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Time-resolve d spectroscop y o f th e polar E U UM a ( = RE1149+28 ) a t th e 6 m telescop e
T.A . Somova , N.N . Somov , J.M . Bonnet-Bidaud , M . Mouchet
a a a b c,d

b

c

d

Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz 369167, Russia Service d'Astrophysique, CEN Saclay, CEA/DSM/DAPNIA/SAp , F-91191 Gif sur Yvette Cedex, France Observatoire de Paris-Meudon, F-92190 Meudon, France Universite Denis Diderot, Place Jussieu, F-75005 Paris Cedex, France

Abstract . W e repor t th e result s o f spectra l an d photometri c observation s o f th e ne w A M Her-typ e syste m E U UM a (=RE1149+28 ) obtaine d wit h th e T V scanne r an d electrophotomete r o f Nasmyth- 1 focu s (NEPh ) o f th e 6 m telescop e o n Februar y 1 4 an d 15 , 1993 . Durin g ou r observation s th e ± 0.1 3 an d V = ± 0.10 . A s a resul t o f spectroscop y wit h a syste m wa s o f V = tempora l resolutio n o f 5 mi n an d spectra l resolutio n o f 2 , a n analysi s o f th e variabilit y o f th e profiles , equivalen t widths , centra l intensities , halfwidth s an d radia l velocitie s o f th e emissio n line s , , HeI I 468 6 durin g th e orbita l perio d wa s made . Th e analysi s ha s show n th e presenc e o f appreciabl e change s i n th e parameter s o f th e line s dependin g o n th e orbita l perio d phase . Th e radia l velocit y curve s measure d for th e peak s an d center s o f gravit y o f th e emissio n line s hav e bee n i t follow s tha t th e constructed . Fro m th e measurement s o f th e radia l velocitie s o f th e peak s o f orbita l perio d o f th e syste m i s 90.0 : 0. 5 min . Th e equivalen t widt h an d relativ e intensit y curve s exhibi t tw o shar p maxim a a t phase s 0.1 5 an d 0.85 , i.e . separate d b y a 72. 5 mi n interva l (th e star t tim e o f ou r exposur e UT=00:51:2 7 correspond s t o zer o o f phas e whic h i s compute d usin g ou r bes t perio d determinatio n o f 90. 0 min.) . Broadenin g o f al l line s togethe r wit h decreasin g o f equivalen t width s an d relativ e intensitie s occu r nea r phas e 0.5 . I n th e rang e o f phase s 0.56-0.6 1 th e line s lin e i s practicall y disappear . Th e radia l velocit y curv e o f th e narro w componen t o f th e HeI I 468 6 a sinusoi d wit h a perio d o f 74. 9 2. 8 min , whic h correlate s wit h th e separatio n o f th e peak s o n th e curve s o f th e distributio n o f th e equivalen t width s an d centra l intensitie s o f th e Balme r emissio n line s wit h orbita l period . Thi s perio d probabl y indicate s tha t a t leas t tw o region s contribut e t o th e narro w component . Thes e ma y b e th e heate d hemispher e o f th e re d dwar f an d par t o f th e horizonta l stream .