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BEGIN:VEVENT
SUMMARY:Effective source formulations in the Regge-Wheeler gauge
DTSTART;VALUE=DATE-TIME:20170621T153000Z
DTEND;VALUE=DATE-TIME:20170621T155500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-23@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Jonathan Thompson (University of Florida)\nIn this s
tatus talk\, I discuss progress being made to adapt effective-source regul
arization techniques to a first-order calculation in the Regge-Wheeler gau
ge.\n\nhttps://wasabi.physics.unc.edu/event/6/contributions/23/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/23/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Regularization via the Detweiler-Whiting Singular Field
DTSTART;VALUE=DATE-TIME:20170619T160000Z
DTEND;VALUE=DATE-TIME:20170619T162500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-24@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Anna Heffernan (University of Florida)\nTBD\n\nhttps
://wasabi.physics.unc.edu/event/6/contributions/24/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/24/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Progress towards multiscale EMRI approximation: zones and scales
DTSTART;VALUE=DATE-TIME:20170619T190000Z
DTEND;VALUE=DATE-TIME:20170619T192500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-25@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Jordan Moxon (Cornell University)\nWe present an upd
ate to the multiscale analytic approximation method for computing EMRI dy
namics. The multiscale method takes advantage of the separation of the rad
iation-reaction timescale to the orbital timescale. By appropriately accou
nting for the slow evolution of the system\, we suggest a framework for co
mputing the waveform with only $\\mathcal{O}(\\epsilon)$ phase error. This
framework will also be useful for computing quantities relevant for compa
risons to Post-Newtonian or Numerical Relativity computations to second or
der in the mass ratio. Full second-order solution requires the introductio
n of `puncture' regions near the horizon\, near the small companion\, and
far from the binary\, which are related to the interaction with the inspir
al via a matched asymptotic expansion. We propose a geometric optics appro
ximation for the region far from the inspiral.\n\nhttps://wasabi.physics.u
nc.edu/event/6/contributions/25/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/25/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Capra roundup: perspective and prospects.
DTSTART;VALUE=DATE-TIME:20170622T203000Z
DTEND;VALUE=DATE-TIME:20170622T210000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-26@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Bernard Whiting (University of Florida)\nI will try
to summarize my perspective on where we stand with respect to the Capra mi
ssion\, mention some highlights from the preceding talks\, and give a list
of topics I consider worthy for group discussion during the remaining day
s of the meeting.\n\nhttps://wasabi.physics.unc.edu/event/6/contributions/
26/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/26/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Merger Simulation Using the Parker Sochacki Method and Finite Elem
ent Analysis\, in a Model Explicitly Consistent with Quantum Mechanics.
DTSTART;VALUE=DATE-TIME:20170619T203000Z
DTEND;VALUE=DATE-TIME:20170619T205500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-27@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Joseph Rudmin (James Madison University)\nThe motion
of two or more sources of a gravitational field is modeled using the Park
er Sochacki Method in adaptive finite element analysis. In rest frames\, t
he metric is isotropic but not conformally flat. A metric equation for the
conjugate mass-energy-momentum equation provides explicit consistency wit
h quantum mechanics: Unitarity is preserved because Planck's Constant is i
nvariant with metric scaling. While a metric is invariant under a local lo
rentz transformation\, it is not invariant in under a lorentz transformati
on at an observer with a different metric scaling. The lorentz-transformed
metric provides the affine connection for the equations of motion\, which
gives the velocities of the rest frames of the metrics at each point in s
pace as seen by an observer at an arbitrary location. The equivalence prin
ciple applied to the continuity equation (or bianchi identities) for the E
instein Tensor as seen by any observer provides the equation which advance
s the Taylor series for the metric scaling: $G^{\\mu\\nu}(g^{2})_{\,\\nu}=
0$\, where the metric scaling $g$ appears in the metric equations in rest
frames as $d\\tau^{2}=dt^{2}/g^{2}-g^{2}d\\vec{r}^{2}$ and $dm_{0}^{2}=g^{
2}E^{2}-d\\vec{p}^{2}/g^{2}$. This method is inherently symplectic because
it uses the Parker Sochacki Method. It is inherently retarded and paralle
lizable because time evolution depends only on local conditions: Each proc
essor can independently track its finite element.\n\nhttps://wasabi.physic
s.unc.edu/event/6/contributions/27/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/27/
END:VEVENT
BEGIN:VEVENT
SUMMARY:General-Relativistic Dynamics of an Extreme Mass-Ratio Binary with
an External Body
DTSTART;VALUE=DATE-TIME:20170621T203000Z
DTEND;VALUE=DATE-TIME:20170621T205500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-35@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Huan Yang (Princeton University)\nWe study the dynam
ics of a hierarchical three-body system in the general-relativistic regime
:an extreme mass-ratio inner binary under the tidal influence of an extern
al body.\nThe inner binary consists of a central Schwarzschild black hole
and a test body moving around it. We discover three types of tidal effects
on the orbit of the test body.\nFirst\, the angular moment of the inner b
inary precesses around the angular momentum of the outer binary. Second\,
the tidal field drives a ``transient resonance" when the radial and azimu
thal frequencies are commensurable.In contrast with resonances driven by t
he gravitational self-force\, this tidal-driven resonance may boost the or
bital angular momentum. Finally\, as an orbit-dynamical effect during the
non-resonant phase\, we calculate the correction to the Innermost Stable
Circular (mean) Orbit due to the tidal interaction. Hierarchical three-bod
y systems are potential sources for future space-based gravitational wave
missions and the tidal effects that we find could contribute significantl
y to their waveform.\n\nhttps://wasabi.physics.unc.edu/event/6/contributio
ns/35/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/35/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Solving for binary inspiral dynamics using renormalization group m
ethods
DTSTART;VALUE=DATE-TIME:20170619T153000Z
DTEND;VALUE=DATE-TIME:20170619T155500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-28@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Chad Galley (Jet Propulsion Laboratory\, California
Institute of Technology)\nSolving the equations of motion describing a com
pact binary's inspiral dynamics is not easy because of stringent accuracy
requirements and the long duration of the orbit. In many cases\, this can
be achieved using numerical integration methods but such an approach is of
ten a computational bottleneck for gravitational wave data analysis applic
ations like parameter estimation. Analytically\, some progress can be made
by averaging out the shorter time scales in the problem. However\, such a
diabatic approximations are often not systematic\, are difficult to estima
te the domain of validity of the approximate solution\, and entail ambigui
ties that make it difficult for assessing accuracy to truth solutions. I d
iscuss some recent and ongoing work that aims to solve these problems usin
g renormalization group theory methods. This approach does not require or
utilize any averaging procedures so that the resulting solutions describe
the binary's real-time orbital configuration at every instant. The basic i
dea rests on naive perturbation theory which\, because of radiation reacti
on and self-force\, produces secularly growing terms in time that renormal
ize the initial data parameters. This process generates a flow in time (i.
e.\, the inspiral) which is described by the renormalization group equatio
ns that\, in many cases\, can be solved analytically. Being based on pertu
rbation theory\, it is straightforward to provide formal errors for the va
lidity of the resulting resummed perturbative solution. I introduce the co
ncepts and steps by sketching out the calculation for post-Newtonian inspi
rals. Other astrophysical applications\, including tidal dissipation and s
pin-locking\, may be discussed if time permits.\n\nhttps://wasabi.physics.
unc.edu/event/6/contributions/28/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/28/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Progress at second order
DTSTART;VALUE=DATE-TIME:20170621T130000Z
DTEND;VALUE=DATE-TIME:20170621T135000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-29@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Adam Pound (University of Southampton)\nI discuss th
e status of second-order self-force formulations and computations\, which
will be necessary for accurate models of EMRIs. \n\nIn the first part of t
he talk\, I describe recent progress on the foundations of the theory. A p
rincipal feature of the second-order field equations is that the retarded
field does not have a distributionally well-defined source\, instead havin
g a free boundary value in a region around the small object. This challeng
e has historically been addressed using a puncture scheme. However\, it ca
n also be eliminated entirely with a judicious choice of gauge\, which may
radically simplify future numerical work.\n\nIn the second part of the ta
lk\, I describe ongoing work to numerically implement a second-order\, two
-timescale puncture scheme for quasicircular orbits in Schwarzschild space
time. This will lead into the talk by Wardell.\n\nhttps://wasabi.physics.u
nc.edu/event/6/contributions/29/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/29/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Towards the self-consistent evolution of a scalar charge around a
Schwarzschild black hole.
DTSTART;VALUE=DATE-TIME:20170620T190000Z
DTEND;VALUE=DATE-TIME:20170620T192500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-30@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Peter Diener (Louisiana State University)\nUsing the
effective source approach and the Discontinuous Galerkin method we have d
eveloped a very accurate time domain code for the evolution of a scalar ch
arge in orbit around a Schwarzschild black hole. In the first incarnation
of the code\, only geodesic motion could be handled\, but we have now adde
d the ability to handle arbitrarily accelerated orbits.\n\nIn this talk I
will present code tests based on comparisons with frequency domain results
for constant accelerated circular orbits and accelerated eccentric orbits
that are periodic. Finally I will present new results for a case that can
not be handled in the frequency domain: the case of a particle on a circu
lar geodesic that experiences a short acceleration event (at constant radi
us) before returning to circular geodesic motion.\n\nI will also discuss t
he prospect of using this code for self-consistent evolutions where the fi
eld and the particle orbit are evolved together.\n\nhttps://wasabi.physics
.unc.edu/event/6/contributions/30/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/30/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The laws of binary black hole mechanics: an update
DTSTART;VALUE=DATE-TIME:20170622T130000Z
DTEND;VALUE=DATE-TIME:20170622T135000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-31@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Alexandre Le Tiec (Observatoire de Paris)\nThe class
ical laws of black hole mechanics can be extended to binary systems of com
pact objects. I will first review the various zeroth and first laws of mec
hanics that have been established in the context of exact general relativi
ty\, in the post-Newtonian approximation and in black hole perturbation th
eory\, for binary systems of black holes and/or point particles. I will th
en discuss various applications of these laws of binary mechanics.\n\nhttp
s://wasabi.physics.unc.edu/event/6/contributions/31/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/31/
END:VEVENT
BEGIN:VEVENT
SUMMARY:First order gravitational self-force on generic bound orbits in Ke
rr spacetime
DTSTART;VALUE=DATE-TIME:20170620T140000Z
DTEND;VALUE=DATE-TIME:20170620T145000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-32@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Maarten van de Meent (AEI Potsdam-Golm)\nIn this tal
k I will review the metric reconstruction machinery used for frequency dom
ain calculations of the first order gravitational self-force on bound geod
esics in Kerr spacetime. In particular\, I will focus on how each step in
this process is affect by relinquishing the up/down reflection symmetry of
equatorial orbits\, and moving to generic (inclined and eccentric) orbits
. \n\nIf the cluster and coding gods are willing\, I will present some fr
esh preliminary results for the gravitational self-force on an inclined an
d eccentric orbit.\n\nhttps://wasabi.physics.unc.edu/event/6/contributions
/32/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/32/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Scalar self-force for generic bound orbits on Kerr
DTSTART;VALUE=DATE-TIME:20170620T200000Z
DTEND;VALUE=DATE-TIME:20170620T202500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-33@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Zach Nasipak (The University of North Carolina at Ch
apel Hill)\nWe perform scalar self-force calculations for inclined\, eccen
tric orbits of a small\, compact body in Kerr spacetime. To implement thes
e calculations with arbitrary numerical precision\, we generalize spectral
source integration (SSI) techniques by introducing the Mino time paramete
r and extending mode decompositions to include a polar frequency for incli
ned motion. Calculations are conducted using a Mathematica code that imple
ments these SSI techniques along with the Mano\, Suzuki\, and Takasugi (MS
T) formalism to determine the inhomogeneous wave function solutions to the
Teukolsky equation. This allows us to improve the accuracy of previous ca
lculations in the literature. We also probe the extended parameter space f
or various orbital inclinations. Further extension to the gravitational ca
se is also considered.\n\nhttps://wasabi.physics.unc.edu/event/6/contribut
ions/33/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/33/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Time-domain metric reconstruction for self-force applications
DTSTART;VALUE=DATE-TIME:20170620T153000Z
DTEND;VALUE=DATE-TIME:20170620T155500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-34@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Leor Barack (University of Southampton)\nWe present
a new method for self-force calculation in Kerr\, based on a time-domain r
econstruction of the metric perturbation from curvature scalars. The appro
ach is computationally cheaper than existing time-domain methods based on
a direct integration of the linearised Einstein's equations in the Lorenz
gauge. It also avoids instability issues that plague those methods. At the
same time\, it retains the utility and flexibility of a time-domain treat
ment\, allowing calculations for any type of orbits (including highly ecce
ntric or unbound ones) and the possibility of self-consistently evolving t
he orbit under the effect of the self-force. Here we formulate our method
for Kerr\, and present a first numerical implementation in Schwarzschild.
\n\nhttps://wasabi.physics.unc.edu/event/6/contributions/34/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/34/
END:VEVENT
BEGIN:VEVENT
SUMMARY:A near-horizon expansion of second-order black hole perturbations
DTSTART;VALUE=DATE-TIME:20170621T160000Z
DTEND;VALUE=DATE-TIME:20170621T162500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-36@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Kei Yamada (Kyoto Universiry)\nThe first detection o
f gravitational waves (GWs) from merger of binary black hole (BH) by advan
ced LIGO has opened a new window to test general relativity. In the future
\, extreme-mass-ratio inspirals (EMRIs)\, in which stellar-mass compact ob
jects of mass $\\mu$ spiral into a supermassive black holes (SMBHs) of mas
s $M$\, are expected to be observed by LISA. Such systems can be expressed
by using the BH perturbation approach\, where we expand equations in the
mass ratio $\\mu/M$. In order to extract physical parameters from GW obser
vations\, the second-order perturbations must be considered. However\, nai
ve calculations lead to a divergence of the second-order perturbations aro
und boundaries. In this talk\, we will seek a counterterm to avoid such a
divergence around the event horizon of the SMBH.\n\nhttps://wasabi.physics
.unc.edu/event/6/contributions/36/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/36/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Scattering events in Schwarzschild spacetime
DTSTART;VALUE=DATE-TIME:20170619T180000Z
DTEND;VALUE=DATE-TIME:20170619T182500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-37@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Seth Hopper (Instituto Superior Técnico)\nThe recen
t LIGO detections of merging black holes represent the culmination of deca
des of research into gravitational waves (GWs). One well-known seminal wor
k by Peters and Mathews predicted the GW luminosity of eccentric binaries
to leading post-Newtonian (PN) order. Driven largely by the desire to dete
ct GWs from inspirals\, the Peters-Mathews work has subsequently been exte
nded through 3.5PN. Less well-known is work by Taylor\, which is directly
analogous to the Peters-Mathews result\, except for scattering binaries. T
his work has only been extended by one PN order.\n\nIn this talk I present
work exploring the overlap regime between PN and black hole perturbation
theory (BHPT). The regime is particularly fertile for bound two-body motio
n wherein the viral theorem links the two PN parameters (speed squared and
inverse separation). For scattering and plunging trajectories\, however\,
both numerical BHPT and analytical PN techniques struggle. I will discuss
a range of potential methods for analyzing unbound motion\, and show some
successes and failures. Finally\, I will consider the potential for using
BHPT to compute (unbound-motion) gauge invariants\, which has been quite
successful for calibrating effective-one-body models.\n\nhttps://wasabi.ph
ysics.unc.edu/event/6/contributions/37/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/37/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Eccentric Orbit EMRIs: Enhanced Method for Determining Analytical
Flux Coefficients to 7 PN.
DTSTART;VALUE=DATE-TIME:20170619T183000Z
DTEND;VALUE=DATE-TIME:20170619T185500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-38@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Christopher Munna (UNC Chapel Hill)\nContinuing the
work of Forseth et *al*. (2016)\, we use high precision comparisons betwee
n perturbation theory and the post-Newtonian expansion to extract new info
rmation on eccentric orbit EMRIs to 7 PN order. Fluxes are calculated by
combining the MST formalism with spectral source integration (SSI) for a m
ultitude of orbits\, whose parameters are then fit over in the PN form. T
his time\, we perform a fit on each LMN mode individually\, exploiting the
patterns contained therein. The result is a significantly enhanced abili
ty to fit for the combinations of transcendentals that appear in the highe
r PN orders.\n\nhttps://wasabi.physics.unc.edu/event/6/contributions/38/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/38/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Evolution of small-mass-ratio binaries with a spinning secondary
DTSTART;VALUE=DATE-TIME:20170620T160000Z
DTEND;VALUE=DATE-TIME:20170620T162500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-40@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Thomas Osburn (Oxford College of Emory University)\n
We calculate the evolution and gravitational-wave emission of a spinning c
ompact object inspiraling into a substantially more massive (non-rotating)
black hole. We extend our previous model for a non-spinning binary [Phys.
Rev. D 93\, 064024] to include the Mathisson-Papapetrou-Dixon spin-curvat
ure force. Using a generalized osculating element prescription we compute
inspirals where the spin and orbital angular momentum are not parallel and
the orbital plane precesses. For spin-aligned binaries we calculate the d
ephasing of the inspiral and associated waveforms with respect to models t
hat do not include spin-curvature effects.\n\nhttps://wasabi.physics.unc.e
du/event/6/contributions/40/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/40/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Scalar self-force and QNM excitation for highly eccentric orbits i
n Kerr spacetime
DTSTART;VALUE=DATE-TIME:20170620T183000Z
DTEND;VALUE=DATE-TIME:20170620T185500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-41@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Jonathan Thornburg (Indiana University\, Astronomy D
ept)\nWe present a computation of the self-force for a scalar-field partic
le\non a bound eccentric orbit (which need not be a geodesic) in Kerr spac
etime.\nOur main interest is in the case of highly eccentric orbits\;\nher
e we present results for eccentricities as high as $0.98$.\nWe use a Loren
z-gauge Barack-Golbourn-Vega-Detweiler effective-source\nregularization fo
llowed by an $e^{im\\phi}$ ("m-mode") Fourier decomposition\nand a separat
e time-domain numerical evolution in $2{+}1$ dimensions for\neach $m$. We
introduce a finite worldtube which surrounds the particle\nworldline and
define our evolution equations in a piecewise manner so that\nthe effectiv
e source is only used within the worldtube. Viewed as a spatial\nregion t
he worldtube moves to follow the particle's orbital motion.\nOur numerical
evolution uses Berger-Oliger mesh refinement with\n4th~order finite diffe
rencing in space and time.\nWe use slices of constant Boyer-Lindquist time
near the black hole\,\ndeformed (following Zenginoglu) so as to be asympt
otically hyperboloidal\nand compactified near the horizon and near $\\math
cal{J}^+$.\nOur present implementation is restricted to equatorial geodesi
c orbits\,\nbut this restriction is not fundamental.\nFor those configurat
ions where the central black hole is highly spinning\,\nthe particle's per
iastron passage is near to or within the light ring\,\nand the orbital ecc
entricity is $\\ge 0.4$\, we find that the particle's\nperiastron passage
excites quasinormal modes of the background (Kerr)\nspacetime\, causing la
rge oscillations (``wiggles'') in the self-force\non the outgoing leg of t
he orbit\, and smaller but still detectable\noscillations in the radiated
field at $\\mathcal{J}^+$.\n\nhttps://wasabi.physics.unc.edu/event/6/contr
ibutions/41/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/41/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Overcharging Higher-dimensional Black holes using point particles
DTSTART;VALUE=DATE-TIME:20170621T200000Z
DTEND;VALUE=DATE-TIME:20170621T202500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-42@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Karl Simon Revelar (University of the Philippines)\n
We investigate the possibility of overcharging charged spherically-symmetr
ic black holes in spacetime dimensions D > 4 by the capture of a charged p
article. We generalize Wald’s classic result that extremal black holes c
annot be overcharged. For nearly extremal black holes\, we study how D aff
ects the overcharging parameter space first discovered by Hubeny in D = 4.
We find that overcharging becomes difficult for nearly-extremal black hol
es in the large D-limit.\n\nhttps://wasabi.physics.unc.edu/event/6/contrib
utions/42/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/42/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Scattering of two spinning black holes and effective-one-body mapp
ings
DTSTART;VALUE=DATE-TIME:20170622T153000Z
DTEND;VALUE=DATE-TIME:20170622T155500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-43@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Justin Vines (Max Planck Institute for Gravitational
Physics)\nThe net results of scattering processes can be seen to fully en
code the gauge-invariant content of (unbound and bound) two-body dynamics.
We present new results for the scattering of two spinning black holes (B
Hs)\, with an arbitrary mass ratio and with generic spin orientations\, in
the first post-Minkowskian (1PM) approximation to general relativity---to
linear order in G\, but to all orders in 1/c\, and to all orders in both
BHs' spins. The results are seen to fully reproduce and "resum" the linea
r-in-G parts of all previous post-Newtonian results for spinning-binary-BH
dynamics\, through 4PN order. The results also reveal a complete equival
ence at 1PM order\, under simple mappings\, between arbitrary-mass-ratio t
wo-spinning-BH dynamics and both (i) the dynamics of a spinning test BH (w
ith all of the spin-induced BH multipoles) in a Kerr spacetime\, and more
surprisingly (ii) geodesic (point-test-mass) motion in a Kerr spacetime.
We discuss implications for effective-one-body models and preview the situ
ation at 2PM order.\n\nhttps://wasabi.physics.unc.edu/event/6/contribution
s/43/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/43/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Effective-one-body modeling of binary black holes in the era of gr
avitational-wave astronomy
DTSTART;VALUE=DATE-TIME:20170622T140000Z
DTEND;VALUE=DATE-TIME:20170622T145000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-44@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Andrea Taracchini (Max Planck Institute for Gravitat
ional Physics Potsdam)\nThe direct observation and characterization of gra
vitational waves from the coalescence of binary black holes by the LIGO an
d Virgo Collaborations is a testament to the crucial role played by wavefo
rm modeling in these discoveries. I will review the effective-one-body app
roach to describing the whole process of inspiral\, merger and ringdown. T
his model implements the idea of a unified description of the dynamics of
compact binaries\, from the comparable-mass regime to the test-particle li
mit\, with the goal of incorporating analytical and numerical information
from different areas of relativity. I will highlight synergetic efforts wi
th black-hole perturbation theory and gravitational self-force. I will als
o discuss applications of this model to the data analysis of the first gra
vitational-wave detections.\n\nhttps://wasabi.physics.unc.edu/event/6/cont
ributions/44/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/44/
END:VEVENT
BEGIN:VEVENT
SUMMARY:The nonspinning binary black hole merger scenario revisited
DTSTART;VALUE=DATE-TIME:20170619T200000Z
DTEND;VALUE=DATE-TIME:20170619T202500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-45@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Carlos Lousto (Rochester Institute of Technology)\nW
e present the results of 14 simulations of nonspinning\nblack hole binarie
s with mass ratios $q=m_1/m_2$ in the range\n$1/100\\leq q\\leq1$. For eac
h of these simulations we perform three runs\nat increasing resolution to
assess the finite difference\nerrors and to extrapolate the results to inf
inite resolution.\nFor $q\\geq 1/6$\, we follow the evolution of the binar
y typically for the last\nten orbits prior to merger.\nBy fitting the resu
lts of these simulations\, we accurately model the peak\nluminosity\, peak
waveform frequency and amplitude\, \nand the recoil of the remnant hole f
or unequal mass \nnonspinning binaries. We verify the accuracy of these ne
w models and\ncompare them to previously\nexisting empirical formulas.\nTh
ese new fits provide a basis for a hierarchical approach to produce\nmore
accurate remnant formulas in the generic precessing case.\nThey also provi
de input to gravitational waveform\nmodeling and allow comparisons with pe
rturbation theory.\n\nhttps://wasabi.physics.unc.edu/event/6/contributions
/45/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/45/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Transient Instabilities of Nearly Extremal Black holes
DTSTART;VALUE=DATE-TIME:20170620T180000Z
DTEND;VALUE=DATE-TIME:20170620T182500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-46@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Aaron Zimmerman (Canadian Institute for Theoretical
Astrophysics)\nI will review recent work on the near-horizon perturbations
of nearly extremal Kerr black holes. These perturbations experience trans
ient growth\, resulting in a "ring up" to strongly enhanced amplitudes. Th
ese transient instabilities connect directly to the slowly growing instabi
lities of extremal horizons\, and may have observable consequences.\n\nhtt
ps://wasabi.physics.unc.edu/event/6/contributions/46/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/46/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Discussion on EMRI/IMRI using numerical relativity
DTSTART;VALUE=DATE-TIME:20170622T193000Z
DTEND;VALUE=DATE-TIME:20170622T194500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-47@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Bernard Schutz (Cardiff University and AEI)\nWhen ma
ss ratios are not very extreme\, perturbation theory becomes difficult. St
andard numerical relativity codes\, however\, are inefficient unless the o
bjects are of comparable mass\, because the time-step and grid size are fi
xed by the smaller object. However\, the smaller the mass ratio\, the less
important is the dynamics of the smaller object. \n\nI propose therefore
a discussion on how to do numerical relativity by excising the smaller obj
ect and replacing it with a parametrized analytic solution. The boundary o
f the excised region becomes a (timelike) boundary of the numerically inte
grated domain. The boundary condition can be a matching condition of the e
xternal geometry to an internal solution in the excised region that has no
inherent dynamics. It can be tidally distorted but this would be treated
as an adiabatic perturbation on the external timescale. The matching bound
ary is\, from the point of view of the inner solution\, in the far-field o
f the compact body.\n\nThis method has heritage as far back as EIH but is
most closely associated with the way Futamase approached the point-particl
e limit of the PN problem for two compact objects\, where the orbit soluti
on was obtained by boundary matching to "inner" solutions for the compact
objects: Physical Review D\, vol. 32\, (1985) pp. 2566-2574. Unlike for th
e PN problem\, however\, in the EMRI/IMRI problem there is no scaling on v
elocity\; the only small parameter is the mass ratio.\n\nhttps://wasabi.ph
ysics.unc.edu/event/6/contributions/47/
LOCATION:Dept. of Physics & Astronomy and the CoSMS Institute\, University
of North Carolina at Chapel Hill Room 011\, Sitterson Hall
URL:https://wasabi.physics.unc.edu/event/6/contributions/47/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Self-force on a scalar charge in circular orbits about a Reissner-
Nordstr\\"{o}m black hole
DTSTART;VALUE=DATE-TIME:20170620T203000Z
DTEND;VALUE=DATE-TIME:20170620T205500Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-48@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Jezreel Castillo (National Institute of Physics\, Un
iversity of the Philippines Diliman)\nWe calculate the self-force exerted
on a scalar charge in a circular orbit about a Reissner-Nordstr\\"{o}m bla
ck hole via mode-sum regularization. We also compute the radiative fluxes
towards infinity and down the black hole. We pay particular attention to t
he dependence of the self-force and radiative fluxes on the black hole's c
harge-to-mass ratio\, the controlling parameter of the Reissner-Nordstr\\"
{o}m geometry. We find that as the black hole approaches extremality\, the
radiative fluxes\, and the self-force decreases.\n\nhttps://wasabi.physic
s.unc.edu/event/6/contributions/48/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/48/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Update on LIGO
DTSTART;VALUE=DATE-TIME:20170619T130000Z
DTEND;VALUE=DATE-TIME:20170619T135000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-49@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Aaron Zimmerman (Canadian Institute for Theoretical
Astrophysics)\nTBA\n\nhttps://wasabi.physics.unc.edu/event/6/contributions
/49/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/49/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Effective Source Calculations Through Second Perturbative Order
DTSTART;VALUE=DATE-TIME:20170621T140000Z
DTEND;VALUE=DATE-TIME:20170621T145000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-50@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Barry Wardell (University College Dublin)\nTBD\n\nht
tps://wasabi.physics.unc.edu/event/6/contributions/50/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/50/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Computing inspirals and waveforms using the self-force
DTSTART;VALUE=DATE-TIME:20170620T130000Z
DTEND;VALUE=DATE-TIME:20170620T135000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-51@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Niels Warburton (University College Dublin)\nIn this
talk I will review methods and results for computing inspirals and their
associated waveforms in the small mass-ratio regime. To leading-order in t
he orbital phase evolution of the binary adiabatic flux balance techniques
can be used. If we desire to track the orbital phase to better than one r
adian we must include post-adiabatic terms in the inspiral model. These po
st-adiabatic terms include first-order (in the mass ratio) conservative ef
fects\, second-order fluxes and effects from the spin of the secondary. I
will discuss geodesic self-force and self-consistent models for incorporat
ing these effects. After reviewing the progress that has been made I will
conclude with a discussion of on-going efforts and future directions.\n\nh
ttps://wasabi.physics.unc.edu/event/6/contributions/51/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/51/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Welcome and Opening Remarks
DTSTART;VALUE=DATE-TIME:20170619T125200Z
DTEND;VALUE=DATE-TIME:20170619T130000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-53@wasabi.physics.unc.edu
DESCRIPTION:Speakers: CoSMS Institute Director Prof. John Wilkerson ()\nht
tps://wasabi.physics.unc.edu/event/6/contributions/53/
LOCATION:UNC Room 011\, Sitterson Hall
URL:https://wasabi.physics.unc.edu/event/6/contributions/53/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Welcome and Opening Remarks
DTSTART;VALUE=DATE-TIME:20170619T124500Z
DTEND;VALUE=DATE-TIME:20170619T125200Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-54@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Senior Associate Dean Prof. Chris Clemens ()\nhttps:
//wasabi.physics.unc.edu/event/6/contributions/54/
LOCATION:UNC Room 011\, Sitterson Hall
URL:https://wasabi.physics.unc.edu/event/6/contributions/54/
END:VEVENT
BEGIN:VEVENT
SUMMARY:Prospects for observing extreme-mass-ratio inspirals with LISA
DTSTART;VALUE=DATE-TIME:20170619T140000Z
DTEND;VALUE=DATE-TIME:20170619T145000Z
DTSTAMP;VALUE=DATE-TIME:20240617T135308Z
UID:indico-contribution-6-57@wasabi.physics.unc.edu
DESCRIPTION:Speakers: Jonathan Gair (University of Edinburgh)\nTBD\n\nhttp
s://wasabi.physics.unc.edu/event/6/contributions/57/
LOCATION:UNC Sitterson 011
URL:https://wasabi.physics.unc.edu/event/6/contributions/57/
END:VEVENT
END:VCALENDAR