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Disk–Wind Connection during the Heartbeats of GRS 1915+105

Zoghbi, Abderahmen and Miller, J. M. and King, A. L. and Miller, M. C. and Proga, D. and Kallman, T. and Fabian, A. C. and Harrison, F. A. and Kaastra, J. and Raymond, J. and Reynolds, C. S. and Boggs, S. E. and Christensen, F. E. and Craig, W. and Hailey, C. J. and Stern, D. and Zhang, W. W. (2016) Disk–Wind Connection during the Heartbeats of GRS 1915+105. Astrophysical Journal, 833 (2). Art. No. 165. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20161216-100202166

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Abstract

Disk and wind signatures are seen in the soft state of Galactic black holes, while the jet is seen in the hard state. Here we study the disk–wind connection in the ρ class of variability in GRS 1915+105 using a joint NuSTAR–Chandra observation. The source shows 50 s limit cycle oscillations. By including new information provided by the reflection spectrum and using phase-resolved spectroscopy, we find that the change in the inner disk inferred from the blackbody emission is not matched by reflection measurements. The latter is almost constant, independent of the continuum model. The two radii are comparable only if the disk temperature color correction factor changes, an effect that could be due to the changing opacity of the disk caused by changes in metal abundances. The disk inclination is similar to that inferred from the jet axis, and oscillates by ~10°. The simultaneous Chandra data show the presence of two wind components with velocities between 500 and 5000 km s^(−1), and possibly two more with velocities reaching 20,000 km s^(−1) (~0.06 c). The column densities are ~5 × 10^(22) cm^(−2). An upper limit to the wind response time of 2 s is measured, implying a launch radius of <6 × 10^(10) cm. The changes in wind velocity and absorbed flux require the geometry of the wind to change during the oscillations, constraining the wind to be launched from a distance of 290–1300 r_g from the black hole. Both data sets support fundamental model predictions in which a bulge originates in the inner disk and moves outward as the instability progresses.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-4357/833/2/165DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/833/2/165/metaPublisherArticle
https://arxiv.org/abs/1610.05772arXivDiscussion Paper
ORCID:
AuthorORCID
Kallman, T.0000-0002-5779-6906
Harrison, F. A.0000-0003-2992-8024
Boggs, S. E.0000-0001-9567-4224
Stern, D.0000-0003-2686-9241
Additional Information:© 2016 The American Astronomical Society. Received 2016 April 13; revised 2016 September 27; accepted 2016 October 17; published 2016 December 15. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work is also based on observations made by the Chandra X-ray Observatory.
Group:Space Radiation Laboratory, NuSTAR
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:accretion, accretion disks – instabilities – X-rays: binaries – X-rays: individual (GRS 1915+105)
Record Number:CaltechAUTHORS:20161216-100202166
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20161216-100202166
Official Citation:Abderahmen Zoghbi et al 2016 ApJ 833 165
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72906
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:16 Dec 2016 18:40
Last Modified:22 Apr 2019 23:06

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