Timing and Spectral Properties of Neutron Star Low-Mass X-ray Binaries Sudip Bhattacharyya Department of Astronomy and Astrophysics Tata Institute of Fundamental.

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Presentation transcript:

Timing and Spectral Properties of Neutron Star Low-Mass X-ray Binaries Sudip Bhattacharyya Department of Astronomy and Astrophysics Tata Institute of Fundamental Research

Different types of NS LMXBs Atoll and Z sources are identified by their tracks in the colour-colour diagrams (CDs) and hardness-intensity diagrams (HIDs). Soft colour: background –subtracted count rate ratio in two softer energy bands. Hard colour: background-subtracted count rate ratio in two harder energy bands. Typical Rossi X-ray Timing Explorer (RXTE) proportional counter array (PCA) energy bands: , , , (all in keV). van der Klis (2006)

Different types of NS LMXBs van der Klis (2006)

Energy spectrum of NS LMXBs Two emission components: accretion disk and NS surface: each of them can emit blackbody; each of them can be partially or fully covered with Comptonizing corona. No spectral model uniquely fits the data. NS LBXB XB : an example with RXTE PCA data Modelχ ν 2 (dof)Model χ ν 2 (dof) diskbb+comptt1.95(30)diskbb+powerlaw 1.95(32) diskbb+cutoffpl1.97(31)diskbb+bknpower 0.52(30) comptt+bbody1.50(30)powerlaw+bbody 2.24(32) cutoffpl+bbody1.65(31)bknpower+bbody 2.39(30) diskbb+bbody2.75(32)comptt+comptt 0.91(28) powerlaw+comptt0.95(30)cutoffpl+comptt 0.91(29) bknpower+comptt0.54(28)powerlaw+powerlaw 32.31(32) cutoffpl+powerlaw2.33(31)bknpower+powerlaw 3.47(30) cutoffpl+cutoffpl1.54(30)bknpower+cutoffpl 0.53(29) bknpower+bknpower3.73(28) Mukherjee and Bhattacharyya (2011)

NS LBXB XB : an example with RXTE PCA data Mukherjee and Bhattacharyya (2011)

Accreting pulsars

 : Orbital frequency r : Radial epicyclic frequency  : Vertical epicyclic frequency  - r : Periastron precession frequency  -  : Nodal or `Lense-Thirring’ precession frequency Kilohertz quasi-periodic oscillations (kHz QPOs) KHz QPOs often appear in a pair in the power spectrum, in the Hz frequency range. Fourier Transform Power spectrum is the Fourier transform of the intensity vs. time curve. This observationally robust timing feature have been detected from many neutron star LMXBs. According to almost all the models, the uniquely high kHz QPO frequencies are either the following accretion disk frequencies, or the beating or resonances among them, or with the neutron star spin frequency spin.

Kilohertz quasi-periodic oscillations (kHz QPOs) Accretion disk frequencies: So when the correct model is identified, kHz QPOs can be used to measure the neutron star parameters M and J. Miller et al. (1998) Such a constraint on the neutron star mass-radius space is possible, if one of the kHz QPO frequencies is , and the corresponding radial distance r is greater than or equal to the neutron star and the ISCO radius. Apart from neutron star parameter measurement, KHz QPOs can be useful to study the matter flow in strong gravity region, and to test a law of gravitation. For example, the general relativistic `Lense-Thirring’ precision (frequency:  -  ) has not yet been detected with certainty in any system.

KHz QPO quality factor vs. frequency: a signature of innermost stable circular orbit (ISCO)? Barret et al.

Spectral origin of kHz QPO: Comptonized component? Gilfanov et al. (2003)

Z sources: (1)Horizontal Branch Oscillations (HBO) : Hz (2)Normal Branch Oscillations (NBO) : about 6 Hz (3)Flaring Branch Oscillations (FBO) : about 10 Hz

Atoll sources: (1)Upper Banana (UB): < 1 Hz power law noise (VLFN) (2)Lower Banana (LB): 10 Hz BLN (3)Lower Left Banana (LLB): Twin kHz QPO (4)Island State (IS): Dominant BLN, becoming stronger and lower frequency as flux decreases

Power spectra in different states

Correlations among various timing features Van der Klis (2006)

ASTROSAT ( India’s proposed multiwavelength astronomy space mission ) In its time, only ASTROSAT will have the capability to study kHz QPOs. First detection and study of fast timing features in hard X-rays.

ASTROSAT ( India’s proposed multiwavelength astronomy space mission ) In its time, only ASTROSAT will have the capability to study kHz QPOs. First detection and study of fast timing features in hard X-rays. Thank you!