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Initial data for binary black holes: the conformal thin-sandwich puncture method : 

Initial data for binary black holes: the conformal thin-sandwich puncture method Mark D. Hannam UTB Relativity Group Seminar September 26, 2003

Overview: the smallest picture possible: 

Overview: the smallest picture possible We want to simulate a (realistic) binary black hole collision. To do that, 1. Rewrite Einstein’s equations as a Cauchy problem 2. Set up initial data for two black holes in orbit 3. Evolve the system. Problems: we can’t do (2) or (3) very well. Partial solution: try to create good initial data close to the interesting physics… Describe two black holes in quasi-circular, quasi-equilibrium orbit just before they plunge together.

Slide3: 

Initial data: Space and time are mixed… Initial value constraints Evolution equations

What quantities are constrained?: 

What quantities are constrained? 12 independent components - 4 constraint equations 8 free quantities: 4 dynamical 4 gauge Which are which? Use a conformal decomposition…

Conformal thin-sandwich decomposition: 

Conformal thin-sandwich decomposition

CTS: the essentials: 

CTS: the essentials Free data: Solve for: Construct:

“Easy” examples: 

“Easy” examples Schwarzschild (single stationary black hole): Brill-Lindquist (multiple stationary black holes)

Orbits in the CTS decomposition: 

Orbits in the CTS decomposition In a corotating reference frame, the black holes will be almost stationary. Choose These choices are physically motivated Free data choices in old decompositions were made for convenience

CTS solutions: 

CTS solutions Gourgoulhon, Grandclément, and Bonazzola (GGB), 2001. Solved with Excised regions containing singularities Employed boundary conditions on excised surfaces (…there were inconsistencies here) I want to avoid inner boundary conditions  Puncture method.

CTS-puncture approach: 

CTS-puncture approach Recall Brill-Lindquist solution: Extend to . The shift has no singular part What corresponds to black holes with Pi and Si ? (what are ci?) Hamiltonian constraint: Constant-K equation: Solve for v Regular if Solve for u

Issues: Slicing choices(for one black hole): 

Issues: Slicing choices (for one black hole) Two principle choices: Schwarzschild But: on some surface… Estabrook (N = 1). but This is a “dynamical” slicing! The stationary Schwarzschild black hole will APPEAR to have dynamics This isn’t necessarily fatal to the method [Ref: MDH, C.R. Evans, G.B. Cook, T.W. Baumgarte, gr/qc-0306028]

Issue #2: The shift vectorConditions at the puncture?: 

Issue #2: The shift vector Conditions at the puncture? The analytic, singular part of the conformal factor gave us a black hole solution, without the need for inner boundary conditions There is no known analytic part of the shift for a black hole with non-zero Pi and Si, and the puncture form of the lapse. We need to impose suitable conditions at the puncture. Methods to date do not give convergent results…

Future work: 

Future work Convert code to Cactus, where much greater resolution is possible Maybe the momentum constraint solver will converge. Construct data with an everywhere positive lapse Examine the level of stationarity of quasi-circular orbits (located by, for example, the effective potential method) Maybe the “Estabrook” lapse choice is Ok.