Plasma torch for ignition, flameholding and enhancement of combustion in high speed flows

Preheating of fuel and injection into a plasma torch plume fro adjacent the plasma torch plume provides for only ignition with reduced delay but improved fuel-air mixing and fuel atomization as well as combustion reaction enhancement. Heat exchange also reduced erosion of the anode of the plasma torch. Fuel mixing atomization, fuel mixture distribution enhancement and combustion reaction enhancement are improved by unsteady plasma torch energization, integral formation of the heat exchanger, fuel injection nozzle and plasma torch anode in a more compact, low-profile arrangement which is not intrusive on a highspeed air flow with which the invention is particularly effective and further enhanced by use of nitrogen as a feedstock material and inclusion of high pressure gases in the fuel to cause effervescence during injection

Molecular Gas in the Powerful Radio Nucleus of the Ultraluminous Infrared Galaxy PKS 1345+12

Millimeter CO(1-0) interferometry and high resolution, Hubble Space Telescope (HST) 1.1, 1.6, and 2.2 micron imaging of the radio compact galaxy PKS 1345+12 are presented. With an infrared luminosity of 2x10^{12} L_sun, PKS 1345+12 is a prime candidate for studying the link between the ultraluminous infrared galaxy phenomenon and radio galaxies. These new observations probe the molecular gas distribution and obscured nuclear regions of PKS 1345+12 and provide morphological support for the idea that the radio activity in powerful radio galaxies is triggered by the merger of gas rich galaxies. Two nuclei separated by 2" (4.0 kpc) are observed in the near-infrared; the extended southeastern nucleus has colors consistent with reddened starlight, and the compact northwestern nucleus has extremely red colors indicative of an optical quasar with a warm dust component. Further, the molecular gas, 3mm continuum, and radio emission are coincident with the redder nucleus, confirming that the northwestern nucleus is the site of the AGN and that the molecular gas is the likely fuel source.Comment: LaTex, 5 pages with 1 postscript and 1 jpg figure, ApJ Letters, in press (August 20, 1999

STIS ultraviolet/optical spectroscopy of `warm' ultraluminous infrared galaxies

(Abridged) We present high spatial resolution ultraviolet and optical spectroscopy, obtained using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope, of nuclear structures within four `warm' Ultraluminous Infrared Galaxies (ULIRGs). We find an AGN in at least three, and probably all four of our sample, hosted in a compact, optically luminous `knot'. In three cases these knots were previously identified as a putative AGN nucleus from multiband optical imaging. Three of the sample also harbor a starburst in one or more knots, suggesting that the optically luminous knots seen in local ULIRGs are the most likely sites of the dust-shrouded starburst and AGN activity that power the infrared emission. The four AGN have a diverse range of properties; two are classical narrow line AGN, one shows both broad and narrow lines and evidence for lines of sight from the narrow through to the broad line regions, and one is plausibly a FeLoBAL AGN. The probable presence in one object of an FeLoBAL AGN, which are extremely rare in the QSO population, supports the idea that LoBAL AGN may be youthful systems shrouded in gas and dust rather than AGN viewed along a certain line of sight. The three starbursts for which detailed constraints are possible show a smaller range in properties; all three bursts are young with two having ages of ~4Myr and the third having an age of 20Myr, suggesting that ULIRGs undergo several bursts of star formation during their lifetimes. None of the starbursts show evidence for Initial Mass Function slopes steeper than about 3.3. The metallicities of the knots for which metallicities can be derived are all at least 1.5 times the Solar value. The properties of one further starburst knot are consistent with it being the forming core of an elliptical galaxy.Comment: ApJ, accepte

Evaluation of movement behaviors to inform toxic baiting strategies for invasive wild pigs (\u3ci\u3eSus scrofa\u3c/i\u3e)

BACKGROUND: Invasive wild pigs damage agriculture, property, and natural ecosystems. To curtail damage, an effective and humane toxic bait containing microencapsulated sodium nitrite is under development. Strategies for delivering the toxic bait are needed to establish adequate spacing of bait sites, and for simultaneously accustoming wild pigs to the novel bait and wild pig-specific bait stations designed to exclude non-target species. RESULTS: We monitored movements of 32 Global Positioning System (GPS)-collared wild pigs relative to 41 bait sites containing placebo bait. Among the bait sites,we compared three experimental baiting strategies (and a control) to evaluate which strategy led to the most wild pigs accessing the placebo bait inside bait stations. We found that bait sites should be spaced 0.5–1 km apart to maximize opportunities for all wild pigs to find and utilize the bait sites. Baiting strategies that allowed ≥ 15 days for accustoming wild pigs to bait stations were most effective and resulted in nearly 90% of wild pigs accessing the placebo bait inside the bait stations. Bait stations excluded all non-target animals, except one instance with a raccoon (Procyon lotor). CONCLUSION: These results demonstrate the potential for toxic bait to be an effective tool for reducing populations of wild pigs with minimal risks to non-target species, if optimized delivery procedures are followed

Measuring Star-formation Rate and Far-Infrared Color in High-redshift Galaxies Using the CO (7-6) and [NII] 205 micron Lines

To better characterize the global star formation (SF) activity in a galaxy, one needs to know not only the star formation rate (SFR) but also the rest-frame, far-infrared (FIR) color (e.g., the 60-to-100 $\mu$m color, $C(60/100)$] of the dust emission. The latter probes the average intensity of the dust heating radiation field and scales statistically with the effective SFR surface density in star-forming galaxies including (ultra-)luminous infrared galaxies [(U)LIRGs]. To this end, we exploit here a new spectroscopic approach involving only two emission lines: CO\,(7$-$6) at 372 $\mu$m and [NII] at 205 $\mu$m. For local (U)LIRGs, the ratios of the CO (7$-$6) luminosity ($L_{\rm CO\,(7-6)}$) to the total infrared luminosity ($L_{\rm IR}$; 8$-$1000 $\mu$m) are fairly tightly distributed (to within $\sim$0.12 dex) and show little dependence on $C(60/100)$. This makes $L_{\rm CO\,(7-6)}$ a good SFR tracer, which is less contaminated by active galactic nuclei (AGN) than $L_{\rm IR}$ and may also be much less sensitive to metallicity than $L_{\rm CO\,(1-0)}$. Furthermore, the logarithmic [NII] 205 $\mu$m to CO (7$-$6) luminosity ratio is fairly steeply (at a slope of $\sim$$-1.4$) correlated with $C(60/100)$, with a modest scatter ($\sim$0.23 dex). This makes it a useful estimator on $C(60/100)$ with an implied uncertainty of $\sim$0.15 [or $\lesssim$4 K in the dust temperature ($T_{\rm dust}$) in the case of a graybody emission with $T_{\rm dust} \gtrsim 30$ K and a dust emissivity index $\beta \ge 1$]. Our locally calibrated SFR and $C(60/100)$ estimators are shown to be consistent with the published data of (U)LIRGs of $z$ up to $\sim$6.5.Comment: 6 pages, 3 figures, 1 table; accepted for publication in the ApJ Lette

Electrophysiological effects of 5-hydroxytryptamine on isolated human atrial myocytes, and the influence of chronic beta-adrenoceptor blockade

<b>1.</b> 5-Hydroxytryptamine (5-HT) has been postulated to play a proarrhythmic role in the human atria via stimulation of 5-HT<sub>4</sub> receptors. <b>2.</b> The aims of this study were to examine the effects of 5-HT on the L-type Ca<sup>2+</sup> current (<i>I</i><sub>CaL</sub>) action potential duration (APD), the effective refractory period (ERP) and arrhythmic activity in human atrial cells, and to assess the effects of prior treatment with β-adrenoceptor antagonists. <b>3.</b> Isolated myocytes, from the right atrial appendage of 27 consenting patients undergoing cardiac surgery who were in sinus rhythm, were studied using the whole-cell perforated patch-clamp technique at 37ºC. <b>4.</b> 5-HT (1 n-10 μM) caused a concentration-dependent increase in <i>I</i><sub>CaL</sub>, which was potentiated in cells from β-blocked (maximum response to 5-HT, E<sub>max</sub>=299±12% increase above control) compared to non-β-blocked patients (E<sub>max</sub>=220±6%, P<0.05), but with no change in either the potency (log EC<sub>50</sub>: -7.09±0.07 vs -7.26±0.06) or Hill coefficient (<i>n</i><sub>H</sub>: 1.5±0.6 vs 1.5±0.3) of the 5-HT concentration-response curve. <b>5.</b> 5-HT (10 μM) produced a greater increase in the APD at 50% repolarisation (APD50) in cells from β-blocked patients (of 37±10 ms, i.e. 589±197%) vs non-β-blocked patients (of 10±4 ms, i.e. 157±54%; P<0.05). Both the APD<sub>90</sub> and the ERP were unaffected by 5-HT. <b>6.</b> Arrhythmic activity was observed in response to 5-HT in five of 17 cells (29%) studied from β-blocked, compared to zero of 16 cells from the non-β-blocked patients (P<0.05). <b>7.</b> In summary, the 5-HT-induced increase in calcium current was associated with a prolonged early plateau phase of repolarisation, but not late repolarisation or refractoriness, and the enhancement of these effects by chronic β-adrenoceptor blockade was associated with arrhythmic potential

Sessile Serrated Adenomas in the Proximal Colon are Likely to be Flat, Large and Occur in Smokers

Aim: To examine the epidemiology and the morphology of the proximal sessile serrated adenomas (SSAs). Methods: We conducted a retrospective study to identify patients with SSAs using a university-based hospital pathology database query from January 2007 to April 2011. Data collected included: age, gender, ethnicity, body mass index, diabetes, smoking, family history of colorectal cancer, aspirin, and statin use. We collected data on morphology of SSAs including site (proximal or distal), size, and endoscopic appearance (flat or protuberant). We also compared proximal SSAs to proximal tubular adenomas detected during same time period

Topological Phases near a Triple Degeneracy

We study the pattern of three state topological phases that appear in systems with real Hamiltonians and wave functions. We give a simple geometric construction for representing these phases. We then apply our results to understand previous work on three state phases. We point out that the ``mirror symmetry'' of wave functions noticed in microwave experiments can be simply understood in our framework.Comment: 4 pages, 1 figure, to appear in Phys. Rev. Let

First Views of a Nearby LIRG: Star Formation and Molecular Gas in IRAS 04296+2923

We present a first look at the local LIRG, IRAS04296+2923. This barred spiral, overlooked because of its location in the Galactic plane, is among the half dozen closest LIRGs. More IR-luminous than either M82 or the Antennae, it may be the best local example of a nuclear starburst caused by bar-mediated secular evolution. We present Palomar J and Pa beta images, VLA maps from 20-1.3cm, a Keck LWS image at 11.7mic and OVRO CO(1-0) and ^13CO(1-0), and 2.7 mm continuum images. The J-band image shows a symmetric barred spiral. Two bright, compact mid-IR/radio sources in the nucleus comprise a starburst that is equivalent to 10^5 O7 stars, probably a pair of young super star clusters separated by 30pc. The nuclear starburst is forming stars at the rate of ~12Msun/yr, half of the total star formation rate for the galaxy of ~25Msun/yr. IRAS04296 is bright in CO, and among the most gas-rich galaxies in the local universe. The CO luminosity of the inner half kpc is equivalent to that of the entire Milky Way. While the most intense CO emission extends over a 15"(2 kpc) region, the nuclear starburst is confined to ~1-2"(150-250 pc) of the dynamical center. From ^13CO, we find that the CO conversion factor in the nucleus is higher than the Galactic value by a factor 3-4, typical of gas-rich spiral nuclei. The nuclear star formation efficiency is M_gas/SFR^nuc = 2.7x10^-8 yr^-1, corresponding to gas consumption timescale, tau_SF^nuc~4x10^7 yrs. The star formation efficiency is ten times lower in the disk, tau_SF^disk~3.3x10^8 yrs. The low absolute star formation efficiency in the disk implies that the molecular gas is not completely consumed before it drifts into the nucleus, and is capable of fueling a sustained nuclear starburst. IRAS04296 is beginning a 100Myr period as a LIRG, during which it will turn much of its 6x10^9Msun of molecular gas into a nuclear cluster of stars. (abridged)Comment: Accepted, Astronomical Journa