X-Ray Observations of XTE J1550–564 during the Decay of the 2000 Outburst. II. Timing

Thumbnail Image

Files

Kalemci_2001_ApJ_563_239.pdf (413.43 KB)

Links to Files

https://iopscience.iop.org/article/10.1086/323690

Permanent Link

https://doi.org/10.1086/323690
 http://hdl.handle.net/11603/30120

Collections

UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
UMBC Physics Department

Author/Creator

Author/Creator ORCID

https://orcid.org/0000-0002-4656-6881

Date

2001-12-10

Type of Work

journal articles
Text

Department

Program

Citation of Original Publication

Kalemci, E., J. A. Tomsick, R. E. Rothschild, K. Pottschmidt, and P. Kaaret. “X-Ray Observations of XTE J1550–564 during the Decay of the 2000 Outburst. II. Timing.” The Astrophysical Journal 563, no. 1 (December 10, 2001): 239. https://doi.org/10.1086/323690.

Rights

This item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.

Subjects

Abstract

We investigate the timing behavior of XTE J1550-564 with the Rossi X-Ray Timing Explorer as the source made a transition to the hard state during the decay of the 2000 outburst. We detect a high-frequency quasi-periodic oscillation (QPO) at 65 Hz in one observation with a fractional rms amplitude of 4.9%. This is the first time that a high-frequency QPO has been detected in a transition to the hard state during outburst decay. We also observe low-frequency QPOs in the 0.36-4.1 Hz range and rich aperiodic variability. The changes in the temporal properties during the decay are very similar to the state transitions observed for other sources. We find a correlation between the low-frequency QPO and the break frequency in the continuum power spectra. We investigate the energy dependence of rms amplitudes of the QPOs. We compare these timing properties with those previously observed for XTE J1550-564 and other Galactic black hole candidates and discuss the implications for QPO models and black hole accretion.