Soumi De1,2, Morgan MacLeod3, Rosa Wallace Everson4,5, Andrea Antoni6, Ilya Mandel7,8,9,5, Enrico Ramirez-Ruiz4,5
1Department of Physics, Syracuse University, Syracuse, NY 13244, USA
2Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA
3Harvard Smithsonian Center for Astrophysics, Cambridge, MA, USA
4Department of Astronomy and Astrophysics, University of
California, Santa Cruz, CA 95064
5DARK, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
6Department of Astronomy, University of California, Berkeley, CA 94720, USA
7School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
8OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery, Australia
9School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, United Kingdom
This page is a companion to the paper arXiv:1910.13333. We present visualizations of one of the hydrodynamical simulations presented in the paper and the fitting formulae derived from the mapping between the input parameters and results of the simulation suites.
Movie of simulation performed with ideal gas equation of state adiabatic constant γ = 4/3, mass ratio qr = 0.1, and upstream Mach number M∞ = 1.69 in the wind-tunnel setup. The top panel shows the formation of the shock and the evolution of the flow past the compact object embedded in the envelope of its companion star. Plotted is the density in units of ρ∞ in the orbital (x-y) plane of the binary, with the white dot at the coordinate origin representing the embedded companion object. The lines with arrowheads in white represent streamlines following the velocity field in the flow. The bottom panel shows the time series of coefficients of accretion Ca (in red) and drag Cd (blue) for the full simulation. The gray vertical line tracks the instantaneous Ca, Cd values as the simulation progresses. The time quoted in the movie is in code units Ra/v∞, where Ra is the accretion radius and v∞ is the relative velocity of the flow past the embedded object.
Presented below are three-dimensional interactive plots showing fitting relations between the coefficient of accretion Ca and coefficient of drag Cd in terms of the mass ratio q and upstream Mach number M∞ obtained on mapping the input parameters to the results from the hydrodynamical simulations.
The red dots represent the log10Ca results obtained from the (Γ, γ) = (4/3, 4/3) hydrodynamical simulations with q and M∞ parameters. The three-dimensional surface shows the best fitting third-order polynomial relation of log10Ca as a function of (q, M∞).
The red dots represent the log10Cd results obtained from the (Γ, γ) = (4/3, 4/3) hydrodynamical simulations with q and M∞ parameters. The three-dimensional surface shows the best fitting third-order polynomial relation of log10Cd as a function of (q, M∞).
The red dots represent the log10Ca results obtained from the (Γ, γ) = (5/3, 5/3) hydrodynamical simulations with q and M∞ parameters. The three-dimensional surface shows the best fitting second-order polynomial relation of log10Ca as a function of (q, M∞).
The red dots represent the log10Cd results obtained from the (Γ, γ) = (5/3, 5/3) hydrodynamical simulations with q and M∞ parameters. The three-dimensional surface shows the best fitting second-order polynomial relation of log10Cd as a function of (q, M∞).
FLASH, yt, Plotly, Matplotlib, astropy.
Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, by the Institute for Advanced Study, by the University of Copenhagen high-performance computing cluster funded by a grant from VILLUM FONDEN (project number 16599), and by Syracuse University.