Cutaneous ectoparasites

Nordlund, James J.

doi:10.1111/j.1529-8019.2009.01273.x

Cited by 18 publications

(21 citation statements)

References 67 publications

(176 reference statements)

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“…Taken together with the reproduction of shifts and asymmetries of spectral lines (e.g. Nordlund et al 2009) and inverse granulation (Cheung et al 2007) by simulation results, our contrast data thus provide evidence for an extension of the convective overshoot to a height of roughly 300 km above the average level of optical depth unity, at which height the rms fluctuations of the vertical velocity reach a local minimum after a steep decrease (by about a factor of 4) from their maximum slightly below the visible surface (optical depth unity).…”

Section: Discussionmentioning

confidence: 99%

Quiet-Sun Intensity Contrasts in the Near-Ultraviolet as Measured From Sunrise

Hirzberger

Feller

Riethmüller

et al. 2010

ApJ

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We present high-resolution images of the Sun in the near ultraviolet spectral range between 214 nm and 397 nm as obtained from the first science flight of the 1-m Sunrise balloon-borne solar telescope. The quiet-Sun rms intensity contrasts found in this wavelength range are among the highest values ever obtained for quiet-Sun solar surface structures -up to 32.8 % at a wavelength of 214 nm. We compare with theoretical intensity contrasts obtained from numerical magneto-hydrodynamic simulations. For 388 nm and 312 nm the observations agree well with the numerical simulations whereas at shorter wavelengths discrepancies between observed and simulated contrasts remain.

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Section: Discussionmentioning

confidence: 99%

Quiet-Sun Intensity Contrasts in the Near-Ultraviolet as Measured From Sunrise

Hirzberger

Feller

Riethmüller

et al. 2010

ApJ

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“…In most stars the thickness of the superadiabatic region is determined by the hydrogen recombination region, and is much less than a pressure scale height. Such details are ignored in both MLT and the vortex model, but they are prominent in simulations (Stein & Nordlund 1998;Nordlund, Stein, & Asplund 2009). The second difference is in the coefficients multiplying these factors, equating them gives…”

Section: The Steady Vortex Modelmentioning

confidence: 99%

Preparing for an Explosion: Hydrodynamic Instabilities and Turbulence in Presupernovae

Smith

Arnett

2014

ApJ

226

232

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Both observations and numerical simulations are discordant with predictions of conventional stellar evolution codes for the latest stages of a massive star's life prior to core collapse. The most dramatic example of this disconnect is in the eruptive mass loss occurring in the decade preceding Type IIn supernovae (SNe). We outline the key empirical evidence that indicates severe pre-SN instability in massive stars, and we suggest that the chief reason these outbursts are absent in stellar evolution models may lie in the treatment of turbulent convection in these codes. The mixing length theory that is used ignores finite amplitude fluctuations in velocity and temperature, and their nonlinear interaction with nuclear burning. Including these fluctuations is likely to give rise to hydrodynamic instabilities in the latest burning sequences, which prompts us to discuss a number of far-reaching implications for the fates of massive stars. In particular, we explore connections to enhanced presupernova mass loss, unsteady nuclear burning and consequent eruptions, swelling of the stellar radius that may trigger violent interactions with a companion star, and potential modifications to the core structure that could dramatically alter calculations of the core-collapse explosion mechanism itself. These modifications may also impact detailed nucleosynthesis and measured isotopic anomalies in meteorites, as well as the interpretation of young core-collapse SN remnants. Understanding these critical instabilities in the final stages of evolution may make possible the development of an early warning system for impending core collapse, if we can identify their asteroseismological or eruptive signatures.

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“…Ferran et al (2009) also realized that a nodular lesion on the sole of a patient who had visited Venezuella contained Tunga penetrans flea. Nordlund, (2009) was also able to diagnose tungiasis from the hands, skin, toes, nails and sole of his patients. Also according to Nordlund (2009) the cases presented in the form of fissures, abscesses, suppurations.…”

Section: Discussionmentioning

confidence: 98%

The Prevalence, Risk Factors and Treatment Methods for Tungiasis among Residents of Musokoto Sub-Location, in Kenya

Ngetich¹

2016

TIJPH

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Tungiasis is a parasitic skin disease caused by sand flea Tunga penetrans. In Kenya, little data has been published regarding tungiasis. In Nambale health centre, tungiasis accounted for 4% of total morbidities. Therefore this study sought to assess the prevalence of, risk factors and treatment methods for tungiasis among residents of Musokoto, in Kenya. Purposive sampling method was used. Logistic regression was used to determine the risks factors associated with tungiasis. A total 1557 participant from 333 randomly selected households took part in the study. Of the 1557 participants, a total of 441(28.3%) at least had jiggers at one point in their life. Out of the 441, 287(65%) were confirmed to have jiggers on examination whereas 9(2%) did not have jigger by the time of the study. Toes on the extreme sites were more infested however the distribution of infestation was moral less the same for the all toes. Above 50% of those infested were aged 10 years and below. Logistical regression analysis revealed that place of sleeping (

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Cutaneous ectoparasites

Cited by 18 publications

References 67 publications

Quiet-Sun Intensity Contrasts in the Near-Ultraviolet as Measured From Sunrise

Quiet-Sun Intensity Contrasts in the Near-Ultraviolet as Measured From Sunrise

Preparing for an Explosion: Hydrodynamic Instabilities and Turbulence in Presupernovae

The Prevalence, Risk Factors and Treatment Methods for Tungiasis among Residents of Musokoto Sub-Location, in Kenya

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