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: http://www.sai.msu.su/gcvs/future/classif.htm
Дата изменения: Thu Oct 17 15:16:46 2013 Дата индексирования: Fri Feb 28 23:06:18 2014 Кодировка: Поисковые слова: accretion disk |
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. |