Contents of: V/121/./notes.dat

The following document lists the file notes.dat from catalogue V/121.
Also available: plain copy of the file with f77 program to read file into arrays or line by line
File is also available in FITS, Tab-separated format, or in HTML.


## (from tabmap V6.0 (2016-08-18)) 2020-09-21T03:34:00
#---------------------------------------------------------------------------
#-- 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.
--------------------------------------------------------------------------------

© Université de Strasbourg/CNRS

    • Contact