196lApJS. . . .5. .3 8IB form acatalogueofthespectrallinesasseenonplatesmediumdispersion.Agroup23selected zero-volt lineswereanalyzedforradial-velocityandintensitychanges.Althoughnochangeinradial several observersprincipallywiththe82-inchtelescopeofMcDonaldObservatorybothduringand after thedeepminimuminlightof1946.IdentificationmeasuresbyTaiandThackeraybefore minimum havebeencombinedwithdetailedmeasuresbythewriterduringandafterminimum,to lying shellinwhichtheTiOisformed.UnlikeRVTauristars,spectraltypefromlineratiosat found tobeasstrongas,orevenstrongerthan,inôCMa.Weaknessofthehydrogenlinesearly minimum lightwasalsoM3.ThespectraltypeaftervariedprogressivelyfromK5ptoG5p, even reachingF8pduringthe“flare-up”of1950.ThebehavioremissioninhydrogenandCaI i.e., Fen,Tin,Sen,Yn,andCm—aswellasstronghydrogenlinesfairly deep minimum. X 4227linesisdiscussed,aswellthepresenceofasharpabsorptioncoreinCaI.Thisalsowas from F8toK5.Priortheunprecedentedlight-minimumof1946spectrumwas reddish incolor,firstappearingsotoSchmidt(1872)ascolor6?5(yellow). the irregularvariableclassificationwasassignedbyCannonandPickering(1907)on probably duetoanoverlyingshell. 1939 maybeevidenceofspectralchangeleadinguptothe1946minimum.Evidenceiscitedforanover- velocity wasdetected,markedchangesinintensitydidoccur.ThehydrogenlinespCas1936were photoelectric six-colorobservation(onAugust 23, 1941[JD2430230])byStebbinsand characteristics ofanF8lasupergiantcompriseverystronglinesionizedmetals— of F8lasupergiants(Morgan,Keenan,andKellman1943).Thegeneralspectral changes. Thispaperpresentsastudyofthespectrumbefore,during,andafterthis minimum thatoccurredin1946,accompaniedbymarkedandextraordinaryspectral Additional photoelectricobservationsofpCasshould bemadetoinvestigatechangesin dening. Conversionofthisobservationtothe B—Vsystemgives=+1.37. Whitford (1945)whenthespectrumwasF8-G0 impliesconsiderableinterstellarred- strong neutralironlines.Theprofilesoftheselinesalsoimplyconsiderableturbulence. plates takenbetween1885and1946.Theirresultsindicatethatthespectrumvaried by Payne-GaposchkinandMayall(1946),whoclassified31Harvardobjective-prism basis of59observationsin1903-1905.Previouslythestarhadbeenrecognizedasbeing 4.1-6.2, Sp.F8lap)isofparticularinterestasaresultanunprecedentedlight- bility (Guthnick1914;GuthnickandHügeler 1920; andGuthnickPavel1920).A color ofthestar. F8, and,atthetime,pCaswasselectedasbeingrepresentativeofspectralclass hm0/ This paperconstitutesananalysisofextensiveseriesspectrogramspCassiopeiaetakenby A discussionofthecharacteristicsspectrumonlowdispersionhasbeenpublished t NowattheAlleghenyObservatory,UniversityofPittsburgh. The starwasdiscoveredtobevariableinlightbyMissLouiseWells(Pickering1901); TTfou irregularvariablepCas(HD224014,qiqoo^23494,Ô1900=+5657,m * ContributionsfromtheMcDonaldObservatory,University ofTexas,No.337. The visuallight-curvefrom1904to1934hasbeen publishedbyHassenstein(1934), Color observationsofpCasbyanumberobservershavealsoindicatedcolorvaria- v © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem THE SPECTRUMOFRHOCASSIOPEIAE.I* Received August20,I960;revisedSeptember16,1960 Wallace R.Beardsley! Yerkes Observatory I. INTRODUCTION ABSTRACT 381 196lApJS. . . .5. .3 8IB íí, creases anddecreasesinintensitywithnoapparentplateaus.Immediately while thephotographiclight-curvefrom1904to1946hasbeenpublishedbyPayne- tinuing toaboutSeptember,1922(JD2423300),thethirdthencontinuingdeep classification spectrograph dispersion 125A/mmatHy;F/2andCGMcDonald Cassegrain spectro- in bothlight-curvesistheexistenceofthreeseparatemodes(seeFig.2Hassenstein both light-curvesistheirregularityofperiodvariationandamplitude.Alsoapparent mode about200days,andforthethird300days.Itwillbeshownlater three modes,themeanperiodforfirstmodebeingabout450days,second 382 graphic curveiscomprisedofcircleswhichrepresentphotoelectricobservationsKos- light-minimum of1946.Asemiregularity,however,appearstoexistforeachthe dots, whichrepresentA.A.V.S.O.10-daymeans[beforeJD2433600the of thespectroscopicobservationsdiscussedinthispaper.Thevisualcurvecomprises scale. Thedatesanddispersions ofthespectrogramsdiscussedbywriterareindicated: X,Yerkes observations arethoseofOravecandAshbrook(Campbell1946,1948;Mayall1950ff.)], mode. and +signs,whichrepresentvisualobservationsbyParenago(1947).Thephoto- graph dispersions76and26 A/mmatH7,respectively.Thedate11-2/19-47refers toaseriesof12 The visualcurvecoverstheentireperiod1943-1954,photographiconly Gaposchkin andMayall(1946).Thelight-curvewascharacterizedbyalternatein- tylev (1947),andXsignswhichrepresentphotographicobservationsbyS.Gaposchkin (see Sec.Ill)thatthespectraltypeF8lawasapparentlyassociatedwiththird 1934), thefirstlastinguntilaboutSeptember,1911(JT>2419300),secondthencon- spectrograms by Greensteintakenwithin that interval. observations byKostylev;X =photographicobservationsbyS.Gaposchkinreduced totheKostylev September, 1954;.=A.A.V.S.O. 10-dayvisualmeans(beforeJD2433600theA.A.V.S.O. observa- 1954. Bothvisualandphotographicobservationsarerepresented,aswellthedates tions arethoseofOravecand Ashbrook);+=visualobservationsbyParenago; o=photoelectric (Payne-Gaposchkin andMayall1946;Gaposchkin1947)reducedtoKostylev’sscale. Figure 1presentsthelight-curveofpCasforperiodOctober,1943,toSeptember, Fig. 1.—Aplotofvisualand photographicmagnitudesofpCasfortheintervalOctober, 1943,to © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem WALLACE R.BEARDSLEY JULIAN DATE> 196lApJS. . . .5. .3 8IB formly toapproximately+0.7onaboutMay1,1947(JD2432307),nearthemiddle observations thereafterthroughNovember,1947(JD2432500).A“phaselag”isap- lines. Becauseofthesurprisingspectralchanges(F8latoMa)thattookplace,ade- asymmetrical, whilethephotographiclight-curveappearsnearlysymmetrical.Itis parent intherelativeshapesofminimum,visuallight-curvebeingdecidedly increased rapidlyto+1.3onaboutDecember15,1945(JD2431805),whichwasnear wg =5.4,itisapparentthatpCasbecameappreciablyredderduringthe1946light- interesting thatthepreviouslymentioned£—Fof+1.37byStebbinsandWhitford one takenjustafterminimum(CG6222-3,November5,1947)byJ.L.Greenstein,and series—one takenduringminimum(CG5171,November22,1946)byW.P.Bidelman, tailed analysisofthespectrumshouldbevalue.Accordingly,threeplatesin grain spectrographofthe82-inchtelescopeMcDonaldObservatory.Thedispersion minimum [seethelight-curvebyS.Gaposchkin(Payne-GaposchkinandMayall1946)]. was alsoobtainedduringthedeclinetoaminimum,althoughitmuchshallower of theinclineinbrightness.Anincreasecolorindextoabout+1.0occurredfor minimum. Fromwg—m=+0.6onaboutJuly15,1945(JD2431652),thecolorindex writer isverygratefultoDr.A.D.Thackerayforpermissionutilizethesemeasures spectrum ofpCasin1939madebyTaiandThackeray(1948),withapproximatelythe one takenwellafterminimum(CG8626,November5,1950)byG.Münch—havebeen the middleofdeclineinbrightness,andthendecreasedslowlymoreorlessuni- for theplatestakenin1939,1946,1947,and1950.Eachsetcomprisesthreecolumns presented inTable1.Thearrangementconsistsoffoursetscolumns,oneseteach same dispersion,anddepositedinthearchivesofRoyalAstronomicalSociety.The carefully measured.Inadditiontothesemeasures,thereareavailablemeasuresofthe was 18A/mmat4000A,26H7,41H0,and79theD Popper, J.L.Greenstein,andothers,principallywiththe500-mmcameraofCasse- the portion1943-1947.IfwesaynormalmagnitudesofpCasarem=4.8and and toDr.R.H.Garstangfortranscribingthem.Thecatalogueofspectralchangesis of thesignificancethesevelocitydifferences. Asecond-ordercorrectionhasbeen on severalstrongFe1linesinthespectrumwithaccompanyingcomparisonlines; lines. Ameancurvethroughthesepointswas usedtodeterminethecorrection.The applied tothemeasurementsbyplottingAXagainst XforallessentiallyunblendedFe1 the followingorder:(1)wavelength,X,correctedforapreliminaryradialvelocitybased very faint,thoughstillwell-definedlineand5 for thestrongestFe1lines.The1939in- scatter aboutthismeancurvewasuniformand consistent inallfourcases.Theaccuracy (1946), anextensiveseriesofobservationswasundertakenbyW.P.Bidelman,D.M. which was±0.05Aforallplates.Sinceblending isseriousatthisdispersionandespe- of asinglemeasurementisestimablefromthe meanmaximumrangeofthescatter, Table oíMoore(1945).Thepreliminaryvelocities(km/sec)were—42.6(1939),—45.7 P satisfactory. Thevisuallyestimatedintensities are arbitrarilybasedonascaleof1for Pv cially sincetheMcDonaldspectrawereobtained onfilm,thisresultshouldbeconsidered (1946), —40.9(1947),and—53.0(1950).Oneshouldapproachwithcautionthequestion (2) visuallyestimatedintensity;and(3)identification,basedontheRevisedMultiplet system bycomparing 1947 intensityestimatesofThackeraywiththe writer’s1947 tensities ofTaiandThackeray,alsoestimatedvisually, havebeenconvertedtotheabove v in intensityof2ormore inTable1shouldbeconsideredsignificant.The spectralchanges estimates, aswellcertain 1939estimateswith1950estimates.Themean scalefactor themselves aremadeparticularly evidentbythearrangementoftable. Linesinvari- ant astoidentificationare enteredacrossonthesameline.Changeisindicated byentry (Tai andThackeray’sestimate dividedbyBeardsley’s)wasfoundtobe 2.40. Adifference on different linesorderedbywave length. Commencing withthediscoveryofunprecedentedlight-minimumbyPopper © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem II. THESPECTRUMOEpCAS,1939-1950 RHO CASSIOPEIAE 383 © American Astronomical Society CATALOGUE OF SPECTRAL CHANGES On M $ oS •§ •§ c c ro o 00 o OO ooOH -ÿ-a c\jH \f\eo ooiH ££ 0O O 0^ £0 Bö ^ Hrr\^t I cr\ JÎCM CAH O vO . I..».I. cn ca-^jt— O it, O 9 bO Provided bytheNASA Astrophysics DataSystem UNIA vO • 384 i? IA >û CO OCA CM H Ôv O r— co o I • -f.A H IA fa fcH r^XA H 1A f^-UA M. CA to O) o O v: CM 'V-f ^ CN 0\
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I • && 38 U\vO ó¿ « • sO CA 18 TASO S TA g ¿a ü N O b • 67.1iU 3 7.26 Ife 1-1$ 67.38 1 7.26 Hg 1-1$ 67.M 2 7.26 Kg 1-1$ 7.27 Mg 1-1$ 7.27 Mg 1-1$ 7.27 Mg I-I5 7.$2 T 1-7 7.52 Y 1-7 7.52 I 1-7 7.67 Ti n-21 7.67 Ti n-21 7.67 Ti 11-21 TABLE 1 - Continuad © American Astronomical Society SO M öS *o © a xO o vO O rs Os c*y fe E-» Os rs •US •US C- Os O « R; R3 $Os iH-rt r-l C\JC\i aaie h££ • Provided bytheNASA Astrophysics DataSystem 408 CM -=T-LT\ rr\ • -^US OsrH CVI Os f’S r>s M JHIsO M HI & C- 77.21 3 (7.32 Nd 11-10) 77.19 3 (7.32 Nd 11-10) 7.59 Co 1-2 7.59 Co 1-2 7.60 Fe 1-13 7.60 Fe 1-18 CTi 00 00 ï—i LO m TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem so M rH >A t^i 0\ O M •§ a O vO 'Lr\XT\vO cm _cro r- 33 i -=i-=r CM -=t-=r ■fvA Os CM Os M CM • • »-N \o CM ¿>0 H M H =ir- (A Os—sO CO A O H l/s -CÎ "LA T SO ooOs VA f*- -^so H CM • * 88*21* le 8.69 Ti 1-220 TABLE 1 - Continued O M © American Astronomical Society -=f NO m On On M On Ö (D ■p § •a <0 T3 ■P o C o cm i-ct iaunoo O CM \A On 0\ Os I MCM • oo > CO CMtk- M OnO O > SO I M • CM On rH CM rH M .1. •H O fn O I H CVI CM CM 0\H-rf r-4 CMP~c>- gösg o • •* IH+ & -si'O -^"LA Provided bytheNASA Astrophysics DataSystem > VTV -ltn CM XfN TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem O M ■S «< NO U UWAViN vO'Of^-f- • # AAI'I NO f—t“- £ XAnO r-iCM LA-ZÍ OCA NOVO GOCO UNMD rHCMC^^tPv •LA-=Í OryrHCM -^■CV OO 'f'VSce rH «HOn iH rHOn ^?!£u &SÖ • * cm co_rr I“* .1..1 I rHCM oo u> _o CM On On rH CM I 00 03COOOOn CA rH CMiHO CA-OnO noH ft, O>•fbt,(It, T'Ytf'fY 9 Q0>O • 411 °0 CNOn vO iHCM -3 Otr- On 00 & On On On o • CVJ O O UN CM C'A V N fm U 02.IS £ 2.03 Fe 1-1*2 2.3S V 11-25 XA O CM I TABLE 1 - Continued © American Astronomical Society no H On M XJ T3 CM <3* o o VA OnCM-3P~ -3 On XA«»•»•» P"- OnPApH pt, bCO O O ^H*H«H VA pH Ä *0 T3 T3 *0'O CM r-O PA OnpH\r\0O •H -H*H^ co wenM> mx xm 'S £.&& O -dpp\ nO 'OA~OOCO ^ nO PA » 'S O -3-PApHOs C— t—pHnOOn On a> M NO CO S PA I VA £ ¿i£ I M I l-H I W CO UN CO -LAOO OO VA I cr> Provided bytheNASA Astrophysics DataSystem CM CM OnH CM 'ft. 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PN -=í P- CO 'S S Eh fn • UN vfi' H M3 pH UN , O On pH t-~ pH .1 t^OO r-co • ^8 CO CM UN I UN PO CO CM CO CM UN P3 UN ,I UN PN M .1. M Provided bytheNASA Astrophysics DataSystem UN r- 466 CO pHH CO _zipH_Cf UN M3 UNPN OUNO M I _3tH pH pH cog g UN NO IAUW/nvO vO 0*0 OUN PN OnCM SS S-4fr,E-< f>0 On 38.86 0 8.60 Ni 1-166 9.27 Fe 1-687 CO On s* ee TABLE 1 - Continued & © American Astronomical Society r- M Os '—— OA OsOi—I Os M.• x> £ ® xl XJ CMO'sOO © 0-=f o m sovn c^fHc^c^v co ^so_a-sO CM II »II» m 1-1 -H© 6-* EhCMO On OfH(HrH III I.1 oosO -CjvO OsOC^- .it. _3-sO COiH sO c—i_r\cm CM sOOOO . I. O HCmE-» Provided bytheNASA Astrophysics DataSystem c«^ cr\r^v co 467 sO Hcm sO CO so CM UN CM OvOH \r\ .1.1. »..1. • Os ~=T S3 ». » 50.77 In (8.85 Ni 1-195) 9.82 Fe I-lll* 1.6b Fe 1-16 (2.12 C 1-12 00 00 ï—i LO m TABLE 1 - Continued © American Astronomical Society £ SO M O- M• O no Os M Os ■O sOOs +3 P«hO 'S ë o "O xO tí • Oh o o lO vO rH CO I sO Os r-i COrH Os ^8 Y Y CO C. O ■LfN Provided bytheNASA Astrophysics DataSystem 468 UO rH vo UO rH .1. E-* E-h r- co no .1 co Os no Os CO O 'S co H Í8 CO rH O no H I O H Ox no I M E-i -tí Ono coco O rH CSJ-tíUO rH HI H Ono O COrHQs «h qH O COrH ^ Osno 1¡"í A _ Osno I MII sO H -=i O no Os C*-0O Scíá £ 00 00 ï—i LO m TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem « SO M Os 00\ Os Os M• 'S xJ csjr- c © 0O "Oc¿ .O est ^ in $ -=î sO cvj r~ ON Os • a> £• ^-s .1. .»..1..». r-s no oo c~- (H r-trH cn r^\ • .1.« H O m I so r- »S -S • 469 so £—r^- M I ( • -=r o. °\ T O CSJ 'H sO o P o as. VO stg 97.81 1 7.00 Fe 1-1092 98.01 1 7.00 Fe 1-1092 8.70 Fe 1-66 8.70 Fe 1-66 TABUS 1 - Contimied © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem in vO M O M Os OsM r-i _ TD m T3 'O t a> 15.56 0 5.1*0 Ni 1-177 15.28 0 5.1*0 Ni 1-177 TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem >0 sO M O M Os -p TJ 87.05 In 6.33 Ti 1-183 8.21 La 11-96 (8.70 Ti 11-70) 8.85 Ca I-U9 00 00 ï—i LO m TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem NO M On r~\ oc.ooco On H•. ON O H 'Ü 'O 00 © C © G IT) O CM M EhO c\j r-oo H tHI On t— rH Oi_f\ ass (0 *H08 H m"Í I -G o r- On O t>~ On I -G nO QXA -G OCA nO O'lt\ OO OCO CO O0O fr Oft, fA rHCO r*N CMCA © G ( 1I >11 CM CM C'A O ro rH CO O M HOCNJ O0_^ CA rH OU.62 3vs I1.52 Cr 1-7 U.58 Fe 1-1 00 00 ï—i LO m TABLE 1 - Continued v\ rH O I Os © American Astronomical Society sO M Os 'O ptfO • in CM M T-TN 'LT\C"—O CM 03 M H t^- HICM O ÎMo M H r~-H cmc^- »h o^ O t* TABLE 1 - Continued vr\ Os O M• Os © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem sO M _d Os Os H Os CA T3 oucc xi 'O -P : G © o O CM lO ■LfNrH m o e*\ Os fc ft, XA fH 1AO CO Os I XAO Os O, CA Os 'S I • O O oo _=r CA Os CA I oo -ci CA Os CA I I m I M sO XA CO OsCs) sO C—CM IA OsCO iH IAI OA'—'' sO I M 476 _=!■ O CO CM -zr O IA ~ZÎ CA H O Et, ü 0) h I fX4 ü 0) ■laOs sû O CMXA Et, E-*O © *HE, M sO O r^v iH -la ci CA I IA _=i-S-a-iA CM SOCA rH OsIA M CM IrH O -J-CM Os rH O Et,& _cr_cí _ztxa CM sOCA CM IrH rH Os M O _3- _=î _=î-3-XA CM IH Os rH O Et,fa rH OsXA O -O.CM o fau I M1 E-i (D©ti • ^ 1?h I Mt I hH • » TABLE 1 - Continued © American Astronomical Society UN o, o M TJ OnOHnOCO +3 Oft, £h © CMNOf^CT)On • 0)0>h(D o cvi in -a-_^^xr,-UNNO CM I(HpH M O OJ pH OnU\QOiH I M Ov â CM M I o M H O C^-CM w I H O r- cm t-* O I CM I CM CM VA CM VA Provided bytheNASA Astrophysics DataSystem PA 477 CO CM H CM I CO -la -3-IA Un. O NOCM f"! .I.• ■cr CMCO I CMrH • oo h C^N O 73.65 0 3.18 Fe 1-553 73.?2 1 3.18 Fe 1-553 3.38 Fe I-11Í4 3.38 Fe l-llj* ií.2U Ce 11-15 Í4.21* Ce II-15 00 00 ï—i LO m TABLE 1 - Continued -=r © American Astronomical Society H On nO H XJ r o CJ m T OO 0O-ZÍf-CNOnfT\ rH OOCNl(HNÛCKO ^ feoÖ(*4O CA fA_ZfIAUNlAnO 4> Oq}hp^4 On I I M Os HU i T M I M _3_=i_3_zr On 1 UN VAnO H NOOnO o 2k.21 1 k.18 Fe 1-553 00 00 ï—i LO m TABLE 1 - Continued IA O W © American Astronomical Society Os rH Os CA Os M TS D in ro u\ rr-lro fi-\ 0\ VA I XA-ÇT CO sO caOs I MII rH XA 8 _01A CO CAOs fe fx. I M w rH fA rH CA lA c I -O r— QO 0OOs Os CA I I. VO I sO oo O no fA I Os csj & co p o o .1. !-• Provided bytheNASA Astrophysics DataSystem Os 480 rA Oseo O £-• tH Œ -n-vA co Ä' M I I CA OAsO r^ iaca no_3 no Os OrH OssO O .1. III S.S rH H O Ö ££ S.& no-O (HI r- co Il IM CO Os Os oocsj lAsO sc0O rH I CC CsjCD rH IT I M0-1 O Pf M H U I-©Jh I M C-O Os CA Os CTi 00 00 ï—i LO m TABLE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem :0 ro o in 1 0O OsOnO' OD r^-OH CM O'CO o cnco ^ Vn OH CM_3C— M W In O© ■LTN U0 1AUN O OH rH r^i O O VO CvJ tSI U h ^ o On CM M H< rH 1>- OH OH-3 (t. 25 © *H r ^-CÍLH Os CMo^. p£< :zo o rH t^-I © -H <"'i -3-LTNcm _j °r? i’O OOfV'v O' CMroo fe 2;O © *H 77.19 0 7.08 La 11-95 81,07 In 1.02 Ti 11-69 81.10 0 1.02 Ti 11-69 81.2h 1 1.02 Ti 11-69 81.3h 1 1.02 Ti 11-69 196lApJS. . . .5. .3 8IB \r\ O M o\ T3 NO l-H © American Astronomical Society On M •O ■V O 7^ cr\ xo r—i ITN M fXH > © I o rO uD M •UNvO M K1 C^v CNJ E-* CO •H Vi I UNNO ONCU "UN ON CO GO rH.O UN O' rp^ pH I ■UN r-tvO c*— C^ TABLE 1 - Continued NO H H -=t © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem On CA On M On ■LO 0\O rH Os O M• _ T3C--OS •o •o ■p O ® 0\i—I ß o to OO rH sC 1-0 CA VO Hla CO io' M « O CNJ M I W t-H "f S CO VO HH I ÍN OO rH t—• M M b-l (3L| I rH LA $ OO O-3-la OO rA NO rH_d- O NO H .I.It-H CO CA ON _q-On O NO On ô^î. I -riHI NO M rH CN-I -t On I M 483 TÍ o NO O NOCNJ rH C— M t-H C— 1_At—\0 fa 5C nO O nOCNiCNJ rH r~-I rH O t— LT\nC ® •HiH I HH I M 1 35 faEh : fa • r®r f LANO -=J ON On I CA -O O LA CNJ rH Eh fa On I 1 I 1 LA CNJ O rH ^ I M ON rH r^LA CA i .» 00 00 ï—i LO m TABLE 1 - Continued H © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem r-M 1 On M On CA TO 68.32 0 (Q.hh Ti 11-102) 00 00 ï—i LO m TABLE 1 - Continued -d' oi—i no M• On PN On M & © American Astronomical Society TJ -O •o NOCM O in "fl NO CM iW O rH a Eh £ *H • § 3 O _d- \nr- M I O PO O I CVJ '-n. OsCO -cfUx Cm co -CílACM UN CM rH CJ CVJrH O CMCO M H O CNJro f— UNO r~-vr\0 I I ti On CO 'S On nOnO UN On CNJ pH UN fin 25 nO C^-C— NO OOn .1 IM O Onun-U H UNI vO vot^- vO OOs o tx, 25CJ TA3IE 1 - Continued © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem UN O (—t On vO H OS OS M CA MO <-l « c X> C ® o to \0 OO oo O oo Eh \D CM r-i o~\ C *LO\ ¿A 0\ t"- M Cm r-vr\ CM M t^-XA I Cm LAXA i—I XAO XA M I CM O M O Cm M o— c—•co O *HM I Me • to tr> o o „3^ OM -U \1_(0U-\ XA UNIA CJ rH 1I Mil o M r-'uooo fcn O & XA M lI i t-iM I M I M o o CM CA o • XA0O M CM M CAXAvO I 486 XA ^9 3xa XA M fc. Cm CD 12.96 2 2.98 Ca 1-1*8 TABLE 1 - Continued ■u\ © American Astronomical Society o i Os o m in NO XT', C-J ^ CO Cn/ OnM M >-i COfr* I U p lAvO COQO tin CO38a -1 1OnON CNJ UN NOCDCOCC r—I IONOn Q> obi'fciib*.' M cxh co3a t HI» I M o'\ l/N COUNON_rt_i3 UN nOC—COCC UN M_3-OnoI—I (i comafsaa MU IM NO «—1 UN NO£N-ooa?OOONCNJ CNJ f-t ICNJOn M ^ O c-N © CO® «¡SO oí*lo o nS’C HaôCo'oMrtj, pp TABUE 1 - Contiinued s? On W H © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem § r* I h 97.i¿ On 1*.73 Cr 1-239 6.22 Gd 1-3 8.33 Cr 1-239 8.51 V 1-35 0. Hi Sc 1-12 TABLE 1 - Continued © American Astronomical Society On vO S On M PN ■P •o c o o IO <0 o -=rsO COdoor^v M I r>-\ CMrr>,H_^o nO On r—r—I Ä, 008S c*oe o ¿ 8-nc i C6*n) ¿5-H cn*5) 8.5-111 ; TABLE 1 - Continued oS H © American Astronomical Society so M a> c t Os Os M •Ö x> <0 O <30 O CM* CD ^ (O \r\ t- c— O â -f'Y r~- cm ITS MO O Ä oo Os o VH I M W 3 © I H oo Os V> ¿3 SB [s_ Os Os ij a) as \. Provided bytheNASA Astrophysics DataSystem M Os CO > 492 ÎÇ CN / V « & \. SO 0O (—I r~ CM y / 196lApJS. . . .5. .3 8IB strong interstellarorcircumstellarreddening. The decreaseinstrengthbelowX4600 trum hadresembledmorenearlythepostminimumphaseofepoch1950,withFeliweak and zero-voltFeilinesstrong(Bidelman1953).Onthebasisofobjective-prismspectra, later. However,ifoneconsidersthatobjective-prismclassificationisusuallysomewhat nearly so.TaiandThackeray,however,pointto thegreatstrengthofsodiumDlines mostly resolved.TwoYerkesBrucespectrographplates—oneofthepCas(August, influenced bytheappearanceofcontinuum,suchanapparentdiscrepancycanbe conflict withtheF8laclassificationsfromslitspectrogramsofhigherdispersionstaken in Figure2.The1937spectrumshowsevidence of ahigherlevelexcitationthaneither tinuum increasesrelativelyinstrengthataboutX4600andisverysimilarappearance directly, discloseamuchdifierentappearanceofthecontinuumforpCas.Thiscon- Payne-Gaposchkin andMayall(1946)classifythespectrumasmuchlaterthanF8ever particularly thoseofFe i-2representedbyX4347,4389,4405,and X 4435.The1944 That thespectrumwasindeedbeginningtoundergo changeatthistimeisillustrated and theapparentweaknessofhydrogenlines asevidenceofpossiblepeculiarity. may beindicativeofageneralmolecularabsorption aswell.Spectratakenatthe since themid-1890’s.Thisresultisbeyonddoubttoabout1920butappearsbein ening oftheionizedlines X4296(Fen),4344(Tiand4394 n)isevidentin to thecontinuumofaKstar.Itseemslikelythat thiseffectisdue,atleastinpart,to graphic magnitudewas approximately5.7(Payne-GaposchkinandMayall 1946).In plate wastakenbyStruve duringashallowminimumthatprecededthe deepminimum. Dominion AstrophysicalObservatoryin1936, at theYerkesObservatoryin1937and The visualmagnitude at thetimewas5.2(Campbell1946,1948), while thephoto- 1923, anddefinitelyF8lainSeptember,1929.Previously,from1906to1910thespec- the 1940or1944spectrum,spectrum beingintermediate.Progressiveweak- 1940, andin1939atCambridgebyTaiThackeray (1948)arealsoF8laorvery 1933) andoneofôCMa(April,1931)—showpCastobeF8labut,whencompared 1940 andespeciallyin1944. Low-excitationlinesweredefinitelystrengthened in1944, vwk =Veryweakintensity(referredtoemissioncores). wk =Weakintensity(referredtoemissioncores), abs =Absorptioncore, str =Strongintensity(referredtoemissioncores), li =IdentificationbasedonIglesias(1956). u =UnclassifiedTiOabsorption, sw =IdentificationbasedonSwensson(1946). MIT =IdentificationbasedonMassachusettsInstituteofTechnology(1939). em =Emissioncore. b =Blended v =Blendonvioletwingofline(TaiandThackeray). med =Mediumintensity(referredtoemissioncores). kk =IdentificationbasedonKiessand(1931). d =Doubleline. BH =Bandhead, vs =Verysharpline. s =Sharpline. nn =Verybroadline. dd =IdentificationbasedonDavis(1947). * =Absorptioncore,intensityIvs,incenterofline4123.44,2. r =Blendonredwingofline(TaiandThackeray). n =Broadline, Bidelman andMcKellar(1957)describethespectrumasnearlyF8lainSeptember, © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem III. DISCUSSIONOFTHESPECTRUMASAWHOLE a) TheSpectrumbeforetheDeepMinimum NOTES TOTABLE1 RHO CASSIOPEIAE 493 196lApJS. . . .5. .3 8IB hydrogen asapossibleexplanation.AsimilarcomparisonwithÔCMa(F8la)should stronger than,thoseof<5CMaandarenotconsistentwiththesuggestionTai follows: for<5CMa,H<54.50AandHy5.20A;pCas,6.46A. grams takenatnearlythesametimes.Aheavy veilingofthespectrum,alsomentioned considered evidenceoffurtherspectralchange.Itispossible,then,thattheapproach Thackeray. Sincespectralchangeshavebeenfoundfor1940ascomparedwith1937 concluded thatthehydrogenlinesforpCasin1939wereweakerthannormal,even Figure 2thespectralclassificationratioX4444/X4325forthisplatecorrespondstoabout be morereliable,andaccordinglythewriterhasmeasuredequivalentwidthsforH3 though thespectrumwasverynearlyF8la,andtheysuggestedanunderabundanceof wings. TaiandThackeray(1948),however,fromacomparisonwithPersei(F5I¿>) ing thebottomplateauofminimum(June and August,1946).HeretheTiObands in April,1947,whenthestarwasm=5.3onitsrisetofullbrightness,TiObands parable brightness,therewasnoevidenceofTiObands.Thackeray(1948)statesthat as showninFigure2,itseemsapparentthattheweaknessofhydrogen1939canbe and sincehydrogenwassomewhatweakinboththe19401944spectrograms, are strong;however,theincreaseinstrength of TiOwithtimeduringtheminimum a shorttimeafterthedeclinetodeepminimumhadcommenced.Thevisualmagni- of thedeepminimum1946washeraldedbyaweakeninghydrogenlinesatleast These valuesimplythatthehydrogenlinesofpCasin1936wereasstrongas,oreven 8 A/mm,andaDominionAstrophysicalObservatoryplateofpCas(26011),10 and H7,utilizingaMcDonaldcoudéplateof<5CMatakenbyH.A.Abt(Cg2277), the starreturnedtom=4.8inmid-1945. occurred throughoutthe periodofdeclineandriseaswell. Also, fortheRV trum theAlObandX4842(seePopperandBidelman 1947)canbediscernedfaintly. noted thestar’sextremefaintness.Figure3alsoillustratestwospectrogramstakendur- bands appearedwhilethestarwasstillfairlybright.In1944,whenofcom- as early1939. existence ofTiObands.Unfortunately,theplateitselfwasratherpoorquality,and tude hadbythendroppedfrom4.8to5.2.Themoststrikingfeatureofthisplateisthe taken inSeptember,1936,byT.S.Jacobsenandkindlylenthim.Theresultsareas Spectral Atlas(Morgan et al.1943)consistentlyyieldM3forallthree dates.Thusthe are present.InpCasa comparison ofthelineratiosX4176/X4200and X4383/X4406 by Thackeray,isparticularlynoticeableinthe regionXX4300-4500.IntheJunespec- noted byThackerayisnotapparenteitheron these orontwo//2McDonaldspectro- time Popper(1946)firstnotedthatTiObandswerepresentinthespectrumandalso were stillpresent,though“almostgone.” the presenceofbandwasnotnotedattime.ItisinterestingtonotethatTiO Mounted aboveitisthe1940spectrumforcomparison.The1945platewastakenonly 494 line ratiosyieldedaspectral typecloselycorrespondingtotheTiObands themselves. Tauri starsRosinoassigns K-typespectralclassesfromlineratioseven whenTiObands This bandappearstohavestrengthenedbyAugust. Theoccurrenceofheavyveiling the TiObandsoccuronlyatdeepestportion oftheminima.InpCasTiObands stars (Rosino1951).However,twoimportantdissimilarities exist.IntheRVTauristars and TiObandsduringtheminimumphaseisstrangely analogoustocertainRVTauri GO (Morganetal.1943).TheGbandhasanappearanceclosetoGl,whiletheratio for McDonaldf/2spectra takeninJune,August,andNovember,1946, withtheYerkes X 4227/HystillcorrespondstoF8.Wehavenorecordofhowthespectrumbehavedas v v H I.—InanF8laspectrumthelinesofhydrogenarestrong,withwell-developed A spectrogramobtainedbyBidelmaninOctober,1945,isillustratedFigure3. The declineprogressedsteadilyuntilm=6AwasreachedinJune,1946.Atthis v © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem b) TheSpectrumduringtheDeepMinimum WALLACE R.BEARDSLEY ro OI X 0> O í$ 0> 4325 4444-^ 4Ü27CaI-2 ‘.f** *** • Cr I 4296FeE-28 4405Fe I 4394 TiH 4435 Fe 1-2 4340 HH 4389 Fe I- 4344 Til- 4347 F® 1-2 Data System © American Astronomical Society • Provided by the NASA Astrophysics ‘vV /- *'* ; »/.Vi'. •.'■'■ ' 'Ä, . :./-■ ??.■ ■' . W.oóyfe- l.Âô.t'Se'î.i'-, MS- Fig. 2.—Preminimum spectral changes of p Cas, 1937-1944 m CTi 00 ï—i 00 Septl94Ô Data System © American Astronomical Society • Provided by the NASA Astrophysics Fig. 3.—Low-dispersion spectra of p Cas taken with the Yerkes classification spectrograph, dispersion 125 A/mm at H7 r m 00 ï—i 00 196lApJS. . . .5. .3 8IB August, 1933;(c),November,1946;(d),1947; (e),November,1950. Fig. 4.—Thespectrumof(a),dCMa(F8la),and(b-è), pCasintheregionXX4540-5015:(ô), © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem 196lApJS. . . .5. .3 8IB J 4214 ZrX-45 Fig. 5.—Theappearanceof the regionsofCaiX4227andH7inpCas,1933-1952 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem 42W SrXX-M 4227 CaI-2— 4230 FeI-41 Col-1 4333 VI-5J 4337 T»3I-20i 4340 HI-1- 4347 FeI-2-« Fel-4Í tí CÔ525I C6532Q C.65I7I IW0737 C69III CÔ8626 C65249 196lApJS. . . .5. .3 8IB as Sci,Til,VI,Cri,Coetc.,wellthoseofrare-earthelements,weremuch high-excitation linessuchasthoseofTin,FeScetc.Linesneutralatoms, minimum datadiscussedbyBidelmanandMcKellar(1957).Theyfoundmanylines, strengthened. MostFeilinesappearedsomewhatstrengthenedcomparedwithpre- ing shell.Velocitymeasuresfortheseshellcomponentsyieldedvelocitiesnearly—70 shortward componentsappearedtobedisplacedcharacteristicofanexpand- particularly stronglinesoffairlylowexcitation,tobedoubleduring1951-1953.The minimum. TheexistenceofashellgasaboutpCasisquitecertainfromlater,post- km/sec, whilethemeanvelocityoflineszero-voltexcitationasdeterminedby velocity. ItalsoseemslikelythattheTiObandswereconnectedwithformationof zero-volt lines,itwouldseem,belongedtotheshellonbasisoftheirstronglynegative of Figure6,showedlittleornodeviationfromthemeanvelocity—60km/sec.All writer (Fig.6)wascloseto—60km/sec.ThevelocitiesofthelinesX4347andX4389 nearly —45km/sec.Thewriterhasfoundthatthesetwolines,overthetimeinterval belonging toFeimultipletNo.2werefoundbyBidelmanandMcKellarbemore mum. InFigure4,c,isillustratedtheregionofHßforNovember,1946.Noemissionwas apparent. AweakabsorptionlinepresumedtobemostlydueHß,however,yieldsa the shell,andthatshellformedearlyindecline,ifnotbefore. lines. StrongemissionwasevidentinX5167despitetheTiObandhead.Inaddition, filled inthevioletwing.InFigure5isanenlargementofH7atsametime.Here, numerous absorptionfeaturesduetoSiH. occurred infairstrengthduringminimum.Identifications,basedonDavis(1947),imply plates (CG5166,CG5171)takeninNovember,1946. broadened byastrongabsorptionwingontheviolet. November, 1946,noemissionwasapparent,buttheabsorptionlineconsiderably wave length(seeTable1)shiftedstronglytothered.Onemayassumethatemission was striking(seeTable1),whilemultipletNo.1 appearedingreatstrengthatminimum of emissioninHandK,eventhoughCa1X4227 wasinemissionatthattime. in Figure5. filled inbyemissionduringthedeepminimum.Severalspectra(i.e.,//28067)takendur- of thatyear.Figure3also illustratesfourspectratakenduringtheinterval from1947 multiplet No.60. ing minimumshowtheHandKregionextremely overexposed.Therewasnoevidence X 5184wasmissinginNovember,1946,presumablybeingfilledbyemission. during minimum. to 1950afterthestarhad regainednormalbrightness.TiOwasnolonger present,AlO (see Sec.IV).Keenanhasalsonotedaweakness duringminimumofthelinesdueto The linespectrumatminimumlightwascharacterizedbyageneralweakeningof H I.—ThackerayhasalreadynotedthepresenceofcoreemissioninHaduringmini- In thefollowingdiscussionterms“strong”and“weak”arerelativeonly. Na I.—StrongDemissionwasnotedbyThackeray.Thisconfirmedontwo Ca I.—StrongcoreemissionwaspresentinX4227duringNovember,1946,asshown Mg I.—Thezero-voltmultipletsshowedcoreemissionanalogoustothatoftheD Fe I.—Theweaknessofthelinesduetomultiplet No.15,firstreportedbyThackeray, Cr. II.—StronginpCasbeforeminimum.No evidence inNovember,1946. Si II.—NotdetectedinNovember,1946,althoughpresent1939.However,1 Rare earths.—Therare-earthelementlinesappeared tohavegenerallystrengthened Sr. I.—Strongduringminimumbutnotobserved beforeminimum. Ca II.—Keenan(1947)foundevidencethatthen-2tripletininfraredwas Rho Casbegantobrighten inFebruary,1947,andreachednormalbrightness inJune Y /,ZrI.—Strongduringminimum. © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem c) TheSpectrumaftertheDeep Minimum RHO CASSIOPEIAE 495 196lApJS. . . .5. .3 8IB virtually invisibleonthehigher-dispersionplates.H/3wasagaindiscerniblebutstill remaining spectra.ThebreakinthespectrumatX4473becameagainasstrong remained inSeptemberandNovember,1947,butalso(seeFig.3)disappearedthe plates, onewithaheadatX4864.0andtheother,verystrong,about for August,1950.TheratioX4383/X4406againseemsthemostreliable.Fromthis illustrated, theratioX4200/X4176seemstoimplyanearlyKtypebutmustbecon- only representaregionofverycrowded,strongabsorptionlines,asthesefeatureswere weaker thanin1940.Theveilinghaddisappeared.Ifoneattemptstoclassifythespectra lines thathadbeenveryprominentnearlydisappeared.AnexaminationoftheX4383/ sidered inconclusive.TheratioX4227/H7isdoubtful,owingtoemission,andstillgives 496 following discussionrefersto1947and1950spectraonly. grain spectratakenbetween1950and1953indicatesthatthespectrumwasthennearly results whichseemtooearlyintype.TheserangefromG8forSeptember,1947,toG1 increased fromm=4.8onaboutJune1,1950,to4.2November surprising asthedeepminimumof1946.Acombinedplot(seeFig.1)Oravec’sand we adoptforSeptember,1947,K5;1948,G8;July,1949,G5;andAugust, X4982. Thereissomequestionabouttherealityofthesefeaturesasbands;theymay Ashbrook’s visualestimatesandA.A.V.S.O.means(Mayall1950fif.)showsthatthestar reaching m=4.6byJuly1,1948.AspectrogramtakenonApril29,1948,wasidentical time duringtheshallowminimum,H7changed fromthesharpcoreemissionandwell- with thatillustratedinFigure5forSeptember, 1948,insofarasH7isconcerned.Some- star remainedabout=5.1untilaroundApril1,1948,whenitbegantobrighten, ber, 1947.Oneachoftheseplatesalsothehydrogencoreemissionwassuccessively in Figure5.ThestrongvioletabsorptionwingwasevidentMay,June,andNovem- cause oftheabnormalstrengthmanylow-voltlines.Withexceptionsasnoted, then declinedrapidlytoabout5.0bythemiddleofDecember.The1950platemeasured a magnitudewhichthestarhadnotattainedsince1915(Hassenstein1934).The 1940. Twounidentifiedbandlikefeaturesbecameapparentonthelower-dispersion but nolongerhavingasharpcoreemissionfeature. AplatetakeninDecember,1948, defined absorptionwingsofNovember,1947,to ashallow,filled-inlinenearlyaswide m =5.1,whichoccurredfromaboutOctober1,1947,toDecember1947.The and thenbyadeclineofcoreemission.ThebehaviorH7inparticularisillustrated theless somewhatlowerthanhadbeenthecasein1929and1939.Itmustbeemphasized have narrowedandwassimilarinappearance to thatillustratedforNovember,1950, still showedthewide,partiallyfilled-inline,but oneinDecember,1949,showedH7to stronger. Themaximumstrengthofthisemissioncoincidedwithadeclineinbrightnessto X 4406ratioonthisplategivesaspectralclassclosetoF8,buttheexcitationwasnever- G5. Thelight-curvefortheperiod1947-1953revealsaflare-upinbrightnessalmostas velocity accompaniedby maximumlightcharacterizestheRVTauristars (Abt1955), violet absorptionwinghaddisappeared.Itisa possibilityherethattheshellwascol- 1947, K5;April,1948,andDecember,G8.ExaminationofMcDonaldCasse- 1950, G3(meanofG1and 55>h(t, C'A COCSJsO so voOs XiMAusOO CM _^COH rH I r—t OsC\J_rj C'A QOr\iso I M I w P~s f— c 453 UAUA O Os PASO CO UAUA o cp\ vOCO r~i UApH o Pl,e-< 77^ • V ®iH PA^-s tíA VA Os C'A VO O JX4 C'A t^- ^ vr\ Vi S< » IM On Provided bytheNASA Astrophysics DataSystem