@article{lambSonicPointSpinResonanceModel2003,
	title = {Sonic-{Point} and {Spin}-{Resonance} {Model} of the {Kilohertz} {QPO} {Pairs}},
	url = {http://adsabs.harvard.edu/abs/2003astro.ph..8179L},
	abstract = {KHz QPOs have now been detected in more than twenty accreting neutron stars in low-mass binary systems. Two kHz QPOs are usually detected in each star. Burst oscillations and two kHz QPOs have recently been detected in the 401 Hz accretion-powered X-ray pulsar SAX J1808.4-3658. In this star the frequency of the burst oscillation is approximately equal to the star's spin frequency nu\_spin whereas the frequency separation of the two kHz QPOs is approximately nu\_spin/2. If as expected the frequency of the burst oscillations in other stars is also approximately nu\_spin, the frequency separation is approximately nu\_spin in some stars but approximately nu\_spin/2 in others. A frequency separation approximately equal to nu\_spin/2 is unexplained in all existing models of the kHz QPOs. Here we propose a modified version of the sonic-point beat-frequency model that can explain within a single framework why the frequency separation is close to nu\_spin in some stars but close to nu\_spin/2 in others. As in the original sonic-point model, the frequency nu\_QPO2 of the upper kHz QPO is close to the orbital frequency nu\_orb at the radius r\_\{sp\} of the sonic point in the disk flow. We show that magnetic and radiation fields rotating with the star will preferentially excite vertical motions in the disk at the
"spin-resonance'' radius r\_\{sr\} where nu\_orb - nu\_spin is equal to the vertical epicyclic frequency, producing vertical motions in the disk that modulate the X-ray flux at approximately nu\_QPO2 - nu\_spin or approximately nu\_QPO2 - nu\_spin/2, depending on whether the disk flow at r\_\{sr\} is smooth or clumped. This sonic-point and spin-resonance model can also explain quantitatively the decrease of the kHz QPO frequency separation with increasing accretion rate that is observed in many sources.},
	urldate = {2020-01-24},
	journal = {arXiv Astrophysics e-prints},
	author = {Lamb, Frederick K. and Miller, M. Coleman},
	month = aug,
	year = {2003},
	keywords = {Astrophysics},
	pages = {arXiv:astro--ph/0308179},
}

{"_id":"GFSC5Gn65odGxGxRo","bibbaseid":"lamb-miller-sonicpointandspinresonancemodelofthekilohertzqpopairs-2003","author_short":["Lamb, F. K.","Miller, M. C."],"bibdata":{"bibtype":"article","type":"article","title":"Sonic-Point and Spin-Resonance Model of the Kilohertz QPO Pairs","url":"http://adsabs.harvard.edu/abs/2003astro.ph..8179L","abstract":"KHz QPOs have now been detected in more than twenty accreting neutron stars in low-mass binary systems. Two kHz QPOs are usually detected in each star. Burst oscillations and two kHz QPOs have recently been detected in the 401 Hz accretion-powered X-ray pulsar SAX J1808.4-3658. In this star the frequency of the burst oscillation is approximately equal to the star's spin frequency nu_spin whereas the frequency separation of the two kHz QPOs is approximately nu_spin/2. If as expected the frequency of the burst oscillations in other stars is also approximately nu_spin, the frequency separation is approximately nu_spin in some stars but approximately nu_spin/2 in others. A frequency separation approximately equal to nu_spin/2 is unexplained in all existing models of the kHz QPOs. Here we propose a modified version of the sonic-point beat-frequency model that can explain within a single framework why the frequency separation is close to nu_spin in some stars but close to nu_spin/2 in others. As in the original sonic-point model, the frequency nu_QPO2 of the upper kHz QPO is close to the orbital frequency nu_orb at the radius r_\\sp\\ of the sonic point in the disk flow. We show that magnetic and radiation fields rotating with the star will preferentially excite vertical motions in the disk at the \"spin-resonance'' radius r_\\sr\\ where nu_orb - nu_spin is equal to the vertical epicyclic frequency, producing vertical motions in the disk that modulate the X-ray flux at approximately nu_QPO2 - nu_spin or approximately nu_QPO2 - nu_spin/2, depending on whether the disk flow at r_\\sr\\ is smooth or clumped. This sonic-point and spin-resonance model can also explain quantitatively the decrease of the kHz QPO frequency separation with increasing accretion rate that is observed in many sources.","urldate":"2020-01-24","journal":"arXiv Astrophysics e-prints","author":[{"propositions":[],"lastnames":["Lamb"],"firstnames":["Frederick","K."],"suffixes":[]},{"propositions":[],"lastnames":["Miller"],"firstnames":["M.","Coleman"],"suffixes":[]}],"month":"August","year":"2003","keywords":"Astrophysics","pages":"arXiv:astro–ph/0308179","bibtex":"@article{lambSonicPointSpinResonanceModel2003,\n\ttitle = {Sonic-{Point} and {Spin}-{Resonance} {Model} of the {Kilohertz} {QPO} {Pairs}},\n\turl = {http://adsabs.harvard.edu/abs/2003astro.ph..8179L},\n\tabstract = {KHz QPOs have now been detected in more than twenty accreting neutron stars in low-mass binary systems. Two kHz QPOs are usually detected in each star. Burst oscillations and two kHz QPOs have recently been detected in the 401 Hz accretion-powered X-ray pulsar SAX J1808.4-3658. In this star the frequency of the burst oscillation is approximately equal to the star's spin frequency nu\\_spin whereas the frequency separation of the two kHz QPOs is approximately nu\\_spin/2. If as expected the frequency of the burst oscillations in other stars is also approximately nu\\_spin, the frequency separation is approximately nu\\_spin in some stars but approximately nu\\_spin/2 in others. A frequency separation approximately equal to nu\\_spin/2 is unexplained in all existing models of the kHz QPOs. Here we propose a modified version of the sonic-point beat-frequency model that can explain within a single framework why the frequency separation is close to nu\\_spin in some stars but close to nu\\_spin/2 in others. As in the original sonic-point model, the frequency nu\\_QPO2 of the upper kHz QPO is close to the orbital frequency nu\\_orb at the radius r\\_\\{sp\\} of the sonic point in the disk flow. We show that magnetic and radiation fields rotating with the star will preferentially excite vertical motions in the disk at the\n\"spin-resonance'' radius r\\_\\{sr\\} where nu\\_orb - nu\\_spin is equal to the vertical epicyclic frequency, producing vertical motions in the disk that modulate the X-ray flux at approximately nu\\_QPO2 - nu\\_spin or approximately nu\\_QPO2 - nu\\_spin/2, depending on whether the disk flow at r\\_\\{sr\\} is smooth or clumped. This sonic-point and spin-resonance model can also explain quantitatively the decrease of the kHz QPO frequency separation with increasing accretion rate that is observed in many sources.},\n\turldate = {2020-01-24},\n\tjournal = {arXiv Astrophysics e-prints},\n\tauthor = {Lamb, Frederick K. and Miller, M. Coleman},\n\tmonth = aug,\n\tyear = {2003},\n\tkeywords = {Astrophysics},\n\tpages = {arXiv:astro--ph/0308179},\n}\n\n","author_short":["Lamb, F. K.","Miller, M. C."],"key":"lambSonicPointSpinResonanceModel2003","id":"lambSonicPointSpinResonanceModel2003","bibbaseid":"lamb-miller-sonicpointandspinresonancemodelofthekilohertzqpopairs-2003","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2003astro.ph..8179L"},"keyword":["Astrophysics"],"metadata":{"authorlinks":{}},"html":""},"bibtype":"article","biburl":"https://bibbase.org/zotero/valepeirano","dataSources":["ftqMNtyNjLWewoxW9"],"keywords":["astrophysics"],"search_terms":["sonic","point","spin","resonance","model","kilohertz","qpo","pairs","lamb","miller"],"title":"Sonic-Point and Spin-Resonance Model of the Kilohertz QPO Pairs","year":2003}