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Title: Black hole spin influence on accretion disk neutrino detection

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Publication Date:
Sponsoring Org.:
OSTI Identifier:
Grant/Contract Number:
FG02-02ER41216(GCM); SC0004786(GCM); SC0013039(RS)
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 93; Journal Issue: 12; Related Information: CHORUS Timestamp: 2016-06-23 11:10:07; Journal ID: ISSN 2470-0010
American Physical Society
Country of Publication:
United States

Citation Formats

Caballero, O. L., Zielinski, T., McLaughlin, G. C., and Surman, R.. Black hole spin influence on accretion disk neutrino detection. United States: N. p., 2016. Web. doi:10.1103/PhysRevD.93.123015.
Caballero, O. L., Zielinski, T., McLaughlin, G. C., & Surman, R.. Black hole spin influence on accretion disk neutrino detection. United States. doi:10.1103/PhysRevD.93.123015.
Caballero, O. L., Zielinski, T., McLaughlin, G. C., and Surman, R.. Wed . "Black hole spin influence on accretion disk neutrino detection". United States. doi:10.1103/PhysRevD.93.123015.
title = {Black hole spin influence on accretion disk neutrino detection},
author = {Caballero, O. L. and Zielinski, T. and McLaughlin, G. C. and Surman, R.},
abstractNote = {},
doi = {10.1103/PhysRevD.93.123015},
journal = {Physical Review D},
number = 12,
volume = 93,
place = {United States},
year = {Wed Jun 22 00:00:00 EDT 2016},
month = {Wed Jun 22 00:00:00 EDT 2016}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1103/PhysRevD.93.123015

Citation Metrics:
Cited by: 5works
Citation information provided by
Web of Science

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  • We examine neutrino oscillations in the context of an accretion disk surrounding a black hole. Because accretion disks produce large quantities of neutrinos, they may be home to interesting neutrino oscillation as well. We model accretion disks associated with stellar collapse for the sake of understanding neutrino oscillations. We find that the neutrino oscillations include phenomena seen in the protoneutron star setting as well as phenomena not seen elsewhere.
  • We re-examine archival Ginga data for the black hole binary system GS 1124–683, obtained when the system was undergoing its 1991 outburst. Our analysis estimates the dimensionless spin parameter a {sub *} = cJ/GM{sup 2} by fitting the X-ray continuum spectra obtained while the system was in the ''thermal dominant'' state. For likely values of mass and distance, we find the spin to be a{sub ∗}=−0.25{sub −0.64}{sup +0.05} (90% confidence), implying that the disk is retrograde (i.e., rotating antiparallel to the spin axis of the black hole). We note that this measurement would be better constrained if the distance tomore » the binary and the mass of the black hole were more accurately determined. This result is unaffected by the model used to fit the hard component of the spectrum. In order to be able to recover a prograde spin, the mass of the black hole would need to be at least 15.25 M {sub ☉}, or the distance would need to be less than 4.5 kpc, both of which disagree with previous determinations of the black hole mass and distance. If we allow f {sub col} to be free, we obtain no useful spin constraint. We discuss our results in the context of recent spin measurements and implications for jet production.« less
  • Neutrino emission significantly affects the evolution of the accretion tori formed in black hole-neutron star mergers. It removes energy from the disk, alters its composition, and provides a potential power source for a gamma-ray burst. To study these effects, simulations in general relativity with a hot microphysical equation of state (EOS) and neutrino feedback are needed. We present the first such simulation, using a neutrino leakage scheme for cooling to capture the most essential effects and considering a moderate mass (1.4 M{sub ☉} neutron star, 5.6 M{sub ☉} black hole), high-spin (black hole J/M {sup 2} = 0.9) system withmore » the K{sub 0} = 220 MeV Lattimer-Swesty EOS. We find that about 0.08 M{sub ☉} of nuclear matter is ejected from the system, while another 0.3 M{sub ☉} forms a hot, compact accretion disk. The primary effects of the escaping neutrinos are (1) to make the disk much denser and more compact, (2) to cause the average electron fraction Y{sub e} of the disk to rise to about 0.2 and then gradually decrease again, and (3) to gradually cool the disk. The disk is initially hot (T ∼ 6 MeV) and luminous in neutrinos (L{sub ν} ∼ 10{sup 54} erg s{sup –1}), but the neutrino luminosity decreases by an order of magnitude over 50 ms of post-merger evolution.« less
  • The observed iron K{alpha} fluorescence lines in Seyfert I galaxies provide strong evidence for an accretion disk near a supermassive black hole as a source of the line emission. These lines serve as powerful probes for examining the structure of inner regions of accretion disks. Previous studies of line emission have considered only geometrically thin disks, where the gas moves along geodesics in the equatorial plane of a black hole. Here we extend this work to consider the effects on line profiles from finite disk thickness, radial accretion flow, and turbulence. We adopt the Novikov{endash}Thorne {alpha}-disk model and find thatmore » within this framework turbulent broadening is the dominant new effect. The most prominent change in the skewed, double-horned line profiles is a substantial reduction in the maximum flux at both red and blue peaks. The effect is most pronounced when the inclination angle is large and when the accretion rate is high. Thus, the effects discussed here may be important for future detailed modeling of high-quality observational data. {copyright} {ital {copyright} 1998.} {ital The American Astronomical Society}« less