Journal
ASTROPHYSICAL JOURNAL
Volume 722, Issue 2, Pages 1816-1820Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/722/2/1816
Keywords
accretion, accretion disks; binaries: close; stars: individual (Holmberg IX X-1); X-rays: binaries
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Funding
- National Science Council of the Republic of China (Taiwan) [NSC 96-2112-M-007-037-MY3]
- Kenda Foundation
- European Community [ITN 215212]
- NSFC [10903004, 10978001]
- 973 program [2009CB824800]
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Holmberg IX X-1 is a well-known ultraluminous X-ray source with an X-ray luminosity of similar to 10(40) erg s(-1). The source has been monitored by the X-ray telescope of Swift regularly. Since 2009 April, the source has been in an extended low luminosity state. We utilize the co-added spectra taken at different luminosity states to study the spectral behavior of the source. Simple power-law and multi-color disk blackbody models can be ruled out. The best overall fits, however, are provided by a dual thermal model with a cool blackbody and a warm disk blackbody. This suggests that Holmberg IX X-1 may be a 10 M-circle dot black hole accreting at seven times above the Eddington limit or a 100 M-circle dot maximally rotating black hole accreting at the Eddington limit, and we are observing both the inner regions of the accretion disk and outflows from the compact object.
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