IPs
AE Aqr
FO Aqr
XY Ari
V405 Aur
HT Cam
MU Cam
DW Cnc
BG CMi
V709 Cas
V1025 Cen
TV Col
TX Col
UU Col
V2306 Cyg
YY Dra
PQ Gem
DQ Her
EX Hya
NY Lup
V2400 Oph
GK Per
AO Psc
WX Pyx
V1223 Sgr
V1062 Tau
EI UMa
IGR 00234
IGR 15094
IGR 17303
Swift J0732
RX J0704
RX J1803
RX J2133
XSS 00564
|
Reimer et al. 2008
- Bibinfo (this paper at ADS)
- Reimer, T.W., Welsh, W.F., Mukai, K., Ringwald, F.A. 2008, ApJ, 678,
376-384.
- Type
- Observational: Optical and X-ray photometry.
- Object(s):
- EI UMa.
- Results
- Optical photometry reveals weak and sometimes undetectable signals at
746 and 770 s. Based on the repeat appearances at the same frequency,
it is argued that these represent the spin period (also seen in X-ray
data) and the spin-orbit sideband. EI UMa appears to have a high
accretion rate and a large magnetic moment.
Please send your comments, suggestions etc. to
Koji.Mukai@nasa.gov
and/or
Koji.Mukai@umbc.edu
|
