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

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dc.creatorZhang, C. M.
dc.creatorYin, H. X.
dc.creatorZhao, Y. H.
dc.creatorChang, H. K.
dc.creatorSong, L. M.
dc.date2004-08-12
dc.date2007-01-30
dc.date.accessioned2026-07-07T10:27:17Z
dc.date.available2026-07-07T10:27:17Z
dc.descriptionIn this paper, we improve the previous work on the MHD Alfven 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 star as ${\rm \lan ρ\ran = 3M/(4πR^{3}) \simeq 2.4\times 10^{14} (g/cm^{3}) (A/0.7)^{2}}$, and we also compare the M-R constraints with the star equations of states. 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 $\sim$~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 $\med$) and Atoll sources ($ 1% \med$) are approximately $10^9$ G and $10^8$ G respectively.
dc.description8 pages, 3 figure accepted by Astronomische Nachrichten (AN), 2007
dc.identifierhttps://arxiv.org/abs/astro-ph/0408233
dc.identifierhttp://arxiv.org/abs/astro-ph/0408233
dc.identifierAstron.Nachr.328:475-482,2007
dc.identifierdoi:10.1002/asna.200710773
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/177107
dc.subjectAstrophysics
dc.titleThe applications of the MHD Alfven wave oscillation model for kHz quasi-periodic oscillations
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