Статья

DISK–WIND CONNECTION DURING THE HEARTBEATS OF GRS 1915+105

Abderahmen ZoghbiDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; [email protected]J. M. MïllerDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; [email protected]A. L. KingStanford UniversityM. Coleman MillerDepartment of Astronomy, University of Maryland, College Park, MD 20742-2421, USADaniel ProgaDepartment of Physics, University of Nevada, Las Vegas, Las Vegas, NV 89154, USAT. R. KallmanNASA Goddard Space Flight Center, Code 662, Greedbelt, MD 20771, USAA. C. FabianInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA, UKFiona A. HarrisonSpace Radiation Laboratory, California Institute of Technology, Pasadena, CA 91125, USAJ. S. KaastraDepartment of Physics and Astronomy, Universiteit Utrecht, P.O. Box 80000, 3508 TA Utrecht, The NetherlandsJ. C. RaymondHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAC. S. ReynoldsDepartment of Astronomy, University of Maryland, College Park, MD 20742-2421, USAS. E. BoggsSpace Science Laboratory, University of California, Berkeley, California 94720, USAFinn E. ChristensenDTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, DenmarkWilliam W. CraigSpace Science Laboratory, University of California, Berkeley, California 94720, USAC. J. HaileyColumbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USADaniel SternJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USAWW ZhangNASA Goddard Space Flight Center, Code 662, Greedbelt, MD 20771, USA

2016en

ABI

Аннотация

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.

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Идентификаторы

DOI: 10.3847/1538-4357/833/2/165

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Цитирований: 2Использованных источников: 0

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