Endometriosis of diaphragm: A case report

Endometriosis affects about 10 of women of reproductive age. Its main feature is the presence of stroma and endometrial glands in sites other than the uterus, mainly in pelvis. Pelvic peritoneum, ovaries, uterine ligaments, bladder, intestines, andcul-de-sac are among the affected areas. Sometimes endometriosis can be found outside of the pelvis and even above abdominal cavity, like indiaphragm.Herein, we present a case of an asymptomatic diaphragmatic endometriosis that was discovered incidentally during laparoscopy of pelvic endometriosis, as well as our appropriately proposed treatment protocol. © 2018, Royan Institute (ACECR). All rights reserved

Pregnancy in non-communicating rudimentary horn of a unicornuate uterus

Diagnosis and management of pre-rupture stage of the pregnant horn are difficult and usually missed on a routine ultrasound scan. Also most cases are detected after rupture of pregnant horn. We presented a 28-year-oldG2 L1 woman with diagnosis of rudimentary horn pregnancy (RHP) at 14 weeks of gestation. We diagnosed her with a normal intrauterine pregnancy, whereas a pregnancy in a right-sided non-communicating rudimentary horn with massive he-moperitoneum was later discovered on laparotomy. RHP has a high risk of death for mother, so there must be a strong clinical suspicion for the diagnosis of RHP. Although there is a major advancement in field of diagnostic ultrasound and other imaging modalities, prenatal diagnosis has remained elusive and a laparotomy surgery is considered as a definitive diagnosis. © 2017, Royan Institute (ACECR). All rights reserved

Pregnancy in non-communicating rudimentary horn of a unicornuate uterus

Diagnosis and management of pre-rupture stage of the pregnant horn are difficult and usually missed on a routine ultrasound scan. Also most cases are detected after rupture of pregnant horn. We presented a 28-year-oldG2 L1 woman with diagnosis of rudimentary horn pregnancy (RHP) at 14 weeks of gestation. We diagnosed her with a normal intrauterine pregnancy, whereas a pregnancy in a right-sided non-communicating rudimentary horn with massive he-moperitoneum was later discovered on laparotomy. RHP has a high risk of death for mother, so there must be a strong clinical suspicion for the diagnosis of RHP. Although there is a major advancement in field of diagnostic ultrasound and other imaging modalities, prenatal diagnosis has remained elusive and a laparotomy surgery is considered as a definitive diagnosis. © 2017, Royan Institute (ACECR). All rights reserved

Uterine leiomyosarcoma: A case report

Introduction: Uterine leiomyosarcoma (LMS) is a rare cancer originated from smooth muscle lining the walls of the uterus. LMS is known as an aggressive tumor with high mortality and morbidity rates as compared to other uterine cancers, despite the disease stage at the time of diagnosis. In most cases, LMS has been misdiagnosed as a benign uterine leiomyoma following hysterectomy or myomectomy. Case Presentation: We presented a 53-year-old G7 L7 woman who had referred to GYN clinic in Amir-al-Momenin hospital for abnormal uterine bleeding (AUB) for 6 months. On physical examination, we found an abdominal mass that had grown rapidly in the last 4 months. The computed tomography (CT) scan results showed a heterogeneous mass extending from the epigastric region to the pelvic area. Following an exploratory laparotomy, histopathology report confirmed the diagnosis of LMS. Her uterus, Fallopian tubes and ovaries were removed during a surgery, and she was referred to a gynecologic oncologist for possible chemotherapy. Conclusion: We found that the surgery is the only treatment for LMS; however, there is a little possibility to diagnose LMS before surgery in the patient with uncertain diagnosis and suspicious of LMS. Analysis of LDH and LDH3 levels along with dynamic diethylenetriaminepentaacetic acid (Gd-DTPA) enhanced, and MRI are recommended. © 2018 The Author (s)

The CARMENES search for exoplanets around M dwarfs: Radial-velocity variations of active stars in visual-channel spectra

Previous simulations predicted the activity-induced radial-velocity (RV) variations of M dwarfs to range from $\sim1$ cm/s to $\sim1$ km/s, depending on various stellar and activity parameters. We investigate the observed relations between RVs, stellar activity, and stellar parameters of M dwarfs by analyzing CARMENES high-resolution visual-channel spectra ($0.5$$-$$1$$\mu$m), which were taken within the CARMENES RV planet survey during its first $20$ months of operation. During this time, $287$ of the CARMENES-sample stars were observed at least five times. From each spectrum we derived a relative RV and a measure of chromospheric H$\alpha$ emission. In addition, we estimated the chromatic index (CRX) of each spectrum, which is a measure of the RV wavelength dependence. Despite having a median number of only $11$ measurements per star, we show that the RV variations of the stars with RV scatter of $>10$ m/s and a projected rotation velocity $v \sin{i}>2$ km/s are caused mainly by activity. We name these stars `active RV-loud stars' and find their occurrence to increase with spectral type: from $\sim3\%$ for early-type M dwarfs (M$0.0$$-$$2.5$V) through $\sim30\%$ for mid-type M dwarfs (M$3.0$$-$$5.5$V) to $>50\%$ for late-type M dwarfs (M$6.0$$-$$9.0$V). Their RV-scatter amplitude is found to be correlated mainly with $v \sin{i}$. For about half of the stars, we also find a linear RV$-$CRX anticorrelation, which indicates that their activity-induced RV scatter is lower at longer wavelengths. For most of them we can exclude a linear correlation between RV and H$\alpha$ emission. Our results are in agreement with simulated activity-induced RV variations in M dwarfs. The RV variations of most active RV-loud M dwarfs are likely to be caused by dark spots on their surfaces, which move in and out of view as the stars rotate.Comment: A&A accepte

High-precision broad-band linear polarimetry of early-type binaries I. Discovery of variable, phase-locked polarization in HD48099

Aims. We investigate the structure of the O-type binary system HD48099 by measuring linear polarization that arises due to light scattering process. High-precison polarimetry provides independent estimates of the orbital parameters and gives important information on the properties of the system.Methods. Linear polarization measurements of HD48099 in the B, V and R passbands with the high-precision Dipol-2 polarimeter have been carried out. The data have been obtained with the 60 cm KVA (Observatory Roque de los Muchachos, La Palma, Spain) and T60 (Haleakala, Hawaii, USA) remotely controlled telescopes during 31 observing nights. Polarimetry in the optical wavelengths has been complemented by observations in the X-rays with the Swift space observatory.Results. Optical polarimetry revealed small intrinsic polarization in HD48099 with similar to 0.1% peak to peak variation over the orbital period of 3.08 d. The variability pattern is typical for binary systems, showing strong second harmonic of the orbital period. We apply our model code for the electron scattering in the circumstellar matter to put constraints on the system geometry. A good model fit is obtained for scattering of light on a cloud produced by the colliding stellar winds. The geometry of the cloud, with a broad distribution of scattering particles away from the orbital plane, helps in constraining the (low) orbital inclination. We derive from the polarization data the inclination i = 17 degrees +/- 2 degrees and the longitude of the ascending node Omega = 82 degrees +/- 1 degrees of the binary orbit. The available X-ray data provide additional evidence for the existence of the colliding stellar winds in the system. Another possible source of the polarized light could be scattering from the stellar photospheres. The models with circumstellar envelopes, or matter confined to the orbital plane, do not provide good constraints on the low inclination, better than i <= 27 degrees, as is already suggested by the absence of eclipses

Primary Black Hole Spin in OJ 287 as Determined by the General Relativity Centenary Flare

OJ 287 is a quasi-periodic quasar with roughly 12 year optical cycles. It displays prominent outbursts that are predictable in a binary black hole model. The model predicted a major optical outburst in 2015 December. We found that the outburst did occur within the expected time range, peaking on 2015 December 5 at magnitude 12.9 in the optical R -band. Based on Swift /XRT satellite measurements and optical polarization data, we find that it included a major thermal component. Its timing provides an accurate estimate for the spin of the primary black hole, ##IMG## [http://ej.iop.org/images/2041-8205/819/2/L37/apjl523055ieqn1.gif] $i =0.313pm 0.01$ . The present outburst also confirms the established general relativistic properties of the system such as the loss of orbital energy to gravitational radiation at the 2% accuracy level, and it opens up the possibility of testing the black hole no-hair theorem with 10% accuracy during the present decade.Peer reviewe

A Search for QPOs in the Blazar OJ287: Preliminary Results from the 2015/2016 Observing Campaign

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.Peer reviewe