Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.inasan.rssi.ru/~malkov/CEV/marginal.txt Дата изменения: Tue Dec 24 10:23:00 2013 Дата индексирования: Sat Jun 28 03:55:25 2014 Кодировка: Поисковые слова: vela

FF Aqr DW Period is significantly greater than typical value
for DW type. According to Pojmanski [45] this star
is DCEP-FU: variable. According to Sipahi et al. [263]
it is one of the few binary systems which consists of
the hot subdwarf and cool chromospherically active
giant components. According to Marilli et al. [264]
it is one of the peculiar system which is defined as
pre-cataclysmic binaries or pre-symbiotics.

HM Aqr Post-AGB Star (proto-PN).

V803 Aql CWA System with A1>0.75, consists of two almost identical
components (Samec et al. [278]).

TT Aur SH A1 is larger than 0.6, the system lies near line of
equal radii. According to Ozdemir et al. [491] TT Aur
is a special example of a close eclipsing binary
system consisting of a pair of young and massive stars
with almost equal radii.

CQ Aur DR Small A1 and large period. Belongs to long-period
RS CVn systems, secondary is more massive and more
larger (volume of the secondary is approximately
100 times larger than that of the primary component).
Primary is the hotter one. According to Popper
[492] sp. type of system is F5+K1 if both components
are the MS stars, but according to Kang [388] both
components are the subgiants.

eps Aur Such a long periods have only DGlate type systems but
their secondary spectra lies in range G8-M2, the
enigmatic binary. At least a part of other DGL systems
are classified as being similar to eps Aur.

SS Boo DR Inverse DR system (Montesinos et al. [493])

RR Cae DW Pre-cataclysmic system (see Bruch [494]), A1 is
greater than 3. Post-common-envelope binary according
to Parsons et al. [495].

RZ Cnc DR Inverse DR system (Montesinos et al. [493])

UU Cnc Semidetached system consisting of a K4 giant
which fills its Roche lobe and unseen primary,
obscured by the optically thick accretion disk
(see Zola et al. [496]). Active interacting algol
binary (like W Cru). But period of the system is not
suitable for SA systems (as for W Cru!).

AC Cnc S2C Too large A2. According to Hoard [110] and Downes
et al. [90] the system is probable member of the NL
type variable group of SW Sex or UX UMa type. The
main part of GCVS gives max=13.80 and minI=15.40 in V,
but in remarks file of GCVS brightness in maximum and
secondary minimum equal to 14.5 and 14.7 respectively.
Thus value of A2 equals to 0.9 if one uses maximum
brightness from main part of GCVS or A2 equals 0.2 for
maximum brightness given in remarks file.
Yamasaki et al. [146] have pointed out to
out-of-eclipse light variations. Range of variations
of the maximum brightness reaches 0.5 mag. According
to data from Yamasaki et al. [146] and Shugarov [147]
the mean value of maximum brightness equals to 14.5
and then A2 has a normal value. Too early Sp2
(usually Sp2>=M)

ES Cnc DR Only one DR system with such small values of A1 and
period. But according to Yakut et al. [540] eclipses
are partial. Additionally system is a hierarchical
triple in which all three are blue stragglers.

HR CMa Because of its period may belong to DGlate only, but
K0III must be assigned to secondary and A1 is smaller
than needed. Barium star, so secondary may be the WD.

V415 Car DGL A1 is lower than typical value for DGL class. The
eclipse is partial with the hotter secondary grazing
the polar region of the primary, so A1 is small.
The A star position is consistent with the model
tracks on HRD, the evolved G-star primary is
substantially too luminous and too blue to lie on the
predicted model track (Brown et al.[436]).

V429 Car Because of its spectra may belong only to DGearly
systems, but has longer period (periods for DGearly
is shorter than 35 days). Eccentric. See Parkin &
Gosset [434] for details.

RX Cas SA Belongs to W Ser type star, "active algol",
according to GCVS textual remarks 9.12<=Min II<=9.49
and this was confirmed by Djurasevic [245]. We think
it is rather SA because of long period.

SX Cas SA Belongs to W Ser type star, "active algol".

AZ Cas Because of its very long period may belong to DGlate
class only, if secondary spectra is later than G3.
According to Podsiadlowski [497] is VV Cep variable.
It is Interesting and probable marginal system.

del Cas Long period is suitable for DGlate only, but not
amplitudes and lum. class of secondary. According to
Rhee et al. [498] infrared excess is registered by
IRAS. According to Hovhannessian & Hovhannessian [499]
is a "Vega-type" disk system.

CQ Cep DG WR binary, the shortest period among known such
systems. Very asymmetric eclipses, wind-wind
interaction. According to Demircan et al. [214]
(based on lc solution) system is overcontact, and is
member of OB1 Cep association.

EK Cep DM Too large A1, far from line M for DM systems
(see Fig.1 in Malkov et al. [324]). According to
Popper [144] the radius and luminosity of the
secondary components are enlarged in comparison with
the MS star. Popper suggested the pre-MS status for
this system. Later Marques et al. [260] have confirmed
the pre-MS nature of the low mass secondary component
of EK Cep.

GP Cep S Is a quadruple system, consisting of WN6o/WCE+O3-6 and
B0:I+B1:V-III Demers et al. [347], why it is S? Both
pairs are eclipsing with P=6.6884 and P=3.4696.

KR Com CWA Amplitudes are small compared to other CWA system.
Star is classified as CWA according to the Zasche1 &
Uhlar [372], triple

alf CrB DM The only one eclipsing binary in the CEV with two MS
stars with such large temperature difference between
two components (~B9 and G5 for primary and secondary
respectively)! One of the widest eclipsing
binaries with detached MS components. Large
eccentricity of the orbit also points to unevolved
status of the system. Binary is onserved as
X-ray source because of activity of G5 secondary.

W Cru Belongs to active algols and has the longest period
among the group of W Ser binaries. So may be SA
system?

CG Cyg DR Inverse DR system (Montesinos et al. [493])

CI Cyg D2S D2S have Sp1 around O, but CI Cyg has Bep type for
hotter component (according to CEV and GCVS). CI Cyg
is a symbiotic system, according to Kenyon et al.
[155] secondary is a MS star (usually secondary star
is white dwarf) with accretion disk. But according to
Siviero et al. [153] secondary is rather WD star
because the accretion disk around MS star would not
be able to account for the outburst states of
CI Cyg. So secondary spectral type in now known
properly.

V380 Cyg DG Both spectra are earlier than B. Apsidal motion! The
system consists of an evolved massive primary with a
mass of 11.1 and a secondary which is still close to
the ZAMS and has a mass of 6.95.

WW Dra DR Inverse DR system (Montesinos et al. [493])

CM Dra DM BY Dra variable, low mass and radius,
compatible spectra and periods, is chromospherically
and flare active.

DE Dra DM Primary rotates much faster than synchronous rate,
relatively young and unevolved system.

RZ Eri DR Long-period RS CVn system. According to
Vivekananda Rao et al. [500] the primary is the hotter
and more massive, but smaller (Rh=2.84, Mbolh=1.35,
mh=1.69, Rc=6.94, Mbolc=1.41 and mc=1.63) so it may be
the inverse DR system (like Z Her), but there is a
solution with q greater than unity too. So status is
unclear? According to Vivekananda Rao et al. [500]
spectra is F0IV+G5-G8III-IV. Also there is
circumstellar envelope or shell around the system
because IR excess was detected. Spectra differs
from those of other DR systems.

TZ For DG Two components with almost equal masses (1.95+2.05),
but different radius: the hotter F star is smaller
(about 4R), G star is greater (about 8.2R) and more
massive. The rotation of the larger star is
synchronized with orbital motion, while smaller star
rotates much faster. Orbit is circular. Both
components have evolved well from the MS,
chromospherically active, but not RS CVn type.
According to Bisikalo et al. [501] it is long-period
RS CVn? Primary (more massive) is in the core helium
burning phase, but secondary is near the "red hook".

YY Gem DM BY Dra variable, low mass and radius,
compatible spectra and periods, is chromospherically
and flare active; YY Gem also is one of the most
flare active star.

OW Gem DGL OW Gem consists of two supergiants and was classified
as DG system but, according to GCVS data and ASAS-3
light curve, it has an extreme value of the phase of
secondary minima (0.23P) which points to the high
eccentricity of the orbit. System consists of two
stars with quite different masses. Terrell et al.
[351] have noted that if the two stars were formed
together both cannot possibly be in the red giant
stage. Also significant mass transfer is ruled out by
very small relative radii of stars and the very large
orbital eccentricity. Eggleton [502] proposed a
suggestion that OW Gem is a former triple system with
the primary having formed from the merger of a close
binary. But the merger product might be expected to
have rapid rotation, and although the primary star
does appear to be rotating faster than the
pseudosynchronous rate, it is not unusually rapid.
Primary could have undergone a G/K supergiant stage
just after the merger and had substantial momentum
removed by stellar wind and magnetic braking angular
during a period of enhanced activity. This hypothesis
needs to be tested.

V1003 Her CB Rucinski et al.[284] based on RV curve shown that
binary is most likely the W UMa type but for full
description high-precision photometry is required,
later Deb & Singh [343] have classified it as CB
system based on solution of ASAS light curve. They
derived very low inclination (about 42 deg) and
temperature difference is around 2000K while dA
is almost 0!. So it is rather near-contact system
with low inclination

AR Lac DR Inverse DR system (Montesinos et al. [493])

FL Lyr DM System with solar like components, detached. There are
a few solar type binaries due to selection effects.

AR Mon DR Inverse DR system (Montesinos et al. [493])

V505 Mon Marginal system, interacting algol with circumbinary
matter and disk. See Mayer et al. [503] for details.

BM Ori DM Possible pre-ms system

V1016 Ori Period is not suitable for any of the classes
(but very close to DGlate values). Spectra in CEV is
appropriate for DGlate too, but secondary spectra is
A0V (Vitrichenko & Plachinda [504]), is the secondary
a pre-MS star (Lloyd & Stickland [505])? Like BM Ori?

AR Pav D2S Too large A1. ASAS-3 gives max=11.0, minI=13.0,
minII=max in V filter (not in CEV till). Values in
GCVS are too large (about 6 mag for A1). According to
Skopal et al. [506] "AR Pav is an eclipsing symbiotic
binary with an orbital period of 605 days. It consists
of a M5 III giant with a mass of ~2 M{sun}. The nature
of the hot companion is under discussion. The presence
of a large accretion disk around a main sequence star
was suggested by several authors (see cites inside
Skopal et al. [506]), but, in contrast,
Schild et al. [508] considered a possibility that
the hot component is a white dwarf and the red
giant underfills its Roche lobe. According to the
observed variations in the UV/optical continuum, the
hot eclipsed object is highly variable in brightness,
size and geometry". In Skopal et al. [507] from light
curve one can see, that in active state magnitude
range is about [10-13], in quiet phase mag range is
about [10.3-13]. More observations are needed?

V718 Per May belong to DGlate class only because of its very
long period, but spectra is needed to be determined
properly. According to Grinin et al. [437] eclipses
are caused by large variable amounts of circumstellar
dust. Grinin et al. have suggested that V718 Per is
pre-MS post-T Tau single star. Deleted from CEV

DV Psc Active RS CVn system, detached according to LC
solution of Zhang et al. [509], so may be DR, but has
very short period for DR class, lc is asymmetric like
for CBV class, but period is shorter than typical
CBV value. May be classified as CB, but secondary
spectra is needed. According to Zhang & Zhang [510] is
near-contact system. See [510] for details. Marginal
and interesting system.

TY Pyx DR A2 is too large for DR class. A2 almost equals to A1.
According to Rao & Sarma [511] it is a unique member
of RS CVn group with both components having the same
mass, radii, temperature, luminosity and pre-MS
contraction phase.

V Sge S2C Too large A1, is novalike variable and prototype for
small group of V Sge subtype NL variables Steiner
[512]. Authors denoted V617 Sgr, DI Cru, WX Cen as
NLV variables also. The three later systems are not
eclipsing.

UU Sge DW Too large A2 and A1 is greater than 3, lies far from
other DW systems. UU Sge is the nucleus of planetary
nebula Abell 63 and thus post-CE binary. According to
Afsar & Ibanoglu [261] radius and temperature of the
secondary component are larger than those expected
for MS star of the same mass. Derived limb darkening
coefficients of the secondary corresponds to a
temperature about 10000K. Perhaps the large value of
A2 is due the reflection effect and overheated face
of the secondary.

V5112 Sgr Very long period is not suitable for any of the
classes, in VSX is denoted as PPN variable. Post-AGB
Star (proto-PN) according to Arkhipova et al. [513]
(and references within). Spectra is uncertain,
binarity is not proved, and it is only
a suggestion. See Arkhipova et al. for details

V5158 Sgr According to Torres et al. [82] system is a
hierarchical triple system composed of a slightly
evolved F6 star (the brighter object) near the end of
its MS phase and an eclipsing binary with a K7-M0V
star orbiting an F4V star.

mu Sgr Very long period is not suitable for any of classes
with such early spectra (DGearly, SH, CE, CG).
Kondo et al. [514]: P Cyg variable profiles, a mass
flow from the primary through inner Lagrangian point,
interaction of this material with stellar wind of the
secondary and is lost from a system. Marginal. But why
period is long?

ups Sgr System is the brightest member of the type of
extremely hydrogen-deficient stars (HdB).The HdB stars
are a rather rare class of evolved binary systems
that are in a second phase of mass transfer where the
primary has ended the core-helium burning phase. Dusty
circumstellar disk is presented. See Netolicky et al.
[515] for details.

V453 Sco DG A2 is larger than 0.3. Josephs et al. [516]: "From the
orbital period, light curve, evidence of circumstellar
gas, and faintness of the mass gainer all suggest that
HD 163181 is related to the W Ser class of massive
interacting binaries". Not DG?

BB Scl DM According to Watson et al. [248] it is visual triple
system HD9770, consists of A+B and C components. A
is of K1V type and possible binary and B is
eclipsing binary system of BY Dra type with both
stars are low mass and radius (~0.7) and
chromospherically active. They also noted that period
of binary is not typical for BY Dra systems and
shorter then usual.

RZ Sct SH A1>1. According to Wilson et al. [517] it is a
double-contact system. This fact was confirmed
by Olson & Etzel [518]. The primary star (gainer)
rapidly rotates.

V411 Ser May belong to DGearly, but lum. class of secondary
differs from limits for other DGearlies (all have lum.
class III-V). According to Conti et al. [519] systems
is evolved and on its way to becoming WR system, both
components well away from ZAMS. e is about 0.5 from
radial curves.

RW Tau SA Too large A1. May belong to W Ser type stars
(Plavec & Dobias [273]).

BE UMa DW Period is greater than 1d. Young pre-cataclysmic
variable (Shimanskii et al. [197]). Strong reflection
effect. Liebert et al. [520] discovered a rarefied
shell with a radius of r approx 1.5 pc in the field of
BE UMa. This shell, which is the remnant of a
planetary nebula, confirms the evolutionary similarity
of the system to other young pre-cataclysmic
variables, but suggests a relatively old age.

GK Vir DW A1 is greater than 3 (about 6). Post-common-envelope
binary according to Parsons et al.
[2010arXiv1005.3958P].

QS Vir DW A1 is greater than 3. Post-common-envelope binary
according to Parsons et al. [495].

Z Vul SH A1>1., the system lies near R line (see Fig.1 in
Malkov et al. [324]). According to Pojmanski [45]
A1=1.22 and smaller than CEV gives, A2 equals to 0.34
and then system will lay below R line. According to
Lazaro et al. [521] it is Sd system with two
components of almost equal radii. Primary (gainer,
more massive, hotter and larger) rotates faster than
synchronous.