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## (from tabmap V6.0 (2016-08-18)) 2024-05-21T15:21:24 #--------------------------------------------------------------------------- #-- V/121 Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999) #-------------------------------------------------------------------------- #---Table: V/121/./notes.dat Individual notes (245 records) # Seq I3 --- Sequential number of the star # Note A76 --- Text of the note -------------------------------------------------------------------------------- Seq|Note ---|---------------------------------------------------------------------------- 1|AN And. Photometric and absolute elements are not reliable. The both 1| components have considerable excess radii for their masses. 3|V805 Aql. The both components (especially primary) have considerable 3| excess radii for their masses. 4|Sig Aql. Obtained elements aren't very reliable. 5|V539 Ara. System has a gaseous streams; the depth of Min I changes with time 7|AR Aur. According to Nordstrom, Johansen (1994A&A...282..787N) a secondary 7| component is stay that is before ZAMS. The system belong to Aur OB I 7| association. 8|EO Aur. Photometric elements and mass ratio of components have been found 8| roughly. 9|HS Aur. Elements are very reliable. 11|ZZ Boo. Both components have considerable excess radii for their masses. 13|SZ Cam. The third light (L3=30%) is the binary system. Evolutional status of 13| system is not very evident. Photometric elements aren't reliable. Light 13| curve is very variable from season to season; perhaps, the system has 13| gaseous streams. There is a near visual satellite, B0 star which has 13| approximately the same brightness as the eclipsing system at a distance 13| 18". Visual satellite (ADS 2984A) is likely to be the binary system that is 13| why it is a sextuple system. Accrording to Kholopov, 1958, Kraft, Landolt, 13| 1959ApJ...129..287K, this system is the member of the very young open 13| cluster NGC 1502 near the center of which that system is. Budding 13| (1975Ap&SS..36..329B) notes the existence of absorbing substance around the 13| system. 14|TU Cam. Eclipses are very small; gaseous streams distort light curves; 14| photometric elements and mass ratio of components have been found roughly, 14| primary component has considerable excess of radius for its mass. 15|AN Cam. Photometric elements are very unreliable. 16|AS Cam. Light curves are asymmetric out of eclipses; there are evident form 16| changes of light curve in time. Probably, there is a gaseous substance in 16| the system. Mass ratio of components is evaluated unreliably. 19|EM Car. Elements are very reliably. 21|YZ Cas. Elements are very reliably. 22|AR Cas. Eclipses are very small. Photometric elements and mass ratio of 22| components has been found roughly. There is a near visual satelite 22| (at a distance 1"). 23|CC Cas. It is likely to be the member of Cam OB I association. 26|SZ Cen. Both components have considerable excess of radii for their masses. 27|V346 Cen. The primary component has considerable excess of radii for 27| its mass. 28|WX Cep. The primary component has considerable excess of radius for its 28| mass and the secondary component has the excess of radius, too. Probably, 28| there are gaseous streams in the system. 29|ZZ Cep. Photometric elements weren't estimated reliably. Secondary 29| component has considerable excess of radius for its mass. Probably, 29| there are gaseous streams in the system. 30|AH Cep. Probably, there is the third body in a system. There is a gaseous 30| substance in the system. 31|CW Cep. Photometric elements aren't reliable. According to Botzula R.A. 31| (1978, Izv. Astron. Obs. Engel. 44, 70), the primary component is 31| surrounded by rare gaseous envelope. It is a young system; It is a member 31| of Cep 0B III association. 32|EI Cep. Both components have considerable excess radii for there masses. 33|EK Cep. According to Popper (1987AJ.....93..672P) the secondary component is 33| the star on pre-main sequence stage. 34|NY Cep. Photometric elements aren't very reliable. Secondary minimum 34| lacks because of the big eccentricity of the orbit. 36|XY Cet. Both components have considerable excess of radii for their masses. 37|RS Cha. At least, one of system components is a physical variable 37| (perhaps, Del Set type). Both components have considerable excess of radii 37| for their masses. 38|RZ Cha. Both components have considerable excess of radii for their masses. 39|TY CrA. Eclipsing pair is a member of the triple system 39| (M3~(2.4+/-0.5)M_{sun}_). The second component (satellite) is likely to be 39| on pre-main sequence stage (Casey et al., 1995AJ....109.2156C). According 39| to data of Vitrichenko E. A. and Shevchenko (1995PAZh...21..434V), the 39| secondary component in eclipsing pair is surrounded by dust envelope it 39| leads to excess of its radius. The system TY CrA and reflective nebula 39| illuminated by it are members of CrA 1 association. 40|alf CrB. Eclipses are very small. Photometric elements have been computed 40| not very reliably. The system is likely to belong to the moving cluster UMa 42|MR Cyg. Components mass ratio was estimated from spectroscopic observations 42| not very reliably. System is very cramped, although it is detached. 42| Early values of the spectrum of system primary component were estimated 42| approximately as AO, however R. H. Hardie (private information mentioned in 42| the paper of Batten, 1967PDAO...13..119B) noticed that really this spectrum 42| is much more early: B3V; all later determinations (spectral and 42| colorimetric) confirm this evaluation. 43|MY Cyg. Both components have some excess of radii for their masses. 43| According to Popper, 1971ApJ...169..549P, both components are Am-stars. 44|V380 Cyg. Depths of minimums are very small; obtained photometric elements 44| are very unreliable. More massive component has considerable excess of 44| radius for its mass. Probably, it is surrounded by extended gaseous 44| envelope (Batten, 1962PDAO...12...91B; Leushin, Snezhko, 44| 1981Ap.....17..315L), as a result its dimensions, estimated from 44| photometric observations, can be exceeded, and its spectrum can belong to 44| brightness class III. 45|V442 Cyg. Elements are very reliable. 46|V453 Cyg. The system likes V447 Cyg, V448 Cyg. It is in the region of the 46| young open cluster NGC 6871; the system can be cosidered as the physical 46| member of this cluster. The both components are on G-R diagramm near the 46| turn point of the cluster. 48|V478 Cyg. The system is bright component of visual-binary system APS 13711; 48| visual satellite is at a distance 3.3". The system is likely to belong 48| to Cyg II. 50|V1765 Cyg. The radial velocities curve of secondary componentt and the 50| masses ratio of components aren't very reliable. 52|BH Dra. Photometric and spectral elements aren't very reliable. The mass 52| ratio of components is estimated approximately. The system is bright 52| component of visual-binary system ADS 18919. Visual satellite is at 52| a distance 10". 54|CM Dra. It is eclipsing variable system with the least known masses of 54| components. Because of spots activity it is obtained a sinusoidal 54| vibrations of brightness ~0.01", rarely in the system happens a 54| considerable outbursts. It is proposed, that CM Dra is a member of type II 54| of stellar population. CM Dra is the one of the nearest to us eclipsing 54| stars. 55|DE Dra. The secondary minimum isn't discovered in light curve, because 55| brightness and sizes of the secondary are very small. A phorometric 55| element hasn't been found surely. There is no spectoscopic and photometric 55| data about the secondary star. But, from computed values of mass and radius 55| of secondary component we can expect that the secondary is the late 55| F- or G-star. 56|CW Eri. Phorometric elements aren't very reliable. 57|YY Gem. It is one of the most active dMe-stars with large x-ray emmision. 57| Changes of light curves out of eclipses are explained by spots activity. 57| It has a photometric and spectroscopic evidences of present a gaseous 57| matter (possibly a gaseous stream) in the system. Brightness of system 57| feels a short-time outbursts, which amount to 1" in filter U. YY Gem is 57| the member of a multiply Castor system (ADS 6165) Castor C. A brighter 57| component Castor A is at a distance 77", components A and B also are 57| the binary. 58|RX Her. It is possible presence of diffuse gaseous matter in the system. 59|TX Her. There are irregular vibrations of brightness out of eclipses. 59| In a primary munimum a light curve is asymmeric; to all appearance the 59| system has a gaseous matter. 61|HS Her. The light curve is strongly distorted at phases 0.5-0.7, to all 61| appearance because the system has gaseous matter (Botzula, 1984, 61| Izv, Astron. Obs. Engel. 48, 15; Hall & Hubbard, 1971PASP...83..459H). 61| Mass ratio has been estimated rougly. 62|V642 Her. Primary component has considerable excess radius for its mass. 62| The system is the considerable evolved from initial point of main sequence. 62| According to (Zissel, 1972AJ.....77..610Z) the both components are Am-stars 63|V819 Her. The eclipses are very small. The system is the spectral triple. 63| The third component is brighter than eclipsing pair. Spectrum of the third 63| component is the G8 IV-III with emission in H and K of CaII. 66|AI Hya. The both components have considerable excess radii for their masses. 66| Bigger, more massive and less hot component is the variable 6 Set type. 68|KW Hya. Primary component have considerable excess radius for its mass. 69|chi2 Hya. Primary component have considerable excess radius for its mass. 71|CO Lac. According to Botzula (1981, Izv. Astron. Obs. Engel. 47, 19; 1984, 71| Izv. Astron. Obs. Engel. 48, 15), it is possible, there is diffuse gaseous 71| matter in the system. 72|EN Lac. The depth of the secondary minimum is very small; therefore a 72| spectrum of the secondary star has been estimated very indefinitely. 72| Primary component is the physical variable {beta} Cep type. The mass ratio 72| of components has been estimates roughly. 73|TX Leo. The eclipses are very fine; obtained photometric elements aren't 73| very reliable. The both components have considerable excess radii for their 73| masses. The mass ratio and elements founded from they aren't very reliable. 73| The system is the bright component of visual binary ADS 7837; visual 73| satellite is at a distance 2.4". 75|RR Lyn. Both components have considerable excess radii for its masses. 75| Main component is Am-star. 76|FL Lyr. It is possible, this system has gas matter that causes distortion 76| light curves. 77|V478 Lyr. Main minimum has small depth, secondary minimum isn't discovered 77| on brightness curve. Satellite spectrum was evaluated approximately. 77| Primary component has spot activity. 78|TZ Men. Elements are very reliable. 79|UX Men. Elements are very reliable. 80|RU Mon. There is the third body in the system that has mass 2.2M_{sun}_ and 80| period 67.6 years. 82|IM Mon. The eclipses are very small. Photometric elements are not reliable. 82| The system is very cramped. 83|U Oph. The system is likely to have gas streams that are responsible for 83| peculiarity on light curve (Popper, 1978ApJ...220L..11P). 84|WZ Oph. Minima are almost equal in depth and shape. The eclipses are almost 84| tangent. 85|VV Ori. It is very cramped massive DMS-system. There are streams of gas in 85| the system according to photometric and spectroscopy data (Duerbeck, 85| 1975A&AS...22...19D). W Ori is spectral-triple system that has very short 85| period of rotation around gravity centre of triple system: according to 85| (Duerbeck, 1975A&AS...22...19D) P=199 days. The third component is 85| invisible photometrically. Budding, Najim, (1980Ap&SS..72..369B) shows that 85| the system is connected with "Belt-subgroup" of association Ori I. 88|V1031 Ori. The system is triple. P1=3500-3700 years. More massive and 88| larger component is a bit colder than satellite. The third component at 88| a distance 0.164". 89|del Ori A. The evoluation of photometric elements presents a large 89| difficulty since the eclipses are very small, curve light is distorted and 89| asymmetrical; at least one component is physical variable. Del Ori A is a 89| very cramped parted system with both components that greatly were evolved 89| from FMS. Del Ori A is a bright component of visual triple system ADS 3144. 89| Very close satellite of almost the same brightness as eclipse system is 89| discovered at a distance 0.15" from Del Ori A (Heintze, 89| 1980ApJS...44..111H). Del Ori A belongs to "Belt-subgroup" of 89| association Ori I. 90|eta Ori. The eclipses are very small. Eta Ori is a multiple system, 90| brightness component of which is spectral-triple (Waelkens & Lampens, 90| 1988Ap&SS.142...99W). 91|BK Peg. The both components have considerable excess of radii for their 91| mass. The less massive component is a bit hotter than more massive 91| component. 92|EE Peg. Absolute elements are very reliable. EE Peg is spectral-third system 92| 0.3M_{sun}_<M_{star}_<0.7M_{sun}_, P1 = 1464 days. Primary component is 92| Am star. 93|AG Peg. The system isn't stationary and it has signs of diffusive substance 93| existence (Botzula P.A., 1984, Izv. Astron. Obs. Engel. 48, 15). AG Peg is 93| a bright component of visual triple system ADS 2990. The nearest visual 93| secondary component is at a distance 0.96". The system belongs to 93| OB-association Per II (Blaauw (1952BAN....11..405B) and Seyfen et al. 93| (1960ApJ...132...58S)). 95|V467 Per. The eclipses are very small, the system is really ellipsoidal 95| variable. Photometric and absolute elements aren't very reliable. 96|zet Phe. Zeta Phe is a bright component of visual triple system; 96| visual secondary component is at a distance 0.6" and 6.4". 97|PV Pup. The system has variable brightness starting with P~1.92 days, 97| different from orbital. The cause of this variable brightness isn't 97| evident. The light curve form in the maximum and in the secondary minimum 97| changes. The visual double ADS 6348, in which PV Pup is feeble part makes 97| visual and not physical pair. 98|TY Pyx. The both components are almost equal in size and surface 98| brightness and they have outstanding excess of radii for their masses. 98| Popper, 1969BAAS....1..257P, discovered emission lines H and K CaII in the 98| system spectrum that belong to both components. Both components are likely 98| to be near the point of leaving the main sequence. 99|VV Pyx. More feeble visual secondary component is observed at a distance 99| 0.3" of eclipsing pair. 100|V1647 Sgr. The system is likely to have feebler visual secondary component. 102|V906 Sco. Both components have considerable excess of radii for their 102| masses. V906 Sco is a physical part of open clump NGC 6475 and it belongs 102| to the brightest stars of this clump. 103|AL Scl. Primary component has outstanding excess of radius for its mass. 104|EG Scr. Photometric elements and radii of components aren't evaluated very 104| reliably. Ratio of component masses is evaluated sufficiently exactly. 104| Both components are likely to have considerable excess of radii for their 104| masses. 105|CD Tau. The both components have considerable excess of radii for their 105| masses. CD Tau is a bright component of visual double system ADS 3866. 105| Visual secondary component is at a distance 10.2". 106|V818 Tau. The depth of secondary minimum is very small. The system is 106| a component of multiple system ADS 8347 L3=0.3. Both components have 106| considerable excess of radii for their masses. 108|CV Vel. The both components have considerable excess of radii for their 108| masses. 109|DM Vir. The both components have considerable excess of radii for their 109| masses. 110|alf Vir. The depths of minimums are very small. Evaluation of photometric 110| elements by brightness curve is difficult because of a very small depth of 110| eclipses and physical variability of primary component (which is likely to 110| be a variable of type {beta} Cep). There are data that the system has gas 110| substance (Struve O. et al., 1958ApJ...128..310S). 111|HD 84207. Photometric components and radii aren't evaluated very reliably. 113|V3903 Sgr. This system is denoted as '100a' in the original article. --------------------------------------------------------------------------------