******************************************************** * * * DESCRIPTION OF TABLE HEADINGS AND OF ABBREVIATIONS * * * * (ONLINE VERSION) * * * ******************************************************** Object Name: Wherever possible, the designation of the object given in the General Catalogue of Variable Stars is used here. Altern.Name: is a frequently used alternative name. Further alternative designations are given in the "Who's Who ?" section. Coordinates: First row right ascension (J2000) in hrs min sec Second row declination (J2000) in deg ' " The coordinates are given in the following format: right ascension: HH MM SS.S declination : DDD MM SS A In the declination field, "A" is the accuracy of of the coordinates in seconds of arc (written as a hexadecimal number, i.e. 10" = a , 11" = b , 12" = c , 13" = d , 14" = e , 15" = f). In a case where "A" > 15" or where the accuracy of the co- ordinates is not known, the "A"-field is left blank. Type: (first and second row), the object type is coarsely characterised using the following abbreviations: AC = AM CVn star, spectrum devoid of hydrogen lines, subtype of NL AM = polar = AM Her system, subtype of NL, contains a synchronously rotating, magnetized white dwarf AS = subtype of AM, with a slowly asynchronously rotating, magnetized white dwarf AS = atoll source, subtype of the LMXBs BH = black hole candidate, subtype of the LMXBs CP = coherent pulsator, contains a coherently pulsating white dwarf DC = source with an accretion disc corona, subtype of the LMXBs DD = system consists of two degenerate components DN = dwarf nova DQ = DQ Her star, contains a non-synchronously rotating, magnetized white dwarf; usually not seen in X-rays DS = detached system ER = ER UMa star = SU UMa star with an extremely short supercycle GC = source in a globular cluster IP = intermediate polar, shows coherent X-ray period from a non-synchronously spinning, magnetized white dwarf; usually a strong X-ray source N = classical nova Na = fast nova (decline from max. by 3 mag. in less than about 100 days) Nb = slow nova (decline from max. by 3 mag. in more than about 100 days) Nc = extremely slow nova (typical time scale of the decline from maximum: decades) NL = nova-like variable Nr = recurrent nova PN = central star of a planetary nebula SH = non-SU UMa star showing either permanent or transient superhumps SS = supersoft X-ray source; CV with stationary hydrogen burning on the white dwarf SU = SU UMa star, subtype of DN SW = SW Sex star, subtype of NL UG = dwarf nova of either U Gem or SS Cyg subtype UX = UX UMa star, subtype of NL VY = VY Scl star (anti dawrf nova), subtype of NL WZ = WZ Sge star = SU UMa star with an extremely long supercycle XB = X-ray burst source XP = X-ray pulsar XT = transient X-ray source ZC = Z Cam star, subtype of DN ZS = Z-source, subtype of the LMXBs Mag1, Mag3 Mag2, Mag4: apparent V magnitude (B magnitude if followed by B) with the following meaning: Mag1 = maximum brightness of novae (N,Na,Nb,Nc,Nr) in minimum DN (UG,ZC,SU) in minimum NL (UX,AC) in normal state NL (AM,VY) in high state XT in quiescence DS outside eclipse Mag2 = minimum brightness, in case of eclipses magn. at mideclipse, of novae (N,Na,Nb,Nc,Nr) in minimum DN (UG,ZC,SU) in minimum NL (UX,AC) in normal state NL (AM,VY) in high state XT in quiescence DS Mag3 = maximum brightness of novae (N,Na,Nb,Nc,Nr) in outburst DN (UG,ZC) in outburst DN (SU) in normal outburst NL (AM,VY) in low state NL (DQ,IP) in flaring state XL (XB,XT) in outburst Mag4 = brightness of ZC in standstill SU in superoutburst = minimum brightness of NL (AM,VY) in low state T1: for DN (UG,ZC), the typical time interval (in days) between two subsequent outbursts for DN (SU), the typical time interval (in days) between two subsequent normal outbursts for XT, the typical time interval (in days) between two subsequent X-ray active states T2: for DN (SU), the typical time interval (in days) between two subsequent superoutbursts Lx/Lo: for LMXBs, the ratio of X-ray to optical luminosity Orb.Per.: orbital period (in days), in case of object type DQ: the spectroscopic period is given here if it is different from the photometric one. SU: if followed by *, the orbital period has been estimated from the known superhump period using the empirical relation given by B. Stolz and R. Schoembs (1984, A&A 132, 187). 2. Per.: second period, in case of object type DQ or IP: photometric period (in days), if it is different from the spectroscopic one. AM: polarization period (in days) = spin period of the white dwarf, if it is different from the presumed orbital period (subtype AS). SU: superhump period (in days), wherever possible, at the beginning of a superoutburst. SH: photometric period (in days), presumably superhump period of either permanent or transient superhumps. DS: spin period (in seconds) of the accretor (white dwarf or neutron star). 3. Per. 4. Per.: additional periods in the system (in seconds), in case of object type CP: 3. Per. = period of coherent pulsation, (transient if followed by T). 4. Per. = second period of coherent pulsation, (transient if followed by T). DQ: 3. Per. = spin period of the white dwarf. 4. Per. = additional period, presumably due to reprocessed X-Rays. IP: 3. Per. = spin period of the white dwarf, usually detected in X-Rays. 4. Per. = additional period, usually seen in the optical and presumably due to reprocessed X-Rays. XP: 3. Per. = pulse period of the pulsar. 4. Per. = optical period, presumably due to reprocessed X-Rays. The occurrence of transient quasi-periodic oscill- ations (QPO) in objects of type N, DN, NL, and in LMXBs is indicated either in the field "3. Per." or "4. Per", as space allows. EB: indicates the occurrence of eclipses if blank no eclipses observed if 1 1 eclipse per orbital revolution observed if 2 2 eclipses per orbital revolution observed if D periodic eclipse-like dips observed SB: type of spectroscopic binary if 1 single-line spectroscopic binary if 2 double-line spectroscopic binary Spectr2: spectral type of the secondary Spectr1: spectral type of the primary the number to the right of the slash indicates the luminosity class , i.e. I = 1 II = 2 III = 3 IV = 4 V = 5 VI = 6 e: first row eccentricity of the orbit second row the corresponding error M1/M2: first row mass ratio M1/M2 second row the corresponding error Incl: first row orbital inclination (in degrees) second row the corresponding error M1: first row mass of the primary (in solar masses) second row the corresponding error R1: first row radius of the primary (in solar radii) second row the corresponding error M2: first row mass of the secondary (in solar masses) second row the corresponding error R2: first row radius of the secondary (in solar radii) second row the corresponding error Uncertain values are followed by a colon.