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Magneti c chemically peculiar stars
I. Catalogu e
I.I . Romanyu k Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz 369167, Russia

Abstract . O n th e basi s o f analysi s o f origina l publication s an d ou r ow n measurement s a Cata logu e o f magneti c chemicall y peculia r (CP ) uppe r main-sequenc e star s ha s bee n established . Th sampl e include s 21 1 magneti c C P star s wit h magneti c field s rangin g fro m hundred s o f gaus s t dozen s o f kilogauss , for 4 9 o f the m th e surfac e magneti c fiel d (B ) ha s bee n measure d fro m th Zeema n splitting .
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e o e

1 . Introductio n
Magneti c field s o f star s wer e discovere d b y Babcoc k i n 1947 . Mor e tha n 5 0 year s ag o h e foun d th e Zeema n effect i n th e spectr a o f th e A p sta r 7 8 Vir . Man y thou san d magneti c measurement s o f differen t typ e star s mad e fro m youn g Herbi g Ae/B e an d T Ta u star s t o magneti c whit e dwarf s a t th e fina l stag e o f evolutio n hav e bee n mad e eve r since . Th e measurement s sho w tha t magnetis m i s a wide-sprea d phenomeno n amon g stars . A s a rule , differen t type s o f bursts , explosion s an d othe r instabili tie s ar e connecte d wit h magneti c fields . Unfortunately , magneti c fiel d measurement s ar e a ver y involve d problem . Fo r example , eve n th e moder n techniqu e ofte n fails t o detec t magneti c field s (eve n ver y strong ) o f comple x topology . Fro m th e lat e 40 s t o th e middl e 80 s mainl y photo graphi c Zeema n spectr a wer e analyzed , thei r lo w S/ N rati o (20-30 ) di d no t permi t fin e analysi s o f lin e pro files , especiall y studyin g distributio n o f circula r an d linea r polarizatio n ove r th e lin e profile . Tha t i s why , th e detectio n o f comple x structur e magneti c field s (of th e typ e o f sola r spots ) wa s im possible . Fortunately , chemicall y peculia r star s hav e or dered , mainl y dipolar , ver y reliabl y measurabl e mag neti c fields . Th e simpl e configuratio n o f thei r mag neti c field s lead s t o Zeema n shift s (ver y rarel y t o mag neti c splitting ) o f line s a s a whole , whil e i n th e cas e o f comple x non-dipola r magneti c fiel d on e need s t o stud y th e fin e structur e o f lin e profiles . Result s o f Babcock' s measurement s ar e presente d i n hi s famou s catalogu e (Babcock , 1958) . Sinc e th e magneti c fiel d valu e i n C P star s i s abou t a few kilogaus s (whic h correspon d t o a Zeema n split tin g o f abou t 0.1-0. 2 A ) onl y spectr a o f narrow-lin e star s ca n b e measure d for detectio n o f magneti c fields .

Th e accurac y o f measurement s i s highl y dependen t o n th e lin e widt h an d therefor e magneti c fiel d mea surement s o f fast-rotatin g C P star s (wit h vsin i > 4 0 km/s ) wer e impossible . Photoelectri c Balmer-lin e magnetometer s wer e firs t use d b y Landstree t i n 1970 . H e measure d circula r polarizatio n i n th e wing s o f hydroge n lines . A Balme r magnetomete r wa s effectivel y use d i n searchin g for magnetis m o f fast-rotatin g stars , ho t helium-stron g an d helium-wea k stars , magneti c whit e dwarfs , wher e photographi c technique s woul d no t b e use d becaus e o f th e smal l numbe r o f broa d line s i n thei r spectra . Th e result s o f magneti c measurement s from 195 8 t o 1982 wer e collecte d b y Didelo n (1983) . Zeema n observation s o f C P star s provid e direc t evidenc e o f magneti c fields , independentl y o f an y models . Variou s assumption s hav e certainl y t o b e mad e whe n constructin g magneti c fiel d configuratio n model s an d fiel d mapping . Ne w digita l techniques : reticon s an d the n CC D detector s permi t stud y th e lin e profile s wit h a hig h S/ N rati o an d a hig h spectra l resolution . Thi s mad e i t possibl e t o star t studyin g magneti c fiel d com ple x structur e (for example , Robinson , 1980) . Man y ne w magneti c star s hav e bee n discovered , especiall y amon g coo l stars . Th e situatio n wit h magneti c fiel d measurement s o f C P star s ha s als o undergon e essentia l changes : th e us e o f CC D permit s studyin g no t onl y averag e parameter s o f line s (equivalen t width , radia l veloc ity , Zeema n shift) , but , usin g th e analysi s o f inten sit y an d polarizatio n profiles , als o simultaneou s map pin g o f chemica l compositio n an d magneti c fiel d o n th e surfac e o f C P star s an d lookin g for connectio n bertwee n them . Separat e attempt s o f doin g thi s wor k wer e mad e earlie r (for example , Khokhlova , 1983) , bu t i t i s a t th e presen t tim e tha t th e wor k ha s be com e extensiv e an d coordinated .

© Special Astrophysical Observatory of the Russian AS, 2000


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A secon d importan t achievemen t i n th e stud y o f C P star s i s du e t o Hipparco s results . Recentl y th e Hipparco s satellit e ha s measure d parallaxe s o f mos t o f the magneti c C P stars . Thi s permit s reliabl e distance s and, a s a result , accurat e absolut e parameter s an d reliable spatia l distributio n o f magneti c C P star s i n our Galax y t o b e found . Magneti c fiel d observation s ar e stil l extremel y rare : ten s o f thousand s o f star s agains t a few hundre d magneti c star s ar e know n t o hav e measure d radia l velocities.

2 . Catalogue
2.1 . Fractio n o f C P star s A Genera l catalogu e o f A p an d A m stars , whic h con tains almos t 670 0 stars , ha s bee n complete d b y Ren son e t al . (1991a) , a databas e for 319 5 A p star s wa s described b y Renso n e t al . (1991b) . Th e numbe r o f C P star s i s essentiall y highe r tha n the numbe r o f magneti c stars . Mor e tha n 90 % o f known C P star s hav e neve r bee n observe d wit h a Zee man analyzer ; mos t o f the m ar e fain t C P star s an d for thei r measurement s on e ha s t o reques t tim e o n th e world's larges t telescopes . I t ca n commonl y b e foun d i n th e literatur e tha t C P star s accoun t for 10-1 5 % o f mai n sequenc e star s o f th e sam e spectra l clas s (e.g . se e Khokhlova , 1983) . Th e Hipparco s tea m (Gome s e t al. , 1998 ) in formed tha t amon g star s brighte r tha n 7.5 ma g on e can fin d 257 8 norma l main-sequenc e star s an d 46 7 different chemicall y peculia r star s i n th e spectra l rang e B5-F 5 i n th e Hipparco s catalogue . Thu s w e ca n cal culate a fractio n a s 467/(257 8 + 467 ) = 15. 3 % . W e hav e enoug h sufficient evidenc e t o b e certai n tha t all chemicall y peculia r star s brighte r tha n 7. 5 mag hav e bee n properl y classifie d becaus e al l brigh t stars hav e bee n analyze d usin g spectr a obtaine d wit h a reasonabl y hig h spectra l resolution . W e ca n als o conclude tha t th e Hipparco s dat a hav e practicall y no t changed th e fractio n o f C P stars . 2.2 . Catalogu e o f magneti c C P star s The las t publishe d catalogu e o f magneti c measure ments (Didelon , 1983 ) contain s informatio n for abou t 140 magneti c chemicall y peculia r stars . Mainl y i t con sists o f Babcock' s catalogu e (1958 ) o f magneti c mea surement s an d als o photoelectri c magneti c measure ments o f Landstree t an d hi s co-authors . However , durin g th e las t 1 5 year s ne w dat a hav e been take n b y observation s wit h ne w digita l device s and man y ne w magneti c C P star s o f th e mai n se quence hav e bee n discovered . Becaus e Didelon' s catalogu e ha s becom e out dated, ou r purpos e i s t o selec t fro m origina l paper s al l

possibl e informatio n abou t magneti c measurement s o f C P stars , t o mak e a ne w lis t o f magneti c C P star s an d t o conduc t a comple x stud y o f th e star s fro m thi s list . W e hav e collecte d abou t 1000 0 magneti c mea surement s o f differen t typ e main-sequenc e star s (pub lishe d an d ou r own) . Takin g int o accoun t unpublishe d result s o r one s availabl e i n th e inaccessibl e publica tions , w e estimat e tha t 2000 0 magneti c measurement s o f abou t 30 0 C P an d 20 0 norma l star s hav e bee n made . Mos t o f the m hav e bee n mad e b y H . Babcock , G . Presto n an d hi s co-authors , J.Landstree t an d hi s co-authors , G . Mathy s wit h hi s co-author s an d b y th e SA O grou p wit h th e 6 m telescop e o f Russia n Academ y o f Sciences . Observation s o f mos t star s yiel d "zero-field " re sults : practicall y all norma l star s (for example , Land street , 1982 ) an d a larg e fractio n o f chemicall y pecu lia r star s d o no t sho w magneti c field s large r tha n th e typica l accurac y o f measurement s (100-30 0 G) . Fo r ver y brigh t narrow-lin e C P star s th e accurac y i s es sentiall y better , sinc e th e standar d erro r i s abou t a few doze n gauss . Publicatio n o f al l measurement s fro m ou r cata logu e i s to o difficult becaus e o f th e larg e bod y o f collecte d data . No w w e ar e makin g th e firs t ste p only : w e presen t a ne w sampl e o f magneti c C P stars . W e hav e include d i n ou r lis t onl y suc h stars , whic h hav e bee n foun d t o b e magneti c b y th e author s o f th e origina l publications . O n th e basi s o f al l collecte d dat a w e hav e mad e a sampl e o f 21 1 magneti c chemicall y peculia r star s wit h reliabl y measure d magneti c fields . W e presen t th e sta r HD/B D number , informatio n abou t th e lon gitudina l fiel d (B ) extrema , surfac e magneti c fiel d (B ) , numbe r o f measurement s [n] an d reference s i n Tabl e 1 .
e S

3 . Conclusio n
Thu s w e hav e foun d 21 1 magneti c C P stars . Surfac e magneti c fiel d (B ) estimate s ar e availabl e for onl y 4 9 o f them . Mgneti c fiel d dat a for th e res t o f th e star s (162 ) o f ou r sampl e hav e bee n obtaine d fro m measur in g th e longitudina l component s (B ) alone . Fo r som e star s th e longitudina l magneti c fiel d (B ) magnitude s derive d fro m dat a o f differen t au thor s ar e dramaticall y different . Sinc e th e ai m o f thi s firs t pape r fro m a serie s o f paper s t o appea r i s t o mak e availabl e a lis t o f magneti c C P star s ( a detaile d anal ysi s o f magneti c field s an d othe r parameter s o f star s i s expecte d t o b e mad e late r on) , w e hav e decide d t o postpon e th e discussio n o f th e difference s an d tabu lat e herei n onl y th e extrem e B values . A sufficientl y larg e numbe r (ove r 10) o f measure ment s o f B hav e bee n mad e for 7 9 magneti c C P stars ,
S e e e e


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Reference s t o Tabl e 1 1 - Babcock , 1958 2 - Adam , 1965 3 - Babcock , 1960 4 - Babcock , 196 3 5 - Preston , Stepien , 1968(a ) 6 - Preston , Sturch , 196 7 7 - Preston , Stepien , 1968(b ) 8 - Preston , 1969 (a ) 9 - Preston , 1969(b ) 10 - Hockey , 196 9 1 1 - Presto n e t al. , 1969 1 2 - Preston , 1969(c ) 13 - Wolff, 1969(a ) 1 4 - Preston , 1969(d ) 1 5 - Cohe n e t al. , 1969 1 6 - Pyper , 1969 1 7 - Kodaira , Unno , 196 9 1 8 - Steinitz , Pyper , 196 9 1 9 - Preston , 1969(e ) 20 - Wolff, 1969(b ) 2 1 - Preston , Wolff, 1970 22 - Wolff, Wolff, 197 0 2 3 - Preston , 1970 2 4 - Conti , 1970 2 5 - Heuve l va n den , 197 1 2 6 - Preston , 197 1 2 7 - Ewans , Elste , 197 1 2 8 - Hockey , 197 1 2 9 - Steinitz , Pyper , 1971(a ) 3 0 - Schoiz , 197 1 (a ) 3 1 - Schoiz , 1971(b ) 32 - Wolff, Wolff, 197 1 3 3 - Steinitz , Pyper , 197 1 (b ) 3 4 - Preston , 1972 3 5 - Kemp , Wolstencroft , 197 3 3 6 - Borra , Dworetsky , 197 3 37 - Wolff, 197 3 3 8 - Adelman , 197 4 3 9 - Hensberge , 197 4 4 0 - Bonsack , Pilachowski , 197 4 4 1 - Jone s e t al. , 197 4 4 2 - Borra , 1974 4 3 - Oetken , Orwert , 197 3 4 4 - Severn y e t al. , 197 4 4 5 - Schoiz , 197 5 4 6 - Bonsac k e t al. , 197 4 4 7 - Huchra , 1972 4 8 - Jones , Wolff, 197 4 49 - Wolff, Morrison , 197 4

50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98

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Hensberge , D e Loore , 197 4 Pilachowsk i e t al. , 197 4 Maitzen , Albrecht , 197 5 Bonsack , 1976(a ) Bonsack , 1976 (b ) Wolff, Hagen , 197 6 Bona , Vaughan , 1976 Borra , Landstreet , 197 7 Bonsack , 1977(a ) Borra , Vaughan , 197 7 Glagolevski j e t al. , 197 7 Floquet , 197 7 Landstreet , Borra , 197 7 Wolff, Wolff, 197 6 Bonsack , 1977(b ) Borra , Vaughan , 197 8 Schoiz , 1978 Borra , Landstreet , 197 8 Freeman , 1978 Landstreet , 197 8 Glagolevski j e t al. , 197 8 Wolff, 197 8 Borra , Landstreet , 197 9 Scholz , 1979 Landstree t e t al. , 197 9 Glagolevski j e t al. , 197 9 Bonsack , 1979 Maitze n e t al. , 1980 Romanyuk , 1980 Borra , Landstreet , 1980 Wolff, Preston , 197 8 Hensler , 197 8 Brow n e t al. , 198 1 Wood , Albrecht , 1981 Glagolevski j e t al. , 198 1 Borra , 198 1 Glagolevski j e t al. , 198 2 (a ) Glagolevski j e t al. , 1982 (b ) Bonsack , 198 1 Chunakov a e t al. , 198 1 Didelon , 198 3 Schoiz , 198 3 Borr a e t al. , 198 3 Thompson , 198 3 Glagolevski j e t al. , 198 4 Mikulase k e t al. , 1984 Romanyuk , 1984 Renson , 1984 Thompso n an d Landstreet , 198 5


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99 100 10 1 102 10 3 10 4 10 5 106 10 7 108 109 110 11 1 112 11 3 114 115 116 117 118 119 120

Glagolevski j e t al. , 198 5 - Chunakov a an d Glagolevskij , 198 5 - Bohlende r e t al. , 198 7 - Thompso n e t al. , 198 7 - Romanyuk , 198 6 - Glagolevski j e t al. , 198 7 - Glagolevski j e t al. , 198 8 - Bohlender , 198 9 - Gerth , 1990 - Landstreet , 1990 - Shor e e t al. , 199 0 - Romanyuk , 199 1 - Mathys , 199 1 - Kopylov a an d Romanyuk , 199 2 - Elkin , 199 2 - Bohlende r e t al. , 199 3 - Elkin , 199 4 - Bohlender , 199 4 - Bychko v e t al. , 199 2 - Romanyu k e t al. , 199 5 - Elkin , Wade , 199 6 - Wad e e t al. , 1996 (a )

12 1 122 123 124 12 5 126 127 128 129 130 13 1 132 13 3 134 13 5 136 137 138 139 140 14 1 142

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Wad e e t al. , 199 6 (b ) Glagolevski j e t al. , 199 5 Romanyu k e t al. , 199 7 Bychko v e t al. , 1997(a ) Bychko v e t al. , 199 7 (b ) Mathy s e t al. , 199 7 Mathys , Hubrig , 199 7 Babel , North , 199 7 Leroy , 199 5 Romanyuk , Kudryavtsev , 199 8 Elkin , 199 9 Wad e e t al. , 199 9 (a ) Romanyu k e t al. , 200 0 Wad e e t al. , 199 7 (a ) Wad e e t al. , 199 7 (b ) Romanyu k e t al. , 199 9 Wad e e t al. , 200 0 (a ) unpublishe d Wad e e t al. , 200 0 (b ) Ziznovsky , Romanyuk , 199 0 Bohlender , Landstreet , 199 0 Hill , Blake , 199 6

2 1 o f whic h ar e slo w rotator s wit h mor e tha n 1 0 sur face magneti c fiel d estimates . Fo r thes e 2 1 star s reli able magneti c fiel d model s ca n b e constructed . Th e numbe r o f star s i s certainl y ver y smal l t o com ply with th e requirement s for observationa l data . Acknowledgements . I would like t o than k m y colleagues from th e Stella r Magnetis m Laborator y of SA O RAS, V.G. Elkin an d D.O . Kudryavtsev , for helpful discussions an d th e Russia n Foundatio n for Basic Researc h for partial financial support .

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