The traveling salesman problem, conformal invariance, and dense polymers

We propose that the statistics of the optimal tour in the planar random Euclidean traveling salesman problem is conformally invariant on large scales. This is exhibited in power-law behavior of the probabilities for the tour to zigzag repeatedly between two regions, and in subleading corrections to the length of the tour. The universality class should be the same as for dense polymers and minimal spanning trees. The conjectures for the length of the tour on a cylinder are tested numerically.Comment: 4 pages. v2: small revisions, improved argument about dimensions d>2. v3: Final version, with a correction to the form of the tour length in a domain, and a new referenc

Vorticity imbalance and stability in relation to convection

A complete synoptic-scale vorticity budget was related to convection storm development in the eastern two-thirds of the United States. The 3-h sounding interval permitted a study of time changes of the vorticity budget in areas of convective storms. Results of analyses revealed significant changes in values of terms in the vorticity equation at different stages of squall line development. Average budgets for all areas of convection indicate systematic imbalance in the terms in the vorticity equation. This imbalance resulted primarily from sub-grid scale processes. Potential instability in the lower troposphere was analyzed in relation to the development of convective activity. Instability was related to areas of convection; however, instability alone was inadequate for forecast purposes. Combinations of stability and terms in the vorticity equation in the form of indices succeeded in depicting areas of convection better than any one item separately

Signatures of the Milky Way's Dark Disk in Current and Future Experiments

In hierarchical structure formation models of disk galaxies, a dark matter disk forms as massive satellites are preferentially dragged into the disk-plane where they dissolve. Here, we quantify the importance of this dark disk for direct and indirect dark matter detection. The low velocity of the dark disk with respect to the Earth enhances detection rates in direct detection experiments at low recoil energy. For WIMP masses M_{WIMP} >~ 50 GeV, the detection rate increases by up to a factor of 3 in the 5 - 20 keV recoil energy range. Comparing this with rates at higher energy is sensitive to M_{WIMP}, providing stronger mass constraints particularly for M_{WIMP}>~100 GeV. The annual modulation signal is significantly boosted by the dark disk and the modulation phase is shifted by ~3 weeks relative to the dark halo. The variation of the observed phase with recoil energy determines M_{WIMP}, once the dark disk properties are fixed by future astronomical surveys. The low velocity of the particles in the dark disk with respect to the solar system significantly enhances the capture rate of WIMPs in the Sun, leading to an increased flux of neutrinos from the Sun which could be detected in current and future neutrino telescopes. The dark disk contribution to the muon flux from neutrino back conversion at the Earth is increased by a factor of ~5 compared to the SHM, for rho_d/rho_h=0.5.Comment: 5 pages, 7 figures, To appear in the proceedings of Identification of Dark Matter 2008 (IDM2008), Stockholm, 18-22 August 2008; corrected one referenc

Dark matter cores all the way down

We use high resolution simulations of isolated dwarf galaxies to study the physics of dark matter cusp-core transformations at the edge of galaxy formation: M200 = 10^7 - 10^9 Msun. We work at a resolution (~4 pc minimum cell size; ~250 Msun per particle) at which the impact from individual supernovae explosions can be resolved, becoming insensitive to even large changes in our numerical 'sub-grid' parameters. We find that our dwarf galaxies give a remarkable match to the stellar light profile; star formation history; metallicity distribution function; and star/gas kinematics of isolated dwarf irregular galaxies. Our key result is that dark matter cores of size comparable to the stellar half mass radius (r_1/2) always form if star formation proceeds for long enough. Cores fully form in less than 4 Gyrs for the M200 = 10^8 Msun and 14 Gyrs for the 10^9 Msun dwarf. We provide a convenient two parameter 'coreNFW' fitting function that captures this dark matter core growth as a function of star formation time and the projected stellar half mass radius. Our results have several implications: (i) we make a strong prediction that if LCDM is correct, then 'pristine' dark matter cusps will be found either in systems that have truncated star formation and/or at radii r > r_1/2; (ii) complete core formation lowers the projected velocity dispersion at r_1/2 by a factor ~2, which is sufficient to fully explain the 'too big to fail problem'; and (iii) cored dwarfs will be much more susceptible to tides, leading to a dramatic scouring of the subhalo mass function inside galaxies and groups.Comment: 20 pages; 9 figures; final version to appear in MNRAS including typos corrected in proo

A Retrospective Case Study of the Thematic Content of Psychotic Experiences in a First Episode Psychosis Population

Background. Historically, the content of psychotic experiences has tended to be of little importance to biological psychiatry, with hallucinations and delusions being seen as symptoms of mental illness rather than meaningful experiences or responses to life circumstances. Aims. This study aims to explore the thematic content of psychotic phenomena in a sample of clients with a first episode of psychosis. Methods. The electronic medical records of 160 services users of two Early Intervention for Psychosis Services were comprehensively reviewed. A thematic analysis was used to explore the thematic content of psychotic symptoms recorded by healthcare professionals. Results. The results illustrate 30 themes and 85 sub-themes. This includes delusional beliefs (e.g. “being harmed, attacked or killed”, “being monitored or followed by others”, “special powers or abilities”) and hallucinations (e.g. “commanding voice”, “derogatory/critical voice”, “commentary”). Conclusions. The results illustrate the extensive and varied experience of psychosis within this sample. Based on the findings of this study, it is hoped that future research studies and mental health services will attend to the meaning and content of psychotic experiences

The Beliefs of Non-Psychiatric Doctors about the Causes, Treatments and Prognosis of Schizophrenia

Objectives To examine the causal beliefs about schizophrenia of non‐psychiatric doctors and whether differential belief in biogenetic vs. psychosocial causes influences doctors’ views about treatments and prognosis. Design and methods Three hundred and five non‐psychiatric doctors working in outpatient community centres completed the ‘Opinions on mental disorders Questionnaire’ after reading a clinical description of people with schizophrenia. Results The factors most frequently reported as causes of schizophrenia were heredity (65.2%) and use of street drugs (54.1%). Seventy‐five per cent of participants endorsed both one or more biological causal factors and one or more psychosocial causal factors. Of the 264 participants who expressed their opinion about the most important cause of schizophrenia, 53.8% indicated a biogenetic cause. Fifty‐two per cent of respondents thought it ‘completely true’ that drugs are useful in schizophrenia, and 33.9% thought it ‘completely true’ that people with schizophrenia must take drugs all their life. Participants stating that the most important cause was biogenetic more frequently recommended a psychiatrist and less frequently a psychologist. Compared to doctors who indicated a psychosocial cause as the most important one, those who indicated a biogenetic cause were more sceptical about recovery, more confident in the usefulness of drugs, and more convinced of the need of lifelong pharmacological treatments in schizophrenia. Conclusions These findings suggest the need to provide some doctors with training on the multiple, interacting causes of schizophrenia and the efficacy of the broad range of available treatments. The education of health professionals regarding stigma and its effects on clinical practice is also needed

Teleconnection in the martian atmosphere during the 2001 planet-encircling dust storm

Introduction: In July 2001 (Martian year 25), Mars was enshrouded by a thick veil of dust which lasted for several months and obscured the observation of its surface to spacecraft cameras and ground-based telescopes. The emergence and rapid evolution (within a few days) of multiple, isolated, regional dust storms which eventually attained planetary scale extent were observed by NASA’s Mars Global Surveyor (MGS) spacecraft using high resolution camera images and the thermal profiles and dust opacity measurements pro-vided by the Thermal Emission Spectrometer (TES) [1, 2]. We have applied a technique used in Terrestrial meteorology (sequential data assimilation, [3]) to ob-tain a complete, four-dimensional evolution of all the atmospheric variables during the period of this planet-encircling dust storm, even those which were not di-rectly observed by the MGS satellite, such as surface pressure and winds. We assimilated TES nadir-pointing thermal profiles and total dust opacities in a global circulation model of the Martian atmosphere, developed jointly by the University of Oxford and the Open University in the United Kingdom, with the col-laboration of the Laboratoire de Météorologie Dyna-mique in Paris (UK-MGCM) [4, 5, 6]

Dense loops, supersymmetry, and Goldstone phases in two dimensions

Loop models in two dimensions can be related to O(N) models. The low-temperature dense-loops phase of such a model, or of its reformulation using a supergroup as symmetry, can have a Goldstone broken-symmetry phase for N<2. We argue that this phase is generic for -2< N <2 when crossings of loops are allowed, and distinct from the model of non-crossing dense loops first studied by Nienhuis [Phys. Rev. Lett. 49, 1062 (1982)]. Our arguments are supported by our numerical results, and by a lattice model solved exactly by Martins et al. [Phys. Rev. Lett. 81, 504 (1998)].Comment: RevTeX, 5 pages, 3 postscript figure