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We present Hubble Space Telescope (HST) transit observations of the Hot-Jupiter WASP-79b acquired with the Space Telescope Imaging Spectrograph (STIS) in the near ultraviolet (NUV). Two transit observations, part of the PanCET program, are used to obtain the transmission spectra of the planet between 2280 and 3070{\AA}. We correct for systematic effects in the raw data using the jitter engineering parameters and polynomial modelling to fit the white light curves of the two transits. We observe an increase in the planet-to-star radius ratio at short wavelengths, but no spectrally resolved absorption lines. The difference between the radius ratios at 2400 and 3000{\AA} reaches $0.0191\pm0.0042$ ($\sim$4.5$-\sigma$). Although the NUV transmission spectrum does not show evidence of hydrodynamical escape, the strong atmospheric features are likely due to species at very high altitudes. We performed a 1D simulation of the temperature and composition of WASP-79b using Exo-REM. The temperature pressure profile crosses condensation curves of radiatively active clouds, particularly MnS, Mg$_2$SiO$_4$, Fe, and Al$_2$O$_3$. Still, none of these species produces the level of observed absorption at short wavelengths and can explain the observed increase in the planet's radius. WASP-79b's transit depth reaches 23 scale height, making it one of the largest spectral features observed in an exoplanet at this temperature ($\sim$1700 K). The comparison of WASP-79b's transmission spectrum with three warmer hot Jupiters shows a similar level of absorption to WASP-178b and WASP-121b between 0.2 and 0.3$\mu$m, while HAT-P-41b's spectrum is flat. The features could be explained by SiO absorption., Comment: Accepted for publication January 31, 2023 in the Journal Astronomy & Astrophysics

Full list of authors: Luque, R.; Fulton, B. J.; Kunimoto, M.; Amado, P. J.; Gorrini, P.; Dreizler, S.; Hellier, C.; Henry, G. W.; Molaverdikhani, K.; Morello, G.; Pena-Monino, L.; Perez-Torres, M.; Pozuelos, F. J.; Shan, Y.; Anglada-Escude, G.; Bejar, V. J. S.; Bergond, G.; Boyle, A. W.; Caballero, J. A.; Charbonneau, D.; Ciardi, D. R.; Dufoer, S.; Espinoza, N.; Everett, M.; Fischer, D.; Hatzes, A. P.; Henning, Th; Hesse, K.; Howard, A. W.; Howell, S. B.; Isaacson, H.; Jeffers, S., V; Jenkins, J. M.; Kane, S. R.; Kemmer, J.; Khalafinejad, S.; Kidwell, R. C., Jr.; Kossakowski, D.; Latham, D. W.; Lillo-Box, J.; Lissauer, J. J.; Montes, D.; Orell-Miquel, J.; Palle, E.; Pollacco, D.; Quirrenbach, A.; Reffert, S.; Reiners, A.; Ribas, I; Ricker, G. R.; Rogers, L. A.; Sanz-Forcada, J.; Schlecker, M.; Schweitzer, A.; Seager, S.; Shporer, A.; Stassun, K. G.; Stock, S.; Tal-Or, L.; Ting, E. B.; Trifonov, T.; Vanaverbeke, S.; Vanderspek, R.; Villasenor, J.; Winn, J. N.; Winters, J. G.; Osorio, M. R. Zapatero.-- This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., We report the discovery of a multiplanetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of Rb = 1.240 ± 0.023 R⊕, a mass of Mb = 2.14 ± 0.34 M⊕, and a bulk density of ρb = 6.2 ± 1.0 g cm−3, and HD 260655 c, with a period of 5.71 d, a radius of , a mass of Mc = 3.09 ± 0.48 M⊕, and a bulk density of g cm−3. The planets have been detected in transit by the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed independently with archival and new precise radial velocities obtained with the HIRES and CARMENES instruments since 1998 and 2016, respectively. At a distance of 10 pc, HD 260655 has become the fourth closest known multitransiting planet system after HD 219134, LTT 1445 A, and AU Mic. Due to the apparent brightness of the host star (J = 6.7 mag), both planets are among the most suitable rocky worlds known today for atmospheric studies with the James Webb Space Telescope, both in transmission and emission. © R. Luque et al. 2022., This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. CARMENES is an instrument at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto (Almería, Spain), operated jointly by the Junta de Andalucía and the Instituto de Astrofísica de Andalucía (CSlC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Científicas (CSIC), the Ministerio de Economía y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium with additional contributions. Some of the observations in this paper made use of the NN-EXPLORE Exoplanet and Stellar Speckle Imager (NESSI). NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. R.L. acknowledges funding from University of La Laguna through the Margarita Salas Fellowship from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation funds. We acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación and the ERDF “A way of making Europe” through projects PID2019-109522GB-C5[1:4]/AEI/10.13039/501100011033 and the Centre of Excellence “Severo Ochoa” and “María de Maeztu” awards to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), Instituto de Astrofísica de Andalucía (SEV-2017-0709), and Centro de Astrobiología (MDM-2017-0737); the Generalitat de Catalunya/CERCA programme; the Deutsche Forschungsgemeinschaft (DFG) through the Major Research Instrumentation Programme and Research Unit FOR2544 “Blue Planets around Red Stars” (RE 2694/8-1, KU 3625/2-1), the Excellence Cluster ORIGINS (EXC-2094 – 390783311) and the Priority Programme “Exploring the Diversity of Extrasolar Planets” (JE 701/5-1); the National Aeronautics and Space Administration under grants 80NSSC21K0367 and 80NSSC22K0165 in support of Cycles 3 and 4 of the TESS Guest Investigator program; the National Science Foundation, Tennessee State University, and the State of Tennessee through its Centers of Excellence Program; and the Bulgarian BNSF program “VIHREN-2021” project No. KP-06-DV/5. The results reported herein benefited from collaborations and/or information exchange within the program “Alien Earths” (supported by the National Aeronautics and Space Administration under agreement No. 80NSSC21K0593) for NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank VeraM. Passegger for a helpful discussion on the photospheric parameters of HD 260655.

Previous studies have related surface temperature maps, obtained with the Doppler imaging (DI) technique, of LQ Hya with long-term photometry. We compare surface magnetic field maps, obtained with the Zeeman Doppler imaging (ZDI) technique, with contemporaneous photometry, with the aim of quantifying the star's magnetic cycle characteristics. We inverted Stokes IV spectropolarimetry into magnetic field and surface brightness maps using a tomographic inversion code that models high signal-to-noise ratio mean line profiles produced by the least squares deconvolution (LSD) technique. The magnetic field and surface brightness maps reveal similar patterns to previous DI and ZDI studies: non-axisymmetric polar magnetic field structure, void of fields at mid-latitudes, and a complex structure in the equatorial regions. There is a weak but clear tendency of the polar structures to be linked with strong radial field and the equatorial ones with the azimuthal. We find a polarity reversal in the radial field between 2016 and 2017 coincident with an activity minimum seen in the long-term photometry. The inverted field strengths cannot easily be related with the observed spottedness, but we find that they are partially connected with the retrieved field complexity. Comparing to global magnetoconvection models for rapidly rotating young Suns, this field topology and dominance of the poloidal field component could be explained by a turbulent dynamo, where differential rotation does not play a major role (so called alpha^2 Omega or alpha^2 dynamos), and axi- and non-axisymmetric modes are excited simultaneously. The complex equatorial magnetic field structure could arise from the twisted (helical) wreaths often seen in these simulations, while the polar feature would be connected to the mostly poloidal non-axisymmetric component having a smooth spatial structure., 13 pages, 8 figures, 7 tables

We present Hubble Space Telescope optical and near-ultraviolet transmission spectra of the transiting hot-Jupiter HD189733b, taken with the repaired Space Telescope Imaging Spectrograph (STIS) instrument. The resulting spectra cover the range 2900-5700 Ang and reach per-exposure signal-to-noise levels greater than 11,000 within a 500 Ang bandwidth. We used time series spectra obtained during two transit events to determine the wavelength dependance of the planetary radius and measure the exoplanet's atmospheric transmission spectrum for the first time over this wavelength range. Our measurements, in conjunction with existing HST spectra, now provide a broadband transmission spectrum covering the full optical regime. The STIS data also shows unambiguous evidence of a large occulted stellar spot during one of our transit events, which we use to place constraints on the characteristics of the K dwarf's stellar spots, estimating spot temperatures around Teff~4250 K. With contemporaneous ground-based photometric monitoring of the stellar variability, we also measure the correlation between the stellar activity level and transit-measured planet-to-star radius contrast, which is in good agreement with predictions. We find a planetary transmission spectrum in good agreement with that of Rayleigh scattering from a high-altitude atmospheric haze as previously found from HST ACS camera. The high-altitude haze is now found to cover the entire optical regime and is well characterised by Rayleigh scattering. These findings suggest that haze may be a globally dominant atmospheric feature of the planet which would result in a high optical albedo at shorter optical wavelengths.

The determinants of the shape of the pulmonary input impedance spectrum were investigated using a mathematical model based on Womersley's equations for pulsatile flow in constrained viscoelastic tubes and structural data (morphometry, elasticity, and rheology) provided for the entire cat lung by Zhuang et al. Mean distending pressures and diameters of vessels were determined from the structural data and four independent variables: cardiac output and left atrial, pleural, and alveolar pressures. Studies were performed in a control model and a model whose structure was designed to imitate that of a subject with pulmonary vascular impairment. Model simplifications were investigated. Increasing left atrial pressure or cardiac output caused passive distention of vessels that increased total blood volume and decreased vascular resistance, creating a slight spectral shift downward and to the right. Increasing pleural pressure decreased total blood volume and increased vascular resistance, creating a spectral shift upward and to the right. Increasing levels of alveolar pressure resulted in increased vascular resistance and pressures and a shift in blood volume from the capillaries to the arteries without significant change in total blood volume, creating a spectral shift that was slightly downward and to the right . Model simplification studies demonstrated that (1) all vessels distal to the tenth generation (arteries with zero distending pressure diameters < 50 μM) can be modelled as a simple resistor or (2) all vessels distal to the fourth generation can be modelled as a modified Windkessel. Results obtained from the passive studies were consistent with those obtained from normal lambs and lambs with chronically elevated pulmonary blood flow. To model a hypertensive state created by injury to the lung microvasculature, the number and size of small vessels and the compliance constants of all arteries were decreased and the viscoelastic constant was increased, which created the requisite shift to the right and upward. To better match the modulus fluctuation and negative phase angles at higher frequencies in the hypertensive animals, the development of a major reflection site between the main and branch arteries was hypothesized.

Light curve analysis by MDW of the photometry and RV data accumulated to date on HD 209458 has made use of a simulations database created for an 8-day HST observing project led by RLG to look for transits in 47 Tuc. We report progress in developing a consistent set of parameters obtained with our versions of the Wilson-Devinney program, WD98 and wd98k93, specially modified to treat large grid sizes, corresponding to objects with radii exceeding 0.7RJ and masses greater than 0.1 MJ.This work is supported in part by grants to EFM by Canadian NSERC and by the Univ. of Calgary Research Grants Committee.

We studied the detailed profiles of blood flow in the right and left pulmonary arteries using 20 MHz pulsed Doppler ultrasound equipment in a lamb model. Fourteen lambs aged four to six weeks were selected. In six lambs, monocrotaline pyrrole was injected parenterally to create pulmonary hypertension (PH group). Eight other lambs served as unaltered controls (control group). The blood flow velocities were sampled in 1mm increments along the anterior-posterior axis of the branch arteries. The maximum velocity of the forward flow in the left pulmonary artery was higher than that in the right pulmonary artery in the control group (71.7 +/- 15.9 cm/s vs 60.2 +/- 13.5; p < 0.05). The fastest backward flow was located at the posterior position of the vessel in the right pulmonary artery in the control group (71.7 +/- 15.9 cm/s vs 60.2 +/- 13.5; p < 0.05). The fastest backward flow was located at the posterior position of the vessel in the right pulmonary artery in the control group. No significant bias in location was shown in the left pulmonary artery. Using indices of P90, acceleration time, P90*AcT, the velocity waveforms in the PH group were compared with those in the control group. In the left pulmonary artery, every index in the control group showed a significantly greater value that in the PH group. On the other hand, no significant differences were found between either group in the right pulmonary artery.

We present a new primary transit observation of the hot-jupiter HD189733b, obtained at 3.6 microns with the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope. Previous measurements at 3.6 microns suffered from strong systematics and conclusions could hardly be obtained with confidence on the water detection by comparison of the 3.6 and 5.8 microns observations. We use a high S/N Spitzer photometric transit light curve to improve the precision of the near infrared radius of the planet at 3.6 microns. The observation has been performed using high-cadence time series integrated in the subarray mode. We are able to derive accurate system parameters, including planet-to-star radius ratio, impact parameter, scale of the system, and central time of the transit from the fits of the transit light curve. We compare the results with transmission spectroscopic models and with results from previous observations at the same wavelength. We obtained the following system parameters: R_p/R_\star=0.15566+0.00011-0.00024, b=0.661+0.0053-0.0050, and a/R_\star=8.925+0.0490-0.0523 at 3.6 microns. These measurements are three times more accurate than previous studies at this wavelength because they benefit from greater observational efficiency and less statistic and systematic errors. Nonetheless, we find that the radius ratio has to be corrected for stellar activity and present a method to do so using ground-based long-duration photometric follow-up in the V-band. The resulting planet-to-star radius ratio corrected for the stellar variability is in agreement with the previous measurement obtained in the same bandpass (Desert et al. 2009). We also discuss that water vapour could not be evidenced by comparison of the planetary radius measured at 3.6 and 5.8 microns, because the radius measured at 3.6 microns is affected by absorption by other species, possibly Rayleigh scattering by haze., Comment: 19 pages, 13 figures, accepted for publication in Astronomy & Astrophysics

For a better understanding of the characteristics of blood flow in the pulmonary artery, we constructed three-dimensional images of velocity profiles of blood flow in the pulmonary artery from pulsed Doppler ultrasound recordings in 14 lambs aged 28-40 days. In 8 lambs, pulmonary hypertension was created by the central venous injection of monocrotaline pyrrole. Six lambs served as unaltered controls. The velocity data were sampled in 2 mm increments along both an anterior-posterior axis and a right-left orthogonal axis in the main pulmonary artery. Using a computer-generated cross-sectional velocity matrix consisting of 0.25 mm square grids, the velocity of blood flow was estimated at each intersection. The cross-sectional velocity matrices were generated at 5 msec intervals during the entire cardiac cycle. In all animals, significant velocity reversal was detected near the posterior wall. In 7 of 14 animals, the peak forward velocity was located near the posterior wall. Three of 8 hypertensive models showed reacceleration during the mid-systolic phase at the center of the velocity waveform, but one reacceleration disappeared at a point only 2 mm away from the center of the vessel toward the posterior wall. Acceleration time correlated well with the mean pulmonary arterial pressure (PAP) (r = -0.85) and the log10 PAP (r = -0.86). Corrected acceleration time (acceleration time divided by the square root of the cardiac cycle length) also correlated with PAP (r = -0.78) and the log10 PAP (r = -0.81).

We present Hubble Space Telescope near-infrared transit photometry of the nearby hot-Jupiter HD189733b. The observations were taken with the NICMOS instrument during five transits, with three transits executed with a narrowband filter at 1.87 microns and two performed with a narrowband filter at 1.66 microns. Our observing strategy using narrowband filters is insensitive to the usual HST intra-orbit and orbit-to-orbit measurement of systematic errors, allowing us to accurately and robustly measure the near-IR wavelength dependance of the planetary radius. Our measurements fail to reproduce the Swain et al. absorption signature of atmospheric water below 2 microns at a 5-sigma confidence level. We measure a planet-to-star radius contrast of 0.15498+/-0.00035 at 1.66 microns and a contrast of 0.15517+/-0.00019 at 1.87 microns. Both of our near-IR planetary radii values are in excellent agreement with the levels expected from Rayleigh scattering by sub-micron haze particles, observed at optical wavelengths, indicating that upper-atmospheric haze still dominates the near-IR transmission spectra over the absorption from gaseous molecular species at least below 2 microns., 9 pages, 7 figures. Accepted for publication in A&A

This study aimed to determine whether the relatively slow growth of wild Pagrus auratus in south‐eastern Australia can be increased in captivity to a rate acceptable for aquaculture. Juvenile snapper from Port Hacking, New South Wales (34°47'S) were reared at ambient water temperatures. The fish were fed on a dry, sinking pellet with 42% protein. At the start of the trial in April 1989, the snapper had a mean fork length (FL) of 121 + 11 mm SD, an average weight of 50 g, and an estimated age of 8 months. After 12.5 months their mean FL was 249 ± 15 mm and their mean weight was 403 ± 70 g. Our data indicate that, like the reproductively isolated population in Japan, growth of Pagrus auratus from Australasia can be rapid enough for aquaculture, and that there is potential to increase growth rate further.

METHODS The nature of the velocity profiles in the main pulmonary artery was examined in two dimensions using growing lambs. Lambs in two age groups--2 weeks and 4 weeks were selected for study. Using an intraluminal 20 MHz pulsed Doppler probe, pulmonary blood velocity waveforms were recorded at 2 mm intervals along two axes: the anteriorposterior axis (AP) and the right-left axis (RL). Instantaneous velocity profiles were computed throughout the cardiac cycle and the characteristics of the profiles examined. Results obtained along the anterior-posterior axis were consistent with findings previously obtained; marked negative velocity along the posterior wall was observed. However, unlike the findings in previous studies, negative velocities of lesser magnitude were evident near the left wall of the right-left axis.

The relationship between wave reflections and ventricular/vascular coupling of lambs with nmal pulmonary pressures (CONT) and pulmonary hypertension (PH) was examined. We compared reflection indexes quantitating changes in magnitude and timing of the positive reflected pressure wave. Results indicate that the reflected wave returns earlier in the PH group compared to the CONT goup (0.39 sec vs 0.62 sec; pd.005). In contrast to the CONT group, in the PH group the duration of the reflected wave is longer in systole (0.61 sec vs 0.38 sec) but shorter in diastole (0.26 sec vs 0.64 sec) (~~0.005). using a frequency domain averaging technique described previously [l]. Forward and reverse pressure and flow waveforms were calculated using the method described by Westerhof et al[21, based on characteristic impedance (2). Zc estimates were obtained by dividing the slope of the upstroke of the pressure wave at max (dPAP/dt) by the slope of the flow waveform at max (dPAQ/dt) [ 11. A global reflection coefficient (REF) was calculated as the ratio of the amplitude of reflected pressure wave to the amplitude of forward pressure wave. Wave reflection indexes quantitating changes in the timing of the positive reflected wave included the following ratios: the onset of the reflected wave/systolic interval (RBT); the duration of the reflected wave during systole/systolic interval (RST); and the duration of the reflected wave during diastole/diastolic interval (RDT).

A six-element lumped parameter model of the pulmonary circulation was used to evaluate two signal-averaging techniques for calculating the pulmonary input impedance spectra of normal lambs. Pulmonary artery pressure and pulmonary artery flow data obtained simultaneously in the main pulmonary artery were subjected to time-domain averaging and frequency-domain averaging techniques. Input impedance was determined by a cross-power spectral method designed to retain the periodicity of the signals. Preliminary studies indicate that the impedance spectra determined from noise-free input flow data to the model closely approximated the model-derived impedance spectra for a wide range of heart rates. The addition of noise signals to the noise-free input data produced impedance spectra that were consistently in agreement with model spectra for the lower-order (1-3) harmonics but not for the higher-order terms. >

The effects of dopamine on pulmonary and systematic vascular beds were investigated in 8 anesthetized goats (mean age 5+or-1 weeks). Pulmonary artery, aortic, left atrial, and central venous pressures and pulmonary and aortic flows were recorded simultaneously during a 10-minute baseline period and while infusion dopamine at 5, 10, 20, 40 160, and 320 mu g/kg/min. Pulmonary vascular resistance increased significantly at the 20 and 40 mu /kg/min infusion rates, while systemic vascular resistance decreased significantly at these rates. Characteristic impedances indicate generally increased trends. The pulmonary global reflection index indicates increased impedance mismatch at the high infusion rates, while the opposite is true for the systemic reflection index. Right heart work and the energy costs of transporting 1 cm/sup 3/ blood exceed systemic work and energy costs at the high rates of increase the resting tone of the pulmonary vascular bed, while the effect on systemic vascular tone remains unclear. The finding that the work and energy requirements of the heart are substantially increased at the higher infusion rates could affect the therapeutic value of dopamine use at these rates. >

Pulmonary input impedance spectra were estimated in one-month-old lambs whose circulation had been altered during the first few days of life to mimic the pulmonary. hemodynamic states observed in infants and children with left-to-right shunts (high flow) and /or pulmonary vascular obstructive disease (high pressure). Spectral results obtained from the animal models were compared with those obtained from a computer simulation based on morphometric and hemorheologic data compiled for the 4 kg cat. Spectral features examined included the frequency of the first modulus minimum (indicative of the pulse wave reflection and/or pulse wave velocity) and characteristic impedance (average resistance to pulsatile flow). High flow (shunt-open/shunt-closed ratio>2.1) resulted in a slight spectral shift to the right with little change in characteristic impedance in both the lamb and the passive computer simulation models. High pressure (mean pulmonary artery pressure >28 mmHg) in the lamb model resulted in a marked shift to the right with a doubling of characteristic impedance. >

Knowledge of right ventricular (RV) shape is important to the understanding of RV mechanical function and for the improvement of clinically important RV volume estimation techniques. Refinements to the simplest conceptions of RV shape are presented statistically here, based on a quantitative analysis of three-dimensional magnetic resonance (MR) images of excised lamb hearts.The passive shape of the heart in six freshly excised lamb hearts was studied with MR imaging with independent passive pressurization of both ventricles. Global features of shape were assessed, including measurement of short-axis, cross-sectional shape parameters associated with the pinched-arc model.The slice-area x apex-base length was found to be highly correlated with the volume of the RV, with little sensitivity to the degree of filling of the ventricle or to the exact slice chosen (r = 0.987; n = 22 from five hearts). The RV was shown to follow a clockwise helical path around the left ventricle of 47 +/- 17 degrees, below the outflow tract, as seen from the apical view, progressing from the apex to the base. Based on the pinched-arc model, the anterior arc is shallower than the posterior arc, with a larger radius of curvature and a smaller angle between the arc and the septal axis. As the RV is passively filled, opposite changes in shape occur between the anterior and posterior regions tending to equalize their shapes.A high degree of regularity of shape does exist in the RV and, thus, can be characterized effectively in terms of a representative cross-sectional shape and in terms of the changes in that shape proceeding from the base to the apex.

We have determined the visual orbit for the spectroscopic binary iota~Pegasi with interferometric visibility data obtained by the Palomar Testbed Interferometer in 1997. iota~Pegasi is a double-lined binary system whose minimum masses and spectral typing suggests the possibility of eclipses. Our orbital and component diameter determinations do not favor the eclipse hypothesis: the limb-to-limb separation of the two components is 0.151 +/- 0.069 mas at conjunction. Our conclusion that the iota~Peg system does not eclipse is supported by high-precision photometric observations. The physical parameters implied by our visual orbit and the spectroscopic orbit of Fekel and Tomkin (1983) are in good agreement with those inferred by other means. In particular, the orbital parallax of the system is determined to be 86.9 +/- 1.0 mas, and masses of the two components are determined to be 1.326 +/- 0.016 M_sun and 0.819 +/- 0.009 M_sun respectively., Comment: ApJ in press. 23 pages, 4 figures & 3-page data table

The effects of pulsatile hemodynamics on right ventricle-pulmonary circulation interactions were studied in control lambs and in two lamb models of altered pulmonary hemodynamics induced at infancy: elevated pulmonary arterial pressure (PAP) was created by the infusion of monocrotaline pyrrole (MCTP), and elevated pulmonary arterial blood flow was obtained by the creation of an arteriovenous fistula (Shunt). High-fidelity PAP, midvessel Doppler blood velocity (PAV), and cardiac output (CO) were measured in open-chest, anesthetized lambs. PAV waveforms were normalized to match the measured CO. Measured pressure and flow signals were separated in the time domain into forward and backward components. Pulmonary input impedance and indexes quantifying the timing of the reflected wave pulse (beginning of reflected pulse, duration of reflected pulse in systole, and duration of reflected wave in diastole) were calculated for each group. Results indicate that in control animals the reflected wave returned late in systole and extended through much of diastole, thereby increasing diastolic pressure like a counterpulsation balloon. No significant differences in the timing indexes were found between Shunt and control animals. In the MCTP group, the reflected wave returned significantly earlier than normal with the peak reflected pulse occurring before valve closure. The resulting augmentation of systolic pressure and, therefore, large pulse pressure is consistent with pressure waveforms observed in clinical pulmonary hypertension. We conclude that early wave reflection exerts a detrimental effect in pulmonary hypertension by unfavorably loading the still-ejecting right ventricle.

In vitro pulsatile flow visualization studies were conducted to assess the effects of varying radii of curvature of the right ventricular outflow tract (RVOT) and main pulmonary artery (MPA) on the flow fields in the main, right, and left pulmonary arteries of a one month lamb pulmonary artery model. Three glass flow-through models were studied; one with no curvature, one with the correct anatomic curvature, and one with an overaccentuated curvature on the RVOT and MPA. All other geometric parameters were held constant. Pulsatile flow visualization studies were conducted at nine flow conditions; heart rates of 70, 100, and 140 bpm, and cardiac outputs of 1.5, 2.5 and 3.5 l/min with corresponding mean pulmonary pressures of 10, 20, and 30 mmHg. Changes were observed in the pulmonary flow fields as the curvature of the outflow tract, heart rate and mean pulmonary pressure were varied. An increase in vessel curvature led to an increase in the overall radial nature of the flow field as well as flow separation regions which formed faster, originated further downstream, and occupied more of the vessel area. At higher heart rates, the maximum size of the separation regions decreased, while flow separation regions appeared earlier in the cardiac cycle and grew more quickly. Heart rate also affected the initiation of flow reversal; flow reversal occurred later in the cardiac cycle at lower heart rates. Both heart rate and mean pulmonary pressure influenced the stability of the pulmonary flow field and the appearance of coherent structures. In addition, an increase in mean pulmonary pressure increased the magnitude of reverse flow. These flow visualization observations have directed more quantitative studies such as pulsed Doppler ultrasound and laser Doppler anemometry velocity measurements.

We have surveyed four years of archival UBV photometry of 69 chromospherically active stars obtained with the Phoenix-10 automatic photoelectric telescope in search of optical flares on these stars. We demonstrate taht, while flares can be detected in these data, the number of events observed on evolved stars remains very small. Flares were found only on UX Arietis, II Pegasi, and AR Piscium.

We have determined spectroscopic orbits for three chromospherically active giants that have hot compact companions. They are HD 160538 (K0 III + wd, P = 904 days), HD 165141 (G8 III + wd, P approximately 5200 days), and HD 185510 (K0 III + sdB, P = 20.6619 days). By fitting an IUE spectrum with theoretical models, we find the white dwarf companion of HD 165141 has a temperature of about 35000 K. Spectral types and rotational velocities have been determined for the three giants and distances have been estimated. These three systems and 39 Ceti are compared with the barium star mass-transfer scenario. The long-period mild barium giant HD 165141 as well as HD 185510 and 39 Ceti, which have relatively short periods and normal abundance giants, appear to be consistent with this scenario. The last binary, HD 160538, a system with apparently near solar abundances, a white dwarf companion, and orbital characteristics similar to many barium stars, demonstrates that the existence of a white-dwarf companion is insufficient to produce a barium star. The paucity of systems with confirmed white-dwarf companions makes abundance analyses of HD 160538 and HD 165141 of great value in examining the role of metallicity in barium star formation.

In April 1989, young-of-the-year snapper (Pagrus auratus) were captured from the wild and injected with tetracycline. The fish were reared on natural food in a large pool with flowing sea water under ambient marine conditions. Two fish were removed every two months for two years, and the growth of their otoliths, relative to the tetracycline mark, was measured. Growth of the otoliths was greatest in spring and summer and least during winter. Opaque marks appeared in the otoliths of fish during both winters of the study. Our results confirm that the opaque marks in otoliths of young snapper can be used to determine the age of the fish in years.

The analysis and results of an occultation of the spectroscopic binary star 1 Vulpeculae by the asteroid (2) Pallas, observed from 130 locations, are presented. Combination of solutions from this and previous occultations shows the triaxial shape of Pallas to be elongated, but not severely, with the ratio of the largest to the smallest axes being less than 1.15. The data provide a separation and a position angle of the secondary component of 1 Vulpeculae and indicate that the star's actual parallax is probably near 0.008 arcsec, half of the published value. The analysis gives a calibration of the accuracy and the reaction time corrections for visual observations of asteroidal occultations. The absence of any confirmed secondary extinctions shows that any satellites of Pallas must be rare or small. The photometric observations seem to rule out a substantial cloud of dust surrounding Pallas postulated previously.

The velocity profile of the main pulmonary artery was determined in nine adult, open-chested, mechanically ventilated mongrel dogs using an intraluminal, needle-mounted, range-gated, pulsed Doppler technique. Mean phasic point velocities were determined at 2 mm intervals across the lumen of the vessel, 2 cm above the pulmonary valve, by recording the Doppler shift of an activated 20 MHz piezoelectric crystal, range-gated 3.5 mm in the direction of the pulmonary valve. Mean Reynolds numbers from the main pulmonary artery ranged from 275 to 1140. Radially normalised intraluminal distance versus mean phasic point velocity plots were constructed which demonstrated a curved profile in all 9 dogs. First order regression analysis demonstrated a poor fit (r: 0.05-0.68). Second order (r:0.61-0.97) and third order (r:0.72-0.99) regression analyses markedly improved the fit, confirming the non-linear nature of the velocity profile. Step-wise third order regression analysis to determine the importance of the entry sequence demonstrated that the most important term for determining the regression coefficient was the X2 term in six dogs. In addition, the velocity profile was noted to be shifted, with the highest velocities recorded between the centre of the vessel and the anterior wall in eight of nine dogs (location of highest velocity: +0.26 radius +/- 0.25 (mean +/- SD).

The velocity profile in the ascending aorta, which has been variously reported as parabolic, skewed or flat, was measured using an intraluminal probe equipped with a miniature piezoelectric crystal activated by a 20 MHz pulsed Doppler with a 1 mm3 sample volume size. Phasic velocities, determined via spectral analyses, were obtained at 2 mm intervals across the aortic lumen of anaesthetised open-chest dogs by sequentially moving the crystal between posterior and anterior walls, maintaining the ultrasound beam parallel to the flow axis. Range-gating allowed data acquisition 3.5 mm proximal to the crystal, thus eliminating probe induced turbulence. Time and spatial distributions of velocities over the cross-section were computed. Expected errors in vessel mean velocity estimates based on point measurements were calculated. Analysis of phasic waveforms showed increased posterior velocities during systole but third order regression analysis of normalised point mean velocities across the lumen showed the best fit was a statistically flat straight line. Centreline referenced analyses indicated the expected difference between point mean velocity and vessel mean velocity was maximal (19.3 +/- 10.1%) 4 mm toward the posterior wall and minimal (4.7 +/- 9.1%) 5 mm toward the anterior wall. Anterior posterior wall referenced analyses indicated the most reliable position for estimating vessel mean velocity from point mean velocity along this axis was 5 mm from the anterior wall.

A new method has been developed that permits constant postoperative monitoring of mean and phasic cardiac output in patients after correction of congenital heart defects. A miniature ultrasound probe is attached to the adventitia of the ascending aorta at the conclusion of the operative procedure. This is connected to the monitoring equipment by means of polyurethane-covered wires that exit the chest wall through a small stab wound. The probe can easily be removed by gentle traction when the patient’s condition is stable. The technique was developed, validated, and refined in extensive animal studies, and this report describes the first series of 20 consecutive human implants, performed between August 1984 and September 1985, in which the absolute cardiac output determination obtained with the ultrasound probe at the time of its application was correlated with cardiac output as measured with a standard electromagnetic flow probe. Fourteen male and six female patients (mean age 5.5 years) were studied. Operations performed included eight atrial septal defect repairs, four procedures for tetralogy of Fallot, three ventricular septal defect repairs, three stenotic valve corrections, and two Senning operations. One operative death occurred, but no complications were related to probe application or removal. The average cardiac output in the 20 patients as measured with the ultrasound probe was 2.2 ± 1.1 L/min (range 0.67 to 5.27 L/min). This is nearly identical to the results noted with the electromagnetic flow probe, where the mean cardiac output was 2.3 ± 1.2 L/min (range 0.7 to 6 L/min). Regression analysis revealed a high linear correlation (r = 0.9) between the two techniques. A monitor can display the cardiac output trend with 1 minute updates, which greatly enhance management of intravenous drug therapy and volume administration. In conclusion, this new extraluminal removable probe allows virtually continuous monitoring of the postoperative cardiac output after correction of congenital heart defects and should become a standard technique in the postoperative care of these patients.

To test the sensitivity and accuracy of pulsed Doppler ultrasonography to detect and quantitate left to right aortopulmonary shunt flow, an arterial allograft aortopulmonary anastomosis was constructed in nine adult mongrel dogs. Cardiac output and allograft flow were measured as the diameter of the allograft was varied. Piezoelectric crystals attached to the carotid artery and proximal descending aorta were energized with 20 MHz pulsed Doppler signals. Negative Doppler shift and negative Doppler shift/positive Doppler shift were calculated for seven dogs. All dogs exhibited negative Doppler shift in the carotid artery at zero allograft flow; five of the seven dogs exhibited a similar pattern in the descending aorta. Increasing negative Doppler shift was measured in all dogs from both sites as the allograft flow increased. Excellent linear correlation existed between allograft flow and negative Doppler shift and negative Doppler shift/positive Doppler shift for each dog from both sampling sites. However, marked interanimal variation in the slopes of the linear regression lines existed, making the composite linear correlation very poor. Detection of small left to right aortopulmonary shunting and single measurements to quantitate accurately left to right aortopulmonary shunting introduce errors due to intersubject variation. However, these results suggest that serial ultrasound measurements made over a short time can accurately predict changes in left to right aortopulmonary shunting.

A new method has been developed that permits constant postoperative monitoring of mean and phasic cardiac output in patients after correction of congenital heart defects. A miniature ultrasound probe is attached to the adventitia of the ascending aorta at the conclusion of the operative procedure. This is connected to the monitoring equipment by means of polyurethane-covered wires that exit the chest wall through a small stab wound. The probe can easily be removed by gentle traction when the patient's condition is stable. The technique was developed, validated, and refined in extensive animal studies, and this report describes the first series of 20 consecutive human implants, performed between August 1984 and September 1985, in which the absolute cardiac output determination obtained with the ultrasound probe at the time of its application was correlated with cardiac output as measured with a standard electromagnetic flow probe. Fourteen male and six female patients (mean age 5.5 years) were studied. Operations performed included eight atrial septal defect repairs, four procedures for tetralogy of Fallot, three ventricular septal defect repairs, three stenotic valve corrections, and two Senning operations. One operative death occurred, but no complications were related to probe application or removal. The average cardiac output in the 20 patients as measured with the ultrasound probe was 2.2 +/- 1.1 L/min (range 0.67 to 5.27 L/min). This is nearly identical to the results noted with the electromagnetic flow probe, where the mean cardiac output was 2.3 +/- 1.2 L/min (range 0.7 to 6 L/min). Regression analysis revealed a high linear correlation (r = 0.9) between the two techniques. A monitor can display the cardiac output trend with 1 minute updates, which greatly enhance management of intravenous drug therapy and volume administration. In conclusion, this new extraluminal removable probe allows virtually continuous monitoring of the postoperative cardiac output after correction of congenital heart defects and should become a standard technique in the postoperative care of these patients.

Relationships between pulmonary artery blood velocity patterns and elevated pulmonary artery pressure and resistance were studied in an animal model of chronic pulmonary hypertension. Monocrotaline pyrrole was injected into the right atria of 1-3-day-old lambs. The animals were subjected to an acute terminal study 4-6 weeks postinjection. Using an intraluminal 20-MHz pulsed Doppler probe, pulmonary blood velocity was measured at 2-mm intervals across the posterior-anterior axis, from which 2-D instantaneous velocity profiles were reconstructed and the characteristics of the waveforms examined. Preliminary computations indicate that the significant increase in pulmonary blood-flow reversal observed near the posterior wall in normal lambs with acute pulmonary hypertension created by hypoxia is not always present in animals with chronic pulmonary hypertension. However, the triangular shape of the waveform associated with pulmonary hypertension is apparent in all studies, and the maximum value of the ratio of reverse flow to forward flow calculated by sampling site correlated significantly with both pulmonary artery pressure and pulmonary vascular resistance. >

Lidocaine is a drug with local anesthetic and antiarrhythmic properties. An inverse relationship is recognized to exist between arterial lidocaine serum levels and cardiac index or liver function [1, 2]. However, the lungs rapidly sequester a significant portion of a lidocaine dose as the drug passes from the right side of the heart into the pulmonary circulation [3]; therefore, a reduction in effective pulmonary blood flow would be expected to raise serum lidocaine concentrations. Hence, patients with congenital heart disease (especially neonates [4]) who have right-to-left intracardiac shunting would potentially be at risk for developing toxic serum lidocaine levels at a lower dose. To test this hypothesis, an animal model of a right-to-left intracardiac shunt was developed to determine the effect of such shunting on lidocaine pharmacokinetics.

The feasibility of measuring pulmonary blood flow (PAQ) continuously using a removable, extraluminal 20 MHz pulsed Doppler probe, which has been used successfully to measure aortic blood flow, was assessed in seven anesthetized mongrel dogs. Simultaneous recordings were made from the Doppler probe (range-gated 5-6 mm from the anterior wall of the main pulmonary artery) and an electromagnetic flow probe (encircling the aorta) over cardiac outputs (CO) ranging from 0.2 to 5.5 L/min. Assuming a flat velocity profile and a fixed cross-sectional area, PAQ was initially calculated as the product of area and mean velocity. Regression analyses (PAQ = a + b X CO) indicated good intraanimal linear correlations in six animals (r greater than or equal to 0.84) and no correlation in one animal (r = 0.003); however, PAQ was consistently higher than CO and interanimal variability was marked, as suggested by large deviations in mean intercept and slope values (a = 1.67 +/- 1.09 L/min and b = 0.70 +/- 0.33). Results improved (r greater than or equal to 0.79 in all animals, a = 0.47 +/- 0.52 L/min, and b = 0.77 +/- 0.21) when the method to estimate PAQ was altered to assume that the starting cross-sectional area was the area that would make baseline PAQ and CO agree, and that the area during each subsequent CO level changed as a function of pulmonary artery pressure and an estimate of pulmonary artery compliance. Results of this study imply that it will be more difficult to use this Doppler probe to monitor CO from the pulmonary artery than it was from the aorta due to the elliptical, more compliant pulmonary vessel walls and the irregular pulmonary artery velocity profile.

Using data obtained intraoperatively from 134 patients (262 data sets), ten algorithms for estimating aortic characteristic impedance from the relative slopes of the aortic pressure and flow (electromagnetic flow probe) waveforms during early systole were compared to the estimate obtained by averaging input impedance modulus values for frequencies between 2 and 16 Hz (Zc). Results clearly confirmed the relationship between these slopes and Zc:r>or=0.80, y intercepts approximately=0.0 and slopes approximately=1.0 for all algorithms tested. However, four algorithms yielded estimates with r >or=0.95. The common trait of these four algorithms was their dependence on portions of the pressure and flow waveforms independently centered around peak derivatives. Results imply that Zc can be estimated successfully in real time, which would be advantageous in critical postoperative periods. Furthermore, cumbersome computational procedures can be eliminated whenever Zc is the only spectral-related parameter to be calculated. >

Ultrasonic measurement of blood flow within the main pulmonary artery (MPA) requires a precise knowledge of the mean blood velocity within this vessel and the cross-sectional area (CSA). Small conformational changes in the elliptical shape of the MPA have substantial effects on the calculation of CSA and, subsequently, flow. We examined the extent of these changes by measuring the pulsatile and mean elliptical dimensions of the MPA in nine anaesthetised, open-chested, mechanically ventilated mongrel dogs using two pairs of 10 MHz ultrasonic, piezoelectric crystals. These custom-made devices were sutured to the PA adventitia along the long and short cross-sectional axes 2 cm distal to the pulmonary valve. Axial dimensions were collected during normal, elevated (via noradrenaline and fluid additions) and reduced (via exsanguination) PA pressures. We confirmed the linear pressure/diameter response in 15/18 axial data sets (r greater than 0.80). Further, the linear axial responses of the long and short diameters were parallel (7/9, p less than 0.05) and have different zero-pressure intercepts (7/9, p less than 0.0001). A mathematical consequence of this parallelism is predictable, although non-constant, eccentricity. Finally, error analysis of multi-axial measurement techniques were shown to improve CSA accuracy by as much as 50% when compared with uni-axial determinations.

This article describes the application and limitations of noninvasive techniques to assess cardiac function and to diagnose pulmonary hypertension in newborn infants in whom PPHN is suspected.

Two infants with cerebral arteriovenous malformation (CAVM), both initially seen with persistent fetal circulation, were studied with cross-sectional echo. The descending aorta, which is dilated in infants with CAVM, was identified in the subxiphoid four-chamber and short-axis views in both infants. In both infants the arteriovenous malformation was readily identified by cross-sectional echo as a lucency within the brain. Pulsation of the cranial lucency was noted in one infant, but only still frames from the head echo were preserved in the other infant, and pulsation was not commented on in that case.

We interviewed 57 parents of 33 children who died of congenital heart disease to obtain their descriptions and perceptions of their own grief. Irrespective of the child's age or length of illness, the parents consistently described a grief reaction characterized by an initial period of shock lasting hours to several weeks which evolved into a four- to six-month period of sadness/depression with somatic complaints, which slowly progressed to resolution through acceptance. No parent described symptoms of pathologic grief. Only four of 33 surviving siblings demonstrated recognizable problems at the time of follow-up. There was physician follow-up of 15 families; only two families received follow-up from local physicians, even though nine children died at home or in community hospitals. All parents expected follow-up and accepted it when offered. Specific follow-up recommendations are made.

Pulmonary artery blood flow velocity was measured in 15 dogs by a recently developed direct intraluminal pulsed Doppler technique. Changes in velocity characteristics under conditions of experimentally induced hypoxic pulmonary hypertension were observed. Experimental conditions (fractional inspired oxygen concentration = 0.10) produced significant increases in mean pulmonary artery pressure and pulmonary vascular resistance. Overall and maximal negative velocity increased with pulmonary hypertension. Negative velocity occurred predominantly in the posterior half of the pulmonary artery during both control and experimental conditions. With pulmonary hypertension, diastolic negative velocity increased only in the posterior half of the pulmonary artery and systolic negative velocity decreased only in the anterior half. More basic knowledge of pulmonary artery blood flow characteristics may facilitate an informed approach to noninvasive detection of pulmonary hypertension. Direct measurements by this recently developed intraluminal technique will be useful in studying various conditions with altered pulmonary blood flow.