Mobile Device Management for Personally Controlled Electronic Health Records: Effective Selection of Evaluation Criteria

Enterprises are faced with the task of managing a plethora of mobile computing devices in the workplace that are employed for both business purposes and private use. This integration can contribute to the demands of security protection and add significant threats to the enterprise. The introduction of the Personally Controlled Electronic Health Record (PCEHR) system is a significant step in e-health for Australia and will likely result in sensitive information being accessed from mobile computing devices. Mobile Device Management (MDM) offers a potential solution to manage these devices, however there is a variety of vendors with a range of solutions. This paper presents preliminary research into a generic methodology that could be used to assist the enterprise in the MDM selection process particularly when mobile devices will eventually integrate with the Australia’s PCEHR

Mobile Device Management for Personally Controlled Electronic Health Records: Effective Selection of Evaluation Criteria

Enterprises are faced with the task of managing a plethora of mobile computing devices in the workplace that are employed for both business purposes and private use. This integration can contribute to the demands of security protection and add significant threats to the enterprise. The introduction of the Personally Controlled Electronic Health Record (PCEHR) system is a significant step in e-health for Australia and will likely result in sensitive information being accessed from mobile computing devices. Mobile Device Management (MDM) offers a potential solution to manage these devices, however there is a variety of vendors with a range of solutions. This paper presents preliminary research into a generic methodology that could be used to assist the enterprise in the MDM selection process particularly when mobile devices will eventually integrate with the Australia’s PCEHR

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst I. The optically thick phase and the origin of moving lines in novae

The nova T Pyx was observed with high resolution spectroscopy (R ~ 65000) spectroscopy, beginning 1 day after discovery of the outburst and continuing through the last visibility of the star at the end of May 2011. The interstellar absorption lines of Na I, Ca II, CH, CH$^+$, and archival H I 21 cm emission line observations have been used to determine a kinematic distance. Interstellar diffuse absorption features have been used to determine the extinction independent of previous assumptions. Sample Fe-peak line profiles show the optical depth and radial velocity evolution of the discrete components. We propose a distance to T Pyx $\geq$4.5kpc, with a strict lower limit of 3.5 kpc (the previously accepted distance). We derive an extinction, E(B-V)$\approx0.5\pm$0.1, that is higher than previous estimates. The first observation, Apr. 15, displayed He I, He II, C III, and N III emission lines and a maximum velocity on P Cyg profiles of the Balmer and He I lines of $\approx$2500 km s$^{-1}$ characteristic of the fireball stage. These ions were undetectable in the second spectrum, Apr. 23, and we use the recombination time to estimate the mass of the ejecta, $10^{-5}f$M$_\odot$ for a filling factor $f$. Numerous absorption line systems were detected on the Balmer, Fe-peak, Ca II, and Na I lines, mirrored in broader emission line components, that showed an "accelerated" displacement in velocity. We also show that the time sequence of these absorptions, which are common to all lines and arise only in the ejecta, can be described by recombination front moving outward in the expanding gas without either a stellar wind or circumstellar collisions.Comment: Accepted for publication in Astronomy & Astrophysics Letters (17/8/11

Ariel - Volume 4 Number 4

Editors David A. Jacoby Eugenia Miller Tom Williams Associate Editors Paul Bialas Terry Burt Michael Leo Gail Tenikat Editor Emeritus and Business Manager Richard J. Bonnano Movie Editor Robert Breckenridge Staff Richard Blutstein Mary F. Buechler Meg Brunt Steve Glinks Len Grasman Alice M. Johnson J.D. Kanofsky Tom Lehman Dave Mayer Bernie Odd

Modulation of Cox-1, 5-, 12- and 15-Lox by popular herbal remedies used in southern Italy against psoriasis and other skin diseases.

Acanthus mollis (Acanthaceae), Achillea ligustica, Artemisia arborescens and Inula viscosa (Asteraceae) are used in Southern Italy against psoriasis and other skin diseases that occur with an imbalanced production of eicosanoids. We here assessed their in vitro effects upon 5-, 12-, 15-LOX and COX-1 enzymes as well as NFκB activation in intact cells as their possible therapeutic targets. All methanol crude extracts inhibited both 5-LOX and COX-1 activities under 200 µg/mL, without significant effects on the 12-LOX pathway or any relevant in vitro free radical scavenging activity. NFκB activation was prevented by all extracts but A. mollis. Interestingly, A. ligustica, A. arborescens and A. mollis increased the biosynthesis of 15(S)-HETE, an anti-inflammatory eicosanoid. A. ligustica (IC50 =49.5 µg/mL) was superior to Silybum marianum (IC50 =147.8 µg/mL), which we used as antipsoriatic herbal medicine of reference. Its n-hexane, dichloromethane and ethyl acetate fractions had also inhibitory effects on the LTB4 biosynthesis (IC50 s=9.6, 20.3 and 68 µg/mL, respectively) evidencing that the apolar extracts of A. ligustica are promising active herbal ingredients for future phytotherapeutical products targeting psoriasis

Clumpy outer Galaxy molecular clouds and the steepening of the IMF

We report the results of high-resolution (~0.2 pc) CO(1-0) and CS(2-1) observations of the central regions of three star-forming molecular clouds in the far-outer Galaxy (~16 kpc from the Galactic Center): WB89 85 (Sh 2-127), WB89 380, and WB89 437. We used the BIMA array in combination with IRAM 30-m and NRAO 12-m observations. The GMC's in which the regions are embedded were studied by means of KOSMA 3-m CO(2-1) observations. The properties the CO and CS clumps are analyzed and compared with newly derived results of previously published single-dish measurements of local clouds (OrionB South and Rosette). We find that the slopes of the clump mass distributions (-1.28 and -1.49, for WB89 85 and WB89 380, respectively) are somewhat less steep than found for most local clouds, but similar to those of clouds which have been analyzed with the same clumpfind program. We investigate the clump stability by using the virial theorem, including all possible contributions (gravity, turbulence, magnetic fields, and pressure due to the interclump gas). It appears that under reasonable assumptions a combination of these forces would render most clumps stable. Comparing only gravity and turbulence, we find that in the far-outer Galaxy clouds, these forces are in equilibium (virial parameter alpha~1) for clumps down to the lowest masses found (a few Msol). For clumps in the local clouds alpha~1 only for clumps with masses larger than a few tens of Msol. Thus it appears that in these outer Galaxy clumps gravity is the dominant force down to a much lower mass than in local clouds, implying that gravitational collapse and star formation may occur more readily even in the smallest clumps. Although there are some caveats, due to the inhomogeneity of the data used, this might explain the apparently steeper IMF found in the outer Galaxy.Comment: 29 pages, including 9 tables, 21 figures. Accepted for Astron. Astrop

Dualism in action

We know what one dualist account of human action looks like, because Descartes gave us one. I want to explore the extent ot which presnet-day accounts of physical action are vulnerable to the charges that may be made against Descartes's dualist account. I once put forward an account of human action, and I have always maintained that my view about the basic shape of a correct ‘theory of aciton’ can be combined with a thoroughgoing opposition to dualism. But the possibility of the combination has been doubted and it will remain doubtful until we have a better understanding of what makes an account objectionably dualistic. In this paper, I hope to deflect some of the criticims aimed what I shall call my account, and to show that when they are turned onto their proper path their actual target is some physicalist accounts

Physical Characteristics of a Dark Cloud in an Early Stage of Star Formation toward NGC 7538: an Outer Galaxy Infrared Dark Cloud?

In the inner parts of the Galaxy the Infrared Dark Clouds (IRDCs) are presently believed to be the progenitors of massive stars and star clusters. Many of them are predominantly devoid of active star formation and for now they represent the earliest observed stages of massive star formation. Their Outer Galaxy counterparts, if present, are not easily identified because of a low or absent mid-IR background. We characterize the ambient conditions in the Outer Galaxy IRDC candidate G111.80+0.58, a relatively quiescent molecular core complex in the vicinity of NGC7538. We conduct molecular line observations on a number of dense cores and analyze the data in terms of excitation temperature, column and volume density, mass and stability. The temperatures (15-20K) are higher than expected from only cosmic ray heating, but comparable to those found in massive cores. Star forming activity could be present in some cores, as indicated by the presence of warm gas and YSO candidates. The observed super-thermal line-widths are typical for star forming regions. The velocity dispersion is consistent with a turbulent energy cascade over the observed size scales. We do not find a correlation between the gas temperature and the line-width. The LTE masses we find are much larger than the thermal Jeans mass and fragmentation is expected. In that case the observed lines represent the combined emission of multiple unresolved components. We conclude that G111.80+0.58 is a molecular core complex with bulk properties very similar to IRDCs in an early, but not pristine, star forming state. The individual cores are close to virial equilibrium and some contain sufficient material to form massive stars and star clusters. The ambient conditions suggest that turbulence is involved in supporting the cores against gravitational collapse.Comment: Accepted for publication in A&A -- 19 pages, 9 figures -- high resolution available at http://www.astro.rug.nl/~frieswyk/Data/Research/OGIRDC/index.htm