V/121 Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999)

V/121/notes.dat Individual notes (245 records)

Seq
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Note
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1AN And. Photometric and absolute elements are not reliable. The both
1 components have considerable excess radii for their masses.
3V805 Aql. The both components (especially primary) have considerable
3 excess radii for their masses.
4Sig Aql. Obtained elements aren't very reliable.
5V539 Ara. System has a gaseous streams; the depth of Min I changes with time
7AR 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.
8EO Aur. Photometric elements and mass ratio of components have been found
8 roughly.
9HS Aur. Elements are very reliable.
11ZZ Boo. Both components have considerable excess radii for their masses.
13SZ 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.
14TU 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.
15AN Cam. Photometric elements are very unreliable.
16AS 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.
19EM Car. Elements are very reliably.
21YZ Cas. Elements are very reliably.
22AR 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").
23CC Cas. It is likely to be the member of Cam OB I association.
26SZ Cen. Both components have considerable excess of radii for their masses.
27V346 Cen. The primary component has considerable excess of radii for
27 its mass.
28WX 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.
29ZZ 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.
30AH Cep. Probably, there is the third body in a system. There is a gaseous
30 substance in the system.
31CW 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.
32EI Cep. Both components have considerable excess radii for there masses.
33EK Cep. According to Popper (1987AJ.....93..672P) the secondary component is
33 the star on pre-main sequence stage.
34NY Cep. Photometric elements aren't very reliable. Secondary minimum
34 lacks because of the big eccentricity of the orbit.
36XY Cet. Both components have considerable excess of radii for their masses.
37RS 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.
38RZ Cha. Both components have considerable excess of radii for their masses.
39TY 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.
40alf 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
42MR 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.
43MY Cyg. Both components have some excess of radii for their masses.
43 According to Popper, 1971ApJ...169..549P, both components are Am-stars.
44V380 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.
45V442 Cyg. Elements are very reliable.
46V453 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.
48V478 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.
50V1765 Cyg. The radial velocities curve of secondary componentt and the
50 masses ratio of components aren't very reliable.
52BH 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".
54CM 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.
55DE 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.
56CW Eri. Phorometric elements aren't very reliable.
57YY 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.
58RX Her. It is possible presence of diffuse gaseous matter in the system.
59TX 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.
61HS 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.
62V642 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
63V819 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.
66AI 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.
68KW Hya. Primary component have considerable excess radius for its mass.
69chi2 Hya. Primary component have considerable excess radius for its mass.
71CO 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.
72EN 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.
73TX 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".
75RR Lyn. Both components have considerable excess radii for its masses.
75 Main component is Am-star.
76FL Lyr. It is possible, this system has gas matter that causes distortion
76 light curves.
77V478 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.
78TZ Men. Elements are very reliable.
79UX Men. Elements are very reliable.
80RU Mon. There is the third body in the system that has mass 2.2M_{sun}_ and
80 period 67.6 years.
82IM Mon. The eclipses are very small. Photometric elements are not reliable.
82 The system is very cramped.
83U Oph. The system is likely to have gas streams that are responsible for
83 peculiarity on light curve (Popper, 1978ApJ...220L..11P).
84WZ Oph. Minima are almost equal in depth and shape. The eclipses are almost
84 tangent.
85VV 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.
88V1031 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".
89del 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.
90eta 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).
91BK 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.
92EE 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.
93AG 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)).
95V467 Per. The eclipses are very small, the system is really ellipsoidal
95 variable. Photometric and absolute elements aren't very reliable.
96zet Phe. Zeta Phe is a bright component of visual triple system;
96 visual secondary component is at a distance 0.6" and 6.4".
97PV 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.
98TY 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.
99VV Pyx. More feeble visual secondary component is observed at a distance
99 0.3" of eclipsing pair.
100V1647 Sgr. The system is likely to have feebler visual secondary component.
102V906 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.
103AL Scl. Primary component has outstanding excess of radius for its mass.
104EG 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.
105CD 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".
106V818 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.
108CV Vel. The both components have considerable excess of radii for their
108 masses.
109DM Vir. The both components have considerable excess of radii for their
109 masses.
110alf 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).
111HD 84207. Photometric components and radii aren't evaluated very reliably.
113V3903 Sgr. This system is denoted as '100a' in the original article.