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

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 ~1037-1038 erg/s, unpredictable, long

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

CD in HMXBs two branches HC makes the difference horizontal at low Lx diagonal at intermediate & high Lx HC makes the difference 4U 0115+63, EXO2030+375 & KS1947+300 as flux increases SC decreases, HC increases V 0332+53 SC decreases, HC decreases

‏

Hardness-Intensity Diagrams

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)1/2 Δ=FWHM/2

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

PSD in HMXBs Lb Ll LLF Ls

PSD in HMXBs Lb Ll LLF Ls

PSD in HMXBs Lb Ll Lu Lu'

PSD in HMXBs Lb Ll Lu

HMXB vs LMXB: similarities two different types 4U 0115+63, EXO 2030+375, KS1947+300 V 0332+53 (~ 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

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 ~ 0.001-0.1 Hz typically Ls noise associated with the pulse noise no apparent correlation between spectral parameters (characteristic frequencies, rms) Mdot