Ford, E. C.Kaaret, P.Chen, K.Tavani, M.Barret, D.Bloser, P.Grindlay, J.Harmon, B. A.Paciesas, W. S.Zhang, S. N.2019-09-251997Ford, E. C., P. Kaaret, K. Chen, M. Tavani, D. Barret, P. Bloser, J. Grindlay, B. A. Harmon, W. S. Paciesas, and S. N. Zhang. 1997. “Energy Spectra and High-Frequency Oscillations in 4U 0614+091.” The Astrophysical Journal 486 (1): L47–50. https://doi.org/10.1086/310827.0004-637X1538-4357http://nrs.harvard.edu/urn-3:HUL.InstRepos:41399740We investigate the behavior of the high-frequency quasi-periodic oscillations (QPOs) in 4U 0614+091, combining timing and spectral analyses of RXTE observations. The energy spectra of the source can be described by a power law (alpha similar to 2.8) and a blackbody (kT similar to 1.5 keV), with the blackbody accounting for 10%-20% of the total energy flux. We find a robust correlation of the frequency, v, of the higher frequency QPO near 1 kHz with the flux of the blackbody, F-BB The slope of this correlation, d log v/d log F-BB,, is 0.27-0.37. The source follows the same relation even in observations separated by several months. The QPO frequency does not have a similarly unique correlation with the total flux or the flux of the power-law component. The rms fraction of the higher frequency QPO rises with energy from 6.8% +/- 1.5% (3-5 keV) to 21.3% +/- 4.0% (10-12 keV). For the lower frequency QPO, however, it is consistent with a constant value of 5.4% +/- 0.9%. The results may be interpreted in terms of a beat-frequency model for the production of the high-frequency QPOs.en-USJournal Article2019-09-2510.1086/310827