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