- ... expected
- Figure 1 and Tables 2, 3 are only available in electronic form at http://www.edpsciences.org
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
- ...IRAF
- IRAF is distributed by the National
Optical Astronomy Observatories.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
- ...
star
- Using LHS399 from Sandy Leggett's library of M-dwarf
spectra, http://ftp.jach.hawaii.edu/ukirt/skl/dM.spectra/
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
- ...
h
- Ritter & Kolb (2003) list five U Gem-type
dwarf novae with
h: CC Cnc is a SU UMa-type dwarf nova
(Kato & Nogami 1997), and we included 587 Lyr, CF Gru, V544 Her,
and FS Aur as dwarf novae with no subtype (XX) due to the lack of
clear observational evidence for a specific subtype.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
- ...
range
- A note of caution among the WZ Sge stars, which mostly
have ultrashort-periods, concerns UZ Boo. Ritter & Kolb (2003)
list a period of
3 h based on quiescent photometry, which is
almost certainly wrong. Intensive time-series of the 2003 outburst of
UZ Boo revealed a superhump period of 89.3 min (Kato,
vsnet-campaign-dn 4064), and we use here this value as an estimate of
the orbital period.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
- ... polar
- Excluding the double-degenerate helium
CVs, which follow a different evolution channel that is not taken into
account in the population models of de Kool (1992) and
Politano (1996).
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.