Re: [AAVSO-DIS] Question About the Variable Types in the Variable StarIndex
- Hi Gene
> Is there a list of the Variable Type field values in theNo, not that I know of.
> Variable Star Index?
> The reason I'm asking is because some of the eclipsingYour expectations are not correct !
> binaries I'm observing/planning to observe (U Cep, Beta Per,
> Epsilon Aur) have "EA" for the type and I expected to see "EB."
EB is the general acronym for "Eclipsing Binary".
But if a var type is meant, its defined as following:
EA = EBs of A = Algol subtype.
EB = EBs of B = beta Lyr subtype.
EW = EWs of W = W UMa subtype.
So giving the var type EA for all these EBs is correct.
Tricky, isn't it ? Sometimes even the experts might not know
if EB means "Eclipsing Binary" or "EB of beta Lyr subtype".
> Most also have a forward slash and a second abreviation.Most var types in the VSX originate from the GCVS.
> I seached for a complete list but couldn't find one. If
These are originally described here:
A short overview of var types by the ATNF:
Short list of var types by the ASSA:
Extended summary with light curves (LCs) by the AEOFV:
and GEA at:
HIP subset of GCVS var types:
If a var type is not in the above GCVS lists, its probably specific
for the paper/catalog that is given in the VXSX references. Some
of the additionally used var types are e.g. defined here:
Ritter & Kolb RKcat:
More modern pulsating var types:
2008CoAst.157..240J - The impact of asteroseismology on the theory
of stellar evolution - Jeffery, C. S.
Figure 1: Schematic Hertzsprung-Russell diagram showing the locus of
major classes of pulsating variable star.
IAUS 272 on Actives OB stars
Wolfgang Renz, Karlsruhe, Germany
> IAUS 272 on Actives OB starsThe SPB and BCEP descriptions in that webpage are interchanged. The longer
period stars are the SPB ones.
You can also add DPV's
Binary Be stars showing the orbital variability (EA, EB or ELL) superposed
to a longer term variation (30-40 times longer than the orbital period)
caused by the periodic formation and dissipation of a disk.
A couple of YSO (Young Stellar Objects) classes are (and can be defined as):
EX= EXors or Subfuors, subspecies of the FU class. They are named after EX
Lupi. They are eruptive T Tauri stars that show brightening episodes of
several magnitudes in time scales of several months or a few years. They
possibly represent an intermediate state between normal T Tauri stars and FU
Ori stars. (Examples: EX Lup, V1118 Ori, V1143 Ori)
UX= UXors (UX Ori stars). Herbig Ae/Be stars that show irregular variations
with a wide range of amplitudes from barely detectable to more than 4 mag in
V. Large-amplitude variability is confined to stars with spectral types
later than B8. There are two principal components: (1) irregular variations
on timescales of days around a mean brightness level that changes on a much
longer timescale (typically years), sometimes in a quasi-cyclic fashion, and
(2) occasional episodes of deep minima, occurring at irregular intervals but
more frequently near the low points of the brightness cycles (extracted from
ref. 0081) (Examples: UX Ori, CQ Tau, BF Ori)