7672butnoobviousemissionfeatures are feature clearlyfilledinbyemission. also thediscussioninFekel,Moffett,andHenry(1986). scopic featuresofthenot-so-wellknownand/orverypeculiar respectively (Table4).TheHaabsorptionlineisveryshallow equivalent widthsof+2Aand+1.1fortheKH line, the individualstars.Forreferencesonmostofactive stars whichhaveolessthan60mÀ,andTable6Bgivesthe consistently inemission.Its equivalent widthishighlyvari- sorption profile,butnoappropriatereferencestarspectrum seems tobealsoanemission feature.ThetwoCanHandK able (Table6B)andinstrength comparabletoV711Tau.He and hasablueshiftedemissionfeatureofabout30±5mA. w BD +26°730:Strongandvariableemissionline.Thespectrafromtwoconsecutivenights(phasedifference~0.5)havebeenshifted in wavelengthto absorption-line profile.HD45088:Filled-inprofilesinadouble-linedspectroscopicbinary(thearrowsindicatethetwo Halines).HR align theirrespectivephotosphericabsorptionfeatures.HD17433:Weakemissionlinewithstrongsuperposedprofile.29 Dm:Filled-in are spectraofreferencestarsthesamespectraltypeandluminosityclass.Allonscalebutshiftedinintensityfor betterdisplay. 1455: CompositeHaabsorptionprofile.ThedeepcoreisprimarilyfromtheG5IIIprimarywhilewingsaredominatedbyanearly Fstar. w 202 3 HD 7672.—StrongCailHandKemissionatafluxlevel HR 339=\pPsc.—ApproximatelythesameCanHand In thefollowingpartwewillbrieflydescribespectro- HD 9746.—BroadCailHandKemissionlineswith HD 12545.—Thisisoneof thefewsystemswithHa Fig. 4.—Haprofilesforfiveprogramstars.EachofthestarsrepresentsatypicalexampleparticulartypeHalineprofile.The dottedlines © American Astronomical Society • Provided by theNASA Astrophysics Data System o STRASSMEIER ETAL (Table 3). spectra showstrongemissionfeaturesabovethecontinuum and mayalsoindicatemoderatevariabilityoftheKline pure emissionprofiletoanabsorptionwithoccasion- 0.64). TheHalineprofileconsistsofanemissionfeaturewith points atafluxleveloflog^(K)-6.3.Thestrongcentral weaker linebelongingtothecooler(presumablymoreactive) level oflogJ^(K)—6.7and6.6fortheG6G4compo- width andresidualintensityUstedinTable6Aareestimates. giant ratherthanaG9dwarfaspreviouslythought(otherwise emission-line fluxoflog^(K)~6.15—ifthestarisasub- needed toresolvetheHand Kpoints.Haisaverystrong reversal obscurestheemissionline,andhighresolution is nent, respectively.Haisadoubleabsorptionfeaturewith the Recently, Boppetal.(1989)foundtheHalinevaryingfrom a our measurementofthelinefluxwouldbe~6.80ifV-R= component. double HandKemission(Fig.10)atanemission-line flux a strongandbroadcentralreversal(Fig.4).Theequivalent absorption linewithanequivalent width440mAlargerthan ally enhancedHaemissionpresumablyrelatedtoflareevents. the referencestaroUMa. x x HD 17433.—StrongCanHandKemissionfeatureswith HR 1023.—TheHandKlineprofilesshow HD 19485.—Thisdouble-linedspectroscopicbinaryshows UX Ari.—Heinemission. 2 2 Vol. 72 19 90ApJS. . .72. .1913 H andKemissionlineswithlargeV/Rratio. Ha No. 1,1990 A componentandweakemissionfromtheBcomponent. ( =theG8IVprimary)andB,withstrongemissionfrom the appears tobeanormalabsorptionfeature. period forachromospherically activestar(310days;Strass- G8 IVcomponent.Haisafilled-in absorptionline. Observations intheredat6430Àshowonlylinesfrom the HR 1176.—OuronlyCanspectrumshowsweakblueshifted HD 25893.—Thestarisaclosevisualbinary,V491Per A HR 1362.—Thissinglestarhas thelongestknownrotation HD 26337.—TheCanKline fluxmightbevariable. V711 Tau.—Heinemission. © American Astronomical Society • Provided by theNASA Astrophysics Data System a ß Vir. ß Com... 70 Vir... HR 6806 HR 166. 7] Boo. 61 CygB 61 CygA /i HerG5IV T Boo. ß Aql. 10 Tau... 8 Eri. oUMa.. ß Gem.. e Boo... eVir .... K Gem.. a BooK1III ß Oph. a Ari.. ß Cnc a Ser.. p Boo.. Star NameType(Â) a TakenfromKeenan1983. F9 V GOV K2V KO V G4 V K5 V K7 V F9 IV-V F6IV GO IV KO IV G8IV Spectral (W) G5 III G8 III KO II-III G8 III K0 III K2III K2III K3 III K2III K4III a Ca ilHANDKHaEMISSION Balmer HaReferenceStars -1.155 -0.565 -0.678 -0.877 -0.947 -1.059 -1.570 -1.367 -1.240 -1.019 -1.002 -1.260 -1.078 -1.056 -1.675 -1.262 -1.909 -1.091 -1.082 -1.007 -0.976 -1.015 -0.999 -1.033 -1.260 -1.148 -1.109 -1.130 -1.137 -1.039 -1.019 -1.052 -1.258 -1.280 -1.077 -1.179 TABLE 5 Subgiants Dwarfs Giants 0.040 0.000 0.017 0.003 0.020 0.009 0.065 0.050 0.006 0.025 0.003 0.001 0.020 0.010 0.003 0.002 0.004 0.009 0.019 0.016 0.004 0.027 0.034 0.010 0.009 0.005 0.052 (Â) chromospheric HandKemission. Our0.21ACCDspectrum candidate listoftheCABScatalog wherewecouldnotdetect of theHaregionshowsacomposite Halineprofileofan are visible(Fig.10),thefluxlevelofthisGOdwarfisnever- theless quitehigh,log^(K)-6.5.However,Haisarather star ßVir. strong absorptionfeature,strongerthanthatinthereference log ^(K)~6.5.Bothemissionlinesshowreversals.Ha ap- meier andHall1988)highCanemission-lineflux of pears tobearathernormalabsorptionline. o (Rc) 0.191 0.261 0.232 0.174 0.205 0.205 0.347 0.395 0.175 0.278 0.228 0.187 0.239 0.181 0.182 0.251 0.290 0.176 0.176 0.251 0.183 0.244 0.205 0.243 0.253 0.249 0.204 0.225 0.193 0.266 0.219 0.270 0.256 0.275 0.289 0.224 HR 1455.—Thisstarisone ofthefewexamplesin HD 27691.—AlthoughnoobviousHandKemissionlines 0.000 0.004 0.005 0.006 0.003 0.004 0.000 0.002 0.003 0.011 0.000 0.000 0.007 0.002 0.000 0.003 0.004 0.003 0.002 0.005 0.007 0.002 0.006 0.005 0.011 0.006 0.011 7 2.1McD0.42 1 KPNOO.4 11 2.1McD0.28 24 Ritter0.3 1 2.7McD0.35 38 Ritter0.3 9 2.1McD0.42 1 KPNOO.4 3 KPNO0.18 12 Ritter0.3 1 2.1McD0.42 Observatory 2.1McD0.28 KNO0.18 Ritter0.3 KPNO0.18 KPNO0.18 KPNO0.18 Ritter0.3 KPNO0.18 KPNOO.21 Ritter0.3 KPNO0.18 2.1McD0.28 KPNO0.18 Ritter0.3 Ritter0.3 KPNO0.18 2.1McD0.42 KPNO0.18 KPNO0.18 Ritter0.3 Ritter0.3 KPNO0.18 Ritter0.3 Ritter0.3 Ritter0.3 Code 203 19 90ApJS. . .72. .1913 © American Astronomical Society •Provided bythe NASA Astrophysics Data System 6 6 6 6 1 6 b b 6 b HR 5110-0.715 be reliable. Strassmeier, Weichinger,andHanslmeier(1986) FK Com<+3.3>''*'2.0 Walter andBasri(1982) 4 UMi lines showpronouncedwingswhich are stronglyblended,andthemeasuredequivalentwidthmightnot HD 80715b... 6 CrB HR 5534 HD 80715a... Barden andNations(1988) 31 Com 24 UMa 35 Cnc HD 116378 HD 116204 HD 115781 HD 113983 61 UMa f UMaB A And cr Gem DF UMa LR Hyab HR 4430 LR Hyaa 28 Mon 54 Cam Bopp, Dempsey,andManiak(1988) HR 9024 VI764 Cyg Gliese 380 HD 65195 HD 45088(c) X Ori V775 Her Gliese 378.1 HD 45088(h) HR 2081 UV CrB f BooB f BooA HR 1908 HD 34198 HD 33798 V492 Per V491 Per* HR 5553 HD 31993 HD 31738 HD 30957 HR 1455 HR 1362 1 Gem HD 27691 HR 1176 UX Ari HR 1023 HD 19485(c) HD 19485(h) HD 17433 HR 454 AY Get HR 339 6 And This paper Star Name<7w a d c b a Correctedforthe presenceoftwocontinua. The largestandarddeviationisprimarily duetoonemeasure. Composite equivalentwidth. Correctedforthepresenceoftwo continua. AlthoughtheHacoresarewellseparated,both d d d û a -1.288 -1.466 -1.145 -1.079 -1.100 -0.920 -2.088 -1.264 -0.649 -1.005 -1.136 -2.397 -1.099 -1.259 -1.038 -0.890 -0.962 -0.608 -0.678 -1.148 -1.241 -1.216 + 1.153 -0.161 -1.127 -1.130 -0.253 -0.663^ -1.072 -1.213 -1.015 -0.987 -1.645 -1.617 -1.030 -0.403 -0.654 -1.205 -1.081 -1.386 -0.909 -1.130 -1.140 -1.193 -1.484 -1.044 -0.865 -1.207 -1.650 -1.005 -1.508 -0.615 -2.185 -0.805 -0.982 +0.091 ~0.0 (A) (Á) Balmer HaEquivalentWidthsandResidualIntensities 0.065 0.050 0.051 0.135 0.032 0.215 0.075 c 017 047 009 048 059 050 004 058 026 036 041 067 010 060 013 010 007 019 0.760 0.476 0.319 0.322 0.436 0.336 0.417 0.445 0.170 0.280 0.590 0.561 0.278 0.265 0.321 0.473 0.657 0.464 0.482 0.825 0.649 0.399 0.437 0.432 0.237 0.442 0.386 0.355 1.35 0.372 0.871 0.611 0.216 0.519 0.404 0.369 0.332 0.227 0.433 0.446 0.424 0.766 0.589 0.219 0.430 0.334 0.308 0.427 0.336 0.645 0.331 0.457 ~1.0 0.622 0.444 0.517 0.201 1.100 < R> c 0.010 0.023 0.016 0.035 0.024 0.030 0.027 TABLE 6A 204 VRc 013 018 071 004 018 005 080 Oil 030 012 045 Oil 003 024 023 002 009 006 -Ö.028 -0.004 +0.544 +0.421 +0.360 -0.138 -0.020 -0.158 -0.259 -0.043 -0.028 -0.020 -0.091 -0.100 -0.057 -0.023 -0.020 -0.438 -0.047 +0.038 -0.138: -0.090 +0.104 +0.381 +0.020 +0.072 -0.144 -0.324 -0.247: +1.718 +0.097 +0.057 +0.135 +0.049 -0.100 +0.736 +0.312 +0.214 +0.061 -0.042 -0.028 +0.024 +0.025 +0.703 +0.093 +0.049 -0.437 +0.020 -0.420: +0.146 + 1.205 +0.054: +0.947 +0.494 +0.374 +0.025 em (A) 95 34 21 4 4 25 9 6 4 12 12 56 6 4 15 3 2 6 6 2 1 1 1 1 1 1 8 10 1 1 1 1 1 1 1 2 2 3 2 1 1 1 13 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 ß Com ß Oph ß Gem /x Her fi Her ß Gem ß Gem ß Oph € Vir ß Cnc ß Gem ß Com ß Cnc ß Gem ß Vir ß Aql oUMa ß Gem ß Oph ^ Aql ß Aql o UMa ß Oph K. Gem HR 166 61 CygB HR 166 HR 166 61 CygB 7/ Boo oUMa fi Her o UMa o UMa 70 Vir 61 CygB 61 CygB HR 6806 oUMa ß Oph a Boo 70 Vir a Boo 6 Eri oUMa HR 6806 HR 6806 a Boo HR 6806 61 CygA 70 Vir HR 166 HR 166 70 Vir Reference Star Vienna 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.1McD0.28 Lick Ritter 0.3 2.1McD0.42 2.1McD0.42 2.1McD0.28 2.1McD0.28 KPNO0.5 Ritter0.3 KPNO0.4 2.1McD0.28 KPN00.4;0.5 Ritter0.3 KPNO0.4 KPNOO.21 KPNOO.21 KPNOO.21 Ritter0.3 Ritter0.3 Ritter0.3 2.1McD0.28 2.1McD0.28 2.1McD0.42 2.lMcD0.28 KPNO CF KPNO CF Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 KPNOO.18 KPN00.4;0.5 KPNO0.4 KPNOO.21 2.1McD0.42 2.1McD0.42 Ritter0.3 Ritter0.3 2.1McD0.42 KPNOO.2 2.1McD0.42 2.1McD0.42 2.7McD0.35 2.1McD0.42 KPNOO.18 KPNOO.18 KPNOO.21 2.1McD0.42 Ritter0.3 2.1McD0.25 KPNOO.2 2.1McD0.42 Ritter0.3 Ritter0.3 KPNOO.18 Observatory Code 19 90ApJS. . .72. .1913 a 2a a 29 Dra HR 6469 a CrB HD 106225 Gliese 410 LQ Hya IL Hya V711 Tau BD+26°730 El Eri 12 Cam HD 12545 Star Name .06/11/1988 07/05/1988 08/25/1983 05/02/1983 05/09/1987 04/30/1987 07/05/1988 07/02/1988 07/01/1988 06/30/1988 06/30/1988 06/27/1988 06/06/1988 07/13/1988 08/27/1983 08/23/1983 04/29/1983 06/17/1987 05/05/1987 06/28/1988 06/27/1988 06/27/1988 06/20/1988 06/13/1988 06/10/1988 06/04/1988 05/27/1988 04/30/1983 10/23/1988 02/24/1986 04/29/1983 05/13/1981 03/13/1985 03/05/1985 02/27/1986 02/26/1986 02/24/1986 05/01/1986 05/02/1983 05/01/1983 04/30/1983 05/01/1986 03/12/1988 08/23/1983 09/30/1985 09/30/1985 03/15/1985 02/27/1986 02/24/1986 05/01/1983 01/22/1981 03/06/1988 08/26/1983 08/24/1983 03/05/1985 03/01/1985 08/25/1983 03/04/1985 03/01/1985 11/08/1986 11/08/1986 10/03/1985 11/11/1986 10/04/1985 10/23/1988 Observation Date of 10/22/1988 American Astronomical Society •Provided bythe NASA Astrophysics Data System Ha EquivalentWidthsfortheStarswitho>0.060Á w Ca ilHANDKHaEMISSION205 -1.384 -1.152 -1.297 -1.302 -1.154 -0.641 -0.772 -0.767 -1.226 -0.970 -1.476 -1.249 -1.018 -1.046 -1.219 -1.426 -1.395 -1.327 -1.298 -1.427 -1.392 -0.601 -0.159 -0.694 -0.342 -0.048 -0.562 -0.748 -1.285 -1.094 -0.047 -0.097 -0.190 -0.099 -0.172 -0.540 -0.402 -0.431 +0.064 +0.075 «0. -0.325 -0.232 -1.049 -1.250 -0.486 +0.433 +0.035 +0.011 -0.341 -0.817 -0.311 +0.453 +0.183 +0.391 + 1.969 + 1.103 + 1.352 +0.189 W +0.805 +0.182 +0.963 +0.895 + 1.961 +0.992 +0.751 (A) a TABLE 6B 0.403 0.377 0.663 0.715 0.729 0.640 0.683 0.656 0.624 0.630 0.662 0.640 0.652 0.534 0.607 0.602 0.728 0.906 0.635 0.552 0.561 0.400 0.485 0.699 0.709 0.668 0.617 0.643 0.634 0.768 0.933 «1. «1. 0.946 0.878 0.946 0.881 0.659 0.744 0.764 0.727 0.475 0.477 0.832 0.819 0.868 0.770 0.877 1.058 1.137 1.046 1.022 1.345 1.291 1.16 1.42 1.26 1.45 1.53 1.13 1.13 1.21 1.27 1.40 1.23 1.22 -0.124 -0.025 +0.268 +0.416 -0.113 +0.399 +0.443 +0.365 +0.992 +0.034 +0.418 +0.273 +0.321 +0.552 +0.351 +0.175 +0.243 +0.272 +0.178 +1.151 +0.698 +0.273 +0.292 +0.166 +0.600 +0.094 +0.524 +0.144 +0.143 +0.486 +1.162 +0.406 +0.565 +1.045 +0.963 +1.021 +0.820 +0.911 +0.638 +0.478 +1.520 +0.913 +0.838 +0.667 +0.748 +0.990 w„ +0.529 +0.744 +0.837 +0.088 + 1.018 +0.956 +0.815 +0.960 +0.484 +3.083 +2.217 + 1.919 +2.458 + 1.288 + 1.295 +2.069 +2.001 +3.067 +2.098 +1.857 (Â) e ß Com ß Gem /x Her ß Gem ß Gem ß Gem ¡i Her 61 CygB 61 CygB 6 Eri HR 166 ¡i Her Reference Star 2.1McD0.42 2.1McD0.42 Ritter0.3 RitterO.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 RitterO.3 2.1McD0.42 2.1McD0.42 2.1McD0.42 RitterO.3 Ritter0.3 RitterO.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 Ritter0.3 KPNOO.18 RitterO.3 2.1McD0.42 2.1McD0.28 2.1McD0.42 2.7McD0.35 KPNOO.5 KPNOO.4 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.1McD0.28 2.7McD0.35 2.1McD0.28 2.1McD0.42 2.1McD0.42 2.7McD0.35 2.1McD0.28 2.1McD0.42 Ritter0.3 KPNOO.18 KPNOO.4 2.1McD0.42 2.1McD0.42 2.1McD0.42 2.1McD0.42 KPNOO.2 KPNOO.2 KPNOO.2 KPNOO.2 KPNOO.5 Ritter0.3 KPNOO.18 KPNOO.2 KPNOO.2 KPNO0.2 KPNO0.4 KPNO0.4 KPNO0.4 Observatory Code 19 90ApJS. . .72. .1913 206 © American Astronomical Society • II Peg11/08/1986 HR 870310/04/1987 Star NameDateofWRReferenceObservatory HR 727505/17/1987 Qcem a Equivalentwidthofthecompositelineisgiven. 09/08/1988 08/26/1988 08/21/1988 Observation (Á)(Â)StarCode 07/14/1988 07/13/1988 07/05/1988 11/11/1986 07/03/1988 07/02/1988 07/01/1988 12/30/1987 11/13/1987 11/04/1987 09/27/1987 11/06/1987 10/28/1987 10/19/1987 10/14/1987 10/04/1987 09/15/1987 09/06/1987 08/18/1987 08/12/1987 07/29/1987 12/31/1987 11/06/1987 10/28/1987 10/19/1987 STRASSMEIER ETAL TABLE 6B—Continued -1.015 0.4930.000 -0.884 0.540+0.131 -0.575 0.680+0.332 -0.702 0.590+0.313 -0.668 0.633+0.347 -0.520 0.671+0.495 -0.184 0.854+0.831 -0.700 0.591+0.315 -0.438 0.712+0.577 -0.728 0.570+0.459 -0.738 0.555+0.449 -0.739 0.593+0.448 -0.931 0.520+0.256 -0.746 0.584+0.441 -0.750 0.550+0.437 -0.842 0.547+0.345 -0.692 0.603+0.495 +0.605 1.41+1.654 +0.350 1.22+1.399 -0.897 0.565+0.290 -0.917 0.486+0.270 -0.868 0.514+0.319 -0.939 0.497+0.248 -0.823 0.548+0.364 -0.779 0.535+0.408 -0.865 0.486+0.322 -0.741 0.557+0.446 -0.723 0.544+0.464 -0.817 0.561+0.370 -0.549 0.617+0.638 -0.504 0.666+0.683 Provided bythe NASA Astrophysics Data System ß OphRitterO.3 8 EriKPNOO.2 a BooRitter0.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 Ritter0.3 RitterO.3 Ritter0.3 RitterO.3 Ritter0.3 KPNOO.2 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 RitterO.3 Vol. 72 19 90ApJS. . .72. .1913 -1 in bychromosphericemission. level oflog^(K)-6.6andaweakHaabsorptionlinefilled but isblendedwiththeCanHemissionline. ble tOthatofthereferencestarßGem.Ahigh-resolution with strongCanemissionlinesatafluxleveloflog^(K)- log ^(K)-6.8,presumablyfromtheG5IVprimary.He value forthereferencestarßOph. lines indicateactivity,whileHaappearsasastrongabsorp- region showHatobeaveryweak,almostabsent,absorption Any HandKemissionfromthelate-typestarwouldbe normal fluxleveloflog^(K)-5.0.Haseemstobealsoa ple (K4),HR1908showsweakHandKemissionlinesata moderately strongHandKemissionbutveryHa 29 ±2kms. 6.3. Haappearstobeanormalabsorptionfeaturecompara- feature filledinbychromosphericemission. might beanemissionfeature.OurobservationsoftheHa spectroscopic binarywithverystrongCanemissionlinesof Ca iiobservationshowsstrongHandKemissionataflux scopic binary(F.C.F.;seeentryintheCABScatalog).Our feature (Table6BandFig.4).Heseemsalsotobeinemission substantially dilutedbytheFstarcontinuum. early Fstar(mostlikelyasubgiant)andG5giant(Fig.4). normal absorptionfeatureor,atmost,veryweaklyfilledinby absorption. 6430 ACCDspectrumshowsrotationallybroadenedlinesof filling (Table6B),butthisneedstobeconfirmed. with arelativelylongorbitalperiodof219days(Beavers and emission ifcompared,e.g.,withtheK4IIIreferencestarß tion line.Itsequivalentwidthisabout300mAlargerthanthe No. 1,1990 Ha appearstobeanormalandconstantabsorptionfeature. flux leveloflog^(K)~6.6.FromoursixHaregionspectra dwarf starareonlymarginallyvisibleinour0.5Aresolution Cnc (Table6A). determine amoreaccurateflux.Haisverystrongabsorp- DAO 0.9Aspectra.Higherresolutionspectraareneeded to Griffin 1979).OurHandKfluxmeasureinTable 3 is spectrum inFigure10,thestarhasafairlylargeemission-line of thissystemas9.6dayswithspectraltypeF5V+G5 II approximately thelowerlimitforreliablefluxesfrom the ondary isundetected.Thus, itisunlikelytobeparticularly ultraviolet istheprimaryof the9.6daybinarywhosesec- estimated fromanultravioletspectrum.Thus,theyimply that fact thesystemistriple.The mid-Fstarwhichdominatesthe and notethatthespectraltypeofsecondary(theFstar) is tion featureevenifcomparedwiththereferencestaroUMa. the systemisadouble-lined binary witha9.6dayperiod.In o 1 HD 30957.—Arecentlydiscovereddouble-linedspectro- BD +26°730=V833Tau.—Haisavariableemission HD 31738.—Thisisalsoanewlydiscovereddouble-lined HD 33798.—ThisstarisarapidlyrotatingsingleK0giant 12 Cam.—TheHaabsorptionlinemayshowvariable HD 31993.—ModeratelystrongCanHandKemission HR 1908.—Beingamongthelatest-typegiantsinthissam- HD 34198.—AnotherrapidlyrotatingsingleK0giantwith X Ori.—AlthoughtheHandKemissionlinesofthisGO HR 2081.—Thisstarisadouble-linedspectroscopicbinary 1 Gem.—Basri,Laurent,andWalter(1985)fisttheperiod © American Astronomical Society • Provided by theNASA Astrophysics Data System Ca ilHANDKHaEMISSION The fluxoftheKlinebottomdoesnotexceedlog^(K)-5.3. mospheric activityfromthiscomponentisalsounexpected. component hasanorbitalperiodof13.4yr.SeeGriffinand Ha seemstobeanormalabsorptionline. Radford (1976)forfurtherdiscussion.Thus,substantialchro- spectroscopic binarywithanorbitalperiodof7days(Tomkin a K0III,dominatesatyellowandredwavelengths.This chromospherically active.Thecontinuumofthelate-typestar, redshifted) onotherspectra.Althoughthisisadouble-lined emission. chromospherically active.Haappearstobeanormalabsorp- of thesingle-linedspectroscopicbinarieslistedin K5/K3 =0.43+0.02forphotosphericlinesand.0.32Ha. accurate fluxdetermination.One0.2AHaregionspectrum spectrum inFigure10buthigherresolutionspectraareneeded 1980). CailHandKemissionisevidentfromthe0.9A present butourspectrumhasinsufficientsignal-to-noiseratio profile withslightlylargerequivalentwidthifcomparedtothe weak ifcomparedtothereferencestarr]Boo. “candidate table”intheCABScatalogwhichturnedouttobe sion linesbutafluxleveloflog^(K)-6.1.Thestarisone shows doubleHaabsorptionlines(Fig.4)withalineratioof reference starßCnc.CanHandKemissionseemstobe width ismeasuredfromthecompositespectrumandfairly estimated spectraltypeofF9IVforbothcomponentsisquite emission. Thissystemisofparticularinterestbecausethe our spectruminFigure10butunshifted(orevenslightly tion featureor,atmost,weaklyfilledinbychromospheric to resolvetheemissionfrombothcomponentsforamore (Fig. 10)tocomputeareliableflux. early forachromosphericallyactivestar.Wenote,however, strengths, onlyonecomponentappearstohaveCanHandK spectroscopic binarywhosecomponentshavesimilarline emission finesbutamoderately strongfluxleveloflogJ^K) emission finesbutfairlyhighfinefluxoflog^(K)-6.5. No Maniak (1988)reportaverystrongHaabsorptionfine. approximately atspectraltypeF0.ThefistedHaequivalent “activity” instarsonornearthemainsequenceoccurs that Wolff,Boesgaard,andSimon(1986)foundonsetof photometric variabilitymakethissystemagoodcandidate for weak andvariableHaabsorption,possibleHeemission, and from bothcomponents(Table6A),withoneofthemvariable. emission fines.BalmerHefrombothcomponent is Ha observationhasbeenobtained. tions didnotrevealanyemissionfines.Bopp,Dempsey,and a monitoringprogram. also evident.BardenandNations(1988)reportHaemission - 6.2.RecentHaobservations byBopp,Dempsey,andMa- 1 HD 65195.—OurCanHandKspectrashowweakemis- a Gem.—ProbablyvariableCanHandKemission. 54 Cam.—TheHandKemissionlinesareblueshiftedin 0(7 Gem=HD45088.—Thisstarisknowndouble-lined 24 UMa.—OurCanobservation showonlyweakHandK Tr UMa.—AsingleGOdwarfwithweakCanHand K 28 Mon.—OursixHaspectrashowanormalabsorption 35 Cnc.—Two0.5Áand0.9AresolutionCanobserva- IL Hya=HD81410.—StrongCanHandKemission, HD 80715.—BothcomponentsshowstrongCanHand K 207 19 90ApJS. . .72. .1913 1 -1 be inemission.Haisaverystrongabsorptionfeature, 61 CygB. sion andalsostrongHeemissionatafluxleveloflog^(He) (Table 6B). emission. OneofourHaspectrashowthelineinabsorp- ent phasethantheCanobservation,showtwoveryweak dwarf components.TheHaregionspectra,takenatadiffer- approximately 100mAstrongerthantheK7Vreferencestar 0.24 ÀCCDobservationinFigure10showsweakHandK flux levelreacheslog^(K)~6.3.OuroneHaregionspec- filled-in Haabsorptionlines. Ca iispectruminFigure10isacompositefromthetwoK0 log ^(K)~6.3butstrongHaabsorption(160mAinexcess variability ofthecompositeemissionline.Thus,wedidnot region spectra,Haappearstobeaverystrongabsorption tion whileinanotherspectrumHaiscompletelyfilled emission. use thisstarintheanalysis.Figure10showsstrongHe dM starwithweakCanemissionandformstogether larger thantheK2IIIreferencestarßOph. feature withanequivalentwidthofapproximately280mA emission atafluxlevelofonlylog^(K)-5.7.From10Ha apparently onlyaveryweakly“active”system,ifatall.The spheric emission. trum showsanabsorptionfeatureslightlyfilledinbychromo- compared tothereferencestarHR166). DF UMaaspectroscopictriplesystemcontainingthreedM while theotherdeterminationsweremadeinblue. blended withotherfeaturesinourredwavelengthspectra, references. Thismaybebecausethebroadlinesare less niak (1988)reportverystrongHaabsorption.Note, our stars. AlthoughlistedinTable6A,thereisalotofHa 208 emission linesatafluxleveloflog&(K)~6.4.Haappears of 80kms"giveninUesugiandFukuda(1982)from six v sinivalueof57kmsissubstantiallylessthanthe almost absentemissionlines.Thefluxlevelisnever- pared tothereferencestarfiHer. theless veryhigh[log^(K)~6.6].Bopp,Dempsey,and Ma- niak (1988)revealanormalabsorptionfeaturewhencom- to beanormalabsorptionfeature. tors weremade.OurthreeCanHandKspectrashowstrong the CABScatalogbecausenoobservationsofactivityindica- -6.1. ~ 6.7andalsovariableHaabsorptionlineprofile(Table6B). ~ 6.5andfilled-inHaabsorption. LQ Hya=HD82558.—VerystrongCailHandKemis- £ UMaB.—CanHandKemissionisratherweakbutthe HD 86856.—StrongCanHandKemission.Healsomight LR Hya=HD91816.—TheHandKemissionlineinour HR 4430.—This75daysingle-linedspectroscopicbinaryis HD 106225.—VeryactiveRSCVnsystemwithlog^(K) diese 410.—AnotherdMestarwithstrongCanHandK HD 113983.—Verylikelynotanactivesystem. 31 Com.—VeryhardtomeasureatCan^anddue DF UMa.—Thevisualcomponent(ADS8242B)isalsoa HD 115781.—ThisstarisUstedinthe“candidatetable” 61 UMa.—AfairlyactivesingleG8dwarfstarwith HD 116204.—VeryactiveRS CVnsystemwithlog^(K) o © American Astronomical Society • Provided by theNASA Astrophysics Data System STRASSMEIER ETAL 7-21 Walter andBasri(1982)othersreportedaverybroad vations revealastrongHaabsorptionfeaturewhichmightbe weak HandKemissionatafluxleveloflog^(K)~5.3, variable Haemissionlinewithequivalentwidthsofsome- having aCanHandKobservation.Ouroneobservation variable. resolution CaiiCCDobservation(Fig.10)showsonlyvery (Fig. 10). log ^(K)—6.6andthusverifiesitschromosphericactivity. mal Haabsorption(seealsoTable6A).FromthreeCan emission linesoflog^(K)~6.15,while14Haregionobser- a constantbutfilled-inHaabsorptionline. at afluxleveloflog^(K)~6.4.SixHaregionspectrashow active. variable absorptionfeature(Table6B). log ^(K)-6.4fromone0.9Àspectrum.Haisaweakand 6.1. star isdecreasedbytheadditionofFstar’scontinuum star andaKstar.TheCanHemissionfromthe times upto10A! double CanHandKemissionlinesoflog(K)-6.5 for reveals aweakandvariableabsorptionlineprofile(Table From 16Haobservationswefindthelinetobevariableand active double-linedbinarystarintheCABScatalogwithout spectra wefindmoderateemission-linefluxesoflog^(K)~ thus thestarshouldnotbeconsideredaschromosphericaUy each component. 6B). emission oflog^(K)-6.5(Table7).OurHamonitoring fiUed-in absorptionline. Balmer Heemissionoflog^(He)~6.5.Haisaweak, fiUed-in. spectroscopic binarywithtworapidlyrotatingcomponents. 10 ergscms.Thesystemis,however,adouble-lined another systemhavingCanKemission-linefluxgreaterthan shows strong(composite)emissionlinesatafluxlevelof to thereferencestaraBoo. strengths areveryweak(compareourspectruminFig.10), the continuumatafluxlevel oflog^(K)-6.4.Hamonitor- tive stars[log^(K)-6.4].Haappearsasanormalabsorp- the emission-linefluxesaretypicalofchromosphericallyac- tion feature. — 6.3.Haappearstobeanormalabsorptionlineifcompared 2 HR 5534.—ThisisanewCAstarhavingHandKemission HR 5110.—TheHaprofileisclearlycomposite,fromanF HR 5553.—FourCaIIspectrashowmoderateHandK 4 UMi.—AlthoughUstedintheCABScatalog,ourhigh- FK Com.—CanKlinesurfacefluxoflog^(K)-7.3! HD 185151.—BroadHandKemissionlinesoflog^(K) HR 7275.—Bopp(1984)reportedstrongCauHand K a CrB.—TogetherwithFKComandLQHya,CrBis 8 CrB.—Bopp,Dempsey,andManiak(1988)reportnor- HD 191262.—Our0.3-ÀCCDspectruminFigure10shows 29 Dra.—CanHandKemissionabovethecontinuum; HD 143313.—ThestarisUstedasachromosphericaUy HR 8703.—StrongCanHand KemissionlinesweUabove HD 116378.—AlthoughtheHandKemission-line V775 Her=HD775742.—StrongCaIIHandKemission. Vol. 72 19 90ApJS. . .72. .1913 No. 1,1990 ing revealsaquitevariableandweakabsorptionlineprofile log ^(K)-6.7.ThreeHaregionspectrashowanormal (Table 6B). we confirmthat5ofthecandidatestars,HD19485, known orquestionedtherewasnoobservationofCaH most ofthesesystems,eithertheirbinarynaturewasun- with anearly-typesecondary,theemissionisprobablystrong star oUMa. significant fluxvariability. probably tooweaktoincludethisstarinthecatalog.Finally, enough toincludethisstarinthecatalog.Thus,itremainson definition. IfHR1176=HD23838hasacompositespectrum spherically activebinaries,accordingtotheCABScatalog absorption linefeaturecomparabletothatofthereference one star,HR1455=HD29104,showsnoCaHandK 30957, HD65195,115781,and191262,arechromo- and Kemission.FromourpresentCaHobservations ically activestarswhichwereobservedmorethantwiceat emission andshouldberejectedfromthecatalog. the candidatelist.TheemissionofHR1023=HD21018is indicators andotherstellarparametersforveryactivestars is hood surveyarelikely. variability becauseonlyfewstarshavebeenobservedmore 40% ofthosestars.WecansayevenlessaboutCauHandK mostly veryactivesystems,largerrotationalmodulations than with amplitudesupto30%,inadditiontheobservational Ha, 14starsshowedlargeequivalentwidthvariationswitha only onceandfromthe96starsobservedatHa,37had about 2timesatHandK2-3Ha,but were foundwhenitwasplotted versustherotationperiod. qualitative relationsandtrendsinthedata. quite dangerousandneedslongertimebaselinesubstan- error. Moreover,sincethestarsinpresentsample are H andKemissionofupto10%long-termactivitycycles standard deviationinexcessof60mA.Thatisapproximately a singleobservation.Forexample,outofthe34chromospher- and Ksolarneighborhoodsurvey(e.g.,VaughanPreston than twice.Howdoesthisaffecttheanalysis?TheCauH the totalof83starsobservedatHandK,54were there aremanystarswhichhaveonlyoneobservation:from chromospheric activity,mostly becausenotightcorrelations tially increasedsampling.Nevertheless,wemaysearch for those foundforthesolar-typedwarfsofsolarneighbor- 1980; Soderblom1985)showedrotationalmodulationofthe 1987) thatRisnottheappropriate parametertodescribe hk X And.—ThreeCanHandKobservationsshowno Table 8oftheCABScataloglisted37candidatestars.For HR 9024.—WeakHandKemissionlinesbutfluxlevelof The starsinthissamplehavebeenobservedonaverage Thus, derivingquantitativerelationshipsbetweenactivity It hasbeenargued(e.g.,Basri 1987;RuttenandSchrijver b) DependenceofActivityonTemperature © American Astronomical Society • Provided by theNASA Astrophysics Data System a) EffectofLimitedSampling V. DISCUSSIONANDANALYSIS Ca ilHANDKHaEMISSION 3 5 10 3 Ä 10 when comparing^'(H+K)betweenstarsofsimilarrotation velocity orperiodateachtype.Therefore,cautionisrequired of thebestfittodata(dashedlines),labeledonleft Figure 5aisplotofthemeanvaluessum is theslopeofbestfitfoundbyKelch,Linsky,and velocity orperiodbutdifferentspectraltype.Thedottedline each spectraltypeand,presumably,widescatterinrotation Landolt-Bömstein (Schmidt-Kaler1982;andreferences spheric contribution,^'(H+K),versuseffective(photo- unnormalized CanHandKlinefluxescorrectedforphoto- Worden (1979)fortheCanKlinefluxesof14stars, therein). ^'(FI+K)declinestowardcoolereffectivetempera- side withT\Notethateffectivetemperaturehasbeenalways spheric) temperature.AlsoincludedinFigure5aistheslope lines, ture. Thistrendemergesdespitewidescatterin^'(II+K)at taken fromthespectraltype-effectivetemperaturetablesin units ofthebolometricflux,Rhk,i.e.,fraction versus effectivetemperature.The~Tdeclinetowardcooler K^corr.) «Tÿ. running horizontallyatR~2-4X10”,whichwehave stellar luminositywhichappearsasemissionintheHandK used todividethestarsupinto“quiet”and“active”chromo- bars indicatethevariationsofstarslistedinTable6B. No sphere starsfortheentryinTable2.Wemayidentifythisgap emission equivalentwidthdescribedin§IIIc.Thevertical rotation rate.Assumingasmoothlyvaryingdecayofchromo- change inthechromosphericcharacteristicsatacertainageor Middelkoop 1982)thatthisgapindicatesadiscontinuous as thewell-knownVaughan-Prestongap(VaughanandPre- stars isnowgone,thescatterreal,andgapcanbeseen relation. K (aK3IIIorK5V)somewhatclearerthanforcoolerstars. data ofmostly“overactive”singleandbinarystars—dwarfs, ston 1980).Ithasbeensuggestedbyseveralauthors(e.g. clearly visibletemperaturedependenceseemstobepresent. stars withacolor-dependentshapeoftheactivity-rotation Rutten (1987)explainsan“absence”ofthegapforcooler spheric behaviortoexplaintheVaughan-Prestongap.Our spheric activitywithage,Hartmannetal(1984)showedthat by ^(Civ)«7¡f.Asa comparison,LinskyandAyres quantitative fitispossible,butitseemsclearthatthere is a evaluate theirslope.AvarietyofslopesrangingfromT to spectroscopic binariesincommonwithourprogramstars to fluxes (theirTable1)of67singlestarsandsingle-lined subgiants, andgiants—showthegapforstarswith7¡>4300 there isnoneedforadiscontinuouschangeinthechromo- (1978) foundfortheMg n klinefluxesof29starsa general increaseinCrvemission-line fluxwithtemperature temperature dependenceof^'(^i) ^1«• T areplottedinFigure5dforcomparisonpurposes. No e HK f ff Figure 5bisaplotoftheCauHandKradiativelossesin We havealsousedSimonandFekel’s(1987)Crvline Figure 5cshowsthesituationforHa.Plottediscore ^HK “^4>V^ ^'(H) +^'(K 1 a7 eff 209 19 90ApJS. . .72. .1913 3 3 7 7 10 Noyes etal(1984),mostly becauseitintroducesmodel- shows thesameamountofscatter astherelation^versus dependence butalsobecause ^versusPforseveralUVions turnover time,r,toscalethe rotationperiodasintroducedby equivalent widthforFKComis3.3A(WalterandBasri1982)but highlyvariable(valuesupto10Àweremeasured).Thisisschematicallyindicatedby emission equivalentwidthvs.TiffTheverticalbarsindicatetherange ofHavariationsseeninsomethestars(Table6B).Themeanemission line) forcomparisonpurposes.Thislinehasbeenarbitrarilyshifted forbetterdisplay.TheSunisalsoindicated(G).(b)Rvs.Tiff-(c)Hacore Indicated istheTslope(dashedlines)foractiveandnonactive starsasdiscussedinthetext.AlsoshownisKelchetai’s(1979)Fslope(dotted Fekel (1987).Severaltemperatureslopesareindicated.Notethatthe activestarsliewellabovethertrendofmostinactiveandless stars. the arrow,(d)log^(Civ)vsTiffThestarsplottedaresameones asintheotherpanels.Civemission-linefluxeshavebeentakenfromSimonand 210 c HK Fig. 5.—Temperature-activityrelationsforthefullsample,(a)Plotted isthesumofcorrectedHjandKjindices,log^'(H+K),vs.Lîf- Rutten andSchrijver(1987)reject theuseofconvective 5 ^ 6.0 O -°J OO p-n, © American Astronomical Society • Provided by theNASA Astrophysics Data System 8.0- 7.0- 4.0- c) DependenceofActivityonRotation 7000 6000 rp3 © §i. Subgiants Giants Dwarfs o'+'-cr...... © Fig. 5a g ;+ 0 îo1 + %•.•°""--, Ä T (eff) 5000 4000 STRASSMEIER ETAL 3000 variations orHandK(*S')index variations.Notethatsome v sini.Theseapproximate periods arecomputedfromour rotation periodsasderivedfrombroad-bandphotometric v sinimeasuresasindicated inTable2withstellarradiifrom the Landolt-Bömsteintables (Schmidt-Kaler1982),andcor- stars havebeenplottedwith arotationperiodderivedfrom P/r. Inthispaperwefollowpreceptandusedirectly the c pLn > O tD Fig. 5d Vol. 72 19 90ApJS. . .72. .1913 _1 recting for(sin/)=tt/4 where theperiodPisindays, theradiusRinsolarradii,and i; sin/inkms.Inthecase ofshort-periodbinarieswithout period P.ThesubgianttotherightisHR1362;itsarrowheadindicates half ofthemeasuredperiod(seetext).TheSunisindicatedasO. (b) part, HD12545,isplottedwiththeorbitalperiodof23.9days. equivalent widthmeanvalueof3.3A.Thesubgiantintheupper right rotation period.ThearrowindicatesthepositionofFKComwithan Ha R vs.rotationperiod,(c)Hacoreemissionequivalentwidth vs. No. 1,1990 hk Fig. 6.—Rotation-activityrelations,(a)logJ^XH+K)vs.rotation X O £ o Ü Ö O OjO -0.5 2.5 2.0 0.5 © American Astronomical Society • Provided by theNASA Astrophysics Data System 0.0 1.5 1.0 4.0- 6.0- 5.0- 8.0 7.0- -10 123 ^rotG sin/)=39.7 + 1 FK Com|-V711Tau Subgiants <3.3 Â> Dwarfs Giants 8 °V^ 0 12 o q.°*J<-• Fig. 6c Fig. 6a « -^.?•.- log P(days) log P(days) ° o + °o• -II Peg 9 R v sini 6.0there isacorrelationbetweenradiative radiative lossintheKlineoflog J'' =6.64butstrongHaabsorptionof pressed aslog^'(H+K)]withslowerrotationandcooler dimensional plotdemonstratesthedeclineofactivity[ex- measured rotationperiodsforthelateKandearlyMdwarf no starscoolerthan«4000Kareplottedduetoalackof rotation tolowtemperatureandslowrotation;(2)notethat ( «6000K)atlongperiods»100days)andcoolerstars figure: (1)themajortrendisfrombackuppercomerto class V,IV,III,singlesandbinaries)inthetemperature-rota- Plotted istheabovementionedsample(starsofluminosity strated inthepseudo-three-dimensionalplotFigure8. stand outfromthegeneraltrendandhavebeenmarked(HD short periods(«1day);(4)severaloftheveryactivestars stars inoursample;(3)alsonotethelackofhotter status andlargemassrange,wedonotattempttoquantify tion-activity space.Theslopeofthesurfaceinthisthree- scheme, butwemayplotoursampleinthe^rotTplane 36705, FKCom,andHR1362). the frontlowercomer,i.e.,fromhightemperatureandfast this behavior.Insteadwewantpointoutsomedetailsin temperature. Duetothemixofstarsdifferentevolutionary and investigateitsdependenceuponactivity.Thisisdemon- -2.1 Á. e{[ -21 Fig. 9.—Toppanel:UnnormalizedCAnKfluxinergscmsvs. £ 2 £

lambda (angstroms)

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