Samus N.N.
Moscow, the GCVS team
Along with the "+" sign (coexistence of two types), it is suggested to introduce the "|" sign (meaning "or") – for classification options for the same object, e.g. EC|Ell, EC|RR.
Pulsating variables
| Present: | Suggested: |
|---|---|
| ACYG | ACyg |
| BCEP, BCEPS | BCep (BCEPS, after Jakate, seem not justified) |
| CEP | Cep |
| DCEP, DCEPS, CEP(B) | DCep, DCep0, DCep1, DCepB01, DCepB12
Remark: 0 – fundamental, 1 – 1st overtone, 01 – fundamental plus overtone, 12 – 1st and 2nd overtones. For non-beat Cepheids, it is safer not to indicate the mode yet |
| CW, CWA, CWB | CW (period will also be given) |
| DSCT, DSCTC, SXPHE | DSct (amplitude will also be given, population membership is not always obvious) |
| L, LB, LC | L, Lb (for red stars) |
| M | M |
| PVTEL | PVTel |
| RR, RRAB, RRC, RR(B) | RR, RR0, RR1, RRB01 |
| RV, RVA, RVB | RV, RVb (if the secondary wave's amplitude is at least equal to that of the main oscillation) |
| SR, SRA, SRB, SRC, SRS | SR (the regularity level should be indicated by the presentation of the light elements; if a star is a supergiant, it will be obvious from its spectral type) |
| SRD | SRd (we feel not inclined to introduce the UU Her type) |
| ZZ, ZZA, ZZB, ZZO | ZZ (subtype is contained in the spectral type) |
| BLBOO | BLBoo |
| GDOR | GDor |
| RPHS | RPHS (rapidly pulsating hot subdwarfs. We repeat our call for suggestions of a better designation). |
| LPB or LBV | SPB |
| Present: | Suggested: |
|---|---|
| FU, I, IA, IB, INA, INB, INT, IT, IN(YY), IS, ISA, ISB | I, TT, TTc, TTw, HAeBe Remark: I is for irregulars with doubts about their being young, TTc for classical and TTw, for weak-lined T Tauri stars, HAeBe for Herbig Ae/Be stars |
| GCAS, BE | Be |
| RCB | RCB |
| RS | Move to rotating variables |
| SDOR | SDor |
| UV, UVN | UV |
| WR | WR |
| New type: PP (a proto-planetary object) | |
| New type: dL (L dwarf), the causes of variability not quite clear yet |
| Present: | Suggested: |
|---|---|
| ACV, SXARI | ACV |
| ACVO | roAp, ACV+roAp |
| BY | BY; also should include chromospherically active giants |
| ELL | Ell |
| FKCOM | FKCom |
| PSR | Psr |
| R | R |
| RS (earlier among eruptive) |
| Present: | Suggested: |
|---|---|
| No subtype: CV | |
| N, NA, NB | N, Nhf (final helium flash; suggestions of a different designation are welcome) |
| NR | Nr, NSym (symbiotic Nova), UGWZ (see below) |
| NC | NSym |
| NL | CV, UXUMa ("permanent outburst"), VY (VY Scl type, fadings from time to time) |
| SN, SNI, SNII | SN (to avoid introducing the current complex classification) |
| AM | AM (including XM from X-ray variables), DQ (intermediate polars) |
| UG, UGSS, UGZ | UG, UGSS, UGZ |
| UGSU | UGSU, UGWZ (WZ Sge type, extremely long supercycles, large amplitudes), UG_ER (ER UMa type, short supercycles and normal cycles, small amplitudes; ideas of a better abbreviation are welcome) |
| ZAND | Sym, NSym |
| Present: | Suggested: |
|---|---|
| E, EA, EB, EW, EP | E, EA, EC – contact (merging EB and EW), EP |
| PN, WD, WR | Remove from the classification, indicate through the spectral type or Remarks |
| RS | If such a star has eclipses, give notation like EA+RS, RS+EA |
| AR, D, DM, DS, DW, K, KE, KW, SD | Remove from the classification: as a rule, these types in the GCVS are based on indirect evidence |
| Present: | Suggested: |
|---|---|
| X, XB, XF, XI, XJ, XND, XNG, XP, XPR, XPRM, XM | AM (move to cataclysmics), X, XN, XNB (approximately corresponds to XNG, a B star orbiting a compact object), Xlm (low mass), Xhm (high mass), Xmq (microquasars). In this class, advice from experts is especially needed. |