v 0.99r
2008-05-15 (Protégé 3.4 build 130)
corrections on keywords/annotations
radio##metric##m
Radio Metric
Binaries, cataclysmic
CV*
Cataclysmic Variable
CataclyV*
cataclysmic##variable##star
Variable stars showing outbursts caused by thermonuclear burst processes in their surface layers (novae) or deep in their interiors (supernovae). We use the term "novalike" for variables that show novalike outbursts caused by rapid energy release in the surrounding space (UG-type stars) and also for objects not displaying outbursts but resembling explosive variables at minimum light by their spectral (or other) characteristics. The majority of explosive and novalike variables are close binary systems, their components having strong mutual influence on the evolution of each star. It is often observed that the hot dwarf component of the system is surrounded by an accretion disk formed by matter lost by the other, cooler, and more extended component.
Binaries:cataclysmic
YSO
yso##young##stellar##object
YSOs
YSOs
Y*O
YSO
IR
Infrared Source
ir##infrared##source
IR
Infrared sources
IV
nebular##continuum
Nebular Continuum
Recombination thermal continuum
Novae
Nova
nova##novae
Novae
Close binary systems with orbital periods from 0.05 to 230 days. One of the components of these systems is a hot dwarf star that suddenly, during a time interval from one to several dozen or several hundred days, increases its brightness by 7-19 mag in V, then returns gradually to its former brightness over several months, years, or decades. Small changes at minimum light may be present. Cool components may be giants, subgiants, or dwarfs of K-M type. The spectra of novae near maximum light resemble A-F absorption spectra of luminous stars at first. Then broad emission lines (bands) of hydrogen, helium, and other elements with absorption components indicating the presence of a rapidly expanding envelope appear in the spectrum. As the light decreases, the composite spectrum begins to show forbidden lines characteristic of the spectra of gas nebulae excited by hot stars. At minimum light, the spectra of novae are generally continuous or resemble the spectra of Wolf-Rayet stars. Only spectra of the most massive systems show traces of cool components.
Some novae reveal pulsations of hot components with periods of approximately 100 s and amplitudes of about 0.05 mag in V after an outburst. Some novae eventually turn out to be eclipsing systems. According to the features of their light variations, novae are subdivided into fast, slow, very slow, and recurrent categories.
N
No*
Nova
emission synchrotron
Synchrotron Emission
Thermonuclear Supernova Explosion
supernova##explosion##thermonuclear##thermo##nuclear
Stellar Object in Association
stellar##object##star##in##association
*iA
*inAssoc
SB##SBa##SBb##SBc##SBd##SBab##SBbc##SBcd##SB0##SB0a
Space velocities
velocity
Velocity
Velocities
eruption##explosion##process
Explosion or Eruption process
Explosion or Eruption process
GinGroup
group##galaxy##gal##galaxies##in
GiG
Galaxy in Group
Emission Process
emission##process
radio##cm##centimetric
Radio Centimetric
type 1##type1##flat##spectrum##radio##quasar##qso
Flat-Spectrum Radio Quasar
B Star
Star of Spectral Type B
bstar##b##star
Stars, B-type
High-mass X-ray Binary
HXB
x##ray##xray##binary##binaries##high##mass##hmxb
A high-mass X-ray binary (HMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is a massive star, usually a Be star or a blue supergiant. A fraction of the stellar wind of the companion star is captured by the compact star, and produces X-rays as it falls onto the compact object.
In HMXB, the massive star dominates the emission of optical light. The compact object is the dominant source of X-rays. The massive stars are very luminous and therefore easily detected. One of the most famous HMXB is Cygnus X-1 which was the first stellar-mass black hole discovered. Soft-gamma rays emitters.
HMXB
High Mass X-Ray Binary
Variable Star of gamma Dor type
gD*
Gamma Doradus variables are variable stars which display variations in luminosity due to non-radial pulsations of their surface. The stars are typically young, early F or late A type main sequence stars, and typical brightness fluctuations are 0.1 magnitudes with periods on the order of one day. This is a relatively new class of variable stars, having been first characterised in the second half of the 1990s, and details on the underlying physical cause of the variations remains under investigation.
Gamma Doradus Variable
gamma##doradus##variable##star
gammaDor
magnetic##field
Magnetic_fields
magnetic Field
Magnetic fields
UV
UV Source
uv##ultraviolet##ultra##violet##source
UV
dE
HI
hi##region##cold
Cold HI Region
HI
Supernova type II
SNII
supernova##typeii##type2##type##2##ii
LSB
LSB_G
Low Surface Brightness Galaxy
low##surface##brightness##lsb##gal##galaxy##galaxies
Lenticular Galaxy
lenticular##gal##galaxy##galaxies
F
Far Infrared
far##infrared
Wavelength > 30 microns
Blue
blue
Low-mass X-ray Binary
Low Mass X-Ray Binary
LXB
LMXB
Low-mass X-ray binaries (LMXBs) are binary stars where one of the components is either a black hole or neutron star. The other component (donor) is usually filling its Roche lobe and therefore transfers mass to the compact star. The donor is less massive than the compact object, and can be on the main sequence, a degenerate dwarf (white dwarf), or an evolved star (red giant). Found in the Milky Way, external galaxies, and in globular clusters.
A typical LMXB emits almost all of its radiation in X-rays, and typically less than one percent in visible light, so they are among the brightest objects in the X-ray sky, but relatively faint in visible light. The apparent magnitude is typically around 15 to 20. The brightest part of the system is the accretion disk around the compact object. The orbital periods of LMXBs range from ten minutes to hundreds of days. Soft-gamma rays emitters.
x##ray##xray##binary##binaries##low##mass##lmxb
star
Star
neutron##star
Neutron Star
Effective Temperature
effective##temperature
Effective temperatures
EUV
Extreme UV sources
EUV sources
Blue Supergiant
blue##super##giant##supergiant
core##dominated##coredominated
Core/Extented Flux Ratio >1
Core Dominated
Stars, G-type
Star of Spectral Type G
G Star
g##gstar##star
Radio-loud AGN
agn##radio##loud##active##galaxy##nucleus
L
Variable Star of delta sct type
delta##scuti##deltascuti
PulsV*delsct
Variables of the Delta Scuti type. These are pulsating variables of spectral types A0-F5 III-V displaying light amplitudes from 0.003 to 0.9 mag in V (usually several hundredths of a magnitude) and periods from 0.01 to 0.2 days. The shapes of the light curves, periods, and amplitudes usually vary greatly. Radial as well as nonradial pulsations are observed. The variability of some members of this type appears sporadically and sometimes completely ceases, this being a consequence of strong amplitude modulation with the lower value of the amplitude not exceeding 0.001 mag in some cases. The maximum of the surface layer expansion does not lag behind the maximum light for more than 0.1 periods. Delta Sct stars are representatives of the galactic disk (flat component) and are phenomenologically close to the SX Phe variables.
Sub-type:
- Low amplitude group of Delta Sct variables (light amplitude <0.1 mag in V). The majority of this type's representatives are stars of luminosity class V; objects of this subtype generally are representative of the Delta Sct variables in open clusters.
Delta Scuti Variable Star
DSCT
dS*
early##type##star##earlytype
Early-type Star
Stars, OB
Stars:early-type
Star of the early spectral types
Stellar Object in Double Star
*i*
*in**
stellar##object##star##in##double
A star that is part of a double star
pm##proper##motion
Proper_Motions
Proper Motion
Proper motions
component of the spacevelocity
Radio
Radio Source
radio##source
Rad
Radio sources
Variable Star of RR Lyr type
RR Lyrae Variable
rr##lyrae##variable##star
Variables of the RR Lyrae type, which are radially-pulsating giant A-F stars having amplitudes from 0.2 to 2 mag in V. Cases of variable light-curve shapes as well as variable periods are known. If these changes are periodic, they are called the "Blazhko effect."
Traditionally, RR Lyrae stars are sometimes called short-period Cepheids or cluster-type variables. The majority of these stars belong to the spherical component of the Galaxy; they are present, sometimes in large numbers, in some globular clusters, where they are known as pulsating horizontal-branch stars. Like Cepheids, maximum expansion velocities of surface layers for these stars practically coincide with maximum light.
Sub-types:
- RR Lyrae variables showing two simultaneously operating pulsation modes, the fundamental tone with the period P0 and the first overtone, P1 (AQ Leo). The ratio P1/P0 is approximately 0.745;
- RR Lyrae variables with asymmetric light curves (steep ascending branches), periods from 0.3 to 1.2 days, and amplitudes from 0.5 to 2 mag in V;
- RR Lyrae variables with nearly symmetric, sometimes sinusoidal, light curves, periods from 0.2 to 0.5 days, and amplitudes not greater than 0.8 mag in V (SX UMa).
RR
RR*
RRLyr
Ultraviolet
Spectra, ultraviolet
Ultraviolet
uv##ultraviolet##ultra##violet
UV
I
Blue objects
blu
Blue_objects
Blue Object
Blue
blue##object
X
X
X-ray sources
X-ray Source
HI
HI
HI Region
H I data
hi##region
HI (neutral) region
high##power##radio##loud##agn##active##galaxy##nucleus##
High-power Radio-loud AGN
l##ltype##type##irregular##star
L-type Irregular Star
Galaxy in Cluster of Galaxies
GinCl
cluster##in##galaxy##gal##galaxies
GiC
Galaxy in Cluster
asteroid
Asteroid
Minor planets
Asteroids
Red Giant
red##redgiant##giant
Association of Stars
Associations
AS*
Associations, stellar
Association of Stars
association##star##stars
Assoc*
Galaxies, Seyfert
SyG
low##power##radio##quiet##agn##active##galaxy##nucleus##seyfert
Seyfert Galaxy
Seyfert
Seyfert Galaxy
Seyfert_Galaxies
barred##spiral##galaxy##gal##galaxies
Barred Spiral Galaxy
BYDra
by##draconis##variable##star
BY
BY*
BY Draconis-type variables, which are emission-line dwarfs of dKe-dMe spectral type showing quasiperiodic light changes with periods from a fraction of a day to 120 days and amplitudes from several hundredths to 0.5 mag in V. The light variability is caused by axial rotation of a star with a variable degree of nonuniformity of the surface brightness (spots) and chromospheric activity.
Some of these stars also show flares similar to those of UV Cet stars, and in those cases they also belong to the latter type and are simultaneously considered eruptive variables.
BY Draconis Variable
Varaible Star of BY Dra type
Stars, distances
Radio continuum
Multiplet
continuum
Radio Lines
Continuum
Equivalent widths
Range allowing the description of the existence of a (noticeable) continuum for a given object
Balmer lines
Line Profiles
Space Velocity
space##velocity
BLLAC
BL Lac-type Object
BL Lac objects
BLLac##BL##Lac##Object##Lacertae
BLL
BLLac
BLLac
BL_Lac_objects
Irregular_V*
Ir*
Stars showing variations of irregular (non-periodic) type. Mostly (?) of eruptive type.
Irregular Variable Star
irregular##variable##star
Variable Star of Irregular type
High-velocity Cloud
HVC
high##velocity##cloud##nebula
HVCld
HVC (High Velocity Cloud)
ch##envelope##type##star
CH Envelope-type Star
CH Envelope-type Star
CH*
CH*
Flux
flux
line##width
Line Width
Starburst Process
star##burst##starburst
Polarization
polarization
Pu*
PulsV*
Pulsating variables are stars showing periodic expansion and contraction of their surface layers. The pulsations may be radial or nonradial. A radially pulsating star remains spherical in shape, while in the case of nonradial pulsations the star's shape periodically deviates from a sphere, and even neighboring zones of its surface may have opposite pulsation phases.
Depending on the period value, on the mass and evolutionary status of the star, and on the scale of pulsational phenomena, different types of pulsating variables may be distinguished.
Pulsating Variable Star
Pulsating Star
pulsating##variable##star
EmG
Emission-line galaxy
EmG
Emission-line Galaxy
emission##line##galaxy##gal##galaxies
Large Separation Lobes
large##separation##lobes##radio
Gamma-ray Source
gamma
gamma##ray##source
gam
pulsation##process
Pulsation Process
Seyfert 1 Galaxy
Sy1
Seyfert_1
Seyfert 1 Galaxy
seyfert##seyfert1##1##galaxy
Stellar Remnant
stellar##remnant
High_z_G
Galaxy with high redshift
Galaxy with High Redshift
HzG
high##redshift##galaxy##gal##galaxies
measure##measurement##measures##measurements
Measurement
Measured observational parameters/properties
Stars:variable
V*
V*
variable##star##stellar##object
Stars, variable
RS
Eruptive variables of the RS Canum Venaticorum type. This type is ascribed to close binary systems with spectra showing Ca II H and K in emission, their components having enhanced chromospheric activity that causes quasi-periodic light variability. The period of variation is close to the orbital one, and the variability amplitude is usually as great as 0.2 mag in V (UX Ari). They are X-ray sources and rotating variables. RS CVn itself is also an eclipsing system.
RS*
rs##canum##venaticorum##cv
Variable of RS CVn type
RSCVn
RS Canum Venaticorum Variable Star
Stars
*
stellar##object
Stellar Object
Star
O
Galaxies, UV-excess
Galaxies, optical
Galaxies, IR
galaxy##gal##galaxies
Galaxy catalogs
G
Galaxy
Galaxies, optical
Galaxies, photometry
Galaxies, spectra
Galaxies, nearby
Galaxies, rotation
Galaxies, Markarian
Galaxies
Photosphere
photosphere
Millimetric/submm sources
sub##millimetric##submillimetric##radio##source
smm
Sub-millimetric Radio Source
Radio(sub-mm)
Ages
Stars, ages
Rotation Process
rotation##process
Supernova type IIb
supernova##typeiib##type2b##type##2##ii##b##typeii##type2
High-mass Star
high##mass##star##highmass
Surface Brightness
s'applique aux objets étendus ( Gal/nebula)
surface##brightness
flux##amplitude##variation
Flux Amplitude Variation
AGN
AGN
Active Galaxy Nucleus
AGN
AGN
Active gal. nuclei
AGN##active##galaxy##nucleus##nuclei##galactic
dust
Dust
Stars, pre-main sequence
pre##main##sequence##star
pr*
Pre-main sequence star
pMS*
Pre-Main Sequence Star
qso##2##quasar##qso2
QSO2
Rotation-powered Pulsar
rotation##powered##pulsar
Interacting Galaxy
IG
IG
interacting##galaxy##galaxies
galaxy in strong interaction with others (within a pair or a group)
temperature
Radio Millimetric
radio##millimetric##mm
Spectra, millimetric/submm
MK spectral classification
Spectral types
Spectral_Classification
Spectral Type
spectral##type
Any class in Morgan Keeman's spectral classification
FU Orionis Variable Star
Variable Star of FU Ori type
FU*
Orion variables (eruptive) of the FU Orionis type. Characterized by gradual increases in brightness by about 6 mag in several months, followed by either almost complete constancy at maximum that is 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). After an outburst, a gradual development of an emission spectrum is observed and the spectral type becomes later. These variables probably mark one of the evolutionary stages of T Tauri-type Orion variables, as evidenced by an outburst of one member, V1057 Cyg, but its decline (2.5 mag in 11 years) commenced immediately after maximum brightness was attained. All presently known FU Ori variables are coupled with reflecting cometary nebulae.
FU
FUOr*
fu##orionis##orion##variable##star
X-Rays
x##ray##xray##rays##xrays
X-Ray
Pulsating Alpha2 Canum Venaticorum
pulsating##alpha##2##alpha2##cv##cvn##canum##venaticorum
near##ir##infrared
Near Infrared
Wavelength < 10 microns
gamma##rays##ray
Gamma-ray
Gamma Rays
Gamma rays
Stars, dwarfs
dwarf
Star of Luminosity Class V
Dwarf
B
mR
Radio(m)
Metric Radio Source
radio##source##metric
2
thing##top##anything
TOP
TOP concept
PaG
PairG
pair##gal##galaxy##galaxies
Galaxy Pair
Rotationally Variable Object
RotV*
Variable stars with nonuniform surface brightness and/or ellipsoidal shapes, whose variability is caused by axial rotation with respect to the observer. The nonuniformity of surface brightness distributions may be caused by the presence of spots or by some thermal or chemical inhomogeneity of the atmosphere caused by a magnetic field whose axis is not coincident with the rotation axis.
Rotationally Variable Star
rotational##rotationally##variable##object##star
Ro*
Accretion-powered Pulsar
accretion##powerred##pulsar
Parallaxes
Parallaxes, trigonometric
*iN
stellar##object##star##in##nebula
*inNeb
Stellar Object in Nebula
emission##maser
Maser Emission
weak##line##t##tau##tauri##star
Weak-line T Tauri
starburst##gal##galaxy##galaxies
StarburstG
SBG
Starburst Galaxy
Pulsars
PSR
Pulsar
Optically variable pulsars (CM Tau), which are rapidly rotating neutron stars with strong magnetic fields, radiating in the radio, optical, and X-ray regions. Pulsars emit narrow beams of radiation, and periods of their light changes coincide with rotational periods (from 0.004 to 4 s), while amplitudes of the light pulses reach 0.8 mag.
pulsar
Pulsar
Pulsar
Psr
Pulsars
Spectra, infrared
IR
ir##infrared
Infrared
super##cluster##supercluster##galaxies
SCG
Super Cluster Of Galaxies
3
SuperClG
Super Cluster of Galaxies
Pl?
Planets
planet
Planet?
Planet
(Extra-solar) Planet Candidate
Compact_Gr_G
compact##galaxy##galaxies##group
CGG
Compact Group of Galaxies
Millimetric Radio Source
Millimetric/submm sources
Radio(mm)
mm
millimetric##radio##source
not##non##radial##pulsation
Non-radial Pulsation
Line Emission
emission##line##lines
LINER
LINER AGN
LIN
liner##agn
LINER-type Active Galaxy Nucleus
LumX
lumx
accretion##disk
Accretion Disk
eruptive##variable##star
Eruptive*
Eruptive variables are stars varying in brightness because of violent processes and flares occurring in their chromospheres and coronae. The light changes are usually accompanied by shell events or mass outflow in the form of stellar winds of variable intensity and/or by interaction with the surrounding interstellar medium.
Eruptive Variable Star
Eruptive Variable Star
Er*
near IR emission, age around 10^6years
INT,IT
TT*
T Tauri Star
t##tauri##star##tau
Alpha2 Canum Venaticorum Variable
alpha##2##alpha2##cv##cvn##canum##venaticorum
Variable Star of alpha2 CVn type
Alpha2 Canum Venaticorum variables. These are main-sequence stars with spectral types B8p-A7p and displaying strong magnetic fields. Spectra show abnormally strong lines of Si, Sr, Cr, and rare earths whose intensities vary with rotation. They exhibit magnetic field and brightness changes (periods of 0.5-160 days or more). The amplitudes of the brightness changes are usually withine 0.01-0.1 mag in V.
Sub-type:
- Rapidly oscillating Alpha2 CVn variables. These are nonradially pulsating, rotating magnetic variables of Ap spectral type (DO Eri). Pulsation periods are in the range of 6-12 mmag (0.004-0.01 days), while amplitudes of light variation caused by the pulsation are about 0.01 mag in V. The pulsational variations are superposed on those caused by rotation.
RotV*alf2CVn
a2*
ACV
Diffuse clouds
dwarf##nova##novae##u##geminorum
Dwarf Nova (U Geminorum-type variable star)
DN*
DwarfNova
UG
U Geminorum-type variables, quite often called dwarf novae. They are close binary systems consisting of a dwarf or subgiant K-M star that fills the volume of its inner Roche lobe and a white dwarf surrounded by an accretion disk. Orbital periods are in the range 0.05-0.5 days. Usually only small, in some cases rapid, light fluctuations are observed, but from time to time the brightness of a system increases rapidly by several magnitudes and, after an interval of from several days to a month or more, returns to the original state. Intervals between two consecutive outbursts for a given star may vary greatly, but every star is characterized by a certain mean value of these intervals, i.e., a mean cycle that corresponds to the mean light amplitude. The longer the cycle, the greater the amplitude. These systems are frequently sources of X-ray emission. The spectrum of a system at minimum is continuous, with broad H and He emission lines. At maximum these lines almost disappear or become shallow absorption lines. Some of these systems are eclipsing, possibly indicating that the primary minimum is caused by the eclipse of a hot spot that originates in the accretion disk from the infall of a gaseous stream from the K-M star. According to the characteristics of the light changes, U Gem variables may be subdivided into three types: SS Cyg, SU UMa, and Z Cam.
Dwarf Nova
absolute##magnitude
Absolute Magnitude
Spectral Index
spectral##index
supernova##typeia##type1b##type##1b##ib##b##1##i
Supernova type Ib
V
Type1.5-Seyfert1.5
Seyfert
Seyfert 1.5 Galaxy
seyfert##seyfert1.5##1.5##galaxy
Power Radio Ghz
power##radio##ghz##radioghz##powerradioghz
Stars:Emission
Emission-line Star
Em*
Em*
Emission-line Star
emission##line##emissionline##star
Core Collapse Supernova Explosion
supernova##explosion##core##collapse
Eclipse
eclipse
flux##ratio##radio5ghz##radio##5Ghx##optical
Flux Ration Radio5Ghz-Optical
Elliptical Galaxy
elliptical##galaxy##gal##galaxies
open##cluster##star##stars
OpCl
OpC
Open Cluster
Open_clusters
Clusters, open
Stars, A-type
Star of Spectral Type A
A Star
a##star##astar
Or*
Variable Star of Orion type
Orion_V*
IN
Orion Variable Star
Orion variables. Irregular, eruptive variables connected with bright or dark diffuse nebulae or observed in the regions of these nebulae. Some of them may show cyclic light variations caused by axial rotation. In the Spectrum-Luminosity diagram, they are found in the area of the main sequence and subgiants. They are probably young objects that, during the course of further evolution, will become light-constant stars on the zero-age main sequence (ZAMS). The range of brightness variations may reach several magnitudes.
This type may be divided into the following subtypes:
- Rapid light variations observed (up to 1 mag in 1-10 days),
- Orion variables of early spectral types (B-A or Ae). They are often characterized by occasional abrupt Algol-like fadings (T Ori);
- Orion variables of intermediate and late spectral types, F-M or Fe-Me (BH Cep, AH Ori). F-type stars may show Algol-like fadings; K-M stars may produce flares along with irregular light variations;
- Orion variables of the T Tauri type. Stars are assigned to this type on the basis of the following (purely spectroscopic) criteria: spectral types are in the range Fe-Me. The spectra of most typical stars resemble the spectrum of the solar chromosphere. The feature specific to the type is the presence of the flourescent emission lines Fe II 4046, 4132 A (anomalously intense in the spectra of these stars), emission lines [Si II] and [O I], as well as the absorption line Li I 6707 A. These variables are usually observed only in diffuse nebulae.
- Some Orion variables (YY Ori) show the presence of absorption components on the redward sides of emission lines, indicating the infall of matter toward the stars' surfaces.
orion##variable##star
dwarf##spiral##galaxy##gal##galaxies
Dwarf Spiral Galaxy
Mass
mass
Masses
A planetary nebula is a nebula surrounding a stellar remnant (white dwarf)
Planetary nebulae
PN
2
Planetary_Nebulae
Planetary Nebula
PN
planetary##nebula##nebulae
QSO
QSOs
high##power##radio##quiet##agn##active##galaxy##nucleus##
QSOs
High-power Radio-quiet AGN
QSO
kstar##k##star
K Star
Star of Spectral Type K
Stars, K-type
Supernova type Ia
supernova##typeia##type1a##type##1a##ia##a##1##i
BlueCompG
Blue Compact Galaxy
BCG
blue##compact##galaxy##gal##galaxies
Blue Compact Galaxy
Eclipse of Beta Lyrae Type
eclipse##beta##lyrae
lpv##long##period##variable
Long-period Variable
dwarf##barred##spiral##galaxy##gal##galaxies
Dwarf Barred Spiral Galaxy
3
Clusters, galaxy
ClG
cluster##galaxy##galaxies
ClG
Clusters_of_galaxies
Cluster of Galaxies
Steep-spectrum Radio Quasar
steep##spectrum##radio##quasar##qso
Protostars
Protostar
protostar##proto##star
Brilliant Giant
Star of Luminosity Class II
brilliant##giant
f##fstar##star
F Star
Stars, F-type
Star of Spectral Type F
S
Reflection of stellar light
Reflection Process
reflection##process
S##Sa##Sb##Sc##Sd##Sab##Sbc##Scd##
Halo
halo
eclipse##algol
Eclipse of Algol Type
Dark Nebula
dark##cloud##nebula
DNe
Nebulae, dark
DkNeb
Luminosity Class
luminosity##class
brown##dwarf
Brown Dwarf
Planetary Nebula Central Star
planetary##nebula##central##star
white##dwarf##wd
Stars, white dwarf
WD*
Stars:white_dwarf
WD*
White Dwarf
A white dwarf or a stellar remnant
These are the classical cepheids, or Delta Cep-type variables.
Comparatively young objects that have left the main sequence and evolved into the instability strip of the Hertzsprung-Russell (H-R) diagram, they obey the well-known Cepheid period-luminosity relation and belong to the young disk population. Delta Cep stars are present in open clusters. They display a certain relation between the shapes of their light curves and their periods.
Sub-type:
- These are Delta Cep variables having light amplitudes <0.5 mag in V (<0.7 mag in B) and almost symmetrical light curves (M-m approx. 0.4 - 0.5 periods); as a rule, their periods do not exceed 7 days. They are probably first-overtone pulsators and/or are in the first transition across the instability strip after leaving the main sequence (SU Cas).
Traditionally, both Delta Cep and W Vir stars are quite often called Cepheids because it is often impossible to discriminate between them on the basis of the light curves for periods in the range 3 - 10 days. However, these are distinct groups of entirely different objects in different evolutionary stages. One of the significant spectral differences between W Vir stars and Cepheids is the presence, during a certain phase interval, of hydrogen-line emission in the former and of Ca II H and K emission in the latter.
Classical Cepheid (delta Cep type)
Classical Cepheid
delta##cepheid##classical##cep##cephei
DCEP
deltaCep
cC*
su*
Substellar Object
sub##substellar##object
Sub-stellar
low##power##radio##loud##agn##active##galaxy##nucleus
Low-Power Radio-loud AGN
Object of Unknown nature
Unknown
?
Object of unknown nature
Variable Star of RV Tau type
PulsV*RVTau
Variables of the RV Tauri type. These are radially pulsating supergiants having spectral types F-G at maximum light and K-M at minimum. The light curves are characterized by the presence of double waves with alternating primary and secondary minima that can vary in depth so that primary minima may become secondary and vice versa. The complete light amplitude may reach 3-4 mag in V. Periods between two adjacent primary minima (usually called formal periods) lie in the range 30-150 days.
Two subtypes are recognized:
- RV Tauri variables that do not vary in mean magnitude (AC Her);
- RV Tauri variables that periodically (with periods from 600 to 1500 days and amplitudes up to 2 mag in V) vary in mean magnitude (DF Cyg, RV Tau).
RV*
RV
RV Tauri Variable Star
rv##tau##tauri##rvtau##rvtauri##star##variable
T
H2G
hii####galaxy##gal##galaxies
HII Galaxy
HII_G
HII Galaxy
Accretion
Portion of Stellar Object
any component of a stellar object
portion##of##stellar##object
Classical T Tauri
classical##t##tauri##star##tau
Binaries:spectroscopic
binary##binaries##spectroscopic
Binaries, spectroscopic
Spectroscopic Binary
SB*
SB
eclipse##wuma##w##ursae##majoris
Eclipse of WUMa Type
DQHer
dq##herculis##variable##star
DQ*
Cataclysmic Variable Star DQ Her type
DQ Herculis
OH/IR
oh##ir##envelope##star
OH*
OH/IR Envelope-type Star
OH/IR Envelope-type Star
IR<10µ
NIR
Near-IR Source
near##ir##infrared##source
Supernova Explosion
supernova##explosion
A system of two or more distinct stars
Multiple_Stars
Multiple Star
Stars, double and multiple
Double or multiple star
**
multiple##star
Rotating ellipsoidal variables (b Per, Alpha Vir). These are close binary systems with ellipsoidal components, which change combined brightnesses with periods equal to those of orbital motion because of changes in emitting areas toward an observer, but showing no eclipses. Light amplitudes do not exceed 0.1 mag in V.
ELL
ellipsoidal##variable##star
RotV*Ell
Ellipsoidal Variable Star
El*
Ellipsoidal Variable Star
portion##of##galaxy
Any component of a galaxy
Portion of Galaxy
ring##gal##galaxy##galaxies
Ring Galaxy
Galaxies, ring
M
Red Object
red
Red
red##object
HI
HI Region Warm
HI
warm##hi##region
dI
ZZ*
PulsWD*
Pulsating White Dwarf
Pulsating White Dwarf
pulsating##white##dwarf##wd
Star of Luminosity Class IV
Subgiant
sub##giant##subgiant
EB*
EB*
E
Eclipsing Binary
Eclipsing Binary
Binaries, eclipsing
Binaries:eclipsing
Binary systems with orbital planes so close to the observer's line of sight (the inclination i of the orbital plane to the plane orthogonal to the line of sight is close to 90 deg) that the components periodically eclipse each other. Consequently, the observer finds changes of the apparent combined brightness of the system with the period coincident with that of the components' orbital motion.
eclipsing##binary##star
Interstellar_Medium
Interstellar medium
Neb
ISM
Interstellar Medium
Cld
Cloud
Neb
inter##stellar##interstellar##medium
rG
Radio Galaxy
Galaxies, radio
RadioG
radio##gal##galaxy##galaxies
variable##object
Object which main particularity is to feature a variability
Variable Object
Maser
Mas
Maser
Masers
Masers##Stars, masers
maser
red##super##giant##supergiant
Red Supergiant
component of the spacevelocity
Radial Velocity
radial##velocity
Radial velocities
value < 300000
asymptotic##giant##branch##star##agb
AGB Star
AG*
AGB*
Asymptotic Giant Branch Star
radio##sub##millimetric##submillimetric
Spectra, millimetric/submm
Radio Submillimetric
radial##pulsation
Radial Pulsation
fanaroff##riley##type##1
Fanaroff-Riley Type-1 Object
Polar Ring Galaxy
polar##ring##gal##galaxy##galaxies
Compound Object Morphology
compound##object##morphology
Sy*
ZAND
Symbiotic*
Symbiotic Star
Symbiotic Star
symbiotic##star
Symbiotic variables of the Z Andromedae type. They are close binaries consisting of a hot star, a star of late type, and an extended envelope excited by the hot star's radiation. The combined brightness displays irregular variations with amplitudes up to 4 mag in V. A very inhomogeneous group of objects.
IR>30µ
Far-IR Source
far##ir##infrared##source
FIR
cm
centimetric##radio##source
Radio(cm)
Centimetric Radio Source
HII_regions
hii##region
HII
HII Region
HII (inonized) region
HII
H II regions
Proplyd
Proplyd
protoplanetary##proto##planetary##disk##proplyd
Class
class##type
Carbon Star
C*
carbon##star##c
Carbon Star
C*
Gravitational_lensing
lensing##process
Lensing Process
Gravitational lensing
WU*
W Ursae Majoris-type eclipsing variables. These are eclipsers with periods shorter than 1 days, consisting of ellipsoidal components almost in contact and having light curves for which it is impossible to specify the exact times of onset and end of eclipses. The depths of the primary and secondary minima are almost equal or differ insignificantly. Light amplitudes are usually <0.8 mag in V. The components generally belong to spectral types F-G and later.
EB*WUMa
Eclipsing Binary of W UMa type
WUMa Eclipsing Binary
eclipsing##binary##star##wuma##w##ursae##majoris
EW
Comet
Comets
comet
chromosphere
Chromosphere
qso##quasi##stellar##object##quasar##type1##type##1
QSO type 1
Core/Extended Flux Ratio < 1)
Lobe Dominated
lobe##dominated##lobedominated
Supergiant
Stars, supergiant
Star of Luminosity Class I
super##giant##supergiant
RfNeb
Reflexion Nebula
RNe
reflexion##nebula
Mi*
mira##ceti##omicron##variable##star
Mira
Variable Star of Mira Cet type
M
Mira Ceti Variable
Mira (Omicron) Ceti-type variables. These are long-period variable giants with characteristic late-type emission spectra (Me, Ce, Se) and light amplitudes from 2.5 to 11 mag in V. Their periodicity is well pronounced, and the periods lie in the range between 80 and 1000 days. Infrared amplitudes are usually less than in the visible and may be <2.5 mag. For example, in the K band they usually do not exceed 0.9 mag.
NL
Nova-like Object
Insufficiently studied objects resembling novae by the characteristics of their light changes or by spectral features. This type includes, in addition to variables showing novalike outbursts, objects with no bursts ever observed; the spectra of novalike variables resemble those of old novae, and small light changes resemble those typical for old novae at minimum light. However, quite often a detailed investigation makes it possible to reclassify some representatives of this highly inhomogeneous group of objects into other types.
novalike##like##nova##object
Nova-like
NL*
HB*
Stars, horizontal branch
hb##star##horizontal##branch
Horizontal-branch Star
Horizontal Branch Star
HB*
Optical
optical
optical
Red
red
power##radio
Power Radio
portion##astroportion
Portion of Astronomical Object
Portion of an astronomical object which is not an astronomical object itself
dwarf##irregular##galaxy##gal##galaxies
Dwarf Irregular Galaxy
Emission Nebula
emission##nebula
Spiral Galaxy
spiral##gal##galaxy##galaxies
Equivalent Width
EquivalentWidth
equivalent##width
Stars, Am
Pe*
Stars:peculiar
Pec*
Stars, Ap
Peculiar Stellar Object
Peculiar Stellar Object
peculiar##star##stellar##object
Stars, peculiar
Stars, barium
Stars, Bp
Stars, metal-deficient
SNI
supernova##typei##type1##type##1##i
Supernova type I
astrobject##astroobject##astronomical##object
Any astronomical object
Astronomical Object
Post-AGB Star
postagb##post##agb##asymptotic##giant##branch##star
post-AGB*
Post-AGB Star
pA*
III
continuum##non##not##thermal
Continuum Non-thermal
Nebula
Nebula
in##pair##galaxy##gal##galaxies
Galaxy in Pair
GinPair
GiP
super##massive##supermasive##black##hole##blackhole
Supermassive Black Hole
spectrum
Spectrum
G
electron##temperature
Electron Temperature
Supernovae
supernova
SN
SN
supernova##supernovae
SN*
SuperNovae
SuperNova
Rapid Irregular Variable Star
Rapid_Irreg_V*
rapid##irregular##variable##star
Rapid irregular variables (class: eruptive) having no apparent connection with diffuse nebulae and showing light changes of about 0.5 - 1.0 mag within several hours or days. There is no strict boundary between rapid irregular and Orion variables. If a rapid irregular star is observed in the region of a diffuse nebula, it is considered an Orion variable. To attribute a variable to this type (R.I.), it is necessary to take much care to be certain that its light changes are really not periodic.
Sub-types:
- Rapid irregular variables of the early spectral types, B-A or Ae;
- Rapid irregular variables of the intermediate and late spectral types, F-M and Fe-Me.
Variable Star with rapid variations
IS
RI*
I
Stellar Object in Cluster
stellar##object##star##in##cluster
*iC
An individual star located in a star cluster
*inCl
atomic##element
Atomic Element
Binaries, X-ray
XB
X-ray Binary
X
x##ray##xray##binary##binaries
Close binary systems that are sources of strong, variable X-ray emission and which do not belong to or are not yet attributed to any other type of variable stars. One of the components of the system is a hot compact object (white dwarf, neutron star, or possibly a black hole). X-ray emission originates from the infall of matter onto the compact object or onto an accretion disk surrounding the compact object. In turn, the X-ray emission is incident upon the atmosphere of the cooler companion of the compact object and is reradiated in the form of optical high-temperature radiation (reflection effect), thus making that area of the cooler companion's surface an earlier spectral type.
XB*
galactic##galaxy##morphology
Galaxy Morphology
HV*
highvelocity##high##velocity##star
Stars, high-velocity
HV*
High-velocity Star
High Velocity Star
Stars, late-type
Star of the late spectral types
Stars, cyanogen
late##type##star##latetype
Late-type Star
Stars:late-type
Stars, S
Stars, carbon
Cataclysmic Variable Star AM Her type
am##herculis##variable##star
AMHer
AM*
AM
AM Herculis
Jet
jet
morphology##morphological##geometry##geometrical##feature##features
Morphology
Geometry or morphology of astronomical objects (including components which are not astronomical objects)
Morphological Feature
supernova##typeic##type1c##type##1c##ic##c##1##i
Supernova type Ic
period
Period
giant
Star of Luminosity Class III
Stars, giant
Giant
PulsV*semi-reg
SR
Semi-regular pulsating star
sr*
Semi-regular Pulsating Star
semi##regular##semiregular##pulsating##star
chromospheric##activity##chromosphere
Corresponds to an important chromosperic activity, usually a source of emission
Chromospheric Activity
Supernova type IILP
supernova##typeiilp##type2lp##type##2##iilpb##typeii##type2
rcb##r##coronae##borealis##variable
RC*
Variable Star of R CrB type
R Coronae Borealis Variable
Variables of the R Coronae Borealis type. These are hydrogen-poor, carbon- and helium-rich, high-luminosity stars belonging to the spectral types Bpe-R, which are simultaneously eruptive and pulsating variables. They show slow nonperiodic fadings by 1-9 mag in V lasting from a month or more to several hundred days. These changes are superposed on cyclic pulsations with amplitudes up to several tenths of a magnitude and periods in the range 30-100 days.
RCB
Erupt*RCrB
Process
process
Phenomenon or associated process
Set of ranges in the electromagnetic spectrum
EM Spectrum Range
em##electromagnetic##specrum##range
K
Envelope
envelope
bL*
EB
eclipsing##binary##star##beta##lyrae
Beta Lyrae Eclipsing Binary
Beta Lyrae-type eclipsing systems. These are eclipsing systems having ellipsoidal components and light curves for which it is impossible to specify the exact times of onset and end of eclipses because of a continuous change of a system's apparent combined brightness between eclipses; secondary minimum is observed in all cases, its depth usually being considerably smaller than that of the primary minimum; periods are mainly longer than 1 day. The components generally belong to early spectral types (B-A). Light amplitudes are usually <2 mag in V.
Eclipsing Binary of Beta Lyr type
EB*betLyr
Abundances, peculiar
Abundances, [Fe/H]
Abundances
Abundances
Gravitationnaly Lensed Image of a Quasar
lensed##quasar##qso##gravitationnaly
Lensed Quasar
LeQ
LensedQ
Optical Source
optical##source
Nonstellar objects
Non-stellar Body
Planets+Asteroids
Nonstellar
Supernova Remnant Shell
SNR
Supernova remnants
supernova##shell##remnant
SNR
SuperNovae_Remnants
Old Disk
Galactic Sperical Component (old disk)
old##disk##galactic##sperical##component
Extended
extended
wolf##rayet##wolfrayet##star##wr
Wolf-Rayet star
Stars:WR
WR*
Wolf-Rayet Star
Stars, Wolf-Rayet
WR*
Variability Time Scale
time##scale##timescale##variability
bok##globule
Bok Globule
Globules
Bok globules
roche##lobe##rochelobe
Roche Lobe
Thermal Continuum
Black Body thermal continuum
thermal##continuum
molecules
Molecules
dwarf##elliptic##galaxy##gal##galaxies
Dwarf Elliptical Galaxy
PN
planetary##nebula##shell
Planetary Nebula Shell
PN
GrG
Group of Galaxies
group##galaxies##galaxy
GroupG
High-proper motion Star
High Proper Motion Star
PM*
PM*
high##proper##motion##star
C
MolCld
molecular##cloud
MoC
Molecular Cloud
Molecular clouds
fanaroff##riley##type##2
Fanaroff-Riley type 2
Double Star
A system of two stars
**
2
double##star
Double or multiple star
spiral##arm
Spiral Arm
Spiral Arm of a galaxy
compact
Compact Morphology
Irregular Galaxy
irregular##galaxy##gal##galaxies
microlensing##micro##lensing
Micro-lensing
Ce*
Cepheid
cepheid##cep##cephei
CEP
Cepheids. Radially pulsating, high luminosity (classes Ib-II) variables with periods in the range of 1-135 days and amplitudes from several hundredths to 2 mag in V (in the B band, the amplitudes are greater). Spectral type at maximum light is F; at minimum, the types are G-K. The longer the period of light variation, the later is the spectral type. The maximum of the surface-layer expansion velocity almost coinciding with maximum light.
Sub-type:
- Cepheids (TU Cas, V 367 Sct) displaying the presence of two or more simultaneously operating pulsation modes (usually the fundamental tone with the period P0 and the first overtone P1). The periods P0 are in the range from 2 to 7 days, with the ratio P1/P0 approx. 0.71.
Cepheid variable star
Cepheid
S-type Star
S*
S*
S-type Star
s##type##stype##star##sstar
Optically Violently Variable Object
OVV##Optically##Variable##Object
OVV
OVV
Optically Violently Variable Object
II
Light Curve
light##curve
M Star
m##star##mstar
Star of Spectral Type M
cosmological##lensing
Cosmological Lensing
E
Giant Elliptical Galaxy
giant##elliptical##galaxy##gal##galaxies
non##not##periodic##process
PartofG
Part Of Galaxy
Part of Galaxy
part##of##galaxy
PoG
EM Source
em##source##electromagnetic##electro##magnetic
Neutral Gas
neutral##gas
flare##star##flarestar
Flare Star
Flare*
Flare Star
Stars, flare
Eruptive variables varying in brightness because of flares occurring in their chromospheres and coronae.
Sub-types:
- Orion variables of late (K-M) spectral types
- Eruptive variables of the UV Ceti type, these are K Ve-M Ve stars sometimes displaying flare activity with amplitudes from several tenths of a magnitude up to 6 mag in V. The amplitude is considerably greater in the ultraviolet spectral region. Maximum light is attained in several seconds or dozens of seconds after the beginning of a flare; the star returns to its normal brightness in several minutes or dozens of minutes.
- Flaring Orion variables of spectral types Ke-Me. These are phenomenologically almost identical to UV Cet variables observed in the solar neighborhood. In addition to being related to nebulae, they are normally characterized by being of earlier spectral type and greater luminosity, with slower development of flares (V389 Ori).
- BY Draconis-type (rotating) variables, which are emission-line dwarfs of dKe-dMe spectral type showing quasiperiodic light changes with periods from a fraction of a day to 120 days and amplitudes from several hundredths to 0.5 mag in V. The light variability is caused by axial rotation of a star with a variable degree of nonuniformity of the surface brightness (spots) and chromospheric activity. Some of these stars also show flares similar to those of UV Cet stars, and in those cases they also belong to the latter type and are simultaneously considered eruptive variables.
Fl*
Radio
Radio
radio
radio##quiet##agn
Radio-quiet AGN
mul
A composite object is made of at least two distinct astronomical objects
Compound object
multiple_object
2
compound##composite##object
Sy2
Seyfert_2
Seyfert 2 Galaxy
seyfert##seyfert2##2##galaxy
Seyfert 2 Galaxy
Blazar
Blazar
Bla
Blazar
Blazar
GlC
globular##cluster##star##stars
Globular_Clusters
GlCl
Globular Cluster
Clusters, globular
stellar##black##hole
Stellar Black Hole
Galaxies, peculiar
Peculiar Galaxy
peculiar##gal##galaxy##galaxies
small##separation##lobes##radio
Close
close
Extremely Red Object
Extremely Red Obejct
ERO
extremely##red##object
RedExtreme
A
EUV
magnetar##pulsar##magnetic##field
Magnetar
flux##ratio
Flux Ratio
Lensed Galaxy
lensed##gravitationnal##gal##galaxy##galaxies
LeG
LensedG
Gravitationnaly Lensed Image of a Galaxy
Redshifts
Redshift
redshift##red##shift
Redshifts
-12 < value < 12
Cluster of Stars
Cl*
3
Cl*
cluster##star##stars
bC*
BCEP
PulsV*bCep
Beta Cephei Variable
Variables of the Beta Cephei type (Beta Cep, Beta CMa), which are pulsating O8-B6 I-V stars with periods of light and radial-velocity variations in the range of 0.1 - 0.6 days and light amplitudes from 0.01 to 0.3 mag in V. The light curves are similar in shape to average radial-velocity curves but lag in phase by a quarter of the period, so that maximum brightness corresponds to maximum contraction, i.e., to minimum stellar radius. The majority of these stars probably show radial pulsations, but some (V649 Per) display nonradial pulsations; multiperiodicity is characteristic of many of these stars.
Sub-type:
- A short-period group of Beta Cep variables. The spectral types are B2-B3 IV-V; periods and light amplitudes are in the ranges 0.02 - 0.04 days and 0.015 - 0.025 days, respectively, i.e., an order of magnitude smaller than the normally observed ones.
cephei##cep##beta##cepheid##cma
Variable of the Beta Cep type
Be Star
Stars, Be
Be*
Be*
Be Star
be##star##bestar
Velocity dispersion
Eclipsing Binary of Algol type
Algol Eclipsing Binary
eclipsing##binary##star##algol##beta##persei
Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes.
EB*Algol
Al*
EA
S0##S0a
shockwave##shock##wave
Shockwave
The shockwave-generating process or the resulting Shockwave
HH
Herbig-Haro Object
herbig##haro##herbigharo##object
HH
accreting##white##wd##dwarf
Accreting White Dwarf
O Star
o##star##ostar
Stars, O
Star of Spectral Type O
Power Radio Mhz
power##radio##mhz##powerradiomhz##radiomhz
Variables of the W Virginis type. These are pulsating variables of the galactic spherical component (old disk) population with periods of approximately 0.8 to 35 days and amplitudes from 0.3 to 1.2 mag in V. They obey a period-luminosity relation different from that for Delta Cep variables. For an equal period value, the W Vir variables are fainter than the Delta Cep stars by 0.7 - 2 mag. The light curves of W Vir variables for some period intervals differ from those of Delta Cep variables for corresponding periods either by amplitudes or by the presence of humps on their descending branches, sometimes turning into broad flat maxima. W Vir variables are present in globular clusters and at high galactic latitudes.
Variable Star of W Vir type
W Virginis Variable Star
PulsV*WVir
WV*
CW
w##virginis##wvirginis##type##variable##star
part##of##cloud
PartofCloud
PoC
Part Of Cloud
is component of
Indicates that the DOMAIN AstrObject is a direct physical component of the RANGE CompositeObject (not a component of a component of the RANGE CompositeObject)
has among its portions
Indicates that the RANGE AstroPortion can be found whithin the DOMAIN CompoundObject or AstroPortion
Indicates that an astronomical object is the location of a Process/has an attached process
has among its processes
has among its measurements
Indicates that the DOMAIN AstrObject has the RANGE Measurement among its (observational) measurements
features an abundance of
is class of
is morphology of
features absorption spectral line(s) for
is a member of the class:
features emission spectral line(s) for
Indicates the Progenitor of a Supernova
has for progenitor
has among its (direct) components
Indicates that the DOMAIN CompoundObject has the RANGE AstrObject among its direct physical components (the RANGE AstrObject cannot be a component of a component of the composite object)
is portion of
features a noticeable emission in
Indicates what ionizes the gas of a given ISM
is ionized by
is measured for
features high measurement(s) for
Indicates that an astronomical object has a related (observational) measurement which value is considered as high
has among its morphological features
the unit associated with the value of an instance of measturement (this annotation should be used only if there actually is a unit)
The operators and values for an instance (of measurement), format is either operator1##value1##operator2##value2, or operator##value if there is only one value
Short code in Simbad's object classification
Main part of the spectral type in SIMBAD (letters only, found at the beginning of SIMBAD's spectral type value)
GCVS code(s) corresponding to a concept of the ontology
tests that should be taken care of outside of the ontology (e.g. check that a value is within sensible boundaries)
textual description/definition of a concept
Standard name in Simbad's object classification
morphological type for galaxies in SIMBAD
name in natural language for display purposes
VizieR keyword corresponding to an item of the ontology
Main part of the luminosity class in SIMBAD (letters only, found within SIMBAD's spectral type value after said spectral type)
keywords for (text) search purposes