58 research outputs found
Conformal symmetry, anomaly and effective action for metric-scalar gravity with torsion
We consider some aspects of conformal symmetry in a metric-scalar-torsion
system. It is shown that, for some special choice of the action, torsion acts
as a compensating field and the full theory is conformally equivalent to
General Relativity on classical level. Due to the introduction of torsion, this
equivalence can be provided for the positively-defined gravitational and scalar
actions. One-loop divergences arising from the scalar loop are calculated and
both the consequent anomaly and the anomaly-induced effective action are
derived.Comment: 15 pages, LaTeX. Essentially extended version, in particular the
discussion of the stability of the conformal factor in gravity theory with
torsion and scalar added. Title also modified. To be published in Physics
Letters
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets
The spins of ten stellar black holes have been measured using the
continuum-fitting method. These black holes are located in two distinct classes
of X-ray binary systems, one that is persistently X-ray bright and another that
is transient. Both the persistent and transient black holes remain for long
periods in a state where their spectra are dominated by a thermal accretion
disk component. The spin of a black hole of known mass and distance can be
measured by fitting this thermal continuum spectrum to the thin-disk model of
Novikov and Thorne; the key fit parameter is the radius of the inner edge of
the black hole's accretion disk. Strong observational and theoretical evidence
links the inner-disk radius to the radius of the innermost stable circular
orbit, which is trivially related to the dimensionless spin parameter a_* of
the black hole (|a_*| < 1). The ten spins that have so far been measured by
this continuum-fitting method range widely from a_* \approx 0 to a_* > 0.95.
The robustness of the method is demonstrated by the dozens or hundreds of
independent and consistent measurements of spin that have been obtained for
several black holes, and through careful consideration of many sources of
systematic error. Among the results discussed is a dichotomy between the
transient and persistent black holes; the latter have higher spins and larger
masses. Also discussed is recently discovered evidence in the transient sources
for a correlation between the power of ballistic jets and black hole spin.Comment: 30 pages. Accepted for publication in Space Science Reviews. Also to
appear in hard cover in the Space Sciences Series of ISSI "The Physics of
Accretion onto Black Holes" (Springer Publisher). Changes to Sections 5.2,
6.1 and 7.4. Section 7.4 responds to Russell et al. 2013 (MNRAS, 431, 405)
who find no evidence for a correlation between the power of ballistic jets
and black hole spi
Current Status of Simulations
As the title suggests, the purpose of this chapter is to review the current
status of numerical simulations of black hole accretion disks. This chapter
focuses exclusively on global simulations of the accretion process within a few
tens of gravitational radii of the black hole. Most of the simulations
discussed are performed using general relativistic magnetohydrodynamic (MHD)
schemes, although some mention is made of Newtonian radiation MHD simulations
and smoothed particle hydrodynamics. The goal is to convey some of the exciting
work that has been going on in the past few years and provide some speculation
on future directions.Comment: 15 pages, 14 figures, to appear in the proceedings of the ISSI-Bern
workshop on "The Physics of Accretion onto Black Holes" (8-12 October 2012
Cherenkov radiation emitted by ultrafast laser pulses and the generation of coherent polaritons
We report on the generation of coherent phonon polaritons in ZnTe, GaP and
LiTaO using ultrafast optical pulses. These polaritons are coupled modes
consisting of mostly far-infrared radiation and a small phonon component, which
are excited through nonlinear optical processes involving the Raman and the
second-order susceptibilities (difference frequency generation). We probe their
associated hybrid vibrational-electric field, in the THz range, by
electro-optic sampling methods. The measured field patterns agree very well
with calculations for the field due to a distribution of dipoles that follows
the shape and moves with the group velocity of the optical pulses. For a
tightly focused pulse, the pattern is identical to that of classical Cherenkov
radiation by a moving dipole. Results for other shapes and, in particular, for
the planar and transient-grating geometries, are accounted for by a convolution
of the Cherenkov field due to a point dipole with the function describing the
slowly-varying intensity of the pulse. Hence, polariton fields resulting from
pulses of arbitrary shape can be described quantitatively in terms of
expressions for the Cherenkov radiation emitted by an extended source. Using
the Cherenkov approach, we recover the phase-matching conditions that lead to
the selection of specific polariton wavevectors in the planar and transient
grating geometry as well as the Cherenkov angle itself. The formalism can be
easily extended to media exhibiting dispersion in the THz range. Calculations
and experimental data for point-like and planar sources reveal significant
differences between the so-called superluminal and subluminal cases where the
group velocity of the optical pulses is, respectively, above and below the
highest phase velocity in the infrared.Comment: 13 pages, 11 figure
A resonant-term-based model including a nascent disk, precession, and oblateness: application to GJ 876
Investigations of two resonant planets orbiting a star or two resonant
satellites orbiting a planet often rely on a few resonant and secular terms in
order to obtain a representative quantitative description of the system's
dynamical evolution. We present a semianalytic model which traces the orbital
evolution of any two resonant bodies in a first- through fourth-order
eccentricity or inclination-based resonance dominated by the resonant and
secular arguments of the user's choosing. By considering the variation of
libration width with different orbital parameters, we identify regions of phase
space which give rise to different resonant ''depths,'' and propose methods to
model libration profiles. We apply the model to the GJ 876 extrasolar planetary
system, quantify the relative importance of the relevant resonant and secular
contributions, and thereby assess the goodness of the common approximation of
representing the system by just the presumably dominant terms. We highlight the
danger in using ''order'' as the metric for accuracy in the orbital solution by
revealing the unnatural libration centers produced by the second-order, but not
first-order, solution, and by demonstrating that the true orbital solution lies
somewhere ''in-between'' the third- and fourth-order solutions. We also present
formulas used to incorporate perturbations from central-body oblateness and
precession, and a protoplanetary or protosatellite thin disk with gaps, into a
resonant system. We quantify these contributions to the GJ 876 system, and
thereby highlight the conditions which must exist for multi-planet exosystems
to be significantly influenced by such factors. We find that massive enough
disks may convert resonant libration into circulation; such disk-induced
signatures may provide constraints for future studies of exoplanet systems.Comment: 39 pages of body text, 21 figures, 5 tables, 1 appendix, accepted for
publication in Celestial Mechanics and Dynamical Astronom
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