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## (from tabmap V6.0 (2016-08-18)) 2024-04-19T02:33:37
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#-- V/121 Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999)
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#---Table: V/121/./notes.dat Individual notes (245 records)
# Seq I3 --- Sequential number of the star
# Note A76 --- Text of the note
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Seq|Note
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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.
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