62 research outputs found
Hybrid Boron Nitride Nanotubes - Carbon Nanostructures Supercapacitor with High Energy Density
No abstract availabl
Estrategias y recursos noolĂłgicos en mujeres sobrevivientes al cĂĄncer de seno
El presente es un ejercicio investigativo, direccionado a comprender las estrategias y los
recursos noolĂłgicos empleados por tres mujeres sobrevivientes al cĂĄncer de mama, para
vivenciar y realizar el sentido de vida, haciendo uso de la fenomenologĂa como mĂ©todo
investigativo y el anĂĄlisis del discurso como estrategia
The effectiveness evaluation of a multimedia hepatitis C prevention program for Hispanic HIV-infected individuals
IntroductionâWith the introduction of highly active antiretroviral therapy the Hepatitis C virus
(HCV) infection has became a primary health problem among individuals suffering from HIV/
AIDS in Puerto Rico, principally those who are injecting drug users (IDUs). A multimedia
educational intervention, based on the Health Beliefs Model and Social Cognitive Theory was
developed and implemented to reduce HCV associated risk behaviors among IDUs.
MethodsâA pre- and post- intervention study evaluated the knowledge and behavioral changes
in a group of HIV-infected persons recruited from February 2006 through December 2008.
ResultsâA total of 110 participants were recruited; all were IDUs; 82% were men; 86.3% were
HIV/HCV co-infected and 24.5% had active injected drugs in the last month (prior to
recruitment). The group mean age was 42.2 ± 9.2 years and mean educational level was 10th
grade. Knowledge of HCV risk behaviors, perception of HCV susceptibility, and perception of
disease severity increased after the intervention. Knowledge of HCV clinical manifestations and
HIV co-infection complications and treatment also improved. In addition, HCV risk behaviors and
injecting drug practice decrease significantly among IDUs.
ConclusionsâThis new multimedia intervention captured and maintained the participants'
attention and interest, in that way facilitating their educational process. Thus, a greater of attention
and interest leads to greater knowledge and prevention improvement
The Creation of a Critical Care Admission Pressure Injury Prevention Cart to Reduce Hospital-Acquired Pressure Injuries
The goal of this process improvement initiative is to reduce hospital-acquired pressure injuries related to Covid-19 with Critical Care patients. Critically ill and ventilated patients require prone position therapy and prolonged ventilator times place the patient at risk for hospital acquired conditions and pressure injuries. The Critical Care team created a Critical Care Admission Pressure Injury Prevention Cart that contains preventative dressings for all pressure areas at risk.
The Critical Care Admission Pressure Injury Prevention Cart has significantly reduced the pressure injury rate. With the emergence of the pandemic and additional surges, pressure injuries continued to be on the rise due to prone position therapy. The Critical Care team worked with the system and developed prone position protocols, which included preventative dressings for all areas at risk.
Prior to the implementation of the admission cart, Critical Care ended fiscal year 2022, quarter one, with fifty-three hospital acquired pressure injuries. Last December and early January 2022 there was another surge of Covid-19. The Critical Care team implemented the admission cart in January 2022. From January 2022 through September 2022, there has been an 98% reduction. The cart has been successful for Critical Care, and Baptist Hospital implemented the cart in all high acuity areas. This cart was a multidisciplinary practice, which consists of nursing, the wound and skin team, respiratory care, and leadership working together towards the goal of patient safety and pressure injury prevention
Simultaneous infrared and optical observations of the transiting debris cloud around WD 1145+017
We present multiwavelength photometric monitoring of WD 1145+017, a white dwarf exhibiting periodic dimming events interpreted to be the transits of orbiting, disintegrating planetesimals. Our observations include the first set of near-infrared light curves for the object, obtained on multiple nights over the span of 1 month, and recorded multiple transit events with depths varying between âŒ20 and 50 per cent. Simultaneous near-infrared and optical observations of the deepest and longest duration transit event were obtained on two epochs with the Anglo-Australian Telescope and three optical facilities, over the wavelength range of 0.5â1.2ÎŒm. These observations revealed no measurable difference in transit depths for multiple photometric pass bands, allowing us to place a 2Ï lower limit of 0.8ÎŒm on the grain size in the putative transiting debris cloud. This conclusion is consistent with the spectral energy distribution of the system, which can be fit with an optically thin debris disc with minimum particle sizes of 10+5â3ÎŒm
A Search for the Transit of HD 168443b: Improved Orbital Parameters and Photometry
The discovery of transiting planets around bright stars holds the potential
to greatly enhance our understanding of planetary atmospheres. In this work we
present the search for transits of HD 168443b, a massive planet orbiting the
bright star HD 168443 V=6.92 with a period of 58.11 days. The high eccentricity
of the planetary orbit e=0.53 significantly enhances the a-priori transit
probability beyond that expected for a circular orbit, making HD 168443 a
candidate for our ongoing Transit Ephemeris Refinement and Monitoring Survey
(TERMS). Using additional radial velocities from Keck-HIRES, we refined the
orbital parameters of this multi-planet system and derived a new transit
ephemeris for HD 168443b. The reduced uncertainties in the transit window make
a photometric transit search practicable. Photometric observations acquired
during predicted transit windows were obtained on three nights. CTIO 1.0 m
photometry acquired on 2010 September 7 had the required precision to detect a
transit but fell just outside of our final transit window. Nightly photometry
from the T8 0.8 m Automated Photometric Telescope (APT) at Fairborn
Observatory, acquired over a span of 109 nights, demonstrates that HD 168443 is
constant on a time scale of weeks. Higher-cadence photometry on 2011 April 28
and June 25 shows no evidence of a transit. We are able to rule out a
non-grazing transit of HD 168443b.Comment: Accepted in ApJ. 25 pages. 8 Figure
Spitzer Reveals Evidence of Molecular Absorption in the Atmosphere of the Hot Neptune LTT 9979b
Non-rocky sub-jovian exoplanets in high irradiation environments are rare.
LTT 9979b, also known as TESS Object of Interest (TOI) 193.01, is one of the
few such planets discovered to date, and the first example of an ultra-hot
Neptune. The planet's bulk density indicates that it has a substantial
atmosphere, so to investigate its atmospheric composition and shed further
light on its origin, we obtained {\it Spitzer} IRAC secondary eclipse
observations of LTT 9979b at 3.6 and 4.5 m. We combined the {\it Spitzer}
observations with a measurement of the secondary eclipse in the {\it TESS}
bandpass. The resulting secondary eclipse spectrum strongly prefers a model
that includes CO absorption over a blackbody spectrum, incidentally making LTT
9979b the first {\it TESS} exoplanet (and the first ultra-hot Neptune) with
evidence of a spectral feature in its atmosphere. We did not find evidence of a
thermal inversion, at odds with expectations based on the atmospheres of
similarly-irradiated hot Jupiters. We also report a nominal dayside brightness
temperature of 2305 141 K (based on the 3.6 m secondary eclipse
measurement), and we constrained the planet's orbital eccentricity to at the 99.7 \% confidence level. Together with our analysis of LTT
9979b's thermal phase curves reported in a companion paper, our results set the
stage for similar investigations of a larger sample of exoplanets discovered in
the hot Neptune desert, investigations which are key to uncovering the origin
of this population.Comment: 12 pages, 5 figures; accepted to ApJ Letter
TOI-2196 b : Rare planet in the hot Neptune desert transiting a G-type star
Funding: C.M.P., M.F., I.G., and J.K. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18, 177/19, 2020-00104). L.M.S and D.G. gratefully acknowledge financial support from the CRT foundation under Grant No. 2018.2323 âGaseous or rocky? Unveiling the nature of small worldsâ. P.K. acknowledges support from grant LTT-20015. E.G. acknowledge the support of the ThĂŒringer Ministerium fĂŒr Wirtschaft, Wissenschaft und Digitale Gesellschaft. J.S.J. gratefully acknowledges support by FONDECYT grant 1201371 and from the ANID BASAL projects ACE210002 and FB210003. H.J.D. acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant PID2019-107061GBC66, DOI: 10.13039/501100011033. D.D. acknowledges support from the TESS Guest Investigator Program grants 80NSSC21K0108 and 80NSSC22K0185. M.E. acknowledges the support of the DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (HA 3279/12-1). K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. N.N. acknowledges support from JSPS KAKENHI Grant Number JP18H05439, JST CREST Grant Number JPMJCR1761. M.S.I.P. is funded by NSF.The hot Neptune desert is a region hosting a small number of short-period Neptunes in the radius-instellation diagram. Highly irradiated planets are usually either small (R âČ 2 Râ) and rocky or they are gas giants with radii of âł1 RJ. Here, we report on the intermediate-sized planet TOI-2196 b (TIC 372172128.01) on a 1.2 day orbit around a G-type star (V = 12.0, [Fe/H] = 0.14 dex) discovered by the Transiting Exoplanet Survey Satellite in sector 27. We collected 41 radial velocity measurements with the HARPS spectrograph to confirm the planetary nature of the transit signal and to determine the mass. The radius of TOI-2196 b is 3.51 ± 0.15 Râ, which, combined with the mass of 26.0 ± 1.3 Mâ, results in a bulk density of 3.31â0.43+0.51 g cmâ3. Hence, the radius implies that this planet is a sub-Neptune, although the density is twice than that of Neptune. A significant trend in the HARPS radial velocity measurements points to the presence of a distant companion with a lower limit on the period and mass of 220 days and 0.65 MJ, respectively, assuming zero eccentricity. The short period of planet b implies a high equilibrium temperature of 1860 ± 20 K, for zero albedo and isotropic emission. This places the planet in the hot Neptune desert, joining a group of very few planets in this parameter space discovered in recent years. These planets suggest that the hot Neptune desert may be divided in two parts for planets with equilibrium temperatures of âł1800 K: a hot sub-Neptune desert devoid of planets with radii of â 1.8â3 Râ and a sub-Jovian desert for radii of â5â12 Râ. More planets in this parameter space are needed to further investigate this finding. Planetary interior structure models of TOI-2196 b are consistent with a H/He atmosphere mass fraction between 0.4% and 3%, with a mean value of 0.7% on top of a rocky interior. We estimated the amount of mass this planet might have lost at a young age and we find that while the mass loss could have been significant, the planet had not changed in terms of character: it was born as a small volatile-rich planet and it remains one at present.Publisher PDFPeer reviewe
TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes
We report the discovery of TOI-1444b, a 1.4- super-Earth on a
0.47-day orbit around a Sun-like star discovered by {\it TESS}. Precise radial
velocities from Keck/HIRES confirmed the planet and constrained the mass to be
. The RV dataset also indicates a possible
non-transiting, 16-day planet (). We report a tentative
detection of phase curve variation and secondary eclipse of TOI-1444b in the
{\it TESS} bandpass. TOI-1444b joins the growing sample of 17
ultra-short-period planets with well-measured masses and sizes, most of which
are compatible with an Earth-like composition. We take this opportunity to
examine the expanding sample of ultra-short-period planets () and
contrast them with the newly discovered sub-day ultra-hot Neptunes
(, TOI-849 b, LTT9779 b and K2-100). We find that
1) USPs have predominately Earth-like compositions with inferred iron core mass
fractions of 0.320.04; and have masses below the threshold of runaway
accretion (), while ultra-hot Neptunes are above the threshold
and have H/He or other volatile envelope. 2) USPs are almost always found in
multi-planet system consistent with a secular interaction formation scenario;
ultra-hot Neptunes (1 day) tend to be ``lonely' similar
to longer-period hot Neptunes(1-10 days) and hot Jupiters. 3) USPs
occur around solar-metallicity stars while hot Neptunes prefer higher
metallicity hosts. 4) In all these respects, the ultra-hot Neptunes show more
resemblance to hot Jupiters than the smaller USP planets, although ultra-hot
Neptunes are rarer than both USP and hot Jupiters by 1-2 orders of magnitude.Comment: Accepted too AJ. 12 Figures, 4 table
TESS discovery of a super-Earth and two sub-Neptunes orbiting the bright, nearby, Sun-like star HD 22946
We report the Transiting Exoplanet Survey Satellite (TESS) discovery of a
three-planet system around the bright Sun-like star HD~22946(V=8.3 mag),also
known as TIC~100990000, located 63 parsecs away.The system was observed by TESS
in Sectors 3, 4, 30 and 31 and two planet candidates, labelled TESS Objects of
Interest (TOIs) 411.01 (planet ) and 411.02 (planet ), were identified on
orbits of 9.57 and 4.04 days, respectively. In this work, we validate the two
planets and recover an additional single transit-like signal in the light
curve, which suggests the presence of a third transiting planet with a longer
period of about 46 days.We assess the veracity of the TESS transit signals and
use follow-up imaging and time series photometry to rule out false positive
scenarios, including unresolved binary systems, nearby eclipsing binaries or
background/foreground stars contaminating the light curves. Parallax
measurements from Gaia EDR3, together with broad-band photometry and
spectroscopic follow-up by TFOP allowed us to constrain the stellar parameters
of TOI-411, including its radius of. Adopting this value,
we determined the radii for the three exoplanet candidates and found that
planet is a super-Earth, with a radius of , while
planet and are sub-Neptunian planets, with radii
of and respectively. By using
dynamical simulations, we assessed the stability of the system and evaluated
the possibility of the presence of other undetected, non-transiting planets by
investigating its dynamical packing. We find that the system is dynamically
stable and potentially unpacked, with enough space to host at least one more
planet between and .(Abridged)Comment: 21 pages, 12 figures. Accepted for publication on A&
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