# Publications

## The impact of occupancy patterns, occupant-controlled ventilation and shading on indoor overheating risk in domestic environments

BUILDING AND ENVIRONMENT **78** (2014) 183-198

## The relative importance of input weather data for indoor overheating risk assessment in dwellings

BUILDING AND ENVIRONMENT **76** (2014) 81-91

## Relabeling symmetry in relativistic fluids and plasmas

Journal of Physics A: Mathematical and Theoretical **47** (2014)

© 2014 IOP Publishing Ltd. The conservation of the recently formulated relativistic canonical helicity (Yoshida et al 2014 J. Math. Phys. 55 043101) is derived from Noether's theorem by constructing an action principle on the relativistic Lagrangian coordinates (we obtain general cross helicities that include the helicity of the canonical vorticity). The conservation law is, then, explained by the relabeling symmetry pertinent to the Lagrangian label of fluid elements. Upon Eulerianizing the Noether current, the purely spatial volume integral on the Lagrangian coordinates is mapped to a space-time mixed three-dimensional integral on the four-dimensional Eulerian coordinates. The relativistic conservation law in the Eulerian coordinates is no longer represented by any divergence-free current; hence, it is not adequate to regard the relativistic helicity (represented by the Eulerian variables) as a Noether charge, and this stands the reason why the 'conventional helicity' is no longer a constant of motion. We have also formulated a relativistic action principle of magnetohydrodynamics (MHD) on the Lagrangian coordinates, and have derived the relativistic MHD cross helicity.

## Relativistic helicity and link in Minkowski space-time

Journal of Mathematical Physics **55** (2014)

A relativistic helicity has been formulated in the four-dimensional Minkowski spacetime. Whereas the relativistic distortion of space-time violates the conservation of the conventional helicity, the newly defined relativistic helicity conserves in a barotropic fluid or plasma, dictating a fundamental topological constraint. The relation between the helicity and the vortex-line topology has been delineated by analyzing the linking number of vortex filaments which are singular differential forms representing the pure states of Banach algebra. While the dimension of space-time is four, vortex filaments link, because vorticities are primarily 2-forms and the corresponding 2- chains link in four dimension; the relativistic helicity measures the linking number of vortex filaments that are proper-time cross-sections of the vorticity 2-chains. A thermodynamic force yields an additional term in the vorticity, by which the vortex filaments on a reference-time plane are no longer pure states. However, the vortex filaments on a proper-time plane remain to be pure states, if the thermodynamic force is exact (barotropic), thus, the linking number of vortex filaments conserves. © 2014 AIP Publishing LLC.

## A current driven electromagnetic mode in sheared and toroidal configurations (vol 56, 035011, 2014)

PLASMA PHYSICS AND CONTROLLED FUSION **56** (2014) ARTN 129501

## The Gaia-ESO Survey: processing FLAMES-UVES spectra

ASTRONOMY & ASTROPHYSICS **565** (2014) ARTN A113

## Interstellar medium. Pseudo-three-dimensional maps of the diffuse interstellar band at 862 nm.

Science (New York, N.Y.) **345** (2014) 791-795

The diffuse interstellar bands (DIBs) are absorption lines observed in visual and near-infrared spectra of stars. Understanding their origin in the interstellar medium is one of the oldest problems in astronomical spectroscopy, as DIBs have been known since 1922. In a completely new approach to understanding DIBs, we combined information from nearly 500,000 stellar spectra obtained by the massive spectroscopic survey RAVE (Radial Velocity Experiment) to produce the first pseudo-three-dimensional map of the strength of the DIB at 8620 angstroms covering the nearest 3 kiloparsecs from the Sun, and show that it follows our independently constructed spatial distribution of extinction by interstellar dust along the Galactic plane. Despite having a similar distribution in the Galactic plane, the DIB 8620 carrier has a significantly larger vertical scale height than the dust. Even if one DIB may not represent the general DIB population, our observations outline the future direction of DIB research.

## The effect of diamagnetic flows on turbulent driven ion toroidal rotation

PHYSICS OF PLASMAS **21** (2014) ARTN 056106

## Equivalence of two independent calculations of the higher order guiding center Lagrangian

PHYSICS OF PLASMAS **21** (2014) ARTN 104506

## Constraining the Galaxy's dark halo with RAVE stars

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY **445** (2014) 3133-3151

## Comparative study of metamodelling techniques in building energy simulation: Guidelines for practitioners

Simulation Modelling Practice and Theory **49** (2014) C

## KINEMATIC MODELING OF THE MILKY WAY USING THE RAVE AND GCS STELLAR SURVEYS

ASTROPHYSICAL JOURNAL **793** (2014) ARTN 51

## The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

ASTRONOMY & ASTROPHYSICS **570** (2014) ARTN A122

## Optimizing stellarators for large flows

PLASMA PHYSICS AND CONTROLLED FUSION **56** (2014) ARTN 094003

## Galactic kinematics and dynamics from Radial Velocity Experiment stars

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY **439** (2014) 1231-1244

## Inboard and outboard radial electric field wells in the H- and I-mode pedestal of Alcator C-Mod and poloidal variations of impurity temperature

NUCLEAR FUSION **54** (2014) ARTN 083017

## Reduction of core turbulence in I-mode plasmas in Alcator C-Mod

NUCLEAR FUSION **54** (2014) ARTN 083019

## The final-parsec problem in nonspherical galaxies revisited

Astrophysical Journal **785** (2014)

We consider the evolution of supermassive black hole binaries at the center of spherical, axisymmetric, and triaxial galaxies, using direct N-body integrations as well as analytic estimates. We find that the rates of binary hardening exhibit a significant N-dependence in all the models, at least for N in the investigated range of 10 5 ≤ N ≤ 10 6 . Binary hardening rates are also substantially lower than would be expected if the binary "loss cone" remained "full," as it would be if the orbits supplying stars to the binary were being efficiently replenished. The difference in binary hardening rates between the spherical and nonspherical models is less than a factor of two even in the simulations with the largest N. By studying the orbital populations of our models, we conclude that the rate of supply of stars to the binary via draining of centrophilic orbits is indeed expected to be much lower than the full-loss-cone rate, consistent with our simulations. We argue that the binary's evolution in the simulations is driven in roughly equal amounts by collisional and collisionless effects, even at the highest N-values currently accessible. While binary hardening rates would probably reach a limiting value for large N, our results suggest that we cannot approach that rate with currently available algorithms and computing hardware. The extrapolation of results from N-body simulations to real galaxies is therefore not straightforward, casting doubt on recent claims that triaxiality or axisymmetry alone are capable of solving the final-parsec problem in gas-free galaxies. © 2014. The American Astronomical Society. All rights reserved.

## LINE-DRIVEN DISK WINDS IN ACTIVE GALACTIC NUCLEI: THE CRITICAL IMPORTANCE OF IONIZATION AND RADIATIVE TRANSFER

The Astrophysical Journal **789** (2014) 19-19

## Intrinsic momentum transport in up-down asymmetric tokamaks

PLASMA PHYSICS AND CONTROLLED FUSION **56** (2014) ARTN 095014