Orbital Sidebands in IPs

Orbital sidebands can appear in IPs for one of two reasons.

One is for matter to be accreted without first being assimilated into an axisymmetric disk - i.e., diskless or disk overflow accretion. This mechanism can create sidebands both in the optical and in the X-rays. One notable signature is the presence, in some cases, of 2\omega-\Omega sideband.

Diskless IP:
- V2400 Oph
Disk Overflow IPs (almost certainly incomplete):
- AO Psc (sometimes detected, undetectable with tight upper limits at other epochs)
- FO Aqr
- TX Col (beat period is dominant some of the time)
- BG CMi
- V1323 Her
- V1223 Sgr
- EX Hya during outburst

The other is reprocessing of the signal in a non-axisymmetric structure such as the secondary, the bright spot, or the non-axismmetric part of the outer disk in general. This only creates the sideband signal at longer wavelengths, usually the optical. The lack of, or the weakness of, the optical sideband signal implies either that the direct emission from the curtain dominates, or that the reprocessing is primarily in the axisymmetric part of the disk. In most IPs, the dominant signal is at the same periods in the X-rays and in the optical, implying the latter. Sideband-dominated IPs are:

Please send your comments, suggestions etc. to Koji.Mukai@nasa.gov and/or Koji.Mukai@umbc.edu

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Orbital Sidebands in IPs