Insertion of an IUD into the uterine cavity could result in an obvious increase in endometrial microcirculation blood volume. The endometrial capillary configuration is a scattered, loose, and irregular capillary network. 8-10 months after IUD insertion in the uterine cavity, remarkable hyperplasia of the capillary and enlargement of the vessel diameter were observed in the IUD area. In the IUD depressed area, the capillaries had obviously increased and come together irregularly with various vessel diameters in the form of bead strings. The diameter of the vessels around most glandular opening enlarged and the capillaries clustered together to form a spherical capillary plexus. The end of the vessel dilated like a small sphere to form a microvascular bell. The more seriously depressed capillary became thinner, atrophied, and even cracked. Then, the newborn capillary trending along the IUD appeared. (author's modified)
Conflicts of interest: none declared. Sir, Chylous reflux from the skin is usually associated with an underlying defect in the lymphatic vessels. We report an unusual case of scrotal cutaneous chylous reflux with clinically numerous vesicles over the scrotum and large amounts of milky fluid draining intermittently from these vesicles. A 17‐year‐old boy had had intermittent whitish discharge from the vesicles of the scrotum for 2–3 years. Each episode could be resolved after compression and bed rest. The size of the vesicles increased after the patient stood for a long time. There was no oedema of the bilateral lower extremities or erectile dysfunction. There was no history of surgery or trauma. His development and growth were within normal limits. Physical examination showed numerous 2–6 mm diameter whitish to yellowish vesicles confluent over the scrotum, with thickening of the scrotal skin (Fig. 1a). In addition, several 1–2 mm diameter whitish vesicles were scattered over the base of the penis and three or four whitish vesicles were grouped over the medial aspect of the upper right thigh. Large amounts of milk‐like fluid discharged intermittently from these vesicles after abrasion (Fig. 1b).
Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated signals from strong lensing by 1) performing targeted searches for subthreshold signals, 2) calculating the degree of overlap amongst the intrinsic parameters and sky location of pairs of signals, 3) comparing the similarities of the spectrograms amongst pairs of signals, and 4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by 1) frequency-independent phase shifts in strongly lensed images, and 2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the non-detection of gravitational-wave lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects.
Abstract Aiming at the problem that the strong structure-soil interaction of rigid abutment integral bridge and semi-flexible abutment integral bridge, a new integral abutment bridge with rigid-flexible abutment was proposed, and the shaking table model test was carried out to study its seismic performance. The test result shows that at the seismic fortification intensity 6, the specimen are relatively intact, and no crack was generated, which shown the integral abutment bridge with rigid-flexible combined abutment has good seismic performance. The first-order and second-order frequency of integral abutment bridge with rigid-flexible combined abutment are about 5.0 Hz and 10 Hz, respectively. The damping ratio coefficient of rigid-flexible combined abutment-pile-soil system is about 0.18~0.25. The soil-rigid-flexible combined abutment-pile interaction amplified from 10.71 times the pile diameter above the bottom of the pile foundation. The maximum dynamic amplification factor of specimen and soil are located at the abutment bottom and the soil surface, respectively.
This paper describes the first all-sky search for long-duration, quasi-monochromatic gravitational-wave signals emitted by ultralight scalar boson clouds around spinning black holes using data from the third observing run of Advanced LIGO. We analyze the frequency range from 20~Hz to 610~Hz, over a small frequency derivative range around zero, and use multiple frequency resolutions to be robust towards possible signal frequency wanderings. Outliers from this search are followed up using two different methods, one more suitable for nearly monochromatic signals, and the other more robust towards frequency fluctuations. We do not find any evidence for such signals and set upper limits on the signal strain amplitude, the most stringent being $\approx10^{-25}$ at around 130~Hz. We interpret these upper limits as both an "exclusion region" in the boson mass/black hole mass plane and the maximum detectable distance for a given boson mass, based on an assumption of the age of the black hole/boson cloud system.
We use 47 gravitational-wave sources from the Third LIGO-Virgo-KAGRA Gravitational-Wave Transient Catalog (GWTC-3) to estimate the Hubble parameter $H(z)$, including its current value, the Hubble constant $H_0$. Each gravitational-wave (GW) signal provides the luminosity distance to the source and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and $H(z)$. The source mass distribution displays a peak around $34\, {\rm M_\odot}$, followed by a drop-off. Assuming this mass scale does not evolve with redshift results in a $H(z)$ measurement, yielding $H_0=68^{+12}_{-7} {\rm km\,s^{-1}\,Mpc^{-1}}$ ($68\%$ credible interval) when combined with the $H_0$ measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the $H_0$ estimate from GWTC-1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of $H_0=68^{+8}_{-6} {\rm km\,s^{-1}\,Mpc^{-1}}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC-1 result and 20% with respect to recent $H_0$ studies using GWTC-2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about $H_0$) is the well-localized event GW190814.
is a multidisciplinary journal of oncology that aims to be a forum for facilitating collaboration and exchanging information on what is happening in different countries of the Asia-Pacifi c region in relation to cancer treatment and care.The journal is ideally positioned to receive publications that deal with diversity in cancer behavior, management and outcome related to ethnic, cultural, economic and other differences between populations.In addition to original articles, the Journal publishes reviews, editorials, letters to the Editor and short communications.Case reports are generally not considered for publication, only exceptional papers in which Editors fi nd extraordinary oncological value may be considered for review.The Journal encourages clinical studies, particularly prospectively designed clinical trials.
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