FILE D: NOTES TO TABLES II AND III. . N1 V478 CYG. PM EL: POPPER,ETZEL(REF 1465) FROM PE OBS OF POPPER IN B AND V.BOTH COMPS HAVE PRACTICALLY EQUAL SIZES AND BRS;X1=X2 IS ADOPTED TO BE .31 IN V AND .36 IN B.EARLIER,VERY SIM PM EL WERE OBTD BY GAPOSCHKIN (REF 1;2) FROM HARVARD PATROL PG OBS. COMPS ESS .40;R2= .30-.32;I=63-64 DEG). TO ALL APPEARANCE,HOWEVER,PM EL OF SCHNELLER AND OF RAMELLA ET AL. CORRESPOND MUCH BETTER TO REALITY,THAN EL FOUND EARLIER FROM PG OBS;IN THAT CASE,COMPS APPEAR TO BE ESS> THAN KEPLERIAN VEL. P IS PROBABLY VAR;ACC TO CATALANO,RODONO(REF 1562),THERE IS APS MOT IN SYSTEM WITH P1 ABOUT 1000 YRS. * IS THE BRIGHTEST COMP OF VIS OCTUPLE SYSTEM ADS 16795;THE CLOSEST VIS CMPN IS 9.3 MAG AT 1.1''. N34 BETA AUR. PM EL: JOHANSEN(REF 157)FROM PE OBS IN 8 COLOURS:IN WIDE-BAND B AND V,IN STR0MGREN 4C-SYSTEM AND IN H-BETA REGION(WITH BAND WIDTH 37A AND 191A).X=.60 IN B;.50 IN V;.49 IN U_;.63 IN V_;.55 IN B_;.48 IN Y_;.59 IN H-BETA (191)AND.46 IN H-BETA(37).ECLIPSES ARE SHALLOW;COMPS HAVE ALMOST EQUAL SURFACE BR;THEREFORE,NOTIONS'OC.'AND'TR.'FOR THIS SYSTEM ARE HIGHLY VAGUE AND EXACT DETERMINATION OF R2/R1 FROM PM DATA IS DIFFICULT.FROM A SERIES OF PM SOLUTIONS OBTD BY JOHANSEN FOR DIFFERENT VALUES OF K(CLOSE TO 1.0)THE MOST REASONABLE SOLUTION WAS CHOSEN;APPROPRIATE PM EL ARE GIVEN IN THE TABLE II.VERY SIM PM EL WERE OBTD EARLIER BY PIOTROWSKI(REF 158)FROM PE OBS OF STEBBINS(REF 159) WITH SELENIUM PHOTOCELL(WL EFF 7000A).THERE EXIST ALSO PM EL OF SHAPLEY(REF 82) AND OF NEKRASOVA(REF 160)FROM IDEM OBS. ALTHOUGH BOTH COMPS HAVE SOME EXCESSES OF RADII,THEIR DIMENSIONS ARE<.90.IN TABLE II AVG FROM GEOM EL AND FROM L1 AND L2 OBTD IN ALL COLOURS IS GIVEN(FOR K=1.00);X=.73 IN U_;.82 IN V_;.73 IN B_AND .61 IN Y_. ALMOST THE SAME PM EL ARE OBTD FROM IDEM OBS BY MEANS OF LC-SYNTHESIS METHOD (USING WOOD'S APPROACH) BY GIURICIN ET AL.(REF 1580). COMPS<2100) PE OBS IN WL EFF 5150A OF CRISTALDI(REF 303);EL ARE COMPUTED BY MEANS OF LC-SYNTHESIS METHOD,USING WOOD,S APPROACH;X ARE ADOPTED EQUAL TO .70+.80;PM SOLUTION IS OBTD,ASSUMING PRESENCE OF ADDITIONAL LIGHT SOURCE L3 IN SYSTEM(L3=17(P.E.=4) PER CENT OF TOTAL LIGHT OF *).LC IS ASYM OUTSIDE ECLIPSES AND IN ,SHOULDERS, OF MIN II;IT IS POSSIBLE EXISTENCE OF GASEOUS STREAMS IN *. EARLIER,FAIRLY SIM PM EL WERE OBTD FROM IDEM OBS BY M. FEDJANIN, V.KUVSHINOV,L.KUVSHINOVA(THESE EL WERE PUBLISHED IN CAT OF SVECHNIKOV(REF 142)). THERE ARE ALSO PM EL OF CRISTALDI HIMSELF FROM HIS PE OBS,FOR CASE ,GR.OC., IN MIN 1,WHICH DIFFER CONSIDERABLY FROM EL GIVEN IN TABLE II. EL OF CRISTALDI ARE OBTD IN ASSUMPTION OF PRESENCE OF ADDITIONAL LIGHT SOURCE(L3 ABOUT 1/3 FROM TOTAL LIGHT OF *) IN SYSTEM. COMPS<.5,OTHERWISE OBSD SIZE OF SECOND WOULD ESS EXCEED ITS RL2. DISCUSSION OF SP AND ABS EL OF * IS GIVEN IN ARTICLES OF PLAVEC(REF 355)AND OF BATTEN(REF 374). SPE OF COMPS ARE ESTIMATED BY CANNON(REF 400)AS A0+K0.STRUVE(REF 395) FROM HIS SP OBS CLASSIFIED PRIM AS B8-B9 AND SECOND AS G_G2.ROMAN(REF 191) HAS DETERMINED SPE2 AS G8III.ACC TO KOCH ET AL.(REF 100),SPE1 IS B7V-B8V; OLSON(REF73)HAS ESTIMATED SPE1 AS B6.AZIMOV(REF 401)HAS OBTD IN MAX SPE OF SYSTEM B8V AND IN MIN I G5 IV-III.FROM SP OBS OF BATTEN(REF 374),SPE OF PRIM IS,APPROXIMATELY,B7V AND THAT OF SECOND G5-K0 III-IV,THE MOST PROBABLE, G8 III-IV.FROM ESTIMATES OF B-V AND U-B FULFILLED BY BROGLIA(UNPUBLISHED), PRIM IS B8V,FROM ANALOGOUS ESTIMATES OF EGGEN(REF 402),IT IS B7V.FROM NARROW- BAND PE OBS OF MC NAMARA(REF 310),SPE1 IS B6V.BATTEN SUPPOSES,THAT ABSORP LINES OF B-STAR ARE FORMED IN EXTENDED ATM-TRANSITIVE LAYER BETWEEN'PROPER' ATM OF B-COMP AND GASEOUS DISK AROUND IT;THEREFORE,IT IS DIFFICULT TO DETERMINE EXACTLY SPE1.PERHAPS,THERE EXIST TEMPORARY CHANGES OF THIS SPE OWING TO VARIATIONS OF PHYS CONDITIONS IN GASEOUS DISK;SOMETIMES,WITH INCREASE OF ACTIVITY OF G-COMP,THIS DISK MAY BE DESTRUCTED,AND WE CAN OBSERVE PERCEPTIBLE GROWTH OF BR AND'NORMAL'SPE OF B-STAR. ROT VEL OF PRIM IS VERY LARGE(ABOUT 300 KM/SEC),ALTHOUGH,ACC TO BATTEN, THIS ESTIMATION IS VERY UNC.OBTD BY BATTEN HIGH-DISP SPECTROGRAMS GIVE DIRECT INDICATIONS FOR MASS-TRANSFER FROM G-COMP TO B-COMP AND SOME EVIDENCES (FROM OBS IN PHS .9P-.95P)OF MASS LOSS FROM THE SYSTEM WITH VERY LARGE VELS (NEARLY 1000 KM/SEC).BATTEN(REF 403) IN 1969 AND NAFTILAN(REF 404)IN 1972 OBSD IN SPE OF *,NEAR THE TOTAL PH,EM IN BALMER-LINES OF H,CONNECTED WITH GASEOUS RING AROUND B-COMP.ACC TO SP OBS OF BATTEN ET AL.(REF 391),DURING PERIOD OF OUTBURST ACTIVITY OF *,IN AUTUMN OF 1974,STRONG EM LINES OF H,CA II, MG II,AND WEAK EM LINES OF HE I AND FE II WERE FOUND IN EACH OBSD MIN I. THIS EM WAS SEEN DURING ALL THE OBSERVABLE ECLIPSES IN SEPTEMBER AND EARLY OCTOBER,FOR 5 WEEKS RUNNING.STRONG EM IN H-ALPHA WAS VISIBLE AT THE SAME TIME EVEN IN FULL LIGHT,WITHOUT ECLIPSES.FOR ABOUT A WEEK(IN THE VERY DIFFERENT PHS)THIS H-ALPHA EM WAS ACCOMPANIED BY DEEP AND SHARP ABSORP COMP WITH DISPLACEMENT TO VIOLET CORRESPONDING TO AVG VEL OF EJECTION OF MATTER FROM THE SYSTEM MORE THAN 400 KM/SEC.THIS IS A DIRECT EVIDENCE OF LARGE MASS LOSS IN SYSTEM DURING THE OUTBURSTS.SPE OF PRIM AT THAT TIME WAS B9-A0 INSTEAD OF NORMAL B7.PM OBS OF PLAVEC,POLIDAN(REF 405)AND OF OLSON(REF 406; 390)SHOW GREAT DISTORTIONS OF LC IN MIN I,DECREASE IN DURATION OF TOTALITY AND LOTS OF OTHER PM ANOMALIES DURING PERIOD OF OUTBURST ACTIVITY. P OF * UNDERGOES CONSIDERABLE VARIATIONS:'SECULAR'INCREASE(OBSD ALREADY DURING OVER 150 YRS)AND IRREGULAR ABRUPT PERIOD CHANGES.VALUE OF P GIVEN IN TABLE II IS VALID ONLY FOR OBS OF LAST 15 YRS.A SERIES OF PAPERS OF DIFFERENT AUTHORS IS DEVOTED TO STUDY OF VARIATIONS OF P OF U CEP;ONE CAN NOTE HERE THOSE OF SVECHNIKOV(REF 407),OF LUKATSKAYA,LITOVCHENKO(REF 408),OF SCHNELLER(REF 409),OF SVECHNIKOV ET AL.(REF 410),OF BATTEN(REF 374),OF HALL (REF 411)AND OF KREINER,ZIOLKOWSKI(REF 412).VALUE OF MASS-LOSS(OR TRANSFER), RESPONSIBLE FOR OBSD CHANGES OF P,IS,ACC TO ESTIMATIONS OF DIFFERENT AUTHORS, ON THE AVG,(2-5)E-6 SOLAR MASS PER YR. * IS BRIGHTER COMP OF VIS DOUBLE SYSTEM ADS 830;VIS CMPN IS 11.2 MAG AT 13.8''. * * * * * N81 Z VUL. PM EL: AVG FROM HIGHLY SIM PM EL OF MINTI,DINESCU(REF 413)AND OF LAVROV(REF 120) FROM PE OBS OF BROGLIA(REF 414) IN UBV;BOTH CALCS OF PM EL ARE FULFILLED ONLY FOR LC IN B(WL EFF 4450A);B_/A_IS GIVEN ACC TO MINTI, DINESCU;X=.23+.80 BY MINTI,DINESCU AND .16+.72 BY LAVROV.FORMERLY,SIM PM EL WERE OBTD BY PLAUT(REF 16)FROM PG OBS OF BAKER(REF 415)AND BY BAKER HIMSELF (IBIDEM).POPPER(REF 416)FROM PE OBS IN COLOURS CLOSE TO B AND V HAS OBTD EL SOMEWHAT DIFFERENT FROM THOSE GIVEN IN TABLE II:R1=R2=.31;I=88 DEG; L1=.77 IN V AND .81 IN B.PM EL VERY SIM TO POPPER'S ONES ARE FOUND BY CESTER ET AL.(REF 350),BY MEANS OF LC-SYNTHESIS METHOD(USING WOOD'S APPROACH), FROM UBV-PE OBS OF BROGLIA. THERE EXIST ALSO PM EL OF * OF KOPAL,SHAPLEY(REF 11)FROM PG OBS,OF WALTER (REF 417) FROM PG OBS,OF FETLAAR(REF 418) FROM VIS OBS AND OF SHAPLEY(REF 82) FROM VIS PM OBS. PRIM ESS.16);OTHER AUTHORS HAVE OBTD,FROM THEIR SP DATA, FAR LESS VALUES OF ECC. SPE OF PRIM IS,ACC TO PEARCE,B9N_;BY HILTNER,SPE OF COMPS ARE B8.5+G_F2; GREWING,HERCZEG ESTIMATE SPE OF COMPS AS B8+G_F2;ACC TO MENDOZA(REF 516), PRIM IS B8 AND SECOND IS G3.MC NAMARA(REF 310)ESTIMATES SPE1 AS B6V.FROM PM SOLUTIONS OF CESTER ET AL.(REF 350),SPE OF COMPS ARE B5V+F9III.FROM OBSD J1/J2, ADOPTING SPE1=B8,SPE2 IS ABOUT G2 IV. P IS VAR.ACC TO PEARCE(REF 512),THERE IS APS MOT WITH P1 ABOUT 30 YRS.PROBABLE PERIODIC CHANGES OF P ARE CONFIRMED IN PAPERS OF PLAVEC(REF 517) AND OF GREWING,HERCZEG(REF 514). * * * * * N93 U CR B. PM EL: AVG FROM VERY SIM PM EL OF CATALANO ET AL.(REF 422) FROM NUMEROUS NARROW-BAND PE OBS(WL EFF 5540A)OBTD IN 1962,AND PM EL OF WOOD(REF 423;424)FROM PE OBS IN YELLOW COLOUR,CLOSE TO V(WL EFF ABOUT 5500A) OBTD IN 1957.LCS BOTH OUTSIDE THE ECLIPSES AND IN MINS ARE DISTORTED BY INFLUENCE OF GASEOUS MATTER IN SYSTEM;HOWEVER,BOTH PM SOLUTIONS FOUND FROM OBS OF DIFFERENT SEASONS ARE IN VERY GOOD AGREEMENT.OBTD BY A-N AUTHORS LIGHTS OF COMPS ARE IN GOOD ACCORDANCE WITH SP DATA OF PEARCE(REF 425),WHO ESTIMATES,THAT PRIM GIVES ABOUT 87 PER CENT OF TOTAL LIGHT OF SYSTEM,AND WITH THOSE OF PETRIE(REF 18),WHO GIVES L1(SP)=.847. CESTER ET AL.(REF 350),FROM PE OBS OF WOOD IN COLOURS CLOSE TO B AND V, HAVE COMPUTED PM EL OF * BY MEANS OF LC-SYNTHESIS METHOD(UTILIZING WOOD'S APPROACH).ALTHOUGH THEIR GEOM EL IN BOTH COLOURS DIFFER SIGNIFICANTLY ONE FROM ANOTHER,AVG FROM THESE EL IS SIM TO GEOM EL GIVEN IN TABLE II,BUT LIGHTS OF COMPS(L1=.956 IN V AND .984 IN B)HIGHLY CONTRADICT TO VISIBILITY OF SPE2 IN SYSTEM AND TO L1=.85-.87 FOUND FROM SP OBS.FAIRLY SIM PM EL WERE OBTD BY BATTEN(REF 426)(FOR CASE'GR.OC.')AND BY KOPAL,SHAPLEY(REF 11)(FOR CASE 'OC.')FROM VIS PM OBS OF DUGAN(PUBLISHED IN ARTICLE OF WOOD ET AL.(REF 427)).BATTEN ALSO NOTES ESS ANOMALIES OF LC,ESP WITHOUT ECLIPSES.THERE ARE EARLIER DETERMINATIONS OF PM EL OF DUGAN,WRIGHT(REF 428)FROM PG OBS,OF LAUSE (REF 429)FROM VIS OBS,OF FETLAAR(REF 430)FROM VIS OBS,OF BAKER(REF 431)FROM PG OBS AND OF SHAPLEY(REF 82)FROM VIS PM OBS,-ALL FOR CASE OF PARTIAL ECLIPSE. PRIM ESS0 IN SYSTEM);14)GRYGAR,HORAK(REF 557)FROM OBS OF HERCZEG,CHEN AND REUNING,CRISTALDI ET AL.,FOR SPHERE-SPHERE AND SPHERE- TRIAXIAL ELLIPSOID MODELS;15)EATON(REF 558)FROM EXTRA-ATMOSPHERIC PE OBS IN WLS 4350,2980,1920 AND 1550A AND IR OBS OF HALL AND OF CHEN,REUNING(PM SOLUTIONS ARE OBTD IN ASSUMPTION,THAT L3 IS EQUAL TO .113 FROM(L1+L2)IN WL 16000A;.108 IN 8660A;.068 IN 4350A;.04 IN 2980A;.03 IN 1920A AND 0 IN 1550A); 16)GUINAN ET AL.(REF 559)FROM NUMEROUS(2425)MIDDLE-BAND PE OBS IN H-ALPHA (BAND-WIDTH 295A)AND H-BETA(BAND-WIDTH 180A)(PM SOLUTIONS ARE FOUND IN ASSUMPTION,THAT L3 IS EQUAL TO .13(L1+L2)IN H-ALPHA AND .12(L1+L2)IN H-BETA); 17)CHEN ET AL.(REF 560)FROM EXTRA-ATMOSPHERIC PE OBS IN WL 3428A(WITH DIFFERENT VALUES OF L3;THE BEST SOLUTION IS OBTD IN ASSUMPTION OF L3=.033 (L1+L2)). A-N AUTHORS OBTD VALUES OF R1 IN LIMITS FROM .191 TO .224;R2 FROM .238 TO .262 AND I FROM 79.7 DEG TO 83.3 DEG,AND THEY UTILIZED DIFFERENT VALUES OF B_/A_ AND X.FOLLOWING THE MOST OF AUTHORS,ONE CAN SUPPOSE,THAT PRIM IS ALMOST SPHERICAL:(B_/A_)1 IS .99-.995;SHAPE OF SECOND IS SIMILAR TO THAT OF RL2,I.E.(B_/A_)2 IS ABOUT .9.LIGHTS OF COMPS ARE GIVEN IN TABLE II ACC TO PM SOLUTIONS OF EATON(FOR WLS 16000,8660,4350,2980,1920 AND 1550A) AND OF GUINAN ET AL.(FOR WLS 6562 AND 4861A)(WITH ABOVE-MENTIONED VALUES OF L3 FOR THESE WLS);WALUES OF L1 AND L2 DEPEND ESS ON ASSUMED VALUES OF L3.THE MOST OF AUTHORS ASSUMED X1 .4-.6 AND X2 .7-.8 IN VIS INTERVAL OF SPECTRUM AND X ABOUT .2-.4 IN IR REGION.SOME OBSERVERS(FOR EXAMPLE,HERCZEG)NOTE SMALL VARIATIONS OF MINIMA'S DEPTH AND CHANGES OF LC WITH TIME;THIS VARIATIONS MAY BE EXPLAINED BY INFLUENCE OF GASEOUS MATTER IN SYSTEM ON LCS. DISTRIBUTION OF GASEOUS MATTER IN SYSTEM AND PHYS CHS OF GASEOUS STREAM, FLOWING FROM SUBGIANT SECOND PRIM,WERE INVESTIGATED IN ARTICLES OF FLETCHER(REF 561)FROM HIGH-DISP SP OBS(BY STUDY OF DISTRIBUTION OF CIRCUMSTELLAR HELIUM IN SYSTEM FROM VARIATIONS OF EQ.W. OF LINE HE I 4471A);OF ANDREWS ((REF 562) FROM MEASUREMENTS OF VARIATIONS OF H-ALPHA EMISSION WITH PH;OF LONGMORE,JAMESON(REF 563) FROM OBS IN FAR IR-REGION:WLS 2.2;3.6;4.8 AND 8.6 MICRONS;OF GUINAN ET AL.(REF 559) FROM NARROW-BAND OBS IN H-ALPHA AND H-BETA,ETC. THERE EXIST A NUMBER OF OTHER ESTIMATES OF PM EL OF BETA PER,FULFILLED BY DIFFERENT AUTHORS FROM DIFFERENT LCS;THE MOST OF THESE PM SOLUTIONS YIELD GEOM EL SIM TO EL GIVEN IN OUR TABLE II.ALGOL IS ONE OF THE BEST EXAMINED SD-SYSTEMS,AND ITS ORBITAL EL ARE ONES OF THE MOST RELIABLE EL FOR ECLIPSING SYSTEMS WITH PARTIAL ECLIPSES. PRIM ESS1000 KM/SEC FROM SMALL REGION,COMPARABLE WITH RADIUS OF ECLIPSING SYSTEM.APPARENTLY,RADIO FLARES ARISE AS A RESULT OF DISCONTINUOUS CHANGES IN INTERNAL STRUCTURE OF STAR EJECTING MASS,I.E.'STARQUAKES'. MASS-LOSS,ESTIMATED FROM RADIO-ASTRONOMICAL OBS(>3E-6 SOLAR MASS DURING ONE PERIOD OF'ACTIVITY'),IS IN GOOD ACCORDANCE WITH VALUES OF MASS-LOSS, OBTD FROM OBS OF IRREGULAR VARIATIONS OF PERIOD OF EB. * IS THE BRIGHTEST COMP OF VIS QUADRUPLE SYSTEM ADS 2362;CLOSEST VIS CMPN IS 12 MAG AT 58''.TRIG PARALLAX OF * IS 0.034''(P.E.=0.002''),ACC TO ASTROMETRIC DATA OF BACHMANN,HERSHEY(REF 572),AND 0.032''(P.E.=0.003''), FROM DATA OF BONNEAU(REF 573).SP PARALLAX OF SYSTEM IS 0.029''(P.E.=0.002''), ACC TO EATON(REF 558). * * * * * N100 RY PER. PM EL: WOOD(REF 289)FROM VIS PM OBS(WL EFF ABOUT 5300A). OUTSIDE ECLIPSES,ONLY FEW OBS WERE OBTD;THEREFORE RECTIFICATION OF LC IS FULFILLED WITH ESS UNCERTAINTY,AND OBTD EL ARE NOT VERY RELIABLE.PM EL OF WOOD ARE REPRESENTED ALSO IN CAT OF KOCH ET AL(REF 43).KOPAL,SHAPLEY(REF 11) FROM IDEM OBS OF WOOD HAVE FOUND VERY SIM PM EL(FOR X=.5+.7).GAPOSCHKIN(REF 581)FROM NUMEROUS(>6000)ESTIMATES OF HARVARD PG PLATES HAS OBTD PM EL,WHICH ACCORD FAIRLY WELL WITH WOOD'S EL.THERE ARE ALSO PM EL OF FETLAAR(REF 384) AND OF SHAPLEY(REF 82)FROM VIS OBS AND PM EL OF PLAUT(REF 16)FROM PG OBS OF GAPOSCHKIN.PM EL OF ZINNER(REF 582)REPRESENT ONLY HISTORIC INTEREST. PRIM<20 TIMES)FOR ITS MASS(SEE SVECHNIKOV(REF 142)). * * * * * N127 X TRI. PM EL: AVG FROM VERY SIM GEOM EL OBTD 1) BY MEZZETTI ET AL. (REF 459)BY MEANS OF LC-SYNTHESIS METHOD(USING WOOD'S APPROACH)FROM PE OBS IN BLUE AND YELLOW(IN SYSTEM CLOSE TO B AND V)OF BOZKURT ET AL.(REF 710); 2)BY BOZKURT ET AL. FROM THE SAME OBS(PM EL ARE FOUND FOR MODEL OF SIM ELLIPSOIDS,BY RUSSELL-MERRILL'S METHOD AND BY KITAMURA'S METHOD),AND 3)BY KUMSIASHVILI(REF 711)FROM THREE-COLOUR PE OBS IN SYSTEM CLOSE TO UBV(PM EL ARE OBTD BY LAVROV'S DIRECT METHOD FOR MODEL OF SPHERIC COMPS).L1 AND L2 IN TABLE II ARE GIVEN ACC TO PM DATA OF KUMSIASHVILI.(B_/A_)1 IS ABOUT .98; (B_/A_)2=.90 IN V AND .89 IN B IN PAPER OF MEZZETTI ET AL.;BOZKURT ET AL. HAVE FOUND B_/A_ ABOUT .975 IN BOTH COLOURS;X=.53+.80 IN V AND .67+.81 IN B,ACC TO MEZZETTI ET AL.;BOZKURT ET AL.ADOPTED VALUES OF X=.52+.63 IN V AND .70+.80 IN B;PM SOLUTIONS OF KUMSIASHVILI WERE FULFILLED FOR X1=X2=.5 IN ALL COLOURS. THERE EXIST SIM PM EL OF SHAW,KUSLER(REF 712)FROM VIS PM OBS(WL EFF 5300A) OF DUGAN(REF 713)AND PG OBS(WL EFF ABOUT 4200A)OF JORDAN(REF 714);PM EL OF KOPAL,SHAPLEY(REF 11)FROM UNPUBLISHED UNFILTERED(WL EFF ABOUT 4500A)PE OBS OF LENOUVEL,VIS PM OBS OF DUGAN AND PG OBS OF JORDAN;PM EL OF MODESITT,MARTIN (REF 715)FROM PG OBS OF JORDAN,AND PM EL OF DUGAN HIMSELF FROM HIS VIS PM OBS. PM EL OF KOPAL(REF 80),OF MC LAUGHLIN(REF 663),OF M.SHAPLEY(REF 716) AND OF GRAFF(REF 717)OBTD FROM VIS OBS DIFFER ESS FROM EL GIVEN IN TABLE II AND REPRESENT NOW ONLY HISTORIC INTEREST. PRIM ESS2000) ESTIMATES OF HARVARD PATROL PG PLATES.WHICH YIELD SLIGHTLY SMALLER SIZES OF BOTH COMPS,AND EARLIER PM EL OF GAPOSCHKIN(REF462)FROM VIS OBS OF GADOMSKI,WHICH DIFFER ESS FROM EL GIVEN IN TABLE II. PRIM<>.09,I.E.OF VALUE OF Q,WHICH FOLLOWS FROM ASSUMPTION,THAT SUBGIANT SECOND STRICTLY FILLS ITS RL2. FROM SP DATA OF JOY,SPE OF COMPS ARE A0+G_G5;ACC TO SP OBS OF AZIMOV (REF 401),SPE OF SYSTEM IN MAX IS B9 V,AND IN TOTAL PH OF MIN I IT IS G8 IV. FROM SP OBS OF HILL ET AL.(REF 600),SPE OF SYSTEM OUTSIDE ECLIPSES APPEARS TO BE A0 V-B8 V.FROM MULTICOLOR PE OBS OF BARNES(REF 879)SPE OF PRIM IS A0 V; ACC TO COL OBS OF CRAWFORD,OLSON(REF 861),SPE OF COMPS ARE (B9-A0)V+S_G_K. FROM OBSD VALUES OF J1/J2(ASSUMING SPE1 TO BE B9 V),SPE OF SECOND IS ESTIMATED AS G9.5 IV. P OF * IS VARIABLE(SEE PLAVEC ET AL.(REF 862),CRAWFORD,OLSON(REF 861)). S CNC IS IN REGION OF GALACTIC CLUSTER NGC 2632(PRAESEPE);IT IS NOT EXCLUDED,THAT IT MAY BE PHYS MEMB OF THIS CLUSTER. * * * * * N158 WW AND. PM EL: WYSE(REF 584)FROM VIS OBS OF LEINER(REF 863);IN TABLE II,AVG FROM EL OBTD BY WYSE IN 'U'-AND 'D'-HYPOTHESES FOR MODEL OF SPHERICAL STARS IS GIVEN;EL ARE UNC.THERE ARE SIM PM EL OF GAPOSCHKIN (REF 462)FOUND FROM IDEM OBS. COMPS<50 SOLAR MASS. SPE OF PRIM IS,ACC TO G.C.V.S.,SUPPL 3,B0.5 III.FROM OBSD VALUES OF J1/J2, SPE2 ABOUT B6 IS ESTIMATED. * * * * * N169 RY SCT. PM EL: MILANO ET AL.(REF 984)FROM PE OBS IN UBV OF CIATTI ET AL.(REF 985).PM EL ARE OBTD BY MEANS OF LC-SYNTHESIS METHOD,USING WILSON- DEVINNEY'S APPROACH;EL ARE OF LOW ACCURACY BECAUSE OF ESS DISTORTION OF LCS CAUSED BY GASEOUS MATTER IN SYSTEM,AND SINCE EB IS SURROUNDED BY COMPACT GAS-DUST NEBULOSITY.VARIATIONS OF LCS WITH TIME MAY BE CAUSED BY CHANGES OF DENSITY OF GASEOUS MATTER OR BY INTRINSIC VARIABILITY OF ONE OF COMPS.(B_/A_)1= .96;(B_/A_)2=.88;X1=X2=.14 IN V;.18 IN B AND .15 IN U.ACC TO MILANO ET AL., * IS 'OVERCONTACT SYSTEM' WITH DEGREE OF OVERCONTACT ABOUT 40 PER CENT. FROM IDEM OBS,GIURICIN,MARDIROSSIAN(REF 986) HAVE FOUND(BY LC-SYNTHESIS METHOD,UTILIZING WOOD'S APPROACH)PM EL FOR MODEL,WHERE HEAVIER COMP IS SURROUNDED BY OPTICAL THICK ELLIPSOIDAL DISK(WITH RELATIVE DIMENSIONS A_= .60-.61;B_=.52-.53;C_=.465),WHICH GIVES SPE B0E_,AND LESS MASSIVE(BUT HOTTER) COMP FILLS ITS RL(B_2 IS ABOUT .31;(B_/A_)2=.95).IF PM SOLUTION OF GIURICIN, MARDIROSSIAN CORRESPONDS BETTER TO TRUTH,RY SCT IS A PECULIAR EB,IN MANY RESPECTS SIM TO BETA LYR. FORMERLY,PM EL WERE FOUND BY GAPOSCHKIN(REF 987;988)FROM STUDY OF HARVARD PATROL PG PLATES;THESE EL(A_1=A_2=.34;B_/A_=.9;I=77 DEG;L1=.6)YIELD ONLY ROUGH NOTION ABOUT GEOM CHS OF SYSTEM. APPARENTLY,COMPS NEARY FILL THEIR RLS(FOR Q=.8,RL1=.395;RL2=.354),AND * IS HIGHLY MASSIVE EVOLVED CE-SYSTEM,WITH PRIM DISPLACED CONSIDERABLY TO THE RIGHT OF ZAMS AND HAVING LARGE EXCESS OF RAD FOR ITS MASS.HOWEVER,IT IS NOT EXCLUDED,THAT * MAY BE PECULIAR SYSTEM(SIM TO BETA LYR),WHERE MORE MASSIVE COMP IS SURROUNDED BY GEOM AND OPTICAL THICK GASEOUS DISK AND IS NOT VISIBLE IMMEDIATELY.THERE EXIST UNDOUBTEDLY ESS MASS-LOSS FROM PRIM (>1E-5 SOLAR MASS/YR). SP EL: COWLEY,HUTCHINGS(REF 989).MOST OF SP LINES APPEAR IN GAS SHELL SURROUNDING THIS SYSTEM,AND ONLY FEW LINES MAY BE ATTRIBUTED TO COMPS OF *. ESTIMATION OF MASS-RATIO OF COMPS FROM SP OBS IS COMPLICATED;ONE CAN ONLY CONCLUDE,THAT Q(SP)=M(B0)/M(07) IS CONTAINED IN LIMITS 1.0-1.26.ACC TO COWLEY, HUTCHINGS,MOST PROBABLE VALUE OF M(07)/M(B0) IS .8.IN SPE OF SYSTEM,STRONG FORBIDDEN LINES OF @FE III! AND OF @SI III! AND FAINTER @O III! NEBULAR LINES ARISING IN EXTENDED GASEOUS ENVELOPE SURROUNDING THE SYSTEM ARE VISIBLE. THERE EXIST EARLIER ESTIMATIONS OF SP EL OF * FULFILLED BY MERRILL(REF 990) AND BY POPPER(REF 981);POPPER EVALUATES TOTAL MASS OF SYSTEM TO BE>100 SOLAR MASS. KING,JAMESON(REF 991) FROM ANALYSIS OF OPTICAL-AND RADIO-SPE OF SYSTEM FIND, THAT * IS SURROUNDED BY COMPACT GAS NEBULOSITY WITH MASS ABOUT 5E-3 SOLAR MASS; FROM RADIO OBS OF HUGHES,WOODSWORTH(REF 992),* IS RADIO-SOURCE SIM TO THAT OF BETA LYR;RADIO-EMISSION COME FROM SMALL(<50 A.U.) REGION OF IONIZ GAS AROUND EB. ACC TO GEISEL(REF 993),* HAS LARGE IR-EXCESS,WHICH IS INTERPRETED AS RADIATION OF DUST IN NEBULOSITY(ENVELOPE) SURROUNDING EB. ESTIMATES OF SPE OF SYSTEM EFFECTUATED IN THE BEGINNING OF XX CENTURY WERE NEAR O5E_.FROM SP OBS OF POPPER,SPE OF SYSTEM IS B0E_.ACC TO COWLEY, HUTCHINGS,* INCLUDES B0-B0.5 AND ESS EARLIER COMPS,EACH HOLDING SUPERGIANT CHS.KING,JAMESON ASSUME,THAT HEAVIER COMP IS B0 VE_-STAR FILLING ITS RL AND TRANSFERING MASS TO HOTTER CMPN WITH SPE NOT LATER THAN O8 V(AND POSSIBLY AS EARLY AS O5.5).MILANO ET AL.(REF 984)EVALUATE SPE2 AS O6-O7. P OF SYSTEM UNDERGOES ESS VARIATIONS,PROBABLY,TIED TO MASS-LOSS(OR MASS TRANSFER)FROM B0E_-COMP.ACC TO MILANO ET AL.,SPEED OF MASS-LOSS ACHIEVES (6-8)E-5 SOLAR MASS PER YR. * * * * * N170 UW C MA. PM EL: LEUNG,SCHNEIDER(REF 938) FROM PE OBS IN B AND V OF OGATA,HUKUSAKU(REF 939)AND EXTRAFOCAL PG OBS OF SEYFERT(REF 940).EL ARE NOT VERY RELIABLE,SINCE LCS ARE ESS ASYM AND ARE DISTORTED BY STRONG VARIABLE IN TIME GASEOUS STREAMS,REVEALED BY SP AND PM OBS;ASCENDING BRANCH OF MIN I IS LARGELY DISTORTED;IT IS POSSIBLE,THAT ONE OF COMPS OF* IS INTRINSIC VAR WITH SMALL AMPLITUDE OF LIGHT CHANGES.PM EL ARE DETERMINED BY LC-SYNTHESIS METHOD,USING WILSON-DEVINNEY'S APPROACH;IN TABLE II OF CAT,PM EL OBTD BY LEUNG,SCHNEIDER FOR Q=.75(THIS Q IS THE MOST PROBABLE VALUE OF MASS-RATIO OF COMPS)ARE GIVEN;HOWEVER,LEUNG,SCHNEIDER HAVE FOUND ALSO PM EL FOR VALUES OF Q .90;1.00;1.17 AND 1.30;(B_/A_)1 IS ABOUT .915 AND (B_/A_)2 ABOUT .90; X1=X2=.14 IN V AND .18 IN B.SURFACE BRS OF COMPS DIFFER INSIGNIFICANTLY. FAIRLY SIM GEOM EL ARE OBTD(BY CLASSICAL METHOD,FOR MODEL OF NON-SIM TRIAXIAL ELLIPSOIDS)BY PARTHASARATHY(REF 941) FROM PE OBS IN B AND V OF DOSS (REF 942);HOWEVER,L1;L2 AND J1/J2 FOUND BY PAPTHASARATHY DIFFER CONSIDERABLY FROM THOSE GIVEN IN TABLE II(J1/J2=3.35 IN V AND 2.65 IN B,POINTING OUT ESS DIFFERENCE OF T OF COMPS). PM SOLUTIONS BOTH OF LEUNG,SCHNEIDER AND OF PARTHASARATHY SHOW UNDOUBTEDLY, IN SPITE OF THEIR LOW ACCURACY,THAT SIZES OF BOTH COMPS OF * ARE CLOSE TO SIZES OF THEIR RLS(FOR .715 SOLAR MASSES) ALSO INDICATES IN FAVOUR OF THIS SUPPOSITION.BOTH COMPS ARE DISPOSED NEAR ZAMS ON H-R DIAGRAM(ALTHOUGH THERE IS SOME UNCERTAINTY CONCERNING SPE,AND CONSEQUENTLY,CONCERNING LUM OF SECOND);THEREFORE,* MAY BE REGARDED AS 'UNEVOLVED EARLY-TYPE CONTACT SYSTEM'. SP EL: POPPER(REF 981),BATTEN(REF 4,N156),FROM LOW-DISP SP OBS.MASS- RATIO OF COMPS IS FOUND FROM DOUBLE-LINED SP ORBIT(Q(SP)=.535);HOWEVER, THIS ESTIMATE IS OF NOT HIGH PRECISION.CHAMBLISS,LEUNG(REF 1043)FROM THEIR PM SOLUTIONS HAVE EVALUATED FAIRLY SIM VALUE OF MASS-RATIO:Q(PM) ABOUT .60. FROM SP OBS OF POPPER,SPE OF COMPS ARE EVALUATED AS B3.5+B3.5,WHEREAS SP ESTIMATIONS OF LIGHT-RATIO OF COMPS YIELD L2/L1 ABOUT .45,WHICH RESULTS IN CONSIDERABLY LESSER SURFACE BR OF SECOND IN COMPARISON WITH THAT OF PRIM (CORRESPONDING TO SPE2 ABOUT B6).FROM UBV-COL OBS,SPE OF PRIM APPEARS TO BE B2-B2.5.FROM OBSD VALUES OF J1/J2,ASSUMING SPE OF PRIM TO BE B3.5 V, SPE OF SECOND IS ESTIMATED AS B6 V. IT IS OF INTEREST,THAT PERIOD OF THIS ECLIPSING SYSTEM APPEARS TO BE DEFINITIVELY CONSTANT THROUGHOUT MORE THAN 50 YRS(SEE CHAMBLISS,LEUNG(REF 1043)). * * * * * N186 Y AQL. PM EL: BREINHORST(REF 1052);KOCH ET AL.(REF 43) FROM PE OBS IN WLS EFF 5800;4550 AND 3650A OF BREINHORST.GEOM ECLIPSES ARE VERY SHALLOW AND LCS ARE LARGELY COMPLICATED,EVIDENTLY,BECAUSE OF INFLUENCE OF GASEOUS STREAMS OBSD IN SYSTEM.MAX I IS ESS BRIGHTER THAN MAX II;SHAPE OF LCS DIFFERS CONSIDERABLY IN TIME.ALL THESE PHENOMENA EMBARRASS DETERMINATION OF PM EL; THAT'S WHY OBTD PM SOLUTIONS ARE VERY UNC,AND THEY DESCRIBE ONLY ROUGHLY GEOM CHS OF *. TO ALL APPEARANCE,COMPS NEARLY FILL THEIR RLS(FOR Q=.12,RL1=.579;RL2= .209),AND * IS CE-SYSTEM WITH VERY LOW VALUE OF Q.BOTH COMPS HAVE CONSIDERABLE EXCESSES OF RADII FOR THEIR MASSES,AND THEY ARE ESS DISPLACED TO RIGHT FROM ZAMS ON H-R DIAGRAM;THEREFORE,* MAY BE REGARDED AS 'EVOLVED EARLY- TYPE CONTACT SYSTEM'. SP EL: JORDAN(REF 1053),BATTEN(REF 4,N549),ONLY FOR PRIM.* WAS REGARDED FOR A LONG TIME AS PURELY ELLIPSOIDAL VARIABLE.MASS-RATIO OF COMPS FOUND IN ASSUMPTION,THAT BOTH COMPS STRICTLY FILL THEIR RLS,IS ABOUT .11; BREINHORST(REF 1052) IN HIS PAPER HAS ESTIMATED Q WITHIN THE LIMITS .11-.14. USING SP EL OF JORDAN AND PM EL GIVEN IN TABLE II OF OUR CAT,WE HAVE OBTD BY M-L METHOD Q(M-L)=.125.FINALLY,WE HAVE ADOPTED Q=.12;WITH THIS VALUE OF Q,ABS EL OF * GIVEN IN TABLE III ARE COMPUTED. ACC TO SP OBS OF JORDAN,SPE OF PRIM IS B8;IN CAT OF KOCH ET AL.(REF 43), SPE OF COMPS B8+ @F0! ARE NOTED.FROM COL OBS,SPE OF SYSTEM APPEARS TO BE B7 V-B8 III.HILL ET AL.(REF 600) FROM SP OBS IN DIFFERENT PHS OUTSIDE ECLIPSES HAVE ESTIMATED SPE OF SYSTEM B8 IV-B8 IV-V.FROM OBSD VALUES OF J1/J2,ASSUMING SPE1 TO BE B8 IV,SPE OF SECOND A1: IS(VERY ROUGHLY)EVALUATED. * * * * * N187 X CAR. PM EL: PAYNE-GAPOSCHKIN(REF 1054)FPOM MEASUREMENTS OF HARVARD PG PLATES;EL ARE VERY UNC.SIM PM EL ARE GIVEN ALSO IN PAPER OF SHAPLEY(REF 82) FROM PRELIMINARY PM SOLUTION OF VIS LC OF ROBERTS(REF 1055). OBSD SIZES OF BOTH COMPS ARE OBVIOUSLY OVERESTIMATED(AND THEY SURPASS ABOUT 15 PER CENT SIZES OF CORRESPONDING RLS,FOR Q=1.0).VALUE OF ORBITAL INCLINATION IS ALSO APPARENTLY OVERESTIMATED. PROBABLY,IN REALITY,COMPS NEARLY FILL THEIR RLS(FOR Q=1.0,RL1=RL2=.374), AND * APPEARS TO BE CE-SYSTEM.HOWEVER,FOR MORE RELIABLE CLASSIFICATION OF X CAR,NEW PM OBS ARE NECESSARY. SP EL: SAHADE(REF 1056),BATTEN(REF 4,N273);EL ARE OF LOW CONFIDENCE. MASS-RATIO OF COMPS IS EVALUATED SPECTROSCOPICALLY(Q(SP)=1.0),BUT THIS ESTIMATE IS ALSO UNC.COMPUTED MASSES OF COMPS ARE ANOMALOUS LOW FOR EARLY A-STARS;IT IS POSSIBLE,THAT THIS UNDERESTIMATION OF MASSES IS CAUSED BY ESS OVERESTIMATION OF VALUE OF I FROM PM DATA. SAHADE FROM HIS SP OBS EVALUATES SPE OF BOTH COMPS AS A0,AND HE NOTES, THAT COMPS HAVE HIGHLY SIM SP CHS.FROM OBSD VALUE OF J1/J2,SPE OF SECOND IS ESTIMATED NEAR A1. * * * * * N188 GK CEP. PM EL: GLEIM(REF 1057)FROM PE OBS IN SYSTEM CLOSE TO UBV (WLS EFF 5430;4350 AND 3600A).LCS ARE DISTORTED BY INFLUENCE OF GASEOUS STREAMS IN SYSTEM;THERE IS ASYM(OBSD IN ALL COLOURS) OF 'SHOULDERS' OF BOTH MINS AND COMPLICATIONS OF LCS WITHOUT ECLIPSES.IN MIN I,ECLIPSE OF TYPE 'P.TR.' TAKES PLACE.OBSD SIZES OF BOTH COMPS ARE SOMEWHAT LESSER THAN THOSE OF THEIR RLS(ABOUT 90 PER CENT OF CORRESPONDING RLS,FOR Q=.92). SIM PM EL WERE OBTD BY BARTOLINI ET AL.(REF 1058;1059)FROM THEIR PE OBS IN B AND V(ALSO FOR CASE OF 'P.TR.' IN MIN I).PM EL,FOUND BY MEANS OF LC- SYNTHESIS METHOD(UTILIZING HUTCHINGS-HILL'S PROCEDURE)FROM GLEIM'S B-AND V- OBS BY HUTCHINGS,HILL(REF 1060) AND CORRECTED AFTERWARDS BY BINNENDIJK (REF 1061),RESULT IN PM SOLUTION OF TYPE 'P.OC.' IN MIN I: HOTTER COMP APPEARS TO BE SMALLER AND LESS MASSIVE ONE. APPARENTLY,COMPS NEARLY FILL RLS(FOR Q=.92,RL1=.382;RL2=.367),AND * MAY BE REGARDED AS CE-SYSTEM(VERY SHORT P OF * ALSO CONFIRMS THIS ASSUMPTION). BOTH COMPS HAVE CERTAIN EXCESSES OF RADII FOR THEIR MASSES,AND THEY ARE DISPLACED PERCEPTIBLEMENT TO RIGHT FROM ZAMS ON H-R DIAGRAM;THEREFORE,IT IS POSSIBLE TO CLASSIFY * AS 'EVOLVED EARLY-TYPE CONTACT SYSTEM'. SP EL:BARTOLINI ET AL.(REF 1062;1058),BATTEN(REF 4,N652)FROM NUMEROUS LOW-DISP SPECTROGRAMS;EL ARE OF NOT HIGH ACCURACY.MASS-RATIO OF COMPS IS DETERMINED FROM DOUBLE-LINED SP ORBIT:Q(SP)=.92.FROM SP OBS,LIGHT-RATIO OF COMPS L2:L1=.8 IS ESTIMATED,IN GOOD ACCORD WITH DATA OF PM OBS.HUTCHINGS (REF 1019);HUTCHINGS,HILL(REF 1060) HAVE EVALUATED Q(SP) ABOUT .9.SIM VALUE OF Q IS FOUND ALSO FROM THEIR PM SOLUTION:Q(PM)=.89(P.E.=.04).THERE EXIST SP EVIDENCES OF PRESENCE OF GAS STREAMS IN SYSTEM. EARLIER ESTIMATES OF SPE OF COMPS WERE(SEE BARTOLINI ET AL.(REF 1062)) ABOUT A0 V+A0 V;HOWEVER,SUBSEQUENTLY,BARTOLINI ET AL.(REF 1058;1059) HAVE EVALUATED SPE OF BOTH COMPS AS A2 V.HILL ET AL.(REF 600)FROM SP OBS IN DIFFERENT PHS YIELD SPE OF SYSTEM A1.5 V-A2 VN_. P OF * UNDERGOES IRREGULAR CHANGES IN TIME. * * * * * N189 S ANT. PM EL: JOY(REF 1063) FROM VIS PM OBS(WL EFF ABOUT 5300A) OF PICKERING(REF 1123)AND OF WENDELL(REF 645),IN 'U'-HYPOTHESIS;EL ARE UNC. LIGHT-RATIO OF COMPS IS ADOPTED TO BE L2:L1=1/2,ACC TO SP DATA;VALUE OF B_/A_ IS EVIDENTLY UNDERESTIMATED(FROM THEOR CONSIDERATIONS,ONE SHOULD EXPECT B_/A_ ABOUT .89).OBSD SIZES OF COMPS APPEAR TO BE SOMEWHAT LESSER (ABOUT 90 PER CENT) THAN SIZES OF THEIR RLS;HOWEVER,THIS DIFFERENCE IS CAUSED,APPARENTLY,SOLELY BY UNDERESTIMATION OF VALUE B_/A_ IN JOY'S PAPER: FOR B_/A_=.88,MEAN RADII OF COMPS COINCIDE,PRACTICALLY,WITH THOSE OF CORRESPONDING RLS(FOR Q NEAR .55). PM SOLUTION OF HOGG,BOWE(REF 1064)OBTD FROM THEIR PE OBS IN WL EFF ABOUT 4000A(B_1=.419;(B_/A_)1=.65;B_2=.172;(B_/A_)2=.6;I=70.1 DEG;L1=.77) SEEMS TO US LESS PROBABLE THAN PM SOLUTION OF JOY,SINCE 1)SIZE OF SECOND APPEARS TO BE FAR LESSER THAN THAT OF RL2;2)OBTD VALUES OF B_/A_ ARE LARGELY UNDERESTIMATED,AND THEY ARE IN ABSOLUTE DISACCORD WITH THEOR VALUES OF B_/A_; 3)LIGHTS OF COMPS DO NOT CORRESPOND TO VALUE L2/L1=.5 OBTD FROM SP DATA, SECOND BEING ESS HOTTER THAN PRIM(J2/J1=1.75),IN EVIDENT CONTRADICTION WITH DATA OF SP AND COL OBS. ADOPTING,THAT BOTH COMPS STRICTLY FILL THEIR RLS(FOR Q=.55),KOPAL,SHAPLEY (REF 11) HAVE EVALUATED(FROM PE LC OF HOGG,BOWE)PM EL OF SYSTEM: B_1=.43; B_2=.32;(B_/A_)1=.94;(B_/A_)2=.955;I=59 DEG;L1=.63;X1=X2=.8.THERE EXIST ALSO ESTIMATES OF PM EL OF * FULFILLED BY MAUDER(REF 1134) FROM NOT NUMEROUS PE OBS OF POPPER. TO ALL APPEARANCE,IN REALITY,COMPS NEARLY FILL RLS(FOR Q=.55,RL1=.431; RL2=.321),AND * IS LOW-MASSIVE CE-SYSTEM;HOWEVER,FOR MORE RELIABLE CLASSIFICATION OF *,NEW MULTICOLOUR PE OBS ARE NECESSARY. SP EL: JOY(REF 1063),POPPER(REF 1065).JOY HAS OBTD RVCS OF BOTH COMPS AND HAS EVALUATED Q(SP) NEAR .55(ALTHOUGH HE NOTED CERTAIN DIFFICULTIES OF DETERMINATION OF RAD VEL FROM SP LINES OF SECOND);HOWEVER,POPPER COULD ONLY DETECT EFFECT OF SP LINES OF SECOND ON THE WINGS OF LINES OF PRIM; BUT IT WAS QUITE IMPOSSIBLE TO OBTAIN RVC OF SECOND FROM HIS SP OBS.AS APPEARS FROM THE ABOVE,ONE SHOULD REGARD VALUES OF Q AND OF K2 OBTD BY JOY AS VERY UNC.MASSES OF COMPS COMPUTED WITH JOY'S SP EL SEEM TO BE ANOMALOUS LOW FOR LATE A-STARS,PROBABLY,BECAUSE OF INEXACT VALUES OF Q AND OF AMPLITUDE OF RVC OF SECOND UTILIZED FOR CALC OF ABS EL OF *. FROM SP OBS OF JOY,SPE OF BOTH COMPS ARE A8.ACC TO POPPER,SPE OF PRIM IS SLIGHTLY EARLIER THAN F0;SPE OF SECOND SEEMS TO BE(FROM H-LINES)NOT EARLIER THAN F5.FROM COL OBS,SPE2 IS ABOUT F0.BINNENDIJK(REF 1066) YIELDS SPE OF COMPS A8+F4;IN G.C.V.S.,SUPPL 2,SPE OF COMPS A9 VN_+F4 ARE GIVEN. FROM OBSD VALUE OF J1/J2,SPE2 IS APPROXIMATELY F0. P IS PROBABLY VARIABLE. * * * * * N190 GO CYG. PM EL: OVENDEN(REF 1067)FROM PE OBS IN YELLOW(WL EFF 5250A) AND BLUE(WL EFF 4200A).LCS OUTSIDE ECLIPSES ARE ASYM;DISTORTIONS OF LCS TIED TO GASEOUS STREAMS IN SYSTEM OR TO INTRINSIC FLUCTUATIONS OF LIGHT OF COMPS ARE NOTED.AFTER RECTIFICATION,MIN II IN BLUE COLOUR PRACTICALLY DISAPPEARS,AND IN YELLOW COLOUR ITS DEPTH APPEARS TO BE VERY SHALLOW(ALTHOUGH OBSD SPE OF COMPS ARE NEARLY SIM:B9N_+A0:N_).PM SOLUTION IS OF TYPE 'P.TR.' IN MIN I;X1=X2 ARE ADOPTED 1.0 IN YELLOW AND .8 IN BLUE.OBTD PM EL ARE OF FAIRLY LOW ACCURACY;SIZES OF BOTH COMPS ARE(WITHIN THE LIMITS OF ERRORS OF DETERMINATION OF PM EL) CLOSE TO THOSE OF CORRESPONDING RLS,FOR Q=.53. EARLIER,FAIRLY SIM PM EL WERE FOUND BY PIERCE(REF 1068)FROM VIS PM OBS (WL EFF ABOUT 5300A),IN 'D'-HYPOTHESIS,WITH BEFOREHAND FIXED (ACC TO DATA OF SP OBS) VALUES L1=.94 AND .92.PM EL OBTD BY MANNINO(REF 1069)FROM PE OBS IN B AND V POINT TO ECLIPSE OF TYPE 'P.OC.' IN MIN I(IN CONTRADICTION WITH RESULTS OF A-N AUTHORS),AND THEY LEAD TO SIZE OF SECOND LARGELY SURPASSING THAT OF RL2 FOR ANY ADMISSIBLE VALUE OF Q(B_1=.382;B_2=.424;B_/A_=.935; I=63 DEG;L1=.680(V) AND .743(B);X1=X2=.8 IN BOTH COLOURS).THEREFORE,EL OF MANNINO SEEM TO US LESS PROBABLE,THAN OVENDEN'S EL GIVEN IN TABLE II OF OUR CAT.THERE ARE ALSO PM EL OF KOULIKOVSKY(REF 1070) FROM PG OBS;PM EL OF LIAU(REF 1171) FROM HIS VIS PM OBS AND PM EL OF KOPAL(REF 126) FROM VIS OBS. APPARENTLY,IN REALITY,COMPS NEARLY FILL THEIR RLS(FOR Q=.53,RL1=.434; RL2=.318),AND * IS CE-SYSTEM;HOWEVER,LOW ACCURACY OF EVALUATION OF PM AND SP EL OF * DOES NOT ALLOW TO GIVE AT PRESENT RELIABLE CLASSIFICATION OF THIS SYSTEM.NEW PE OBS AND NEW PM AND SP ANALYSES OF * ARE NECESSARY. SP EL: PEARCE(REF 1071),BATTEN(REF 4,N627).MASS-RATIO OF COMPS FOUND BY PEARCE FROM RVCS OF BOTH COMPS:Q(SP)=.85 IS OBVIOUSLY OVERESTIMATED AND LEADS TO ANOMALOUS LOW MASSES OF COMPS(MASS1 ABOUT 1.1 AND MASS2 ABOUT .95 SOLAR MASS).LOW LIGHT-RATIO OF COMPS(L2/L1=.06-.08)ESTIMATED BY PEARCE FROM HIS SP DATA MAKES US REGARD WITH CAUTION THE POSSIBILITY OF EVALUATION OF RVC OF SECOND FROM SP OBS.POPPER(REF 358)QUESTIONED VISIBILITY OF SPE OF SECOND.OVENDEN(REF 1067)FROM ANALYSIS OF SP DATA HAS CONCLUDED,THAT,IN REALITY,VALUE OF Q COULD NOT BE DETERMINED PRECISELY;IT WAS POSSIBLE INDICATE ONLY THE LIMITS OF PROBABLE LOCATION OF Q: .44.08;BY E.BERTHIER(PRIVATE COMMUNICATION,CITED IN PAPER OF TAPIA,WHELAN):Q=.11. SPE OF SYSTEM IS,FROM DATA OF COUSINS(REF 1137),F2 V;THIS ESTIMATE IS CONFIRMED BY COL OBS OF CRAWFORD,BARNES(REF 1139);POPPER(REF 255) HAS ESTIMATED FROM HIS SP OBS SPE OF * AS F5;ACC TO HERNANDEZ,SAHADE(REF 1138) AND TO PRIVATE COMMUNICATION OF R.M.HUMPHREYS(CITED IN PAPER OF TAPIA,WHELAN),SPE OF SYSTEM IS NEAR F0 V.HERNANDEZ,SAHADE(REF 1132) FROM THEIR SP OBS FIND SPE OF PRIM ABOUT F0 V;SPE OF SECOND MUST BE NEARLY SIM TO THAT OF PRIM; BUT FROM COL OBS SPE OF * IS ESTIMATED AS F3 V-F4 V.FROM OBSD VALUES OF J1/J2, ASSUMING SPE1 TO BE F0V,WE HAVE ESTIMATED SPE OF SECOND ABOUT F2. SP PARALLAX OF * IS,ACC TO TAPIA,WHELAN, .029''(P.E.=.004'');ITS TRIG PARALLAX GIVEN IN CAT OF JENKINS(REF 831) IS EQUAL TO .023''(P.E.=.009''). * * * * * N204 SW LAC. PM EL: BOOKMYER(REF 1140) FROM NUMEROUS PE OBS IN YELLOW (WL EFF 5300A) AND BLUE(WL EFF 4420A) COLOURS.LCS ARE ASYM BOTH IN MINS AND OUTSIDE ECLIPSES;SHAPE OF LCS VARIES SIGNIFICANTLY FROM ONE SEASON OF OBS TO ANOTHER;THERE EXIST ALSO MORE RAPID CHANGES OF LIGHT OF *,WHICH OCCUR FROM NIGHT TO NIGHT.VARIABILITY OF LIGHT IS PRONOUNCED MORE DISTINCTLY WITHOUT ECLIPSES,AND IT IS TIED APPARENTLY TO PRESENCE OF ABSORBING GAS MATTER OF VARIABLE DENSITY WITHIN THE SYSTEM,BETWEEN COMPS.ASYM AND VARIABILITY OF LCS,PRESENCE OF GASEOUS MATTER IN SYSTEM AND PARTIAL CHARACTER OF ECLIPSES LARGELY COMPLICATE DETERMINATION OF PM EL OF *. FAIRLY SIM TO GIVEN IN TABLE II OF CAT GEOM EL ARE FOUND ALSO FROM FOLLOWING PM SOLUTIONS: 1)OF DUMITRESCU,DINESCU(REF 1141) FROM PE OBS IN V OBTD BY B.PACZYNCKI AND PUBLISHED IN ARTICLE OF RUCINSKI(REF 1142);2)OF BROGLIA (REF 1143) FROM PE OBS IN WLS EFF 5820;4450 AND 3670A(PM SOLUTIONS WERE OBTD,ASSUMING,PRESENCE OF ADDITIONAL LIGHT L3 IN SYSTEM);3) OF BROWNLEE(REF 1144) FROM PE OBS IN B AND V(FOR CASE OF 'P.TR.' IN MIN I),AND 4)OF SCHILT (REF 1145) FROM HIS PG OBS;HOWEVER,LIGHTS AND SURFACE BRS OF COMPS OBTD BY THESE AUTHORS DIFFER SIGNIFICANTLY.MAUDER(REF 1134) CONFIRMS BOOKMYER'S PM SOLUTION. THERE ARE DETERMINATIONS OF PM EL OF * FULFILLED BY NIARCHOS(REF 1098) BY MEANS OF NEW KOPAL'S METHOD(OF FREQUENCY DOMAIN-ANALYSIS) FROM PE OBS IN YELLOW AND BLUE COLOURS OF BOOKMYER,WHICH RESULT IN SIZE OF LESS MASSIVE COMP ESS LESSER THAN SIZE OF ITS RL(R2 ABOUT .21-.23).A NUMBER OF LIMITING PM SOLUTIONS WAS FOUND ALSO BY SERKOWSKI(REF 1146) FROM HIS VIS PM OBS(WL EFF NEAR 5300A). KOPAL,SHAPLEY(REF 11)(FROM PE OBS IN B AND V OF BROWNLEE(REF 1144) AND PG OBS OF DIFFERENT AUTHORS),AND HINDERER(REF 1147)(FROM HIS UNFILTERED PE OBS) HAVE EVALUATED PM EL OF * IN ASSUMPTION,THAT BOTH COMPS STRICTLY FILL THEIR RLS(FOR Q=.85);THESE ESTIMATES LEAD TO DIMENSIONS OF SECOND COMP ESS DIFFERENT FROM THOSE OBTD BY ALL A-N AUTHORS. LUCY(REF 1148;1173) AND RUCINSKI(REF 1149;1136) MADE AN ATTEMPT TO DETERMINE GEOM CHS OF * IN SUPPOSITION,THAT COMPS ARE IN DEEP OVERCONTACT,WITH COMMON CONVECTIVE ENVELOPE;HOWEVER,THEIR RESULTS ARE AT VARIANCE WITH DATA OF SP AND PM OBS,WHICH REVEAL PRESENCE OF GASEOUS MATTER(OF VARIABLE DENSITY) BETWEEN THE COMPS OF SYSTEM AND SUDDEN IRREGULAR CHANGES OF P,TIED TO NON-STATIONARY MASS-LOSS BY MORE MASSIVE COMP.DISCOVERED BY MIKOLAJEWSKA,MIKOLAJEWSKI(REF 1150) RAPID LIGHT VARIATIONS IN MINS ARE ALSO IN DISACCORD WITH SUPPOSITION OF COMMON OPTICAL THICK ENVELOPE SURROUNDING COMPS OF *.LATER,LUCY(REF 1151; 1152) HAS RENOUNCED MODEL OF COMMON ENVELOPES FOR W U MA -SYSTEMS AND HAS PROPOSED MODEL OF 'THERMAL RELAXATION OSCILLATIONS' FOR CLOSE BINARIES OF THIS TYPE;ACC TO THIS MODEL,W U MA-SYSTEMS ARE NEAR MARGINAL CONTACT STATE, SOMETIMES ENTERING INTO SUPERFICIAL CONTACT,SOMETIMES TURNING OUT 'SEMI- DETACHED' SYSTEMS,WITH SECOND DISTINCTLY LESSER THAN ITS RL2('BROKEN-CONTACT' PH OF OSCILLATIONS). ACC TO PM SOLUTION OF BOOKMYER,GIVEN IN TABLE II OF OUR CAT,AND TO PM SOLUTIONS OF A NUMBER OF OTHER AUTHORS(NIARCHOS;DUMITRESCU AND DINESCU; BROGLIA;BROWNLEE;SCHILT),SIZE OF LESS MASSIVE SECOND APPEARS TO BE CONSIDERABLY LESSER,THAN SIZE OF RL2;MORE MASSIVE PRIM NEARLY FILLS ITS RL1(FOR Q=.88, RL1=.386;RL2=.362).* IS CW-SYSTEM WITH VERY LARGE FOR SUCH SYSTEMS VALUE OF Q(BEING APPARENTLY IN BROKEN-CONTACT PH). SP EL: STRUVE(REF 1153;1154),FROM DOUBLE-LINED SP ORBIT;LATER,SP EL OF * WERE RECOMPUTED(USING STRUVE'S SP OBS) BY BOOKMYER(REF 1140).MASS-RATIO OF COMPS FOUND BY STRUVE IS Q(SP)=.85,BOOKMYER HAS OBTD Q(SP)=.88;WITH THIS LATTER VALUE OF Q,ABS EL OF * GIVEN IN TABLE III OF OUR CAT WERE CALC.STRUVE NOTES,THAT RELATIVE INTENSITIES OF SPE OF COMPS VARY WITH PH DURING THE ORBITAL PERIOD. ACC TO SP OBS OF WYSE(REF 584),SPE OF COMPS ARE SIM:G3P_+G3P_;STRUVE CONFIRMS THIS CLASSIFICATION.FROM SP DATA OF ROMAN(REF 191),SPE OF SYSTEM IS K0 V.HILL ET AL.(REF 600) FROM THEIR SP OBS EVALUATE SPE OF * AS G3:N_E_ IN PH .774P AND AS G2N_ IN PH .841P.FROM OBSD VALUES OF J1/J2,ADOPTING SPE1 TO BE G3,SPE OF SECOND IS ESTIMATED AS G0-G1. P OF * UNDERGOES CONSIDERABLE VARIATIONS:THERE EXIST 'SECULAR' CONTINUOUS INCREASE AND SUDDEN IRREGULAR CHANGES OF P(SEE BROGLIA(REF 1143);BOOKMYER (REF 1140);PURGATHOFER,PROCHAZKA(REF 1072);MIKOLAJEWSKA,MIKOLAJEWSKI(REF 1150)). PANCHATSARAM,ABHYANKAR(REF 1609) EXPLICATE CHANGES OF P BY MOTION OF EB IN QUADRUPLE SYSTEM. * * * * * N205 U PEG. PM EL: RIGTERINK(REF 1155) FROM NUMEROUS PE OBS IN V AND B. LCS ARE ASYM OUTSIDE ECLIPSES,LIGHT OF SYSTEM IN MAX I IS PERCEPTIBLY BRIGHTER THAN IN MAX II.COMPARISON WITH_PE LCS OF OTHER OBSERVERS: LA FARA (REF 1156);HURUHATA ET AL.(REF 1125);HINDERER(REF 1147);BINNENDIJK(REF 1157) AND SAITO(REF 1158) REVEALS CHANGES OF SHAPE OF LCS FROM ONE SEASON OF OBS TO ANOTHER;ESP,CONSIDERABLE CHANGES OF LCS OCCURED AFTER 1952,WHEN TOOK PLACE LARGE SUDDEN VARIATIONS OF P.ASYM OF LCS AND PARTIAL CHARACTER OF ECLIPSES ESS COMPLICATE DETERMINATION OF RELIABLE PM EL OF *.OBSD SIZE OF PRIM IS PRACTICALLY EQUAL TO THAT OF CORRESPONDING RL(FOR Q=.80),OBSD SIZE OF SECOND IS CONSIDERABLY(ALMOST 17 PER CENT) LESSER,THAN THAT OF ITS RL; EVIDENTLY,THIS DIFFERENCE R2 FROM RL2 IS REAL. A NUMBER OF PM SOLUTIONS IS OBTD BY BINNENDIJK(REF 1157) FROM HIS PE OBS IN YELLOW(WL EFF 5300A) AND BLUE(WL EFF 4420A) COLOURS;PM SOLUTION ESTIMATED BY BINNENDIJK AS THE BEST(FOR R2/R1=.70) APPEARS TO BE SIM TO THAT GIVEN IN TABLE II OF OUR CAT,AND IT LEADS TO VALUE OF R2 ESS LESSER THAN THAT OF RL2(R2=.30).PM SOLUTIONS EFFECTUATED BY NIARCHOS(REF 1098) FROM PE OBS OF RIGTERINK AND OF BINNENDIJK,BY MEANS OF NEW KOPAL'S METHOD(OF FREQUENCY DOMAIN-ANALYSIS),RESULT ALSO IN VALUE OF R2 CONSIDERABLY LESSER THAN THAT OF RL2(R2 ABOUT .21-.22).MAUDER(REF 1134) FROM BINNENDIJK'S PE OBS,ASSUMING ROCHE MODEL FOR COMPS,HAS OBTD PM EL,WHICH RESULTED IN VALUE OF R2 SOMEWHAT GREATER THAN THAT OF RIGTERINK(BUT STILL ESS LESSER THAN THAT OF RL2): R1=.39; R2=.33;I=73 DEG;L1=.56. KOPAL,SHAPLEY(REF 11)(FROM TWO-COLOUR PE OBS OF LA FARA(REF 1156) AND THREE-COLOUR PE OBS OF HURUHATA ET AL.(REF 1125)) AND HINDERER(REF 1147) (FROM HIS PE OBS IN WLS EFF 5050 AND 4200A) HAVE EVALUATED PM EL OF * IN ASSUMPTION,THAT BOTH COMPS STRICTLY FILL THEIR RLS;THESE ESTIMATES LEAD TO SIZE OF SECOND ESS DIFFERENT FROM THAT OBTD BY A-N AUTHORS. LUCY(REF 1173) AND RUCINSKI(REF 1136) ATTEMPTED TO EVALUATE GEOM CHS OF * FOR MODEL OF COMPS WITH COMMON CONVECTIVE ENVELOPE(DUMBELL-MODEL);HOWEVER, THEIR RESULTS ARE AT VARIANCE WITH DATA OF PM OBS(SEE BELOW) CONCERNING PRESENCE OF GASEOUS MATTER BETWEEN THE COMPS AND OCCURENCES OF 'FLARING' IN *. THERE EXIST ALSO EVALUATIONS OF PM EL OBTD BY LA FARA(REF 1156) FROM HIS PE OBS IN WLS EFF 5350 AND 4500A;BY GAPOSCHKIN(REF 462) FROM PG OBS OF SCHILT(REF 1159),AND BY SHAPLEY(REF 82) FROM VIS PM OBS(WL EFF ABOUT 5300A) OF WENDELL(REF 645).PM SOLUTION OF ROBERTS(REF 1160) FROM WENDELL'S VIS PM OBS IS NOW ONLY OF HISTORICAL INTEREST. IN DECEMBRE OF 1951 AND IN WINTER OF 1952-1953,HURUHATA ET AL.(REF 1125) OBSD REPEATEDLY 'FLARES' NEAR MAXIMA OF LIGHT OF *,WITH DURATION TO 0.5 HOUR AND WITH AMPLITUDE ATTAINING ABOUT 0.3 MAG IN UV(WL EFF 3830A);IN BLUE COLOUR(WL EFF 4620A),THESE 'FLARES' WERE HARDLY PERCEPTIBLE,AND IN YELLOW (WL EFF 5550A),THEY WERE NOT DETECTED AT ALL.SIM PHENOMENA WERE REVEALED ALSO FOR SOME OTHER CW-SYSTEMS: FOR I_ BOO(SEE EGGEN(REF 1161)) AND FOR W U MA(SEE KUHI(REF 1162)).ALL REGISTERED 'FLARES' WERE OBSD NEAR EPOCHS OF SUDDEN RAPID CHANGES OF P OF THESE CW -SYSTEMS;SO LONG AS THEY WERE DISCOVERED ALWAYS NEAR MAXIMA OF LIGHT,PHYS EVENTS RESPONSIBLE FOR 'FLARES' HAVE TO OCCUR IN REGIONS BETWEEN COMPS OF THESE W U MA-TYPE SYSTEMS(WHICH IS AT VARIANCE WITH SUPPOSITION,THAT ABOVE-MENTIONED CW-SYSTEMS ARE IN DEEP OVERCONTACT,WITH COMMON OPTICAL THICK ENVELOPES AROUND THEIR COMPS). AS IT FOLLOWS FROM PM SOLUTIONS OF RIGTERINK AND OF A NUMBER OF OTHER AUTHORS,MORE MASSIVE PRIM NEARLY FILLS RL1;OBSD SIZE OF SECOND IS ESS LESS THAN THAT OF ITS RL2(FOR Q=.80,RL1=.395;RL2=.354).* IS CW-SYSTEM WITH LARGE FOR W U MA-TYPE EB VALUE OF Q(APPARENTLY,IN 'BROKEN CONTACT' PH). SP EL: STRUVE ET AL.(REF 67);BATTEN(REF 4,N734).MASS-RATIO OF COMPS IS EVALUATED SPECTROSCOPICALLY,FROM DOUBLE-LINED SP ORBIT: Q(SP)=.80;THIS ESTIMATE IS UNC,SINCE AMPLITUDE OF RVC OF SECOND IS OBTD ONLY FROM 4 SPECTROGRAMS.WITH VALUE OF Q=.80,ABS EL OF * GIVEN IN TABLE III OF CAT ARE COMPUTED. SPE OF * IS F3,ACC TO ADAMS ET AL.(REF 1163);FROM SP DATA OF ADAMS ET AL. (REF 773),SPE OF SYSTEM IS G3.FROM SP OBS OF STRUVE ET AL.,SPE OF COMPS ARE F3+F3;THESE SPE ARE INDICATED ALSO IN G.C.V.S.,SUPPL 3.HILL ET AL.(REF 600) FROM THEIR SP OBS OUTSIDE ECLIPSES ESTIMATE SPE OF * AS G:N_.FROM OBSD VALUES OF J1/J2,ADOPTING SPE1 TO BE F3,SPE OF SECOND IS EVALUATED AS F1. P UNDERGOES CONSIDERABLE VARIATIONS:THERE IS SMALL CONTINUOUS DIMINUTION AND SUDDEN IRREGULAR CHANGES OF PERIOD(SEE BINNENDIJK(REF 1164;1157); PURGATHOFER,PROCHAZKA(REF 1072);RIGTERINK(REF 1155)).ESS SUDDEN CHANGES OF P TOOK PLACE ABOUT 1952,NEAR EPOCH OF 'FLARING' OF LIGHT OF *. * * * * * N206 XY LEO.PM EL(CASE 1):KOCH,SHANUS(REF 1165) FROM PE OBS IN YELLOW(WL EFF 5400A) AND BLUE(WL EFF 4300A) COLOURS OF KOCH(REF 1166) IN 1955-1956,AND PE OBS IN YELLOW COLOUR OF AUTHORS IN 1978.PM EL ARE EVALUATED BY LC- SYNTHESIS METHOD(USING WILSON-DEVINNEY'S APPROACH) FOR OBS OF DIFFERENT SEASONS SEPARATELY.WHEREAS LCS OF 1955-1956 SEASON HAVE NO PERCEPTIBLE ASYMMETRY,LC OF 1978 IS ESS ASYM.IN TABLE II OF OUR CAT,AVG VALUES OF GEOM EL OBTD FROM VERY SIM PM SOLUTIONS OF KOCH,SHANUS FOR EPOCHS OF 1955-1956 AND OF 1978 ARE GIVEN;L1,L2 AND J1/J2 ARE ADOPTED FROM PM SOLUTION OF LCS OF 1955-1956;(B_/A_)1 IS ABOUT .93 FOR EPOCH OF 1955-1956; AND .95 FOR 1978;(B_/A_)2 IS ABOUT .91 AND .93 FOR THESE SEASONS OF OBS,RESPECTIVELY;X IS ADOPTED EQUAL TO .80 IN B AND V FOR BOTH COMPS.SMALLER AND LESS MASSIVE COMP IS SLIGHTLY BRIGHTER THAN MORE MASSIVE PRIM.PM SOLUTIONS ARE OBTD,ASSUMING PRESENCE IN * OF ADDITIONAL LIGHT: L3 ACHIEVES 7(P.E.=2) PER CENT OF TOTAL LIGHT OF SYSTEM FOR 1955-1956 AND 6(P.E.=4) PER CENT FOR 1978 IN YELLOW;IN BLUE COLOUR,L3 IS 2(P.E.=1) PER CENT OF TOTAL LIGHT OF *.OBSD SIZES OF BOTH COMPS ARE,PRACTICALLY,EQUAL TO THOSE OF THEIR RLS(FOR Q=.79);KOCH,SHANUS HAVE ESTIMATED * TO BE SLIGHTLY(ABOUT 6 PER CENT) 'OVERCONTACT' FROM OBS OF 1955-1956,AND SLIGHTLY 'UNDERCONTACT' FROM OBS OF 1978;HOWEVER,THESE DIFFERENCES ARE EVIDENTLY WITHIN THE LIMITS OF ERRORS OF PM SOLUTIONS.UNDOUBTEDLY,* IS NEAR MARGINAL CONTACT. PM EL(CASE 2): ISTOMIN,STARITSYN(REF 1610) FROM YELLOW PE OBS OF KOCH, SHANUS;EL ARE OBTD BY CLASSICAL METHOD,AND THEY ARE SIM TO THOSE OF KOCH, SHANUS,WITH EXCEPTION OF LESSER VALUE OF R2(WHICH IS ABOUT 90 PER CENT FROM RL2),AND OF GREATER VALUE(ABOUT .85) OF J1/J2. EARLIER PM SOLUTIONS OF KOCH(REF 1166),FULFILLED BY CLASSICAL METHODS FROM HIS PE OBS OF 1955-1956,RESULTED IN TOO LOW VALUE OF SIZE OF SECOND (R2<.20) AND IN IMPROBABLY HIGH LIGHT RATIO OF COMPS(L1:L2>9),WHICH WAS AT VARIANCE WITH SP OBS OF TWO COMPARABLE SPECTRA.LIMITING PM SOLUTION OF KOCH (FOR I=90 DEG) WAS IN BETTER ACCORD WITH DATA OF SP OBS,BUT IT WAS OBTD WITH HARDLY PROBABLE ASSUMPTION OF PRESENCE IN SYSTEM OF ADDITIONAL LIGHT-SOURCE, WHICH REACHED >60 PER CENT OF TOTAL LIGHT OF *. THERE ARE ALSO ESTIMATIONS OF PM EL,OBTD BY HILDITCH(REF 1167) FROM HIS PE OBS IN DDO-SYSTEM BY MEANS OF RUCINSKI'S LC-SYNTHESIS METHOD(SUITABLE FOR OVERCONTACT CONFIGURATIONS).VALUES OF Q(PM)(.47-.57) FOUND BY HILDITCH FROM HIS PM SOLUTIONS DIFFER CONSIDERABLY FROM Q(SP)=.79;* IS ESTIMATED AS SLIGHTLY OVERCONTACT(FACTOR F_ APPEARS TO BE WITHIN THE LIMITS .8-.9); THEOR LCS ARE IN UNSATISFACTORY ACCORD WITH DATA OF OBS.EARLIER,LUCY(REF 1173) AND RUCINSKI(REF 1136) HAVE EVALUATED GEOM CHS OF * FROM KOCH'S PE OBS,AND THEY HAVE FOUND XY LEO TO BE IN MARGINAL CONTACT(FILL-OUT PARAMETER F_=1). TO ALL APPEARANCE,BOTH COMPS OF * NEARLY FILL RLS(FOR Q=.79,RL1=.396; RL2=.353),AND * APPEARS TO BE LOW-MASSIVE CW-SYSTEM WITH HIGH VALUE OF Q, WHICH IS NEAR MARGINAL CONTACT (OR SLIGHTLY 'UNDERCONTACT'). SP EL: STRUVE,ZEBERGS(REF 1168);BATTEN(REF 4,N308).MASS-RATIO OF COMPS IS EVALUATED FROM DOUBLE-LINED SP ORBIT: Q(SP)=.79;WITH THIS VALUE OF Q, ABS EL GIVEN IN TABLE III OF CAT ARE COMPUTED.KOCH,SHANUS(REF 1165) HAVE EVALUATED FROM THEIR PM SOLUTIONS Q(PM)=.82-.84.VALUES OF Q(PM) FOUND BY HILDITCH(REF 1167) FROM HIS PM SOLUTIONS(Q(PM) WITHIN .47-.57) DIFFER ESS FROM Q(SP).ACC TO SP DATA OF STRUVE,ZEBERGS,THERE ARE EM LINES OF CA II IN SPE OF *;PRESENCE OF EM LINES,AS WELL AS CHANGES OF SHAPE OF LCS WITH TIME AND SUDDEN IRREGULAR VARIATIONS OF P,MAY BE AN ARGUMENT IN FAVOUR OF EXISTENCE OF GAS STREAMS IN SYSTEM TIED TO MASS-LOSS FROM ONE OF ITS COMPS. SPE OF COMPS ARE,FROM SP OBS OF STRUVE,ZEBERGS,K0N_+K0;FROM COL OBS OF KOCH,SPE OF SYSTEM IS K2 V-K3 V;ACC TO DATA OF VYSSOTSKY,BALZ(REF 1169),SPE OF * IS G5.HILL ET AL.(REF 600) FROM THEIR SP OBS OUTSIDE ECLIPSES HAVE ESTIMATED SPE OF SYSTEM AS K0N_.FROM OBSD VALUES OF J1/J2,ASSUMING SPE OF HOTTER (SECOND)COMP TO BE K0,SPE OF MORE MASSIVE COMP IS EVALUATED AS K2, ACC TO KOCH,SHANUS AND K1,ACC TO ISTOMIN,STARITSYN. P UNDERGOES SUDDEN IRREGULAR CHANGES(SEE KOCH(REF 1166);GEHLICH ET AL. (REF 1170)). * * * * * N207 YY ERI. PM EL: MAUDER(REF 1174) FROM PE OBS IN B AND V OF A.PURGATHOFER, I.PURGATHOFER(REF 1175);LCS REVEAL PRONOUNCED ASYM.PM EL ARE DETERMINED BY ORIGINAL AUTHOR'S METHOD,UTILIZING FOURIER EXPANSION OF LCS.CALC SIZE OF PRIM IS ALMOST EQUAL TO THAT OF CORRESPONDING RL,SECOND IS ABOUT 10 PER CENT LESSER THAN ITS RL2(FOR Q=.65);HOWEVER,THIS DIFFERENCE IS APPARENTLY WITHIN THE LIMITS OF ERRORS OF DETERMINATION OF GEOM EL.EARLIER,MAUDER(REF 1134) HAS FOUND FROM THE SAME OBS SOMEWHAT DIFFERENT PM EL: R1=.41;R2=.33;I=79 DEG; L1=.59.PM EL OBTD FROM IDEM OBS BY BINNENDIJK(REF 1176) BY MEANS OF CLASSICAL METHOD RESULT IN SMALLER VALUE OF R2 AND SOMEWHAT GREATER VALUE OF L1(B_1=.42; B_2=.25;B_/A_=.895;I=79.0 DEG;L1=.725 IN V AND .714 IN B).NIARCHOS(REF 1098), USING NEW KOPAL'S METHOD(OF FREQUENCY-DOMAIN ANALYSIS),HAS ALSO FOUND R2 ESS LESSER THAN SIZE OF CORRESPONDING RL(R2=.228-.234). LUCY(REF 1173) AND RUCINSKI(REF 1136) FROM PE OBS OF A. AND I.PURGATHOFER IN YELLOW HAVE EVALUATED GEOM EL OF * BY MEANS OF LC-SYNTHESIS METHODS FOR OVERCONTACT CONFIGURATIONS(DUMBELL-MODEL),FOR Q=.59,AND THEY HAVE FOUND * TO BE IN SHALLOW OVERCONTACT('FILL-OUT PARAMETER' F_ IS ABOUT .92 IN LUCY'S SOLUTION AND .8 IN RUCINSKI'S SOLUTION).EARLIER,KOPAL,SHAPLEY(REF 11) FROM TWO-COLOUR PE OBS OF CILLIE(REF 1177) AND 3-COLOUR PE OBS OF HURUHATA ET AL. (REF 1178) HAVE DETERMINED PM EL OF SYSTEM IN ASSUMPTION,THAT BOTH COMPS OF * FILL STRICTLY THEIR RLS(FOR Q=.65). THERE EXIST ALSO PM EL FOUND BY MEANS OF CLASSICAL METHODS BY HURUHATA ET AL. THEMSELVES,IN ABOVE-MENTIONED PAPER. TO ALL APPEARANCE,IN REALITY,PRIM NEARLY FILLS RL1,AND SIZE OF SECOND IS SOMEWHAT LESSER THAN THAT OF RL2(OR EQUAL TO ITS RL2)(FOR Q=.65,RL1=.415; RL2=.335).* APPEARS TO BE CLOSE TO MARGINAL CONTACT,AND AVAILABLE PM DATA ARE INSUFFICIENT IN ORDER TO DRAW DEFINITIVE CONCLUSION,WHETHER * IS SLIGHTLY 'UNDERCONTACT'(AS IT SEEMS MORE PROBABLE) OR SLIGHTLY 'OVERCONTACT' W U MA- TYPE SYSTEM. SP EL: STRUVE(REF 708);BATTEN(REF 4,N116).MASS-RATIO OF COMPS EVALUATED BY STRUVE FROM DOUBLE-LINED SP ORBIT IS Q=.65.HURUHATA ET AL.(REF 1178); KITAMURA(REF 1179) HAVE RE-EVALUATED SP EL OF * FROM STRUVE'S SP OBS WITH NEW VALUE OF P,TAKING INTO ACCOUNT EFFECT OF REFLECTION ON OBSD MASS OF SYSTEM;THEIR VALUE OF Q(SP) IS.59.HOWEVER,LATER J.SAHADE(PRIVATE COMMUNICATION, 1971,CITED IN PAPER OF MAUDER(REF 1174)) HAS CONFIRMED ORIGINAL VALUE Q(SP)= .65 OBTD BY STRUVE;WITH THIS Q,ABS EL OF * GIVEN IN TABLE III ARE CALC. THERE EXIST GASEOUS STREAMS IN SYSTEM,WHICH INFLUENCE RVCS OF COMPS(AND PRESENCE OF GASEOUS MATTER BETWEEN COMPS OF SYSTEM MAY BE AN ARGUMENT IN FAVOUR OF 'UNDERCONTACT' CONFIGURATION OF *).SPE OF COMPS ARE,ACC TO SP DATA OF STRUVE,G5+G5;FROM OBSD VALUES OF J1/J2,SECOND HAS TO BE A BIT HOTTER THAN PRIM(G4.5-G5). P OF * IS VARIABLE(SEE A.PURGATHOFER,I.PURGATHOFER(REF 1175)). * * * * * N208 AB AND. PM EL: RIGTERINK(REF 1180) FROM HIS PE OBS IN B AND V;LCS ARE ASYM,AND THEY CHANGE FROM ONE EPOCH OF OBS TO ANOTHER.PM EL ARE FOUND BY MEANS OF LC-SYNTHESIS METHOD,USING WILSON-DEVINNEY'S APPROACH;X1=X2 IS ADOPTED TO BE .70 IN V AND .80 IN B;COMPUTED SIZES OF BOTH COMPS ARE SOMEWHAT LESSER THAN THOSE OF CORRESPONDING RLS(FOR Q=.62).DETERMINATION OF PM EL OF *, FULFILLED BY RIGTERINK FROM IDEM OBS BY MEANS OF RUSSELL-MERRILL'S CLASSICAL METHOD,RESULTS IN VERY SIM GEOM EL,WITH THE EXCEPTION OF PERCEPTIBLY LESSER SIZE OF SECOND(B_2 ABOUT .27).PM EL VERY SIM TO THOSE OBTD BY RIGTERINK BY MEANS OF RUSSELL-MERRILL'S METHOD WERE FOUND BY CLASSICAL METHOD BY L.F. ISTOMIN(1975,PRIVATE COMMUNICATION) FROM PE OBS IN YELLOW(WL EFF 5500A) OF BINNENDIJK(REF 1181): B_1=.409;B_2=.278;B_/A_=.89;I=79 DEG;L1=.630;X1=X2=.6. FROM IDEM OBS,MINTI(REF 1182) HAS OBTD,BY MEANS OF LC-SYNTHESIS METHOD,PM EL SIM TO THOSE OF RIGTERINK(GIVEN IN TABLE II OF OUR CAT): PRIM NEARLY FILLS ITS RL1;SIZE OF SECOND IS SOMEWHAT LESSER THAN THAT OF RL2.PM SOLUTION OF BERTHIER(REF 1183)(SEE ALSO BINNENDIJK(REF 1061)) FOUND FROM RIGTERINK'S PE OBS BY LC-SYNTHESIS METHOD YIELDS,PRACTICALLY,THE SAME VALUE OF R2,THAT PM SOLUTION OF RIGTERINK,BUT R1 AND I OBTD BY BERTHIER ARE PERCEPTIBLY GREATER: B_1=.440;(B_/A_)1=.935;B_2=.323;(B_/A_)2=.90;I=87.3 DEG. NIARCHOS(REF 1098) INVESTIGATED * BY NEW KOPAL'S METHOD(OF FREQUENCY-DOMAIN ANALYSIS) FROM BINNENDIJK'S PE OBS IN YELLOW AND BLUE COLOURS,AND HE HAS OBTD SIZE OF SECOND ESS LESS THAN THAT OF RL2(R2=.255-.258).EARLIER,MAUDER (REF 1134) AND MINTI,GANEA(REF 1184) HAVE ALSO FOUND FROM BINNENDIJK'S PE OBS PM EL OF * YIELDING R2 ABOUT .28,I.E. ESS LESS THAN RL2. LUCY(REF 1173) AND RUCINSKI(REF 1136) HAVE EVALUATED PM EL OF * BY MEANS OF METHODS ELABORATED FOR CONTACT CONFIGURATIONS(DUMBELL-MODEL),AND THEY HAVE FOUND * TO BE NEAR MARGINAL CONTACT('FILL-OUT PARAMETER' F_=.9,ACC TO RUCINSKI, AND ABOUT .97,ACC TO LUCY).EARLIER,HINDERER(REF 1147) FROM HIS PE OBS IN WL EFF=5050A,AND KOPAL,SHAPLEY(REF 11) FROM PG OBS OF GUTHNICK,PRAGER(REF 1185), OF JORDAN(REF 1186) AND OF OOSTERHOFF(REF 1187) HAVE ESTIMATED PM EL OF *, ASSUMING,THAT BOTH COMPS STRICTLY FILL THEIR RLS(FOR Q=.62);PM SOLUTION OF HINDERER BEING OBTD IN SUPPOSITION OF PRESENCE OF ADDITIONAL LIGHT L3 TIED TO GASEOUS MATTER IN SYSTEM. THERE EXIST ALSO PM EL OF KALCHAEV,TRUTZE(REF 1188) FROM THEIR PE OBS IN YELLOW(WL EFF 5600A) AND BLUE(WL EFF 4250A) COLOURS;PM EL OF GAPOSCHKIN (REF 462) FROM PG OBS OF GUTHNICK,PRAGER(VERY UNC),AND PM EL OF WALTER(REF 417) FROM JORDAN'S PG OBS. TO ALL APPEARANCE,SIZE OF PRIM IS,PRACTICALLY,EQUAL TO THAT OF CORRESPONDING RL;OBSD DIMENSIONS OF SECOND APPEAR TO BE SLIGHTLY SMALLER THAN THOSE OF RL2 (FOR Q=.62,RL1=.419;RL2=.331).* IS EVIDENTLY NEAR MARGINAL CONTACT,POSSIBLY, IN 'BROKEN-CONTACT PHASE'(ALTHOUGH RELIABILITY OF DETERMINATION OF GEOM EL IS INSUFFICIENT TO DRAW DEFINITIVE CONCLUSION,WHETHER R2