Secondary Bursts Research Articles

Air valve arrangement criteria for preventing secondary pipe bursts in long-distance gravitational water supply systems

Abstract Pipe burst incidents in long-distance gravitational water supply systems (LGWSSs) result in hydraulic characteristic variations and pose significant challenges. This study aims to prevent secondary pipe bursts by addressing the propagation of water hammer waves triggered by primary pipe bursts. Based on an analysis of pipe burst incidents and considering different pipe laying methods, air valve arrangement criteria are developed to mitigate the risk of secondary bursts in LGWSS pipelines. The principal results include a reasonable mathematical analysis model for understanding pipe bursts and the determination of air valve arrangement criteria which considers potentially dangerous pressure variations resulting from primary pipe bursts. This model aims to mitigate the adverse effects of pipe bursts and minimize the likelihood of secondary bursts. Implementing the proposed criteria has important engineering applications, thus improving the reasonable and effective placement of air valves to prevent secondary pipe bursts in LGWSSs. The conclusion involves optimizing the placement of air valves to enhance the flexibility and reliability of LGWSSs. By implementing the proposed air valve arrangement criteria, water supply systems can minimize the potential damage caused by pipe bursts and improve overall operational efficiency.

Molecular Gas Reservoirs in Massive Quiescent Galaxies at z ∼ 0.7 Linked to Late-time Star Formation

We explore how the presence of detectable molecular gas depends on the inferred star formation histories (SFHs) in eight massive, quiescent galaxies at z ∼ 0.7. Half of the sample have clear detections of molecular gas, traced by CO(2–1). We find that the molecular gas content is unrelated to the rate of star formation decline prior to the most recent 1 Gyr, suggesting that the gas reservoirs are not left over from their primary star formation epoch. However, the recent SFHs of CO-detected galaxies demonstrate evidence for secondary bursts of star formation in their last Gyr. The fraction of stellar mass formed in these secondary bursts ranges from f burst ≈ 0.3%–6% and ended between t end-burst ≈ 0–330 Myr ago. The CO-detected galaxies form a higher fraction of mass in the last Gyr () compared to the CO-undetected galaxies (). The galaxies with gas reservoirs have enhanced late-time star formation, highlighting this as a contributing factor to the observed heterogeneity in the gas reservoirs in high-redshift quiescent galaxies. We find that the amount of gas and star formation driven by these secondary bursts are inconsistent with that expected from dry minor mergers, and instead are likely driven by recently accreted gas, i.e., gas-rich minor mergers. This conclusion would not have been made based on SFRUV+IR measurements alone, highlighting the power of detailed SFH modeling in the interpretation of gas reservoirs. Larger samples are needed to understand the frequency of low-level rejuvenation among quiescent galaxies at intermediate redshifts, and to what extent this drives the diversity of molecular gas reservoirs.

Inertia–Gravity Waves Breaking in the Middle Atmosphere at High Latitudes: Energy Transfer and Dissipation Tensor Anisotropy

Abstract We present direct numerical simulations of inertia–gravity waves breaking in the middle–upper mesosphere. We consider two different altitudes, which correspond to the Reynolds number of 28 647 and 114 591 based on wavelength and buoyancy period. While the former was studied by Remmler et al., it is here repeated at a higher resolution and serves as a baseline for comparison with the high-Reynolds-number case. The simulations are designed based on the study of Fruman et al., and are initialized by superimposing primary and secondary perturbations to the convectively unstable base wave. Transient growth leads to an almost instantaneous wave breaking and secondary bursts of turbulence. We show that this process is characterized by the formation of fine flow structures that are predominantly located in the vicinity of the wave’s least stable point. During the wave breakdown, the energy dissipation rate tends to be an isotropic tensor, whereas it is strongly anisotropic in between the breaking events. We find that the vertical kinetic energy spectra exhibit a clear 5/3 scaling law at instants of intense energy dissipation rate and a cubic power law at calmer periods. The term-by-term energy budget reveals that the pressure term is the most important contributor to the global energy budget, as it couples the vertical and the horizontal kinetic energy. During the breaking events, the local energy transfer is predominantly from the mean to the fluctuating field and the kinetic energy production is in balance with the pseudo kinetic energy dissipation rate.

Fin and body neuromuscular coordination changes during walking and swimming in Polypterus senegalus.

The ability to modulate the function of muscle is integral to an animal's ability to function effectively in the face of widely disparate challenges. This modulation of function can manifest through short-term changes in neuromuscular control, but also through long-term changes in force profiles, fatiguability and architecture. However, the relative extent to which shorter-term modulation and longer-term plasticity govern locomotor flexibility remains unclear. Here, we obtain simultaneously recorded kinematic and muscle activity data of fin and body musculature of an amphibious fish, Polypterus senegalus After examining swimming and walking behaviour in aquatically raised individuals, we show that walking behaviour is characterized by greater absolute duration of muscle activity in most muscles when compared with swimming, but that the magnitude of recruitment during walking is only increased in the secondary bursts of fin muscle and in the primary burst of the mid-body point. This localized increase in intensity suggests that walking in P. senegalus is powered in a few key locations on the fish, contrasting with the more distributed, low intensity muscle force that characterizes the stroke cycle during swimming. Finally, the increased intensity in secondary, but not primary, bursts of the fin muscles when walking probably underscores the importance of antagonistic muscle activity to prevent fin collapse, add stabilization and increase body support. Understanding the principles that underlie the flexibility of muscle function can provide key insights into the sources of animal functional and behavioural diversity.

New insights into the quasi-periodic X-ray burster GS 0836–429

GS 0836-429 is a neutron star X-ray transient that displays Type-I X-ray bursts. In 2003 and 2004 it experienced two outbursts in X-rays. We present here an analysis of the system bursting properties during these outbursts. We studied the evolution of the 2003-2004 outbursts in soft X-rays using RXTE (2.5-12 keV; ASM), and in hard X-rays with INTEGRAL (17-80 keV, IBIS/ISGRI). Using data from the JEM-X monitor onboard INTEGRAL we detected 61 Type-I X-ray bursts, and confirm that the source displayed a quasi-periodic burst recurrence time of about 2.3 hours. We improve the characterization of the fuel composition, as well as the description of the typical burst durations and fluences. We estimate the average value of $\alpha$ to be $49\pm\,3$. This value together with the observed burst profiles indicate a regime of a mixed He/H runaway triggered by unstable helium ignition. In addition, we report the detection of four series of double bursts, with burst recurrence times of $\leq\,20$ minutes. The measured recurrence time in double bursts is too short to allow the accretion of enough fresh material, necessary to trigger a Type-I X-ray burst. This suggests the presence of left-over, unburned material from the preceding burst which gets ignited in a time scale of minutes. The energies and time scales of the secondary bursts suggest a lower fraction of hydrogen compared to that estimated for the primary bursts. The persistent emission was roughly constant during the period when the Type I X-ray bursts were detected. We derive an average accretion rate during our observations of $\dot{m}\sim\,8\,\%\,\dot{m}_{Edd}$. The spectrum of the persistent emission can be fit with a non-thermal component, indicative for the source to be in a hard state when the INTEGRAL observations were performed.

Studies of the stellar populations of galaxies using two-color diagrams

Variations in the photometric parameters of stellar systems as a function of their evolution and the stellar populations comprising them are investigated. A set of seven evolutionary models with an exponential decrease in the star-formation rate and 672 models with a secondary burst of star formation are considered. The occurrence of a secondary burst of star formation can shift the position of a stellar system on two-color diagrams to the right or left of the normal color sequence for galaxies and the extinction line. This makes it possible to estimate the composition of the stellar population of a galaxy with a nonmonotonic star formation history from its position on two-color diagrams. Surface photometry in both the optical (UBVRI) and near-IR (JHK) is used to study the stellar populations and star-formation histories in the structural components (nucleus, bulge, disk, spiral arms, bar, ring) of 26 galaxies of various morphological types (from S0 to Sd). Components (nucleus, bulge, bar) with color characteristics corresponding to stellar systems with secondary bursts of star formation are indicated in 10 of the 26 galaxies. The parameters of these secondary bursts are estimated. Five of the 10 galaxies with complex star-formation histories display clear structural perturbations. Appreciable differences in the photometric characteristics of relatively red early-type galaxies (S0-Sb) and relatively blue later-type galaxies (Sb-Sd) have been found. Galaxies of both early and late types are encountered among the Sb-galaxies. Lenticular galaxies do not display different photometric characteristics from early-type spiral galaxies.

STAR FORMATION IN NUCLEAR RINGS OF BARRED GALAXIES

Nuclear rings in barred galaxies are sites of active star formation. We use hydrodynamic simulations to study temporal and spatial behavior of star formation occurring in nuclear rings of barred galaxies where radial gas inflows are triggered solely by a bar potential. The star formation recipes include a density threshold, an efficiency, conversion of gas to star particles, and delayed momentum feedback via supernova explosions. We find that star formation rate (SFR) in a nuclear ring is roughly equal to the mass inflow rate to the ring, while it has a weak dependence on the total gas mass in the ring. The SFR typically exhibits a strong primary burst followed by weak secondary bursts before declining to very small values. The primary burst is associated with the rapid gas infall to the ring due to the bar growth, while the secondary bursts are caused by re-infall of the ejected gas from the primary burst. While star formation in observed rings persists episodically over a few Gyr, the duration of active star formation in our models lasts for only about a half of the bar growth time, suggesting that the bar potential alone is unlikely responsible for gas supply to the rings. When the SFR is low, most star formation occurs at the contact points between the ring and the dust lanes, leading to an azimuthal age gradient of young star clusters. When the SFR is large, on the other hand, star formation is randomly distributed over the whole circumference of the ring, resulting in no apparent azimuthal age gradient. Since the ring shrinks in size with time, star clusters also exhibit a radial age gradient, with younger clusters found closer to the ring. The cluster mass function is well described by a power law, with a slope depending on the SFR. Giant gas clouds in the rings have supersonic internal velocity dispersions and are gravitationally bound.

The stellar masses of ∼ 40 000 UV selected Galaxies from the WiggleZ survey at 0.3

We characterise the stellar masses and star formation rates in a sample of almost 40000 spectroscopically confirmed UV luminous galaxies at 0.3<z<1.0 selected from within the WiggleZ Dark Energy Survey. In particular, we match this UV bright population to wide-field infrared surveys such as the near infrared UKIDSS LAS and the mid infrared WISE All-Sky Survey. We find that ~30% of the UV luminous WiggleZ galaxies are detected at >5sigma in the UKIDSS-LAS at all redshifts. An even more luminous subset of 15% are also detected in the WISE 3.4 and 4.6um bands. We compute stellar masses for this very large sample of extremely blue galaxies and quantify the sensitivity of the stellar mass estimates to various assumptions made during the SED fitting. The median stellar masses are log10(M*/M0)=9.6\pm0.7, 10.2\pm0.5 and 10.4\pm0.4 for the IR-undetected, UKIDSS detected and UKIDSS+WISE detected galaxies respectively. We demonstrate that the inclusion of NIR photometry can lead to tighter constraints on the stellar masses. The mass estimates are found to be most sensitive to the inclusion of secondary bursts of star formation as well as changes in the stellar population synthesis models, both of which can lead to median discrepancies of the order of 0.3dex in the stellar masses. We find that the best-fit M/LK is significantly lower (by ~0.4 dex) than that predicted by simple optical colour based estimators, in particular for the bluer galaxies with younger best-fit ages. The WiggleZ galaxies have star formation rates of 3-10 M0/yr and mostly lie at the upper end of the main sequence of star-forming galaxies at these redshifts. Their rest-frame UV luminosities and stellar masses are comparable to both local compact UV-luminous galaxies as well as Lyman break galaxies at z~2-3.(abridged)

THE OPTICAL SPECTRA OFSPITZER24 μm GALAXIES IN THE COSMIC EVOLUTION SURVEY FIELD. II. FAINT INFRARED SOURCES IN THE zCOSMOS-BRIGHT 10k CATALOG

We have used the zCOSMOS-bright 10k sample to identify 3244 Spitzer/MIPS 24-micron-selected galaxies with 0.06< S(24um)< 0.50 mJy and I(AB)<22.5, over 1.5 deg^2 of the COSMOS field, and studied different spectral properties, depending on redshift. At 0.2<z<0.3, we found that different reddening laws of common use in the literature explain the dust extinction properties of around 80% of our infrared (IR) sources, within the error bars. For up to 16% of objects, instead, the Halpha/Hbeta ratios are too high for their IR/UV attenuations, which is probably a consequence of inhomogenous dust distributions. In only a few of our galaxies at 0.2<z<0.3 the IR emission could be mainly produced by dust heated by old rather than young stars. Besides, the line ratios of ~22% of our galaxies suggest that they might be star-formation/nuclear-activity composite systems. At 0.5<z<0.7, we estimated galaxy metallicities for 301 galaxies: at least 12% of them are securely below the upper-branch mass-metallicity trend, which is consistent with the local relation. Finally, we performed a combined analysis of the Hdelta equivalent-width versus Dn(4000) diagram for 1722 faint and bright 24um galaxies at 0.6<z<1.0, spanning two decades in mid-IR luminosity. We found that, while secondary bursts of star formation are necessary to explain the position of the most luminous IR galaxies in that diagram, quiescent, exponentially-declining star formation histories can well reproduce the spectral properties of ~40% of the less luminous sources. Our results suggest a transition in the possible modes of star formation at total IR luminosities L(TIR)=(3 +/-2)x10^11 Lsun.

The Optical Spectra of 24 μm Galaxies in the COSMOS Field. I.SpitzerMIPS Bright Sources in the zCOSMOS‐Bright 10k Catalog

We study zCOSMOS-bright optical spectra for 609 Spitzer MIPS 24 μm-selected galaxies with S24 μ m > 0.30 mJy and I < 22.5 (AB mag) over 1.5 deg2 of the COSMOS field. From emission-line diagnostics we find the following: (1) SFRs derived from the observed Hα λ6563 and Hβ λ4861 lines underestimate, on average, the total SFR by factors of ~5 and 10, respectively. (2) Both the Calzetti et al. and the Milky Way reddening laws are suitable to describe the extinction observed in IR sources in most cases. (3) Some IR galaxies at z < 0.3 have low abundances, but many others with similar IR luminosities and redshifts are chemically enriched. (4) The average [O III] λ5007/Hβ λ4861 ratios of ν L24 μ mν > 1011 L☉ galaxies at 0.6 < z < 0.7 are ~0.6 dex higher than the average ratio of all zCOSMOS galaxies at similar redshifts. Massive star formation and AGNs could simultaneously be present in those galaxies with the highest ionizing fluxes. (5) Roughly of the galaxies with metallicity measurements at 0.5 < z < 0.7 lie below the general mass-metallicity relation at the corresponding redshifts. The strengths of the 4000 Å break and the Hδ EW of our galaxies show that secondary bursts of star formation are needed to explain the spectral properties of most IR sources. The LIRG and ULIRG phases occur, on average, between 107 and 108 yr after the onset of a starburst on top of underlying older stellar populations. These results are valid for galaxies of different IR luminosities at 0.6 < z < 1.0 and seem independent of the mechanisms triggering star formation.

Discovery of X-ray burst triplets in EXO 0748-676

Type-I X-ray bursts are thermonuclear flashes that take place on the surface of accreting neutron stars. The wait time between consecutive bursts is set by the time required to accumulate the fuel needed to trigger a new burst; this is at least one hour. Sometimes secondary bursts are observed, approximately 10 min after the main burst. These short wait-time bursts are not yet understood. We observed the low-mass X-ray binary and X-ray burster EXO 0748-676 with XMM-Newton for 158 h, during 7 uninterrupted observations lasting up to 30 h each. We detect 76 X-ray bursts. Most remarkably, 15 of these bursts occur in burst triplets, with wait times of 12 min between the three components of the triplet, T1, T2, and T3. We also detect 14 doublets with similar wait times between the two components of the doublet, D1 and D2. We characterize this behavior to try and obtain a better understanding of bursts with short wait times. We measure the burst peak flux, fluence, wait time and time profile, and study correlations between these parameters and with the persistent flux representing the mass accretion rate. (i) For all bursts with a long wait time, the fluence is tightly correlated with the wait time, whereas burst with short wait times generally have higher fluences than expected from this relationship; (ii) wait times tend to be longer after doublets and triplets; (iii) the time profile of single bursts, S1, and of the first burst in a double or triple burst, D1 and T1, always contains a slow component which is generally absent in the D2, T2 and T3 bursts; (iv) the peak flux is highest for S1, D1 and T1 bursts, but this is still a factor of 7 lower than the highest peak flux ever seen for a burst in this system; (v) the persistent flux, representing the mass accretion rate onto the neutron star, is about 1% of Eddington, which is among the lowest value so far measured for this system. The amount of energy per gram of accreted mass liberated during bursts is consistent with a fuel mixture of hydrogen-rich material. The characteristics of the bursts indicate that possibly all bursts in this system are hydrogen-ignited, in contrast with most other frequent X-ray bursters in which bursts are helium-ignited, but consistent with the low mass accretion rate in EXO 0748-676. Possibly the hydrogen ignition is the determining factor for the occurrence of short wait-time bursts. For example the 12 min wait time may be associated with a nuclear beta decay timescale. Appendix is only available in electronic form at http://www.aanda.org

The role of hind limb flexor muscles during swimming in the toad, Bufo marinus

Most work examining muscle function during anuran locomotion has focused largely on the roles of major hind limb extensors during jumping and swimming. Nevertheless, the recovery phase of anuran locomotion likely plays a critical role in locomotor performance, especially in the aquatic environment, where flexing limbs can increase drag on the swimming animal. In this study, I use kinematic and electromyographic analyses to explore the roles of four anatomical flexor muscles in the hind limb of Bufo marinus during swimming: m. iliacus externus, a hip flexor; mm. iliofibularis and semitendinosus, knee flexors; and m. tibialis anticus longus, an ankle flexor. Two general questions are addressed: (1) What role, if any, do these flexors play during limb extension? and (2) How do limb flexors control limb flexion? Musculus iliacus externus exhibits a large burst of EMG activity early in limb extension and shows low levels of activity during recovery. Both m. iliofibularis and m. semitendinosus are biphasically active, with relatively short but intense bursts during limb extension followed by longer and typically weaker secondary bursts during recovery. Musculus tibialis anticus longus becomes active mid way through recovery and remains active through the start of extension in the next stroke. In conclusion, flexors at all three joints exhibit some activity during limb extension, indicating that they play a role in mediating limb movements during propulsion. Further, recovery is controlled by a complex pattern of flexor activation timing, but muscle intensities are generally lower, suggesting relatively low force requirements during this phase of swimming.

$X$-Pinches in Dielectric Frames

The experiments reported here were designed to test X-pinch wire-loading configurations using a simple plastic frame that might enable the X-pinch wires to be changed under vacuum after a pulse. Several frame configurations and materials were tested, some of which suffered from early surface flashover and current shunting away from the X-pinch. Fiberglass frames proved to be successful both in minimizing the current shunting up to the time of the X-pinch X-ray burst and, in most tests, in substantially reducing X-ray emission from energetic electrons and secondary soft X-ray bursts following the first X-ray burst. Both of these features are beneficial for using X-pinches for point-projection radiography as well as for recording X-ray spectra from the X-pinches or other nearby plasmas

Espécies ativas de oxigênio na resposta de defesa de plantas a patógenos

A explosão oxidativa é uma resposta de defesa da planta após o reconhecimento do patógeno, conduzindo à reação de hipersensibilidade (HR). Esta resposta é devido à geração de espécies ativas de oxigênio (ROS ou EAO's), tais como H2O2, O2-, e OH- As espécies ativas de oxigênio possuem várias funções na resposta de defesa da planta. Peróxido de higrogênio (H2O2) pode ser diretamente tóxico ao patógeno e está envolvido com o fortalecimento da parede celular, uma vez que o H2O2 é necessário para a biossíntese de lignina. Peróxido de hidrogênioatua também como mensageiro secundário, sendo responsável pela ativação da hidrolase do ácido benzóico, enzima responsável pela conversão do ácido benzóico em ácido salicílico. A explosão oxidativa não está confinada somente à HR macroscópica, uma vez que explosões oxidativas secundárias poderão ocorrer nos tecidos distantes, causando micro-HR's e conduzindo à resistência sistêmica adquirida (SAR), a qual é mediada pelo ácido salicílico como um sinal. Portanto, a ocorrência de HR e SAR é dependente da cascata de sinalização derivada da explosão oxidativa, que por sua vez é um evento inicial na resposta da planta contra a invasão do patógeno.

Feedback Processes in Early‐Type Galaxies

We present a simple phenomenological model of feedback in early-type galaxies that tracks the evolution of the interstellar medium gas mass, metallicity, and temperature. Modeling the star formation rate as a Schmidt law with a temperature-dependent efficiency, we find that intermittent episodes of star formation are common in moderate-size ellipticals. Our model is applicable in the case in which the thermalization time from supernovae is sufficiently long that spatial variations are relatively unimportant, an appropriate assumption for the empirical parameters adopted here, but one that can only be demonstrated conclusively through more detailed numerical studies. The departure from a standard scenario of passive evolution implies significantly younger luminosity-weighted ages for the stellar populations of low-mass galaxies at moderate redshifts, even though the more physically meaningful mass-weighted ages are changed only slightly. Secondary bursts of star formation also lead to a natural explanation of the large scatter in the near-UV-optical relation observed in clusters at moderate redshift and account for the population of E+A galaxies that display a spheroidal morphology. As the late-time formation of stars in our model is due to the gradual cooling of the interstellar medium, which is heated to temperatures ~1 keV by the initial burst of supernovae, our conclusions do not rely on any environmental effects or external mechanisms. Furthermore, a simple estimate of the X-ray emission from this supernova-heated gas leads to an LX-LB correlation that is in good agreement with observed values. Thus, feedback processes may be essential to understanding the observed properties of early-type galaxies from the optical to the X-ray.

Characterization of density fluctuationsduring ELMs in the DIII-D tokamak

Bursts of turbulence associated with ELMshave been studied systematically in DIII-D with a multichannelphase contrast imaging (PCI) diagnostic, which is sensitive to the longpoloidal wavelength components of the density fluctuations in the outeredge of the tokamak. A comparison of the temporal dynamics of theturbulence with the signature Dα signal from the divertor has revealedsystematic differences between type I and type III ELMs: even thoughprecursor fluctuations are sometimes seen before type I ELMs, the PCIsignal level remains high until the peak in the Dα signal; bycontrast, in type III ELMs the fluctuation burst precedes theDα peak by 0.4-0.6 ms. Type I ELMs can generate `echoes',i.e. secondary bursts, in the scrape-off layer. Coherent modes areobserved during type III ELMs only. The radial and temporal correlationstructures and the spectral properties of the turbulence during thetransient ELM phase have been reconstructed by averaging over multipleELMs, in order to improve the statistical accuracy. ELM turbulence isfound to share many properties with L mode turbulence, including themain qualitative features of radial wavenumber and frequency spectraand radial dispersion relations. However, features unique to ELMturbulence are also identified.

Computer modeling of swallow using acoustic measures

Although cervical level auscultation of the human swallow has long been discussed as a potential adjunct to the clinical dysphagia examination, there has been little research to quantify the acoustic parameters of the procedure. After initially examining the relative timing of these events in a normal population of +250 subjects, algorithms capable of generating computer models based on relative timing of acoustic data were developed. Procedure: In addition to physiological profile and medical/social history, a sample swallow is recorded and 6 raw measurements data points are identified: initiation of deglutition apnea (dA), leading and trailing edges of both the initial and secondary bursts as well as the terminal acoustic event. From this an additional seven measurements are derived: duration of dA, relative midpoint of dA, durations and midpoints of initial and secondary bursts, the interburst duration, and the relative midpoint of the bolus transport signal (BTS). Conclusion: It is possible for the computer to generate an optimal swallow profile for an individual and through statistical analyses predict the range, median and relative timing for each event reporting profile and the degree of confidence based on the subset n. [Equipment for capturing data and computer analysis provided by Welsh/Allyn Corporation.]

Prolonged epileptiform bursting induced by 0-Mg 2+ in rat hippocampal slices depends on gap junctional coupling

The transition from brief interictal to prolonged seizure, or ‘ictal’, activity is a crucial event in epilepsy. In vitro slice models can mimic many phenomena observed in the electroencephalogram of patients, including transition from interictal to ictaform or seizure-like activity. In field potential recordings, three discharge types can be distinguished: (1) primary discharges making up the typical interictal burst, (2) secondary bursts, lasting several hundred milliseconds, and (3) tertiary discharges lasting for seconds, constituting the ictal series of bursts. The roles of chemical synapses in these classes of burst have been explored in detail. Here we test the hypothesis that gap junctions are necessary for the generation of secondary bursts. In rat hippocampal slices, epileptiform activity was induced by exposure to 0-Mg 2+. Epileptiform discharges started in the CA3 subfield, and generally consisted of primary discharges followed by 4–13 secondary bursts. Three drugs that block gap junctions, halothane (5–10 mM), carbenoxolone (100 μM) and octanol (0.2–1.0 mM), abolished the secondary discharges, but left the primary bursts intact. The gap junction opener trimethylamine (10 mM) reversibly induced secondary and tertiary discharges. None of these agents altered intrinsic or synaptic properties of CA3 pyramidal cells at the doses used. Surgically isolating the CA3 subfield made secondary discharges disappear, and trimethylamine under these conditions was able to restore them. We conclude that gap junctions can contribute to the prolongation of epileptiform discharges.

Evoked epileptiform discharges in the rat anterior piriform cortex: generation and local propagation

The purpose of this study was to identify cellular and synaptic properties of neurons in a small region within the anterior piriform cortex (aPC), termed the area tempestas (AT), responsible for triggering forebrain seizures in rats. Using a brain slice preparation, we performed whole-cell patch recordings from neurons in the regions overlapping the functionally defined AT. Local electrical stimulation activated synaptic inputs to neurons in these regions, collectively termed the deep aPC (daPC). Synaptic inputs were blocked by selective ionotropic glutamate receptor antagonists. Excitatory bursts were evoked from 59% of daPC neurons as the stimulus intensity was raised above a precise threshold. Secondary bursts (6–15 Hz) occurred in 34% of daPC neurons. Evoked bursts were synaptically driven, as they were blocked by TTX (1 μM) or 2,3-dihydroxy-6-nitro-7-sulfamoyl-benzo( f)quinoxaline (NBQX, 1 μM), but not by inclusion of cesium and N-(2,6-dimethylphenylcarbamoylmethyl) triethylammonium (QX-314) in the internal patch solution. Neither augmentation of excitatory nor suppression of inhibitory transmission were required to evoke bursts from daPC neurons. However, bicuculline (20 μM) lowered the threshold intensity for evoking discharges and increased the incidence and duration of evoked bursts, indicating active inhibitory control of daPC neurons. Stimulation in the daPC evoked epileptiform field potentials from layer II of the adjacent PC and bursts from layer II pyramidal neurons. This work demonstrates that synaptically dependent excitatory burst discharges can be evoked from daPC neurons without altering the balance between synaptic excitation and inhibition. Stimuli that trigger bursts in daPC neurons also generate epileptiform activity in layer II pyramidal cells, indicating that propagation of excitatory activity triggered from the daPC to the pyramidal neurons of the aPC can contribute to the initiation of seizures induced by disinhibition of the AT in vivo.

Seizure-like events in disinhibited ventral slices of adult rat hippocampus.

Epileptic discharges lasting 2-90 s, were studied in vitro in slices from the ventral hippocampus of adult rats, in which inhibition was blocked acutely with bicuculline methiodide (BMI, 5-30 microM) and potassium ([K(+)](o)) raised to 5 mM. These seizure-like events (SLEs) comprised three distinct phases, called here primary, secondary, and tertiary bursts. Primary bursts lasted 90-150 ms. Secondary bursts lasted a further 70-250 ms, comprising a short series of afterdischarges riding on the same depolarization as the primary burst. Finally a train of tertiary bursts started with a peak frequency of 5-10 Hz and could last >1 min. Slices from the ventral hippocampus showed significantly higher susceptibility to SLEs than did dorsal slices. SLEs proved sensitive to alpha-amino-3-hydroxy-5-methyl-4-isoxazolepropionic acid (AMPA) receptor antagonists. They were insensitive to N-methyl-D-aspartate (NMDA) receptor antagonists; 50 microl D-2-amino-5-phosphonopentanoic acid (D-AP5) did block the transient secondary bursts selectively. SLEs were restricted to the hippocampus proper even if the entorhinal cortex was present. Entorhinal bursts could last <2 s and were only coupled with hippocampal bursts in a minority of slices. Reentry of epileptic bursts occasionally occurred during interictal discharges, but not during the later stages of SLEs. Full-length SLEs always started in CA3 region and could be recorded in minislices containing CA3 plus dentate hilus. Ion-sensitive microelectrodes revealed that interictal discharges were followed by short (2-3 s) [K(+)](o) waves, peaking at approximately 7.5 mM. SLEs were always accompanied by increases in [K(+)](o) reaching approximately 8.5 mM at the start of tertiary bursts; [K(+)](o) then increased more slowly to a ceiling of 11-12 mM. After the end of each SLE, [K(+)](o) fell back to baseline within 10-15 s. SLEs were accompanied by significant increase in synaptic activity, compared with baseline and/or interictal activity, estimated by the variance of the intracellular signal in the absence of epileptic bursts and action potentials (0. 38 mV(2), compared with 0.13 mV(2), and 0.1 mV(2), respectively). No significant increases were observed in the interval preceding spontaneous interictal activity. These studies show that focal assemblies of hippocampal neurons, without long reentrant loops, are sufficient for the generation of SLEs. We propose that a key factor in the transition from interictal activity to SLEs is an increase in axonal and terminal excitability, resulting, at least in part, from elevations in [K(+)](o).