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This work studies the significance of the lightcurve intrinsic variability in the numerical modeling of contact binaries. Using synthetic light curves we are showing that the starspot-based intrinsic variability increases the apparent mass ratio by $\Delta q=5$%. For systems with orbital period $P>0.3 d$ the effect of intrinsic variability averaged over long time cancels each other out with the Kepler Mission-like phase smearing. Further, we analyse 47 totally eclipsing Kepler Mission contact binaries. We found a sharp cutoff of the intrinsic variability at P = 0.45 d. With the light curve numerical modeling and observational relations we derive physical parameters of the 47 systems. At least 53% of binaries have a possible third companion. 21 binaries show the O`Connell effect in the averaged phase curve. 19 of them have a primary maximum lower than the secondary, suggesting a stationary dark region on the trailing side. Using the P = 0.45 d cutoff we propose a new approach on the Period-Color relation. The only parameter correlating with the magnitude of the intrinsic variability is the apparent effective temperature ratio. We conclude that instead of describing the system parameters, the A/W-subtype division should be applicable only to the lightcurves, as a tentative phenomenon., Comment: Accepted to the Monthly Notices of the Royal Astronomical Society

Full list of authors: Valtonen, Mauri J.; Dey, Lankeswar; Zola, S.; Ciprini, S.; Kidger, M.; Pursimo, T.; Gopakumar, A.; Matsumoto, K.; Sadakane, K.; Caton, D. B.; Nilsson, K.; Komossa, S.; Bagaglia, M.; Baransky, A.; Boumis, P.; Boyd, D.; Castro-Tirado, A. J.; Debski, B.; Drozdz, M.; Escartin Perez, A.; Fiorucci, M.; Garcia, F.; Gazeas, K.; Ghosh, S.; Godunova, V; Gomez, J. L.; Gredel, R.; Grupe, D.; Haislip, J. B.; Henning, T.; Hurst, G.; Janik, J.; Kouprianov, V. V.; Lehto, H.; Liakos, A.; Mathur, S.; Mugrauer, M.; Naves Nogues, R.; Nucciarelli, G.; Ogloza, W.; Ojha, D. K.; Pajdosz-Smierciak, U.; Pascolini, S.; Poyner, G.; Reichart, D. E.; Rizzi, N.; Roncella, F.; Sahu, D. K.; Sillanpaa, A.; Simon, A.; Siwak, M.; Soldan Alfaro, F. C.; Sonbas, E.; Tosti, G.; Vasylenko, V.; Webb, J. R.; Zielinski, P., OJ 287 is a BL Lacertae type quasar in which the active galactic nucleus (AGN) outshines the host galaxy by an order of magnitude. The only exception to this may be at minimum light when the AGN activity is so low that the host galaxy may make quite a considerable contribution to the photometric intensity of the source. Such a dip or a fade in the intensity of OJ 287 occurred in 2017 November, when its brightness was about 1.75 mag lower than the recent mean level. We compare the observations of this fade with similar fades in OJ 287 observed earlier in 1989, 1999, and 2010. It appears that there is a relatively strong reddening of the B− V colours of OJ 287 when its V-band brightness drops below magnitude 17. Similar changes are also seen in V− R, V− I, and R− I colours during these deep fades. These data support the conclusion that the total magnitude of the host galaxy is V = 18.0 ± 0.3, corresponding to MK = −26.5 ± 0.3 in the K-band. This is in agreement with the results, obtained using the integrated surface brightness method, from recent surface photometry of the host. These results should encourage us to use the colour separation method also in other host galaxies with strongly variable AGN. In the case of OJ 287, both the host galaxy and its central black hole are among the biggest known, and its position in the black hole mass–galaxy mass diagram lies close to the mean correlation. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society., SZ would also like to acknowledge support of the NCN grant no. 2018/29/B/ST9/01793, and KM JSPS KAKENHI grant no. 19K03930., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We report on the results of a multiwavelength monitoring campaign of the bright, nearby Seyfert galaxy, Ark 120 using a ~50-day observing programme with Swift and a ~4-month co-ordinated ground-based observing campaign, predominantly using the Skynet Robotic Telescope Network. We find Ark 120 to be variable at all optical, UV, and X-ray wavelengths, with the variability observed to be well-correlated between wavelength bands on short timescales. We perform cross-correlation analysis across all available wavelength bands, detecting time delays between emission in the X-ray band and the Swift V, B and UVW1 bands. In each case, we find that the longer-wavelength emission is delayed with respect to the shorter-wavelength emission. Within our measurement uncertainties, the time delays are consistent with the \tau ~ \lambda^{4/3} relation, as predicted by a disc reprocessing scenario. The measured lag centroids are \tau_{cent} = 11.90 +/- 7.33, 10.80 +/- 4.08, and 10.60 +/- 2.87 days between the X-ray and V, B, and UVW1 bands, respectively. These time delays are longer than those expected from standard accretion theory and, as such, Ark 120 may be another example of an active galaxy whose accretion disc appears to exist on a larger scale than predicted by the standard thin-disc model. Additionally, we detect further inter-band time delays: most notably between the ground-based I and B bands (\tau_{cent} = 3.46 +/- 0.86 days), and between both the Swift XRT and UVW1 bands and the I band (\tau_{cent} = 12.34 +/- 4.83 and 2.69 +/- 2.05 days, respectively), highlighting the importance of co-ordinated ground-based optical observations., Comment: 15 pages, 9 figures, 4 tables; accepted for publication in MNRAS

We developed a method that allows to classify the light curves of eclipsing binaries of the W UMa type (EW) with respect to their intrinsic variability. The algorithm measures several features of light curves, such as the amplitude of the O’Connell effect, the separation and location of maxima brightness as well as depths of the minima in subsequent orbital periods. This method is capable of distinguishing systems with presumed magnetic activity present from these without it, as well as recognizing systems with starspots migration and those with other types of intrinsic variability manifestation. The classification is done in an automatic way without a time consuming, visual inspection of light curves.

We present the results of our power spectral density analysis for the BL Lac object OJ\,287, utilizing the {\it Fermi}-LAT survey at high-energy $\gamma$-rays, {\it Swift}-XRT in X-rays, several ground-based telescopes and the {\it Kepler} satellite in the optical, and radio telescopes at GHz frequencies. The light curves are modeled in terms of continuous-time auto-regressive moving average (CARMA) processes. Owing to the inclusion of the {\it Kepler} data, we were able to construct \emph{for the first time} the optical variability power spectrum of a blazar without any gaps across $\sim6$ dex in temporal frequencies. Our analysis reveals that the radio power spectra are of a colored-noise type on timescales ranging from tens of years down to months, with no evidence for breaks or other spectral features. The overall optical power spectrum is also consistent with a colored noise on the variability timescales ranging from 117 years down to hours, with no hints of any quasi-periodic oscillations. The X-ray power spectrum resembles the radio and optical power spectra on the analogous timescales ranging from tens of years down to months. Finally, the $\gamma$-ray power spectrum is noticeably different from the radio, optical, and X-ray power spectra of the source: we have detected a characteristic relaxation timescale in the {\it Fermi}-LAT data, corresponding to $\sim 150$\,days, such that on timescales longer than this, the power spectrum is consistent with uncorrelated (white) noise, while on shorter variability timescales there is correlated (colored) noise., Comment: ApJ accepted

We present results from an observational campaign on the close binary system 2MASS J16211735+4412541 and a preliminary model based on the photometric data gathered during the quiescent and outburst levels. The modeling, done with the Wilson-Devinney code and its improvements, failed to reproduce the observational properties of the system. A secondary minimum obtained within the stellar model that is too shallow, as well as the evidence provided by the spectroscopic observations performed at outburst and quiescence, point toward an accretion disk surrounding one component, likely a white dwarf, as the cause of the outburst. Using a simple disk model, we modeled the observed multicolor light curves taken two (2016 August) and eight (2017 March) months after the outburst. We obtained a reasonable fit to the 2016 August light curves but those from 2017 March cannot be explained with the same parameters. We conclude that J1621 is an eclipsing cataclysmic binary, with an accretion disk still present almost a year after outburst, and not a contact-type system as previously classified. The binary is seen at an inclination of about 84° and there is evidence of changing accretion rates and disk parameters as a result of the outburst. Our results indicate that more cataclysmic variables may be hidden among contact binaries.

The cyclic behaviour of (O-C) residuals of eclipse timings in the sdB+M eclipsing binary NSVS 14256825 was previously attributed to one or two Jovian-type circumbinary planets. We report 83 new eclipse timings that not only fill in the gaps in those already published but also extend the time span of the (O-C) diagram by three years. Based on the archival and our new data spanning over more than 17 years we re-examined the up to date system (O-C). The data revealed systematic, quasi-sinusoidal variation deviating from an older linear ephemeris by about 100 s. It also exhibits a maximum in the (O-C) near JD 2,456,400 that was previously unknown. We consider two most credible explanations of the (O-C) variability: the light propagation time due to the presence of an invisible companion in a distant circumbinary orbit, and magnetic cycles reshaping one of the binary components, known as the Applegate or Lanza-Rodono effect. We found that the latter mechanism is unlikely due to the insufficient energy budget of the M-dwarf secondary. In the framework of the third-body hypothesis, we obtained meaningful constraints on the Keplerian parameters of a putative companion and its mass. Our best-fitting model indicates that the observed quasi-periodic (O-C) variability can be explained by the presence of a brown dwarf with the minimal mass of 15 Jupiter masses rather than a planet, orbiting the binary in a moderately elliptical orbit (~ 0.175) with the period of ~ 10 years. Our analysis rules out two planets model proposed earlier., Comment: 17 pages, 9 figures, 4 tables, accepted to AJ

We report optical photometric and polarimetric observations of the blazar OJ 287 gathered during 2016/17. The high level of activity, noticed after the General Relativity Centenary flare, is argued to be part of the follow-up flares that exhibited high levels of polarization and originated in the primary black hole jet. We propose that the follow-up flares were induced as a result of accretion disk perturbations, travelling from the site of impact towards the primary SMBH. The timings inferred from our observations allowed us to estimate the propagation speed of these perturbations. Additionally, we make predictions for the future brightness of OJ 287. © 2017 by the authors.

We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in the high-frequency domain both in the ground-based data and in Kepler observations. In the longer-period domain, the Lomb–Scargle periodogram revealed several peaks above the 99% significance level. The longest one—about 95 days—corresponds to the innermost stable circular orbit (ISCO) period of the more massive black hole. The 43-day period could be an alias, or it can be attributed to accretion in the form of a two-armed spiral wave.

We analyse the light curve in the R-band gathered during the 2015/16 observing season of OJ287. We did a search for QPOs using several methods in wide time domain. No statistically significant periods were found in the high frequency domain both in the ground data and also in K2 observations. In the longer periods domain the Lomb-Scargle periodogram revealed several peaks above the 99\% significance level. The longest one, about 95-day, corresponds to the ISCO period of the more massive SMBH. The 43-day period could be an alias or can be attributed to accretion in the form of two armed spiral wave.

We report on the analysis of 34 years of photometric observations of the pulsating helium atmosphere white dwarf GD358. The complete data set includes archival data from 1982-2006, and 1195.2 hours of new observations from 2007- 2016. From this data set, we extract 15 frequencies representing g-mode pulsation modes, adding 4 modes to the 11 modes known previously. We present evidence that these 15 modes are ell = 1 modes, 13 of which belong to a consecutive sequence in radial overtone k. We perform a detailed asteroseismic analysis using models that include parameterized, complex carbon and oxygen core composition profiles to fit the periods. Recent spectroscopic analyses place GD358 near the red edge of the DBV instability strip, at 24,000 plus or minus 500 K and a log g of 7.8 plus or minus 0.08 dex. The surface gravity translates to a mass range of 0.455 to 0.540 solar masses. Our best fit model has a temperature of 23,650 K and a mass of 0.5706 solar masses. That is slightly more massive than suggested by most the recent spectroscopy. We find a pure helium layer mass of 10^-5.50, consistent with the result of previous studies and the outward diffusion of helium over time., Comment: 94 pages, 14 figures, 7 tables, Accepted for publication in the ApJ

Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the binary black hole model for OJ~287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the binary black hole central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level., 24 pages, 11 figures, 3 tables, accepted for publication in ApJ

Detection of periodicity in the broad-band non-thermal emission of blazars has so far been proven to be elusive. However, there are a number of scenarios which could lead to quasi-periodic variations in blazar light curves. For example, orbital or thermal/viscous period of accreting matter around central supermassive black holes could, in principle, be imprinted in the multi-wavelength emission of small-scale blazar jets, carrying as such crucial information about plasma conditions within the jet launching regions. In this paper, we present the results of our time series analysis of $\sim 9.2$ year-long, and exceptionally well-sampled optical light curve of the BL Lac OJ 287. The study primarily uses the data from our own observations performed at the Mt. Suhora and Krak\'ow Observatories in Poland, and at the Athens Observatory in Greece. Additionally, SMARTS observations were used to fill in some of the gaps in the data. The Lomb-Scargle Periodogram and the Weighted Wavelet Z-transform methods were employed to search for the possible QPOs in the resulting optical light curve of the source. Both the methods consistently yielded possible quasi-periodic signal around the periods of $\sim 400$ and $\sim 800$ days, the former one with a significance (over the underlying colored noise) of $\geq 99\%$. A number of likely explanations for such are discussed, with a preference given to a modulation of the jet production efficiency by highly magnetized accretion disks. This supports the previous findings and the interpretation reported recently in the literature for OJ 287 and other blazar sources., Comment: 7 pages, 5 figures, ApJ accepted

Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for 128 SUUMa-type dwarf novae observed mainly during the 2015-2016 season and characterized these objects. The data have improved the distribution of orbital periods, the relation between the orbital period and the variation of superhumps, and the relation between period variations and the rebrightening type in WZSge-type objects. Coupled with new measurements of mass ratios using growing stages of superhumps, we now have a clearer and statistically greatly improved evolutionary path near the terminal stage of evolution of cataclysmic variables. Three objects (V452 Cas, KK Tel, and ASASSN-15cl) appear to have slowly growing superhumps, which is proposed to reflect the slow growth of the 3 : 1 resonance near the stability border. ASASSN-15sl, ASASSN-15ux, SDSSJ074859.55+312512.6, and CRTS J200331.3-284941 are newly identified eclipsing SUUMa-type (or WZ Sge-type) dwarf novae. ASASSN- 15cy has a short (0.050 d) superhump period and appears to belong to EI Psc-type objects with compact secondaries having an evolved core. ASASSN-15gn, ASASSN- 15hn, ASASSN-15kh, and ASASSN-16bu are candidate period bouncers with superhump periods longer than 0.06 d. We have newly obtained superhump periods for 79 objects and 13 orbital periods, including periods from early superhumps. In order that future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines on how to organize observations of various superoutbursts., This work was supported by the Grant-in-Aid “Initiative for High-Dimensional Data-Driven Science through Deepening of Sparse Modeling” (25120007) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan.

We tested the hypothesis that mental rotation would delay response-related processing as indicated by transient slowing of the heart beat. Thirty college-age subjects (half female) were presented with normal and mirror image letters rotated at 0, 60, 120, and 180 degrees. Three letters were assigned to a right-hand response; a separate three to a left-hand response. Responses were only required for letters in one orientation, mirror or normal. Continuous measures of interbeat interval (IBI) of the heart, respiration, and muscle tension were collected. Performance results were largely consistent with prior findings. Greater angular displacement of the stimuli was associated with greater lengthening of IBI immediately after the stimulus. IBI was influenced equally by angle of rotation in respond and inhibit trials. The lengthening of IBI was interpreted as due to a delay in response selection and execution due to mental rotation.

We investigated the inhibitory regulation of perceptual-motor processing streams in a task that switched between spatially compatible and incompatible stimulus-response mappings. Thirty male and female college-aged participants performed a reaction time (RT) task in which the response was either spatially compatible or not depending on a cue immediately preceding the stimulus. The cue-to-stimulus interval (CI) was either 50 or 500 ms. Incompatible mapping yielded the typical slower responses than compatible mapping at 500 ms, but not at 50 ms. Changes in cardiac interbeat interval (IBI) and performance suggested that automatic responses to compatible stimuli were suppressed at 50 ms. Both performance and IBI changes as well as individual differences in these measures suggested a precue preparatory schema or set biased toward suppressing the compatible mapping. An alternate hypothesis of a cue-induced suppression was questioned. The results illustrate the operation of different supervisory processes in the anticipatory and online control of action.

We examined the coordination of processing streams when two reaction stimuli are presented with minimal temporal separation (the psychological refractory period, PRP, paradigm). We tested the hypothesis that individuals that grouped responses to the two stimuli would schedule response preparation later than those not-grouping their responses would. Performance measures were combined with a cardiac measure interpreted as an index of response inhibition. Forty-two college-aged participants performed an auditory choice task followed in 50, 100 or 400 ms by a visual choice reaction time (RT) task. Performance results replicated prior work. The timing of cardiac inter-beat intervals (IBIs) showed that participants grouping their reactions did appear to delay response preparation; while Non-Groupers promptly initiated response selection for the initial task. These results generally supported the importance of preparation for understanding the coordination of processing streams.

Continuing the project described by Kato et al. (2009, PASJ, 61, S395, arXiv:0905.1757), we collected times of superhump maxima for 56 SU UMa-type dwarf novae mainly observed during the 2013-2014 season and characterized these objects. We detected negative superhumps in VW Hyi and indicated that the low number of normal outbursts in some supercycle can be interpreted as a result of the disk tilt. This finding, combined with the Kepler observation of V1504 Cyg and V344 Lyr, suggests that the disk tilt is responsible for modulating the outburst pattern in SU UMa-type dwarf novae. We also studied the deeply eclipsing WZ Sge-type dwarf nova MASTER OT J005740.99+443101.5 and found evidence of a sharp eclipse during the phase of early superhumps. The profile can be reproduced by a combination of the eclipse of the axisymmetric disk and the uneclipsed light source of early superhumps. This finding confirms the lack of evince of a greatly enhanced hot spot during the early stage of WZ Sge-type outburst. We detected growing (stage A) superhumps in MN Dra and give a suggestion that some of SU UMa-type dwarf novae situated near the critical condition of tidal instability may show long-lasting stage A superhumps. The large negative period derivatives reported in such systems can be understood a result of the combination of stage A and B superhumps. The WZ Sge-type dwarf novae AL Com and ASASSN-13ck showed a long-lasting (plateau-type) rebrightening. In the early phase of the rebrightening, both objects showed a precursor-like outburst, suggesting that the long-lasting rebrightening is triggered by a precursor outburst., Comment: 73 pages, 88 figures, accepted for publication in PASJ

A stop signal paradigm in combination with heart rate measures were used to test the hypothesis of deficient inhibitory processing in boys with attention deficit hyperactivity disorder (ADHD). The authors measured the inhibitory process initiated by a stop signal by observing its success, its latency using a horse race model, and its impact on the timing of the heartbeat. Boys with ADHD performed well and showed appropriate psychophysiological changes. Inhibition latencies were longer in the boys with ADHD, particularly those with concurrent oppositional defiant disorder, than in the controls. Cardiac evidence suggested that greater preparation was associated with inhibition failures in controls, but not in the boys with ADHD. Boys with ADHD seem capable of attending carefully to control responses, but this control appears less effective and arguably is more effortful than in other boys.

Insulin-like growth factor-I is involved in mammary gland development, promoting proliferation and inhibiting apoptosis of mammary epithelial cells (MECs). Mitogenic actions of IGF-I are mainly mediated by the phosphatidylinositol-3 kinase (PI3K)/Akt signaling pathway. We have found that in the presence of IGF-I bovine BME-UV1 MECs cultured on reconstituted basement membrane form large spheroids with disrupted polarity and no cavity in the center. These cells showed enhanced phosphorylation of Akt, decreased level of cleaved caspase-3, and sustained proliferative activity throughout the 16-d period of 3-dimensional culture. Inhibition of the PI3K/Akt pathway by a specific inhibitor of PI3K, LY294002, resulted in the restoration of the normal acinar phenotype. However, this effect was noted only when LY294002 was added in the second week of 3-dimensional culture, which corresponded with the time of cell cycle arrest and polarity formation under control conditions. Normal development of acini was also obtained when BME-UV1 cells were treated simultaneously with IGF-I and 17β-estradiol. The addition of 17β-estradiol regulated Akt activation, enabling the subsequent initiation of polarization processes. 17β-Estradiol also increased the level of IGFBP-3 protein in MECs cultured on Matrigel in the presence of IGF-I. The presented results indicate important interactions between signaling pathways activated by estrogen and IGF-I, which regulate alveologenesis in bovine mammary gland.

We report new mid-eclipse times of the two close binaries NSVS14256825 and HS0705+6700, harboring an sdB primary and a low-mass main-sequence secondary. Both objects display clear variations in the measured orbital period, which can be explained by the action of a third object orbiting the binary. If this interpretation is correct, the third object in NSVS14256825 is a giant planet with a mass of roughly 12 M_Jup. For HS0705+6700, we provide evidence that strengthens the case for the suggested periodic nature of the eclipse time variation and reduces the uncertainties in the parameters of the brown dwarf implied by that model. The derived period is 8.4 yr and the mass is 31 M_Jup, if the orbit is coplanar with the binary. This research is part of the PlanetFinders project, an ongoing collaboration between professional astronomers and student groups at high schools., Comment: Accepted by Astron. and Astrophys

Male rats of Wistar strain (n = 48) were fed a vitamin A deficient diet for 3 days of adaptation period and then a 10 day experimental period to reduce slightly the body stores of this vitamin. Half of the animals were subjected to physical training and/or oral vitamin A supplementation. Four different doses of supplementation were used--0, 7.5, 15 and 60 microg/d/rat, which is equivalent to 0, 25, 50 and 200 IU of vitamin A, respectively. Animals from the defined groups ran on a treadmill with a rate of 2.0 m/s for 15 minutes per day for 10 days. After overnight fasting, the rats were sacrificed, and insulin in blood serum and hepatic retinol concentrations were estimated. Daily feed intake and daily body gains were similar in groups of sedentary and physically trained rats. A moderate level of oral vitamin A supplementation (the highest supplemented dose was about 6 x the above recommended NRC level) did not cause any changes in these zootechnical parameters. Oral Vitamin A supplementation resulted in an increase in retinol concentration in the liver (F = 15.2, p0.001), but without significant difference between trained and untrained animals. Physical training of rats caused a statistically significant decrease of insulin concentration in blood serum (1.53 +/- 0.18 vs. 1.73 +/- 0.20). This difference was highly significant (F = 11.1, p0.001). Vitamin A supplementation was found not to influence the concentration of this hormone, which is responsible for energy metabolism regulation in the body. Based on estimated parameters, the necessity of vitamin A excessive use in physically trained subjects was not proven.

This study was conducted to determine the effect of a 3-month dietary protein restriction - protein provided 9% of energy (20% in control group). In this dietary restriction folic acid, vitamins B(2) and B(6) were delivered in amount three times above the standard level. It was observed that animals fed a protein restricted (PR) diet weighed about 5% less than animals consuming adequate diet, but the difference was not statistically significant. Enrichment of PR diet with vitamin B or folic acid caused tendency to further suppression of weight gain, and in case of vitamin B(6) these differences were statistically significant. However, such body weight (BW) suppression was not observed when all studied vitamins were used together. Significant reductions in relative liver weight (vitamin B(2) addition), the heart (folic acid) and the lungs (vitamin B(6)) were observed. The PR diet, when all vitamins were added together, caused a decrease in weights of the lungs, heart and liver scaled to BW of rats, simultaneously with a significant increase in testis weight. Feed intake and feed conversion ratio were higher in animals given PR diet without a significant influence of vitamin supplementation (except vitamin B(6) causing further increase in feed conversion ratio). Hepatic fatty acids composition of rats was not affected by protein restriction, as well as by single vitamin supplementation. However, dietary supplementation of all examined vitamins together caused a decrease in monounsaturated fatty acids followed by an increase in polyunsaturated fatty acids participation in total fatty acids pool. It seems that enrichment of PR diet with a mixture of folic acid, vitamins B(2) and B(6) resulted in a partial reverse of growth suppression and reduction in testis size in rats.

Laboratory method for studies of clinical disorders of beta-oxidation is described. The effects of other diet components such as microelements (Cr3+ ions) and non-digestible oligofructans (inulin and oligofructose) as stimulatory factors on the activity of beta-oxidation and cholesterol and triacylglyceroles levels lowering are reported.

Disorders in energetical processes are described from the point of view of energy production and the possibility of substitution of substrates for ATP synthesis. The effects of other diet components such as microelements (Cr3+ ions) and non-digestible oligofructans (inulin and oligofructose) as stimulatory factors on the activity of beta-oxidation and cholesterol and triacylglyceroles levels lowering are reported.

We investigated the inhibitory regulation of perceptual-motor processing streams in a task that switched between spatially compatible and incompatible stimulus-response mappings. Thirty male and female college-aged participants performed a reaction time (RT) task in which the response was either spatially compatible or not depending on a cue immediately preceding the stimulus. The cue-to-stimulus interval (CI) was either 50 or 500 ms. Incompatible mapping yielded the typical slower responses than compatible mapping at 500 ms, but not at 50 ms. Changes in cardiac interbeat interval (IBI) and performance suggested that automatic responses to compatible stimuli were suppressed at 50 ms. Both performance and IBI changes as well as individual differences in these measures suggested a precue preparatory schema or set biased toward suppressing the compatible mapping. An alternate hypothesis of a cue-induced suppression was questioned. The results illustrate the operation of different supervisory processes in the anticipatory and online control of action.

We examined the coordination of processing streams when two reaction stimuli are presented with minimal temporal separation (the psychological refractory period, PRP, paradigm). We tested the hypothesis that individuals that grouped responses to the two stimuli would schedule response preparation later than those not-grouping their responses would. Performance measures were combined with a cardiac measure interpreted as an index of response inhibition. Forty-two college-aged participants performed an auditory choice task followed in 50, 100 or 400 ms by a visual choice reaction time (RT) task. Performance results replicated prior work. The timing of cardiac inter-beat intervals (IBIs) showed that participants grouping their reactions did appear to delay response preparation; while Non-Groupers promptly initiated response selection for the initial task. These results generally supported the importance of preparation for understanding the coordination of processing streams.

Leguminous seeds contain a lot of antinutritional factors (ANFs) such as protease inhibitors, lectins and condensed tannins which can affect bioavailability of nutrients. Detrimental effect of protease inhibitors can be decreased by sulphur amino acids addition. Moreover, most of the leguminous ANFs are thermolabile. Hence, legumes tested in our study were extruded and/or diets were supplemented with methionine and cystine (0.15% + 0.15%). The present experiment was performed for 28 days on 90 Wistar rats divided into nine feeding groups. Semipurified diets (10% casein) were supplemented (10%), except the control one, with soybean (S) or faba bean (F), raw (R) or extruded (E), with addition of sulphur amino acids (SAA) or without them. The Cr concentration was determined in the femur bone. Total feed intake during whole trial widely varied among the groups and was the lowest in SR (289 g) and FR (294 g) groups. There was no correlation between feed intake and Cr content in the femur bone. Generally, 10% soybean in the diet decreased Cr concentration in the bones, and faba bean increased it. The SAA addition to diets generally increased femur Cr content. However, there was a significant interaction between SAA supplementation and extrusion of faba bean, hence, the effect of their combination was unclear.

The experiment was performed on Sprague-Dawley male rats weighting 203, 103 and 53 g, and female 99 g. Animals were fed for 2 weeks a diet containing 0.1 and 2.0 ppm of Se (Na2SeO3 added). It was observed that the daily Se intake per kg of BW is lowered with an increase in animals body weight. Se-supplementation caused a significant increase of Se content in plasma and red blood cells. The highest concentration of Se in plasma and in RBC was found in females. GSH-Px activity was higher in RBC of all male rats receiving a Se-supplemented diet, but not in females. In plasma these differences between Se-adequate and supplemented rats were significant in youngest male rats and in females. These results suggest that age and sex of rats affect the concentration of Se and GSH-Px activity in plasma and RBC of rats.

Zusammenfassung Der Einflus des Hungerns auf Plasma-Aminosauren-Indices und Stickstoffausscheidungen im Harn bei Woll- und Fleisch-Kaninchen Es wurde der Stoffwechseleffekt einer Hypoinsulinamie verursacht durch einen dreitagigen Nahrungsentzug bei Woll- (Weise Angoras) und Fleisch- (Hollander Riesen) Kaninchen verglichen. Der Muskeleiweisumsatz wurde mit Hilfe der 3-Methyl-Histidin-Ausscheidung im Harn bzw. Plasma-Aminosauren-Indices ermittelt. Unter Standardfutterung wurden bei Angora-Kaninchen hohere Plasmagehalte an Insulin, freien Aminosauren, freien Fettsauren aber niedrigere Plasmagehalte an Harnstoff als beim Hollander-Kaninchen gemessen. Nahrungsentzug fuhrte zu einer Verringerung des Muskelprotein-Abbaus, indiziert durch einen Abfall der 3-Methyl-Histidin-Ausscheidung im Harn. Unabhangig von der Kaninchenrasse nahm das Korpergewicht der Tiere, der Insulin- und der Glucosegehalt im Blutplasma ab, wahrend die Konzentrationen an freien Fettsauren und Harnstoff im Plasma anstiegen. Bei Fleischkaninchen war ein betrachtlicher Anstieg an freien Aminosauren im Plasma nach einer 3-tagigen Hungerperiode zu beobachten. Davon waren verzweigtkettige Aminosauren, 3-Methyl-Histidin, Alanin, Threonin, Tyrosin, Phenylalanin und Histidin betroffen. Bei der Wollrasse waren nur Valin, 3-Methyl-Histidin und Citrullin erhoht. Die Ausscheidung von Orotsaure und Harnstoff mit dem Harn fiel im Hungerzustand bei beiden Rassen ab. Zwischen der Ausscheidung von Orotsaure und Harnstoff mit dem Harn wurde eine hoch signifikante Beziehung (r = 0,76) gefunden.

Summary The influence of different intensities of hyperammonaemia on portal venous blood flow (P. V. B. F.) in rabbits was investigated. Different doses of NH4Cl (2, 10 and 50 μmol × kg bw−1 × min−1) were given in 10 min infusions into the common carotid artery. Animals in the control group received 0.9% NaCl by the same methods. The P. V. B. F. was measured using an electromagnetic method and the concentration of ammonia in the blood of the common carotid artery, portal and jugular veins was estimated. During the NH4Cl infusion the highest concentration of ammonia occurred in the blood of the common carotid artery. After completion of ammonium chloride infusion, the level of ammonia in the blood of this artery dropped rapidly below the level observed in the jugular vein. The lowest dynamic changes of ammonia concentration were found in the portal blood. The smallest NH4Cl dose (2 μmol × kg bw−1 × min−1) caused a decrease of P. V. B. F. A further increase of ammonia concentration in peripheral blood abolished this effect (dose 10 μmol × kg bw−1 × min−1) and in the case of the highest NH4Cl dose (50 μmol × kg bw−1 × min−1) an increase of P. V. B. F. was seen. The response of P. V. B. F. to increasing peripheral ammonia concentration is discussed. Zusammenfassung Veranderungen im portalen Blutflus bei Kaninchen mit erhohter Blutammoniakkonzentration: Es wurde der Einflus einer verschiedenartig erhohten Ammoniakkonzentration im Blut auf den Blutflus in der Pfortader (P. V. B. F.) bei Kaninchen untersucht. Wahrend 10 minutiger Infusionen in die Arteria carotis communis wurden verschiedene Dosen von NH4Cl (2, 10 und 50 μmol × kg−1 [Korpergewicht] × min−1) verabreicht. Den Kontrolltieren wurde 0,9%ige NaCl-Losung infundiert. Der Blutflus wurde mit einem elektromagnetischen Mesverfahren bestimmt. Die Ammoniakkonzentration wurde im Blut der Arteria carotis communis, der Pfortader und der Vena jugularis ermittelt. Wahrend der NH4Cl-Infusion trat die hochste Ammoniakkonzentration im Blut der Arteria carotis communis auf. Nach Abschlus der Infusion fiel die Ammoniakkonzentration in diesem Gefas unter diejenige der Vena jugularis ab. Die geringsten Veranderungen der Ammoniakkonzentration wurden im Pfortaderblut gefunden. Die kleinste NH4Cl-Dosis (2 μmol × kg−1 × min−1) verursachte eine Abnahme des portalen Blutflusses. Eine daruber hinausgehende Erhohung der Ammoniakkonzentration im peripheren Blut (Dosis: 10μmol × kg−1 × min−1) eliminierte diesen Effekt. Bei der hochsten NH4Cl-Dosis (50 μmol × kg−1 × min−1) ergab sich eine Steigerung des P. V. B. F. Die Reaktion des P. V. B. F. auf einen Anstieg der peripheren Ammoniakkonzentration wird diskutiert.

The experiment was conducted on sheep receiving NH4Cl infusions into v. mesentericta anterior. During first 3 h animals received ammonia in a dose of 13 mumol X min-1 X kg body wt.-1 and then next 3 h in a dose of 30 mumol X min-1 X kg body wt.-1. When ammonia was administered in smaller doses its concentration increased to 0.65 and 0.22 mmol/l in portal and peripheral blood, respectively. Simultaneous slight increase of ATP and marked of 2,3-diphosphoglycerate (2,3-DPG) was observed. These effects of moderate ammonia loading are probably caused by the rise of glucose utilization in erythrocytes. Ammonia given in a higher dose induced further rise of its concentration to 1.1 and 0.51 mmol/l in portal and peripheral blood, respectively. Such NH4Cl infusion caused a further rise of 2,3-DPG concentration connected with the drop of ATP level in ovine red blood cells. It seems that a decrease of ATP level was mainly the result of local high 2,3-DPG level which inhibits glycolytic enzymes.

Summary The alloxan-like compound dehydrouramil hydrate hydrochloride (DHU) significantly decreased insulin, and elevated glucose and urea concentration in the blood of Angora White rabbits. An increase of urinary orotic acid, and urea excretion during 5 days after DHU injection was observed. There was a significant positive correlation (r = 0.54, P < 0.001) between urine flow rate and orotic acid excretion. Zusammenfassung Die Ausscheidung von Orotsaure uber den Harn bei Kaninchen mit Diabetes Die Alloxan-ahnliche Verbindung Dehydrouramylhydrat-Hydrochlorid (DHU) bewirkte bei Angora-Kaninchen eine signifikante Abnahme des Insulin-Spiegels sowie einen Anstieg der Glucose- und Harnstoffkonzentration des Blutes. Im Verlauf von 5 Tagen nach der DHU-Injektion wurde eine Zunahme der Ausscheidung von Orotsaure und Harnstoff uber den Harn beobachtet. Zwischen dem Harnflus und der Orotsaureexkretion ergab sich eine positive Korrelation (r = 0,54, p < 0,001).

The experiment was carried out on 85 female breed Wistar rats divided into five groups. All groups of animals except 1 got NH4Cl in the feed in increasing amounts: 2-nd group 1%, 3-rd 2%, 4-th 4% and 5-th group 8%. After two weeks the animals were killed and then the slides of muscles and liver were taken. The levels of ATP, ADP and sum of ATP and ADP in the tissues were marked. In both tissues it was shown that there was an increase of ATP level in the case of higher level of NH4Cl up to 2% and a decrease in cases of lower concentration. Probably the decrease was caused by augmented hydrolysis of ATP to ADP, which is confirmed by the increase of ADP level. We could suppose, that small amounts of NH4Cl (1--2%) accelerate the synthesis of ATP in muscles and liver. The disposal of ADP levels by augmented concentration NH4Cl in fodder is different in both tissues. In the case of muscles there was a decrease of their level to 3-rd group (2% NH4Cl) and an increase to 5-th group. We could presume that further rise of level depends on the penetration of ADP from mitochondria to cytoplasma. The disposal of ADP level in liver is similar to the disposal of ATP. We can see a rise to 3-rd group and a fall to 4-th group. This decrease probably is connected with the production of phosphocreatine needed as a source of energy for the work of muscles.

The blood plasma concentration of pseudouridine was estimated in 104 healthy adult subjects, and 108 patients suffering from malignant proliferative diseases. The HPLC method for simultaneous determination of pseudouridine and creatinine was applied. The average physiological concentration of pseudouridine in blood plasma was 2.43 +/- 0.97 mumol.l-1 or 29.15 +/- 7.40 mmol.mol-1 creatinine. The physiological urinary excretion of pseudouridine was 14.32 +/- 5.20 mumol.24 h-1.kg-0.75 or 19.60 +/- 5.22 mmol.mol-1 creatinine. Renal clearance of pseudouridine and endogenous creatinine were 4.04 +/- 0.99 and 5.50 +/- 1.46 ml.kg-0.75, respectively. A positive correlation (r = 0.55, P < 0.01) was found between age (in the range 20-92 years) and blood plasma pseudouridine concentration (mumol.l-1). By expressing plasma pseudouridine in relation to plasma creatinine, the apparent influence of non-metabolic factors (age, renal insufficiency, blood dilution) on the plasma pseudouridine concentration were largely excluded. Among haematological proliferative diseases the highest values of plasma pseudouridine concentrations were observed in chronic lymphocytic leukaemia (8.19 mumol.l-1; 54.9 mmol.mol-1 creatinine) and multiple myeloma (7.02 mumol.l-1; 52.5 mmol.mol-1 creatinine). In multiple myeloma, but not in chronic lymphocytic leukaemia, the plasma pseudouridine concentration depended on the clinical stage. A lower, but still significant response in non-Hodgkin's lymphoma was noted (4.03 mumol.l-1; 40.88 mmol.mol-1 creatinine). A significant increase of the plasma pseudouridine concentration was characteristic of adenocarcinomas of the large intestine, and it occurred in the early stages of malignant growth. In patients with lung cancer the plasma pseudouridine concentration was elevated only in advanced cases with metastases.(ABSTRACT TRUNCATED AT 250 WORDS)