V455 And
V515 And
AE Aqr
FO Aqr
XY Ari
V405 Aur
V647 Aur
HT Cam
MU Cam
DW Cnc
V709 Cas
V1033 Cas
V1025 Cen
TV Col
TX Col
UU Col
V2069 Cyg
V2306 Cyg
YY Dra
PQ Gem
V418 Gem
DQ Her
V1323 Her
EX Hya
NY Lup
V2400 Oph
V2731 Oph
V598 Peg
GK Per
AO Psc
V667 Pup
WX Pyx
V1223 Sgr
CC Scl
V1062 Tau
AX J1740.1
AX J1740.2
AX J1853.3
IGR J08390
IGR J15094
IGR J16500
IGR J16547
IGR J17195
IGR J18173
IGR J18308
IGR 19267
RX J2133

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Semena et al. 2014

Bibinfo (this paper at ADS)
Semena, A.N., Revnivtsev, M.G., Buckley, D.A.H., Kotze, M.M. Khabibullin, I.I., Breytenbach, H., Gulbis, A.A.S, Coppejans, R., Potter, S.B. 2014, MNRAS, 442, 1123-1132.
Observational: Optical photometry.
EX Hya.
On the assumption that the lack of 2-s QPOs in EX Hya is due to short cooling time, the optical power spectrum can be interpreted as to imply the cooling time-scale of less than 0.3-0.5 s, implying a very small footprint of the accretion region and a very high specific accretion rate (conclusions contrary to well-established studies of this source).

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