1. Are there atoll/Z sources in HMXB
Are there atoll/Z sources in HMXB? A rapid aperiodic timing analysis of 4 accreting X-ray pulsars in outburst Pablo Reig IESL, Foundation for Research & Technology-HELLAS Astronomy Group, Physics Dept. University of Crete

2. Be/X-ray binaries HMXB Accreting X-ray pulsars Mainly transients
Be + NS
Accreting X-ray pulsars
Mainly transients
Two types of outbursts
Type I: Lx < 1037 erg/s, (quasi)periodic Porb, short
Type II: Lx ~ erg/s, unpredictable, long

3. CD in LMXBs
Atoll sources Z sources
van der Klis (2006)‏

4. CD in HMXBs two branches HC makes the difference horizontal at low Lx
diagonal at intermediate & high Lx
HC makes the difference
4U , EXO & KS
as flux increases
SC decreases, HC increases V
SC decreases, HC decreases

5. ‏

6. Hardness-Intensity Diagrams

7. PSD in LMXBs LLF Ll Lb' Lb'' Lb Lu Lb LLF Ll Lu
Atoll source
Z source
LLF Ll
Lb'
Lb'' Lb Lu
van Straaten et al. (2002)‏ Lb
LLF Ll Lu
Belloni et al. (2002)‏
νmax =(ν02 + Δ2)1/ Δ=FWHM/2

8. multi-Lorentzian profile
4 BLN (Lb, Ll, Lu, Lu’) & 2 PN ≈ QPO (LLF, Ls)
νb < νLF < νl < νu
νs ≈ νspin --> coupling periodic/aperiodic var.

9. PSD in HMXBs Lb Ll
LLF Ls

10. PSD in HMXBs Lb Ll
LLF Ls

11. PSD in HMXBs Lb Ll Lu
Lu'

12. PSD in HMXBs Lb Ll Lu

13. HMXB vs LMXB: similarities
two different types
4U , EXO , KS
V (~ Z)‏
spectral branches
smooth motion without jumps
horizontal branch
low flux & high rms
PSD: multi-Lorentzian
broad (zero-centred L) noise for low and high frequencies
peaked noise for intermediate frequencies

14. HMXB vs LMXB: differences
different topology
slower motion along the branches
hr-days in LMXBs, days-weeks in HMXBs
~ one order of magnitude longer time scales
mHz QPOs, ν ~ Hz typically
Ls noise
associated with the pulse noise
no apparent correlation between spectral parameters (characteristic frequencies, rms) Mdot