v 0.99y 2008-07-15 (Protégé 3.4 build 506) removed transitivity on hasComponent and isComponentOf (back to ALCIN) removed useless datatype property segment from annotation properties declarations (no datatype at all anymore) revamped disjoints radio##metric##m Radio Metric Binaries:cataclysmic Binaries, cataclysmic Cataclysmic Variable cataclysmic##variable##star##stars##binaries##binary##double##cv##variables 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. CataclyV* CV* yso##young##stellar##object##objects YSOs YSOs YSO Y*O YSO Nebular Continuum nebular##continuum Recombination thermal continuum Infrared Source Infrared sources ir##infrared##source IrS IR IR No* N nova##novae Nova Novae Nova Nova 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. Novae IV Synchrotron Emission emission synchrotron supernova##explosion##thermonuclear##thermo##nuclear Thermonuclear Supernova Explosion *inAssoc *iA Stellar Object in Association stellar##object##star##in##association##stars##objects##associations SB##SBa##SBb##SBc##SBd##SBab##SBbc##SBcd##SB0##SB0a Velocities Velocity Space velocities velocity association##star##stars##associations##ob##o##b Explosion or Eruption process Explosion or Eruption process eruption##explosion##process Galaxy in Group group##galaxy##gal##galaxies##in##g GinGroup GiG emission##process Emission Process Radio Centimetric radio##cm##centimetric type##1##type1##flat##spectrum##radio##quasar##qso Flat-Spectrum Radio Quasar Star of Spectral Type B B Star bstar##b##star##stars##bstars Stars, B-type High Mass X-Ray Binary 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. HXB HMXB x##ray##xray##binary##binaries##high##mass##hmxb#hmxrb High-mass X-ray Binary gamma##doradus##variable##variables##stars##star gammaDor Gamma Doradus Variable gD* Variable Star of gamma Dor type 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. magnetic##field Magnetic fields Magnetic_fields magnetic Field UV UV UV Source uv##ultraviolet##ultra##violet##source dE Cold HI Region hi##region##cold##regions HI HI Supernova type II supernova##supernovae##super##nova##novae##sn##supernovae##super##nova##novae##sn##typeii##type2##type##2##ii SNII Low Surface Brightness Galaxy LSB low##surface##brightness##lsb##gal##galaxy##galaxies##g LSB_G F Lenticular Galaxy lenticular##gal##galaxy##galaxies##g Far Infrared far##infrared Wavelength > 30 microns Blue blue 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. LXB Low Mass X-Ray Binary LMXB x##ray##xray##binary##binaries##low##mass##lmxb##lmxrb Low-mass X-ray Binary star##stars Star Neutron Star neutron##star##stars EUV EUV sources Extreme UV sources effective##temperature Effective temperatures Effective Temperature Blue Supergiant blue##super##giant##supergiant##giants##supergiants Core Dominated core##dominated##coredominated Core/Extented Flux Ratio >1 g##gstar##star##gstars##stars Star of Spectral Type G Stars, G-type G Star agn##radio##loud##active##galactic##nucleus##nuclei##galaxy Radio-loud AGN L Delta Scuti Variable Star 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. DSCT Variable Star of delta sct type delta##scuti##deltascuti##variable##variables##stars##star dS* PulsV*delsct Star of the early spectral types Stars, OB Early-type Star Stars:early-type early##type##star##earlytype##stars A star that is part of a double star Stellar Object in Double Star *in** *i* stellar##object##star##in##double##stars##objects component of the spacevelocity Proper Motion Proper motions Proper_Motions pm##proper##motion Rad Radio Radio sources RadioS Radio Source radio##source RR RRLyr RR* 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 Lyrae Variable rr##lyrae##variable##star##stars##variables##rrlyrae Variable Star of RR Lyr type Spectra, ultraviolet uv##ultraviolet##ultra##violet UV Ultraviolet Ultraviolet I Blue_objects Blue objects Blue Object Blue blue##object blu Blue* X X-ray Source X X-ray sources XRayS HI H I data HI (neutral) region HI Region HI hi##region##regions high##power##radio##loud##agn##active##galactic##nucleus##nuclei##highpower##radioloud##galaxy High-power Radio-loud AGN L-type Irregular Star l##ltype##type##irregular##stars##star Galaxy in Cluster of Galaxies cluster##in##galaxy##gal##galaxies##g Galaxy in Cluster GinCl GiC asteroid##asteroids Minor planets Asteroids Asteroid Red Giant red##redgiant##giant##redgiants##giants Assoc* Associations, stellar Associations AS* Association of Stars *Ass association##star##stars##associations Association of Stars Barred Spiral Galaxy barred##spiral##galaxy##gal##galaxies##g Seyfert Seyfert Galaxy Seyfert Galaxy Galaxies, Seyfert low##power##radio##quiet##agn##active##galaxy##nucleus##seyfert##galactic##nuclei##seyferts SyG Seyfert_Galaxies Varaible Star of BY Dra type 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 by##draconis##variable##star##stars##variables BYDra Stars, distances continuum Equivalent widths Multiplet Range allowing the description of the existence of a (noticeable) continuum for a given object Line Profiles Radio continuum Balmer lines Radio Lines Continuum space##velocity Space Velocity BL Lac-type Object BL_Lac_objects BLL BLLAC bllac##bl##Lac##object##lacertae##objects BLLac BLLac BL Lac objects Ir* Stars showing variations of irregular (non-periodic) type. Mostly (?) of eruptive type. irregular##variable##star##variables##stars Irregular_V* Variable Star of Irregular type Irregular Variable Star High-velocity Cloud HVC HVCld high##velocity##cloud##coulds##hvc##hvcld HVC (High Velocity Cloud) CH* CH Envelope-type Star ch##envelope##type##star CH Envelope-type Star CH* flux Flux line##width Line Width Starburst Process star##burst##starburst pulsating##variable##star##variables##stars Pulsating Star Pulsating Variable Star PulsV* Pu* 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. Polarization polarization Emission-line Galaxy emission##line##galaxy##gal##galaxies##g Emission-line galaxy EmG EmG large##separation##lobes##radio Large Separation Lobes Gamma-ray Source gam GammaS gamma gamma##ray##source pulsation##process Pulsation Process Sy1 Seyfert_1 seyfert##seyfert1##1##low##power##radio##quiet##agn##active##galaxy##nucleus##galactic##nuclei##seyferts Seyfert 1 Galaxy Seyfert 1 Galaxy Stellar Remnant stellar##remnant##remnants Galaxy with High Redshift HzG High_z_G high##redshift##galaxy##gal##galaxies##g Galaxy with high redshift Measurement measure##measurement##measures##measurements Measured observational parameters/properties Stars:variable Stars, variable V* V* variable##star##stellar##object##objects##variability##stars V* RS* RSCVn 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. Variable of RS CVn type RS Canum Venaticorum Variable Star RS rs##canum##venaticorum##cv##rscv##binary##binaries O Stars stellar##object##objects * Stellar Object Star * Galaxies, rotation Galaxies, UV-excess Galaxies, optical Galaxies Galaxies, Markarian Galaxies, spectra Galaxy Galaxies, photometry Galaxies, nearby Galaxies, IR Galaxy catalogs G Galaxies, optical G galaxy##gal##galaxies##g Photosphere photosphere Millimetric/submm sources Radio(sub-mm) smm sub##millimetric##submillimetric##radio##source Sub-millimetric Radio Source Ages Stars, ages Rotation Process rotation##process supernova##supernovae##super##nova##novae##sn##typeiib##type2b##type##2##ii##b##typeii##type2 Supernova type IIb High-mass Star high##mass##star##highmass##stars Surface Brightness s'applique aux objets étendus ( Gal/nebula) surface##brightness