Source: http://sunguoyou.lamost.org/vvv.html
Timestamp: 2019-04-19 11:14:39+00:00

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7. other symbols (BLLAC, CST, GAL, L:, QSO, S, *, +, :).
cesses, the classification adopted in the Catalogue is far from perfect.
variables; X-ray sources; and peculiar objects.
have been added in the Name-Lists 67- 77 and in the GCVS vol.V.
and CIV absorpion lines in their spectra.
of light. The total range of light variations may reach 4-5 mag V.
variation is about 0.5-1.0mag V (KV Vel).
BE for the type of variability.
EP Stars showing eclipses by their planets. Prototype: V0376 Peg.
probably high-overtone pulsators. Prototype: AU Ari.
from several tenths of a day to slightly in excess of one day.
non-radial pulsators. Prototype: gamma Dor.
magnitude. Prototype: V361 Hya = EC 14026-2647.
considerably brighter by luminosity (BL Boo = NGC 5466 V19).
sustained for long periods of time or slow decline by 1-2 mag.
Spectral types at maximum are in the range Ae(alpha) – Gpe(alpha).
variables are coupled with reflecting cometary nebulae.
IA Poorly studied irregular variables of early (O-A) spectral type.
symbol for the type may be accompanied by the symbol “YY”.
variables, and even extragalactic BL Lac objects.
mag in V lasting from a month or more to several hundred days.
cyclic) light changes with amplitudes in the range 1-7 mag in V.
They belong to the brightest blue stars of their parent galaxies.
surrounded by expanding envelopes (P Cyg, Eta Car).
brightness in several minutes or dozens of minutes.
variables with irregular variations superimposed by flares.
of He I and He II as well as C II-C IV, O II-O IV, and N III-N V.
particular, by nonstable mass outflow from their atmospheres.
its surface may have opposite pulsation phases.
periods. Cycles from several days to several weeks are observed.
characteristic of many of these stars.
magnitude smaller than the normally observed ones.
expansion velocity almost coinciding with maximum light.
fundamental tone with the period P0 and the first overtone P1).
CWB W Vir variables with periods shorter than 8 days (BL Her).
the shapes of their light curves and their periods.
the main sequence (SU Cas).
phenomenologically close to the SX Phe variables.
representative of the Delta Sct variables in open clusters.
often attributed to this type because of being insufficiently studied.
of about 1 mag in V (TZ Cas).
symbol for that type (SR).
Bp stars with weak hydrogen lines and enhanced lines of He and C.
interval of about a year.
than 0.8 mag in V (SX UMa).
vice versa. The complete light amplitude may reach 3-4 mag in V.
magnitude (DF Cyg, RV Tau).
several magnitudes (usually 1-2 mag in V).
periods is from 30 to 1100 days (SX Her, SV UMa).
absorption lines in their spectra.
with spectral types B8p-A7p and displaying strong magnetic fields.
on those caused by rotation.
of the surface brightness (spots) and chromospheric activity.
are simultaneously considered eruptive variables.
eclipses. Light amplitudes do not exceed 0.1 mag in V.
types with broad H and K Ca II emission and sometimes Halpha.
of EW (W UMa) close binary systems (see below).
light pulses reach 0.8 mag.
with variable-intensity He I and Si III lines and magnetic fields.
stars are high-temperature analogs of the ACV variables.
and even Mira variables. Outburst amplitudes may reach 10 mag.
years have been observed (T CrB).
outburst, their brightnesses by 20 mag and more, then fade slowly.
features, supernovae are subdivided into types I and II.
the rate of fading is 0.1 mag per day.
SS Cyg, SU UMa, and Z Cam.
five times longer (wider), and occur several times less frequently.
several cycles retain a magnitude between maximum and minimum.
amplitudes are from 2 to 5 mag in V.
up to 4 mag in V. A very inhomogeneous group of objects.
physical and evolutionary characteristics of their components.
types of eclipsing binary systems that we use are given below.
close to 90 deg) that the components periodically eclipse each other.
quite different and may reach several magnitudes.
are usually <2 mag in V.
spectral types F-G and later.
components may be a main sequence star.
number and total area of spots on the star’s surface vary.
WD Systems with white-dwarf components.
WR Systems having Wolf-Rayet stars among their components (V 444 Cyg).
subgiants not filling their inner equipotential surfaces.
stars and do not fill their inner Roche lobes.
below), but not in contact.
K Contact systems, both components filling their inner critical surfaces.
close in size to their inner critical surfaces.
ponent is close to its inner Roche lobe.
data field. Examples are: E/DM, EA/DS/RS, EB/WR, EW/KW, etc.
area of the cooler companion’s surface an earlier spectral type.
object surrounded by an accretion disk and a dA – dM-type dwarf.
giant primary component and a hot compact object as a companion.
XPR X-ray pulsar systems featuring the presence of the reflection effect.
reach 4-5 mag in V (AM Her, AN UMa).
the X-ray symbol by a “+” sign (e.g., E+X, ELL+X).
the Catalogue in the future, too.
L: Unstudied variable stars with slow light changes.
earlier were erroneously considered to be variable stars.
S Unstudied variable stars with rapid light changes.
insufficiently studied members of future new types of variables.
(GCVS I-III and NL 67 – 79).

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