Open AccessKilohertz quasi‐periodic oscillations difference frequency exceeds inferred spin frequency in 4U 1636−53
Author(s) -
Jonker Peter G.,
Méndez M.,
Klis M. van der
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05781.x
Subject(s) - physics , oscillation (cell signaling) , astrophysics , beat (acoustics) , quasi periodic , neutron star , low frequency , binary number , acoustics , astronomy , genetics , arithmetic , mathematics , biology
Recent observations of the low‐mass X‐ray binary 4U 1636−53 with the Rossi X‐ray Timing Explorer show, for the first time, a kilohertz quasi‐periodic oscillation (kHz QPO) peak separation that exceeds the neutron star spin frequency as inferred from burst oscillations. This strongly challenges the sonic‐point beat‐frequency model for the kHz QPOs found in low‐mass X‐ray binaries. We detect two simultaneous kHz QPOs with a frequency separation of 323.3 ± 4.3 Hz in an average Fourier power spectrum of observations obtained in 2001 September and 2002 January. The lower kHz QPO frequency varied between 644 and 769 Hz. In previous observations of this source the peak separation frequency was ∼250 Hz when the lower kHz QPO frequency was ∼900 Hz. Burst oscillations occur in 4U 1636−53 at ∼581 Hz and also possibly at half that frequency (290.5 Hz). This is the first source where the peak separation frequency is observed to change from less than (half) the burst oscillation frequency to more than that. This observation contradicts all previously formulated implementations of the sonic‐point beat‐frequency model except those where the disc in 4U 1636−53 switches from prograde to retrograde.