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THE MAIN COMPONENT OF A REDUCIBLE HILBERT CURVE OF CONIC FIBRATIONS
Fania, Maria Lucia,Lanteri, Antonio Korean Mathematical Society 2021 대한수학회지 Vol.58 No.5
The study of reducible Hilbert curves of conic fibrations over a smooth surface is carried on in this paper and the question of when the main component is itself the Hilbert curve of some ℚ-polarized surface is dealt with. Special attention is paid to the polynomial defining the canonical equation of the Hilbert curve.
Glen Gejerman,Patrick Ciccone,Martin Goldstein,Vincent Lanteri,Burton Schlecker,John Sanzone,Michael Esposito,Sergey Rome,Michael Ciccone,Eric Margolis,Robert Simon,Yijun Guo,Sri-Ram Pentakota,Hossein 대한비뇨의학회 2017 Investigative and Clinical Urology Vol.58 No.6
Purpose: To evaluate the impact that the 2012 US Preventive Services Task Force (USPSTF) prostate-specific antigen (PSA) screening guidelines have had on the diagnosis of prostate cancer, we compared the incidence and distribution of new cases diagnosed in 2011-before the USPSTF PSA screening recommendations versus 2014 at which time the guidelines were widely adopted. Materials and Methods: We identified all prostate biopsies performed by a large urology group practice utilizing a centralized pathology lab. We examined total biopsies performed, percentage of positive biopsies, and for those with positive biopsies examined for differences in patient age, PSA, and Gleason score. Results: A total of 4,178 biopsies were identified – 2,513 in 2011 and 1,665 in 2014. The percentage of positive biopsies was 27% in 2011 versus 34% in 2014 (p<0.0001). Among patients with positive biopsies, we found statistically significant differences between the 2 cohorts in the median ages and Gleason scores. Patients were about 1 year younger in 2014 compared to 2011 (t-test; p=0.043). High Gleason scores (8–10) were diagnosed in 19% of the 2014 positive biopsies versus 9% in the 2011 positive biopsies (chi square; p<0.0001). Conclusions: After the widespread implementation of the 2011 USPTF PSA screening guidelines, 34% fewer biopsies were performed with a 29% increase in positive biopsy rates. We found a significantly higher incidence of high grade disease in 2014 compared with 2011. The percentage of patients with positive biopsies having Gleason scores 8–10 more than doubled in 2014. The higher incidence of these more aggressive cancers must be part of the discussion regarding PSA screening.
Silvotti, R.,Schuh, S.,Kim, S.-L.,Lutz, R.,Reed, M.,Benatti, S.,Janulis, R.,Lanteri, L.,Østensen, R.,Marsh, T. R.,Dhillon, V. S.,Paparo, M.,Molnar, L. Springer-Verlag 2018 Astronomy and astrophysics Vol.611 No.-
<P>V391 Peg (alias HS 2201+2610) is a subdwarf B (sdB) pulsating star that shows both <I>p</I>- and <I>g</I>-modes. By studying the arrival times of the <I>p</I>-mode maxima and minima through the O-C method, in a previous article the presence of a planet was inferred with an orbital period of 3.2 years and a minimum mass of 3.2 <I>M</I>Jup. Here we present an updated O-C analysis using a larger data set of 1066 h of photometric time series (~2.5× larger in terms of the number of data points), which covers the period between 1999 and 2012 (compared with 1999-2006 of the previous analysis). Up to the end of 2008, the new O-C diagram of the main pulsation frequency (<I>f</I>1) is compatible with (and improves) the previous two-component solution representing the long-term variation of the pulsation period (parabolic component) and the giant planet (sine wave component). Since 2009, the O-C trend of <I>f</I>1 changes, and the time derivative of the pulsation period (<I>p</I><SUP>.</SUP>) passes from positive to negative; the reason of this change of regime is not clear and could be related to nonlinear interactions between different pulsation modes. With the new data, the O-C diagram of the secondary pulsation frequency (<I>f</I>2) continues to show two components (parabola and sine wave), like in the previous analysis. Various solutions are proposed to fit the O-C diagrams of <I>f</I>1 and <I>f</I>2, but in all of them, the sinusoidal components of <I>f</I>1 and <I>f</I>2 differ or at least agree less well than before. The nice agreement found previously was a coincidence due to various small effects that are carefully analyzed. Now, with a larger dataset, the presence of a planet is more uncertain and would require confirmation with an independent method. The new data allow us to improve the measurement of <I>p</I><SUP>.</SUP> for <I>f</I>1 and <I>f</I>2: using only the data up to the end of 2008, we obtain <I>p</I><SUP>.</SUP>1 = (1.34 ± 0.04) × 10<SUP>−12</SUP> and <I>p</I><SUP>.</SUP>2 = (1.62 ± 0.22) × 10<SUP>−12</SUP>. The long-term variation of the two main pulsation periods (and the change of sign of <I>p</I><SUP>.</SUP>1) is visible also in direct measurements made over several years. The absence of peaks near <I>f</I>1 in the Fourier transform and the secondary peak close to <I>f</I>2 confirm a previous identification as <I>l</I> = 0 and <I>l</I> = 1, respectively, and suggest a stellar rotation period of about 40 days. The new data allow constraining the main <I>g</I>-mode pulsation periods of the star.</P>