Power Spectrum Of Variability Research Articles

An improved model for the non-linear velocity power spectrum

Abstract The velocity divergence power spectrum is a key ingredient in modelling redshift-space distortion effects on quasi-linear and non-linear scales. We present an improved model for the z=0 velocity divergence auto and cross power spectrum which was originally suggested by Jennings et al. Using numerical simulations we measure the velocity fields using a Delaunay tessellation and obtain an accurate prediction of the velocity divergence power spectrum on scales k < 1 h Mpc−1. We use this to update the model which is now accurate to 2 per cent for both Pθθ and Pθδ at z= 0 on scales k < 0.65 h Mpc−1 and k < 0.35 h Mpc−1, respectively. We find that the formula for the redshift dependence of the velocity divergence power spectra proposed by Jennings et al. recovers the measured z > 0 P(k) to markedly greater accuracy with the new model. The non-linear Pθθ and Pθδ at z=1 are recovered accurately to better than 2 per cent on scales k < 0.2 h Mpc−1. Recently, it was shown that the velocity field shows larger differences between modified gravity cosmologies and Λ cold dark matter (ΛCDM) compared to the matter field. An accurate model for the velocity divergence power spectrum, such as the one presented here, is a valuable tool for analysing redshift-space distortion effects in future galaxy surveys and for constraining deviations from general relativity.

The non-linear matter and velocity power spectra in f(R) gravity

We study the matter and velocity divergence power spectra in a f(R) gravity theory and their time evolution measured from several large-volume N-body simulations with varying box sizes and resolution. We find that accurate prediction of the matter power spectrum in f(R) gravity places stronger requirements on the simulation than is the case with LCDM, because of the nonlinear nature of the fifth force. Linear perturbation theory is shown to be a poor approximation for the f(R) models, except when the chameleon effect is very weak. We show that the relative differences from the fiducial LCDM model are much more pronounced in the nonlinear tail of the velocity divergence power spectrum than in the matter power spectrum, which suggests that future surveys which target the collection of peculiar velocity data will open new opportunities to constrain modified gravity theories. A close investigation of the time evolution of the power spectra shows that there is a pattern in the evolution history, which can be explained by the properties of the chameleon-type fifth force in f(R) gravity. Varying the model parameter |f_R0|, which quantifies the strength of the departure from standard gravity, mainly varies the epoch marking the onset of the fifth force, as a result of which the different f(R) models are in different stages of the same evolutionary path at any given time

Holocene climate variability in north-eastern Italy: potential influence of the NAO and solar activity recorded by speleothem data

Abstract. Here we present high-resolution stable isotope and lamina thickness profiles as well as radiocarbon data for the Holocene stalagmite ER 76 from Grotta di Ernesto (north-eastern Italy), which was dated by combined U-series dating and lamina counting. ER 76 grew between 8 ka (thousands of years before 2000 AD) and today, with a hiatus from 2.6 to 0.4 ka. Data from nine meteorological stations in Trentino show a significant influence of the North Atlantic Oscillation (NAO) on winter temperature and precipitation in the cave region. Spectral analysis of the stable isotope signals of ER 76 reveals significant peaks at periods of 110, 60–70, 40–50, 32–37 and around 25 a. Except for the cycle between 32 and 37 a all periodicities have corresponding peaks in power spectra of solar variability, and the 25-a cycle may correspond to NAO variability. This suggests that climate variability in northern Italy was influenced by both solar activity and the NAO during the Holocene. Six periods of warm winter climate in the cave region were identified. These are centred at 7.9, 7.4, 6.5, 5.5, 4.9 and 3.7 ka, and their duration ranges from 100 to 400 a. The two oldest warm phases coincide with the deposition of sapropel S1 in the Mediterranean Sea indicating that the climate in the cave region was influenced by this prominent pluvial phase in the Mediterranean area. For the younger warm phases it is difficult to establish a supra-regional climate pattern, and some of them may, thus, reflect regional climate variability. This highlights the complexity of regional and supra-regional scale Holocene climate patterns.

Redshift-space distortions in f(R) gravity

We use large volume N-body simulations to predict the clustering of dark matter in redshift space in f(R) modified gravity cosmologies. This is the first time that the nonlinear matter and velocity fields have been resolved to such a high level of accuracy over a broad range of scales in this class of models. We find significant deviations from the clustering signal in standard gravity, with an enhanced boost in power on large scales and stronger damping on small scales in the f(R) models compared to GR at redshifts z<1. We measure the velocity divergence (P_\theta \theta) and matter (P_\delta \delta) power spectra and find a large deviation in the ratios \sqrt{P_\theta \theta/P_\delta \delta} and P_\delta \theta/P_\delta\delta, between the f(R) models and GR for 0.03<k/(h/Mpc)<0.5. In linear theory these ratios equal the growth rate of structure on large scales. Our results show that the simulated ratios agree with the growth rate for each cosmology (which is scale dependent in the case of modified gravity) only for extremely large scales, k<0.06h/Mpc at z=0. The velocity power spectrum is substantially different in the f(R) models compared to GR, suggesting that this observable is a sensitive probe of modified gravity. We demonstrate how to extract the matter and velocity power spectra from the 2D redshift space power spectrum, P(k,\mu), and can recover the nonlinear matter power spectrum to within a few percent for k<0.1h/Mpc. However, the model fails to describe the shape of the 2D power spectrum demonstrating that an improved model is necessary in order to reconstruct the velocity power spectrum accurately. The same model can match the monopole moment to within 3% for GR and 10% for the f(R) cosmology at k<0.2 h/Mpc at z=1. Our results suggest that the extraction of the velocity power spectrum from future galaxy surveys is a promising method to constrain deviations from GR.

X-ray variability of 104 active galactic nuclei

AGN, powered by accretion onto SMBHs, are thought to be scaled up versions of Galactic black hole X-ray binaries (BH-XRBs). In the past few years evidence of such correspondence include similarities in the broadband shape of the X-ray variability power spectra, with characteristic bend times-scales scaling with mass. We have performed a uniform analysis of the power spectrum densities (PSDs) of 104 nearby (z<0.4) AGN using 209 XMM-Newton/pn observations. The PSDs have been estimated in three energy bands: 0.2-10, 0.2-2, and 2-10 keV. The sample comprises 61 Type-1 AGN, 21 Type-2 AGN, 15 NLSy1, and 7 BLLACS. We have fitted each PSD to two models: (1) a single power-law model and (2) a bending power-law model. Among the entire sample, 72% show significant variability in at least one of the three bands tested. A high percentage of low-luminosity AGN do not show any significant variability. The PSD of the majority of the variable AGN was well described by a simple power-law with a mean index of 2. In 15 sources we found that the bending power law model was preferred with a mean slope of 3 and a mean bend frequency of 2.E-04 Hz. Only KUG1031+398 (REJ1034+396) shows evidence for quasi-periodic oscillations. The `fundamental plane' relating variability timescale, black hole mass, and luminosity is demonstrated using the new X-ray timing results presented here together with a compilation of the previously detected timescales from the literature. Both quantitative (i.e. scaling with BH mass) and qualitative (overall PSD shapes) found in this sample of AGN are in agreement with the expectations for the SMBHs and BH-XRBs being the same phenomenon scaled-up with the size of the BH. The steep PSD slopes above the high frequency bend bear a closer resemblance to those of the `soft/thermal dominated' BH-XRB states than other states.

Estimation of plasma parameters in an accretion column near the surface of accreting white dwarfs from their flux variability

We consider the behavior of matter in the accretion column that emerges under accretion in binary systems near the surface of a white dwarf. The plasma heated in a standing shock wave near the white dwarf surface efficiently radiates in the X-ray energy band. We suggest a method for estimating post-shock plasma parameters, such as the density, temperature, and height of the hot zone, from the power spectrum of its X-ray luminosity variability. The method is based on the fact that the flux variability amplitude for the hot region at various Fourier frequencies depends significantly on its cooling time, which is determined by the parameters of the hot zone in the accretion column. This allows the density and temperature of the hot matter to be estimated. We show that the characteristic cooling time can be efficiently determined from the break frequency in the power spectrum of the X-ray flux variability for accreting white dwarfs. The currently available X-ray instruments do not allow such measurements to be made because of an insufficient collecting area, but this will most likely become possible with new-generation large-area X-ray spectrometers.

Variations in discharge current waveforms and their power spectra injected from contact discharges of ESD‐gun with different arrangements

AbstractThe International Electrotechnical Commission (IEC) has prescribed an immunity test (IEC61000‐4‐2) of electronic equipment against electrostatic discharges (ESDs), in which a discharge current to be injected onto equipment under test is specified. As for the waveform, however, not the whole waveform but only the rise time, the first peak, and the current amplitudes at 30 and 60 ns are given in the time domain together with their uncertainties, which are required to check on the condition that an ESD generator (ESD‐gun) shall be arranged vertically to an IEC‐recommended calibration target and its earth return wire is kept away as far as possible from a vertical ground plane (IEC standard arrangement). In this study, to clarify how arrangements of an ESD‐gun and its earth return wire affect discharge currents, we measured discharge current waveforms for contact discharges of an ESD‐gun onto an IEC calibration target with respect to various inclinations of the ESD‐gun and arrangements of its earth return wire, and also calculated their current power spectra normalized to that of the discharge current for the IEC standard arrangement. As a result, we found that inclinations of the ESD gun affect the first peak current, which increases current power spectra by 14 dB at frequencies over 300 MHz, and that arrangements of the return wire influence the current waveforms between the first and second peaks, which provides variations in power spectra by ±12 dB in the frequency range from 10 MHz to 200 MHz. This finding suggests that arrangements of an ESD‐gun and its earth return wire are likely to cause different immunity test results. It was also found that in comparison with measured discharge currents for the standard arrangement, the calculated waveform of a discharge current from a formula, which has been included in the recent standard, has a more gentle falling waveform, and produces power spectra of +15 dB in the frequency range from 10 MHz to 200 MHz and –12 dB at frequencies over 300 MHz. © 2012 Wiley Periodicals, Inc. Electr Eng Jpn, 180(1): 9–14, 2012; Published online in Wiley Online Library (wileyonlinelibrary.com). DOI 10.1002/eej.21270

On the change of the inner boundary of an optically thick accretion disk around white dwarfs using the dwarf nova SS Cyg as an example

We present the results of our studies of the aperiodic optical flux variability for SS Cyg, an accreting binary systemwith a white dwarf. The main set of observational data presented here was obtained with the ANDOR/iXon DU-888 photometer mounted on the RTT-150 telescope, which allowed a record(for CCD photometers) time resolution up to 8 ms to be achieved. The power spectra of the source's flux variability have revealed that the aperiodic variability contains information about the inner boundary of the optically thick flow in the binary system. We show that the inner boundary of the optically thick accretion disk comes close to the white dwarf surface at the maximum of the source's bolometric light curve, i.e., at the peak of the instantaneous accretion rate onto the white dwarf, while the optically thick accretion disk is truncated at distances 8.5e9 cm ~10 R_{WD} in the low state. We suggest that the location of the inner boundary of the accretion disk in the binary can be traced by studying the parameters of the power spectra for accreting white dwarfs. In particular, this allows the mass of the accreting object to be estimated.

Effects of Acupuncture on Stress-Induced Gastrointestinal Dysmotility in Conscious Dogs

Background: Stress is involved in the pathogenesis of functional dyspepsia (FD) and an impaired gastric phase III of interdigestive contractions has been shown in subset of patients who have FD. Objective: This study attempted to determine whetherelectro-acupuncture (EA) has a beneficial effect on an impaired gastric phase III associated with stress. Methods: Strain gauze force transducers were chronically implanted on the gastric body, antrum, duodenum, and proximal jejunum in dogs. Three electrodes for electrocardiography (ECG) were implanted at the back and shoulders of the animals. The dogs were allowed 2 weeks to recover from the surgery. Twenty minutes after finishing gastric phase III, the dogs were forced to hear intensely loud music through earpieces for 90 minutes, to create acoustic stress (AS). Main Outcome Measures: After a 16-hour fast, gastrointestinal contractions and ECG were recorded in while the dogs were in a conscious state. High frequency (HF; 0.15–0.4 Hz) and low frequency (LF; 0.04-0.15 Hz) bands of the heart rate variability (HRV) power spectrum of ECG were used as markers of vagal and sympathetic activity, respectively. Results: The occurrence of gastric phase III, but not intestinal phase III, was significantly inhibited during AS loading. Increased LF and reduced HF were observed in response to AS, suggesting increased sympathetic and reduced parasympathetic activity. EA at ST 36, but not at BL 21, significantly restored the occurrence of gastric phase III (P<0.01). EA at ST 36 increased HF and reduced LF during AS loading (P<0.05). Conclusions: EA at ST 36 may increase parasympathetic activity, resulting in the restoration of impaired gastric phase III contractions in stressful conditions.

Heart rate variability in patients with idiopathic Parkinson’s disease with and without obstructive sleep apnea syndrome

BackgroundObstructive sleep apnea syndrome (OSAS) is associated with repeated apnea-induced sympathetic surges leading to specific alterations of the power spectrum of heart rate variability (HRV). Sympathetic dysfunction evolves early in idiopathic Parkinson’s disease (PD), but the consequences on cardiac autonomic response to OSAS have not been studied so far in PD patients. MethodsSixty-two patients with PD (35 without OSAS (PD-wo), 27 with OSAS (PD-OSAS)) and 62 age-matched control subjects (25 without OSAS (Co-wo), 37 with OSAS (Co-OSAS)) were included. HRV variables – including mean R–R interval, standard deviation of all normal-to-normal R–R intervals (SDNN), both low frequency (LF) and high frequency (HF) power bands, and the LF/HF ratio – were computed automatically from full-night polysomnography and calculated separately for each sleep stage. ResultsHRV variables were similar in PD-wo and PD-OSAS. In contrast, Co-OSAS showed significantly higher LF power in NREM1 and NREM2 sleep and higher LF/HF ratio in NREM1, NREM2 and slow wave sleep than Co-wo. Similarly, correlations between HRV variables and parameters of OSAS severity were found only in controls but not in PD patients. ConclusionOur results suggest that the sympathetic response to OSAS is blunted in PD, giving further clinical evidence of the sympathetic denervation commonly observed in this neurodegenerative disorder.

Automatic filtering of outliers in RR intervals before analysis of heart rate variability in Holter recordings: a comparison with carefully edited data

BackgroundUndetected arrhythmic beats seriously affect the power spectrum of the heart rate variability (HRV). Therefore, the series of RR intervals are normally carefully edited before HRV is analysed, but this is a time consuming procedure when 24-hours recordings are analysed. Alternatively, different methods can be used for automatic removal of arrhythmic beats and artefacts. This study compared common frequency domain indices of HRV when determined from manually edited and automatically filtered RR intervals.Methods and ResultsTwenty-four hours Holter recordings were available from 140 healthy subjects of age 1-75 years. An experienced technician carefully edited all recordings. Automatic filtering was performed using a recursive procedure where RR intervals were removed if they differed from the mean of the surrounding RR intervals with more than a predetermined limit (ranging from 10% to 50%). The filtering algorithm was evaluated by replacing 1% of the beats with synthesised ectopic beats. Power spectral analysis was performed before and after filtering of both the original edited data and the noisy data set. The results from the analysis using the noisy data were used to define an age-based filtering threshold. The age-based filtration was evaluated with completely unedited data, generated by removing all annotations from the series of RR intervals, and then comparing the resulting HRV indices with those obtained using edited data. The results showed equivalent results after age-based filtration of both the edited and unedited data sets, where the differences in HRV indices obtained by different preprocessing methods were small compared to the mean values within each age group.ConclusionsThe study showed that it might not be necessary to perform the time-consuming careful editing of all detected heartbeats before HRV is analysed in Holter recordings.In most subjects, it is sufficient to perform the regular editing needed for valid arrhythmia analyses, and then remove undetected ectopic beats and artefacts by age-based filtration of the series of RR intervals, particularly in subjects older than 30 years.

EVOLUTION OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM ACROSSWILKINSON MICROWAVE ANISOTROPY PROBEDATA RELEASES: A NONPARAMETRIC ANALYSIS

Using a nonparametric function estimation methodology, we present a comparative analysis of the WMAP 1-, 3-, 5-, and 7-year data releases for the CMB angular power spectrum with respect to the following key questions: (a) How well is the power spectrum determined by the data alone? (b) How well is the $\Lambda$CDM model supported by a model-independent, data-driven analysis? (c) What are the realistic uncertainties on peak/dip locations and heights? Our results show that the height of the power spectrum is well determined by data alone for multipole l approximately less than 546 (1-year), 667 (3-year), 804 (5-year), and 842 (7-year data). We show that parametric fits based on the $\Lambda$CDM model are remarkably close to our nonparametric fits in $l$-regions where data are sufficiently precise. In contrast, the power spectrum for an H$\Lambda$CDM model gets progressively pushed away from our nonparametric fit as data quality improves with successive data realizations, suggesting incompatibility of this particular cosmological model with respect to the WMAP data sets. We present uncertainties on peak/dip locations and heights at the 95% ($2 \sigma$) level of confidence, and show how these uncertainties translate into hyperbolic "bands" on the acoustic scale ($l_A$) and peak shift ($\phi_m$) parameters. Based on the confidence set for the 7-year data, we argue that the low-l up-turn in the CMB power spectrum cannot be ruled out at any confidence level in excess of about 10% ($\approx 0.12 \sigma$). Additional outcomes of this work are a numerical formulation for minimization of a noise-weighted risk function subject to monotonicity constraints, a prescription for obtaining nonparametric fits that are closer to cosmological expectations on smoothness, and a method for sampling cosmologically meaningful power spectrum variations from the confidence set of a nonparametric fit.

Spectro-timing analysis of Cygnus X-1 during a fast state transition

We present the analysis of two long, quasi-uninterrupted RXTE observations of Cygnus X-1 that span several days within a 10 d interval. The spectral characteristics during this observation cover the region where previous observations have shown the source to be most dynamic. Despite that the source behavior on time scales of hours and days is remarkably similar to that on year time scales. This includes a variety of spectral/temporal correlations that previously had only been observed over Cyg X-1's long-term evolution. Furthermore, we observe a full transition from a hard to a soft spectral state that occurs within less than 2.5 hours - shorter than previously reported for any other similar Cyg X-1 transition. We describe the spectra with a phenomenological model dominated by a broken power law, and we fit the X-ray variability power spectra with a combination of a cutoff power law and Lorentzian components. The spectral and timing properties are correlated: the power spectrum Lorentzian components have an energy-dependent amplitude, and their peak frequencies increase with photon spectral index. Averaged over 3.2-10 Hz, the time lag between the variability in the 4.5-5.7 keV and 9.5-15 keV bands increases with decreasing hardness when the variability is dominated by the Lorentzian components during the hard state. The lag is small when there is a large power law noise contribution, shortly after the transition to the soft state. Interestingly, the soft state not only shows the shortest lags, but also the longest lags when the spectrum is at its softest and faintest. We discuss our results in terms of emission models for black hole binaries.

Very low frequency oscillations in the power spectra of heart rate variability during dry supine immersion and exposure to non-hypoxic hypobaria

The origin of very low frequency (VLF) oscillations in the power spectra of heart rate variability (HRV) is controversial with possible mechanisms involving thermoregulation and/or renin-angiotensin-aldosterone system. Recently, a major contribution from vagal influences has been suggested. The present study investigated the behaviour of VLF (0.004–0.040 Hz) components of HRV power spectra in a group of healthy male volunteers during their exposure to (1) dry, supine, immersion in thermo-neutral water for 6 h (n = 7) and (2) non-hypoxic hypobaria (breathing 40–60% oxygen at 15 000′ simulated in a decompression chamber) for 5 h (n = 15). The two manoeuvres are established to increase vagal outflow. During both the manoeuvres, all the frequency domain indices of HRV exhibited a significant increase. Increase in HRV was much more than that in the R-R interval. At 6 h of immersion, the R-R interval increased by ∼15% but the total power increased ∼fourfold. Similarly, at 5 h of exposure to hypobaria, total power increased ∼twofold with a very modest increase in an R-R of ∼9%. Increase in spectral power was appreciable even after normalization with mean R-R2. Increase in VLF during immersion was more than reported during enalaprilat blockade of angiotensin convertase enzyme. Plasma renin activity did not vary during hypobaria. There was a significant increase in pNN50, an established marker of cardiac vagal activity. Centre frequencies of the spectra and slope (β) of the relation between log(PSD) and log(frequency) did not change. Results were supportive of the notion that the parasympathetic system is pre-potent to influence slower (than respiratory) frequency components in HRV spectrum. Additionally, such an effect was without a change in the time constant of effector responses or pacemaker frequencies of VLF and LF periodicities and HRV was not a simple linear surrogate for cardiac vagal effects. An invariance of spectral exponent (β) ruled out contamination of VLF and LF spectra from fractal power as an alternate explanation.

Variations in Discharge Current Waveforms and its Power Spectra Injected from Contact Discharges of ESD-Gun with Different Arrangements

The International Electrotechnical Commission (IEC) has prescribed an immunity test (IEC61000-4-2) of electronic equipment against electrostatic discharges (ESDs), in which a discharge current to be injected onto equipment under test is specified. As for the waveform, however, not the whole waveform but only the rise time, the first peak, and the current amplitudes at 30 ns and 60 ns are given in the time domain together with their uncertainties, which are required to check on the condition that an ESD generator (ESD-gun) shall be arranged vertically to an IEC recommended calibration target and its earth return wire is kept away as far as possible from a vertical ground plane (IEC standard arrangement). In this study, to clarify how arrangements of an ESD-gun and its earth return wire affect discharge currents, we measured discharge current waveforms for contact discharges of an ESD-gun onto an IEC calibration target with respect to various inclinations of the ESD-gun and arrangements of its earth return wire, and also calculated their current power spectra normalized to that of the discharge current for the IEC standard arrangement. As a result, we found that inclinations of the ESD gun affect the first peak current, which increases current power spectra by 14 dB at frequencies over 300 MHz, and that arrangements of the return wire influence the current waveforms between the first and second peaks, which provides variations in power spectra by ±12 dB in the frequency range from 10 MHz to 200 MHz. This finding suggests that arrangements of an ESD gun and its earth return wire are likely to cause different immunity test results. It was also found that in comparison with measured discharge currents for the standard arrangement, the calculated waveform of a discharge current from a formula, which has been included in the recent standard, has a more gentle falling waveform, and produces power spectra of +15dB in the frequency range from 10 MHz to 200 MHz and -12 dB at frequencies over 300 MHz.

Observational evidence for matter propagation in accretion flows

We study simultaneous X-ray and optical observations of three intermediate polars, EX Hya, V1223 Sgr and TV Col, with the aim of understanding the propagation of matter in their accretion flows. We show that in all cases the power spectra of the flux variability of binary systems in X-ray and optical bands are similar to each other, and the majority of X-ray and optical fluxes are correlated with time lag <1 s. These findings support the idea that the optical emission of accretion discs in these binary systems largely originates as the reprocessing of the X-ray luminosity of their white dwarfs. In the best obtained data set of EX Hya we see that the optical light curve unambiguously contains some component that leads the X-ray emission by ∼7 s. We interpret this in the framework of the model of propagating fluctuations and thus deduce the time of travel of matter from the innermost part of the truncated accretion disc to the white dwarf surface. This value agrees very well with the time expected for matter threaded on to the magnetosphere of the white dwarf to fall to its surface. The data sets of V1223 Sgr and TV Col in general confirm these findings, but have poorer quality.

Modelling redshift space distortions in hierarchical cosmologies

The anisotropy of clustering in redshift space provides a direct measure of the growth rate of large scale structure in the Universe. Future galaxy redshift surveys will make high precision measurements of these distortions, and will potentially allow us to distinguish between different scenarios for the accelerating expansion of the Universe. Accurate predictions are needed in order to distinguish between competing cosmological models. We study the distortions in the redshift space power spectrum in $\Lambda$CDM and quintessence dark energy models, using large volume N-body simulations, and test predictions for the form of the redshift space distortions. We find that the linear perturbation theory prediction by Kaiser (1987) is a poor fit to the measured distortions, even on surprisingly large scales $k \ge 0.05 h$Mpc$^{-1}$. An improved model for the redshift space power spectrum, including the non-linear velocity divergence power spectrum, is presented and agrees with the power spectra measured from the simulations up to $k \sim 0.2 h$Mpc$^{-1}$. We have found a density-velocity relation which is cosmology independent and which relates the non-linear velocity divergence spectrum to the non-linear matter power spectrum. We provide a formula which generates the non-linear velocity divergence $P(k)$ at any redshift, using only the non-linear matter power spectrum and the linear growth factor at the desired redshift. This formula is accurate to better than 5% on scales $k<0.2 h $Mpc$^{-1}$ for all the cosmological models discussed in this paper. Our results will extend the statistical power of future galaxy surveys.

Properties of the transmission of pulse sequences in a bistable chain of unidirectionally coupled neurons

We study the propagation of pulse sequences in a chain of neurons with sigmoidal input–output relations. The propagating speeds of pulse fronts depend on the widths of the preceding pulses and adjacent pulse fronts interact attractively. Sequences of pulse widths are then modulated through transmission. Equations for changes in pulse width sequences are derived with a kinematical model of propagating pulse fronts. The transmission of pulse width sequences in the chain is expressed as a linear system with additive noise. The gain of the system function increases exponentially with the number of neurons in a high-frequency region. The power spectrum of variations in pulse widths due to spatiotemporal noise also increases in the same manner. Further, the interaction between pulse fronts keeps the coherence and mutual information of initial and transmitted pulse sequences. Results of an experiment on an analog circuit confirm these properties.

Cardiac Neural Regulation Oscillates with the Estrous Cycle in Freely Moving Female Rats: The Role of Endogenous Estrogens

Both estrogens levels and sleep/wakefulness states have been separately reported to affect cardiac autonomic regulation. In this study, we examined the integrated effects of the estrous and sleep cycles on cardiac autonomic activity in freely moving adult female rats. Cardiac autonomic activities were measured by analyzing the power spectrum of heart rate variability. High-frequency power (HF) and low-frequency power to HF ratio are closely correlated with cardiac parasympathetic and sympathetic activity, respectively. Ten days after electrodes were implanted, electroencephalogram, electromyogram, and electrocardiogram were recorded 6 h daily for 12 consecutive days to cover at least two estrous cycles. Estrous-cycle stages were determined using vaginal smears. Sleep cycle-related heart rate variability parameter oscillations were seen in all rats. However, the estrous cyclicity and estrous-cycle-related changes were only observed in the control rats and not in ovariectomized or the estrogen receptor antagonist, tamoxifen, treatment rats. A significantly higher HF was observed in estrous rats compared with diestrous rats or ovariectomized rats no matter whether the rats were asleep or awake. However, a significantly low-frequency power to HF ratio was only observed in quiet sleep (QS) during estrus. All these differences disappeared after treatment with tamoxifen. Our results suggest that estrous-cycle-related changes in cardiac neural regulations can be mainly attributed to endogenous estrogens, and these effects are most obviously manifest during QS. Estrous rats during QS would be equivalent to the late follicular phase of the women menstrual cycle and involve strong vagal tone but weak sympathetic activity.

The X-ray binary analogy to the first AGN quasi-periodic oscillation

The narrow line Seyfert 1 galaxy REJ 1034+396 is so far unique amongst active galaxies (AGN) in showing a quasi-periodic oscillation (QPO) in its variability power spectrum. There are multiple types of QPO seen in black hole binary (BHB) systems, so we need to identify which BHB QPO corresponds to the one seen in the AGN. A key hint is the ‘hot disc dominated’ energy spectrum of REJ 1034+396 which is sufficiently unusual that it suggests a mildly super-Eddington flow, also favoured by the most recent mass estimates for the AGN. This suggests the 67 Hz QPO seen occasionally in the mildly super-Eddington BHB GRS 1915+105 as the most likely counterpart, assuming mass scaling of the QPO frequency. This is supported by the fact that these data from GRS 1915+105 have an energy spectrum which is also dominated by a ‘hot disc’ component. Here we show that the underlying broad band power spectral shape and normalization are also similar, providing further consistency checks for this identification. Thus the AGN QPO adds to the growing evidence for a simple mass scaling of the accretion flow properties between stellar and supermassive black holes.