The applications of the MHD Alfvén wave oscillation model for kHz quasi-periodic oscillations

Details The applications of the MHD Alfvén wave oscillation model for kHz quasi-periodic oscillations The applications of the MHD Alfvén wave oscillation model for kHz quasi-periodic oscillations

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007an....328..491z&link_type=abstract

Astronomische Nachrichten, Vol.328, Issue 6, p.491

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5

Accretion: Accretion Disks, Stars: Neutron, Binaries: Close, X-Rays: Binaries, X-Rays: Stars

Scientific paper

In this paper, we improve the previous work on the MHD Alfvén wave oscillation model for the neutron star (NS) kHz quasi-periodic oscillations (QPOs), and compare the model with the updated twin kHz QPO data. For the 17 NS X-ray sources with the simultaneously detected twin kHz QPO frequencies, the stellar mass M and radius R constraints are given by means of the derived parameter A in the model, which is associated with the averaged mass density of the star as { < ρ R_An = 3M/(4π R3) ≃ 2.4× 1014 (A/0.7)2} g/cm3, and we also compare the M-R constraints with the stellar equations of state. Moreover, we also discuss the theoretical maximum kHz QPO frequency and maximum twin peak separation, and some expectations on SAX J1808.4-3658 are mentioned, such as its highest kHz QPO frequency ˜ 870 Hz, which is about 1.4-1.5 times less than those of the other known kHz QPO sources. The estimated magnetic fields for both Z sources (about Eddington accretion rate \dot {M}Edd) and Atoll sources (˜ 1% \dot {M}Edd) are approximately ˜ 10^9 G and ˜ 10^8 G, respectively.

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