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The possible origin of high frequency quasi-periodic oscillations in low mass X-ray binaries

Published online by Cambridge University Press:  30 December 2019

Chang Sheng Shi Open the ORCID record for Chang Sheng Shi [Opens in a new window] ,
Shuang Nan Zhang  and
Xiang Dong Li
Chang Sheng Shi
Affiliation:
College of Material Science and Chemical Engineering, Hainan University, Hainan 570228, China email: [email protected] Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210046, China
Shuang Nan Zhang
Affiliation:
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China Department of Astronomy, Nanjing University, Nanjing 210046, China; National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Xiang Dong Li
Affiliation:
Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210046, China Department of Astronomy, Nanjing University, Nanjing 210046, China;
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Abstract

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We summarize our model that high frequency quasi-periodic oscillations (QPOs) both in the neutron star low mass X-ray binaries (NS-LMXBs) and black hole LMXBs may originate from magnetohydrodynamic (MHD) waves. Based on the MHD model in NS-LMXBs, the explanation of the parallel tracks is presented. The slowly varying effective surface magnetic field of a NS leads to the shift of parallel tracks of QPOs in NS-LMXBs. In the study of kilohertz (kHz) QPOs in NS-LMXBs, we obtain a simple power-law relation between the kHz QPO frequencies and the combined parameter of accretion rate and the effective surface magnetic field. Based on the MHD model in BH-LMXBs, we suggest that two stable modes of the Alfv́en waves in the accretion disks with a toroidal magnetic field may lead to the double high frequency QPOs. This model, in which the effect of the general relativity in BH-LMXBs is considered, naturally accounts for the 3:2 relation for the upper and lower frequencies of the QPOs and the relation between the BH mass and QPO frequency.

Keywords

accretionaccretion disksMHDX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 277 - 280
Copyright
© International Astronomical Union 2019 

References

Abramowicz, M. A., Bulik, T., Bursa, M., & Kluźniak, W. 2003, A&A, 404, L21 Google Scholar
Abramowicz, M. A., & Kluźniak, W. 2001, A&A, 374, L19 Google Scholar
Barret, D., Kluźniak, W., Olive, J. F., Paltani, S., & Skinner, G. K. 2005, MNRAS, 357, 1288 10.1111/j.1365-2966.2005.08734.xCrossRefGoogle Scholar
Begelman, M. C., & Pringle, J. E. 2007, MNRAS, 375, 1070 10.1111/j.1365-2966.2006.11372.xCrossRefGoogle Scholar
De Villiers, J. P., & Hawley, J. F. 2003, ApJ, 589, 458 10.1086/373949CrossRefGoogle Scholar
Erkut, M. H., Psaltis, D., Alpar, M. A. 2008, ApJ, 687, 1220 10.1086/592142CrossRefGoogle Scholar
James, M., Paul, B., Devasia, J., & Indulekha, K. 2010, MNRAS, 407, 285 10.1111/j.1365-2966.2010.16880.xCrossRefGoogle Scholar
Li, X.-D., & Zhang, C.-M. 2005, ApJL, 635, L57 10.1086/499204CrossRefGoogle Scholar
Miller, M. C., Lamb, F. K., & Psaltis, D. 1998, ApJ, 508, 791 CrossRefGoogle Scholar
Osherovich, V., & Titarchuk, L. 1999, ApJL, 522, L113 10.1086/312225CrossRefGoogle Scholar
Parthasarathy, V., Kluźniak, W., čemeljić, M. 2017, MNRAS, 470, L34 CrossRefGoogle Scholar
Shi, C.-S. 2011, Research in Astronomy and Astrophysics, 11, 1327 CrossRefGoogle Scholar
Shi, C.-S., & Li, X.-D. 2010, ApJ, 714, 1227 10.1088/0004-637X/714/2/1227CrossRefGoogle Scholar
Shi, C.-S., Zhang, S.-N., & Li, X.-D. 2014, ApJ, 791, 16 10.1088/0004-637X/791/1/16CrossRefGoogle Scholar
Shi, C. 2010, Science China Physics, Mechanics, and Astronomy, 53, 247 10.1007/s11433-010-0042-0CrossRefGoogle Scholar
Shi, C., & Li, X.-D. 2009, MARAS, 392, 264 10.1111/j.1365-2966.2008.14041.xCrossRefGoogle Scholar
Stella, L., & Vietri, M. 1999, Physical Review Letters, 82, 17 10.1103/PhysRevLett.82.17CrossRefGoogle Scholar
Strohmayer, T. E., Zhang, W., Swank, J. H., et al. 1996, ApJL, 469, L9 CrossRefGoogle Scholar
van der Klis, M. 2006, in: Lewin, W. & van der Klis, M. (eds.), Compact stellar X-ray sources, Cambridge Astrophysics Series No. 39 (Cambridge, UK: Cambridge University Press), p. 39 10.1017/CBO9780511536281.003CrossRefGoogle Scholar
Zhang, C. 2004, A&A, 423, 401 Google Scholar