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The patient reported a persistence of epigastric pain, retrosternal pain irradiated posteriorly, nausea, and bloating. Considering the patient's history, the clinical presentation, failure of the medical therapy, and diverticulum's size, laparoscopic surgical treatment was proposed to the patient. Discussion Gastric diverticula are a rare form of diverticular disease with an incidence ranging from 0.01 to 0.11%.[1] They are classified as congenital and acquired:[1],[2] the first one typically involves all the layers and is located on the posterior wall in the area near the gastric fundus, and the second one is generally a false diverticulum and it is located in the prepyloric region. [Extracted from the article]

Context. Period variations have been detected in a number of eclipsing close compact binary subdwarf B stars (sdBs) and these have often been interpreted as being caused by circumbinary massive planets or brown dwarfs. According to canonical binary models, the majority of sdB systems are produced from low mass stars with degenerate cores where helium is ignited in flashes. Various evolutionary scenarios have been proposed for these stars, but a definite mechanism remains to be established. Equally puzzling is the formation of these putative circumbinary objects which must have formed from the remaining post-common envelope circumbinary disk or survived its evolution. Aims. In this paper we review the eclipse time variations (ETVs) exhibited by seven such systems (EC 10246-2707, HS 0705+6700, HS 2231+2441, J08205+0008, NSVS 07826147, NSVS 14256825, and NY Vir) and explore whether there is conclusive evidence that the ETVs observed over the last two decades can reliably predict the presence of one or more circumbinary bodies. Methods. We report 246 new observations of the seven sdB systems made between 2013 September and 2017 July using a worldwide network of telescopes. We combined our new data with previously published measurements to analyse the ETVs of these systems. Results. Our data show that period variations cannot be modelled simply on the basis of circumbinary objects. This implies that more complex processes may be taking place in these systems. These diffculties are compounded by the secondary star not being spectroscopically visible. From ETVs, it has historically been suggested that five of the seven binary systems reported here had circumbinary objects. Based on our recent observations and analysis, only three systems remain serious contenders.We find agreement with other observers that at least a decade of observations is required to establish reliable ephemerides. With longer observational baselines it is quite conceivable that the data will support the circumbinary object hypothesis of these binary systems. Also, we generally agree with other observers that higher values of (O,C) residuals are found with secondary companions of spectral type M5/6 (or possibly earlier as a result of an Applegate type mechanism). [ABSTRACT FROM AUTHOR]

The article reviews the transit time variations (TTVs) exhibited by HS0705 eclipsing binary system, over the last thirteen years as of 2015 and explore whether there is conclusive evidence that these TTVs can predict the presence of a third body. Topics include the HS0705 identified as an subdwarf (sdB) star and their subsequent analyses since 2001, 25 new measurements taken between late 2013 and early 2014 using Sierra Stars and iTelescope robotic telescope.

TW Coronae Borealis (TW CrB) is a binary system likely to be active, showing evidence of starspots and a hotspot. We calculated a new ephemeris based on all available timings from 1946 and find the period to be 0.58887492(2) days. We have revised the average rate of change of period down from 1.54(16)×10-7 days/yr to 6.66(14)×10-8 days/yr. Based on lightcurve simulation analysis we conclude that the two stars are close to filling their Roche lobes, or possibly that one of the stars' Roche lobe has been filled. The modelling also led to a hotspot and two starspots being identified. Conservative mass transfer is one of a number of possible mechanisms considered that could explain the change in period, but the mass transfer rate would be significantly lower than previous estimates. We found evidence that suggests the period was changing in a cyclical manner, but we do not have sufficient data to make a judgement on the mechanism causing this variation. The existence of a hotspot suggests mass transfer with a corresponding increase in the amplitude in the B band as compared with the R and V bands. The chromospheric activity implied by the starspots makes this binary system a very likely X-ray source. [ABSTRACT FROM AUTHOR]