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Isao Kanda,Roberto Basaldud,Nobuji Horikoshi,Yukiyo Okazaki,Sandy-Edith Benítez-Garcia,Abraham Ortínez,Victor Ramos Benítez,Beatriz Cárdenas,Shinji Wakamatsu 한국대기환경학회 2014 Asian Journal of Atmospheric Environment (AJAE) Vol.8 No.3
An abnormal decrease in ozonesonde sensor signaloccurred during air-pollution study campaigns in November2011 and March 2012 in Mexico City MetropolitanArea (MCMA). Sharp drops in sensor signalaround 5 km above sea level and above were observedin November 2011, and a reduction of signal overa broad range of altitude was observed in the convectiveboundary layer in March 2012. Circumstantialevidence indicated that SO2 gas interfered withthe electrochemical concentration cell (ECC) ozonesensors in the ozonesonde and that this interferencewas the cause of the reduced sensor signal output. The sharp drops in November 2011 were attributedto the SO2 plume from Popocatépetl volcano southeastof MCMA. Experiments on the response of theECC sensor to representative atmospheric tracegases showed that only SO2 could cause the observedabrupt drops in sensor signal. The vertical profileof the plume reproduced by a Lagrangian particlediffusion simulation supported this finding. A neargroundreduction in the sensor signal in March 2012was attributed to an SO2 plume from the Tula industrialcomplex north-west of MCMA. Before and atthe time of ozonesonde launch, intermittent high SO2concentrations were recorded at ground-level monitoringstations north of MCMA. The difference betweenthe O3 concentration measured by the ozonesondeand that recorded by a UV-based O3 monitorwas consistent with the SO2 concentration recordedby a UV-based monitor on the ground. The verticalprofiles of the plumes estimated by Lagrangian particlediffusion simulation agreed fairly well with theobserved profile. Statistical analysis of the wind fieldin MCMA revealed that the effect Popocatépetl wasmost likely to have occurred from June to October,whereas the effect of the industries north of MCMA,including the Tula complex, was predicted to occurthroughout the year.
<i>Euphausia pacifica</i> brood sizes: a North Pacific synthesis
Feinberg, L. R.,Shaw, C. T.,Peterson, W. T.,Dé,cima, M.,Okazaki, Y.,Ju, S.-J. Oxford University Press 2013 Journal of plankton research Vol.35 No.6
<P><I>Euphausia pacifica</I> occupy a remarkably wide range of ecosystems. We examined the differences in brood sizes from eight regions of the North Pacific to explore how variation in the brood size might contribute to their success over such a range. We show a compilation and analysis of short-term <I>E. pacifica</I> brood size incubations from around the North Pacific rim, ranging from the Yellow Sea (YS) (Korea) to southern California (SC), USA. Brood sizes for <I>E. pacifica</I> are highly variable in all regions and range from 5 to 697 eggs overall. Median brood sizes were largest in the YS and off Newport, Oregon and the maximum brood sizes were greatest in the regions off the coasts of Oregon and Washington, USA followed by the YS. Quantile regression analysis revealed that there was a significant relationship between the female length and the maximum brood size (95% quantile) for broods from SC, Oregon, and Washington, USA as well as Toyama Bay, Japan, indicating that the maximum brood size is limited by the female length in these regions. This suggests that other factors, hydrographic conditions, food quantity/quality or physiological condition of females, may limit maximum brood sizes in the other regions examined here.</P>
Tam, P. H. T.,Li, K. L.,Takata, J.,Okazaki, A. T.,Hui, C. Y.,Kong, A. K. H. IOP Publishing 2015 ASTROPHYSICAL JOURNAL LETTERS - Vol.798 No.1
<P>The binary system PSR B1259-63/LS 2883 is well sampled in radio, X-rays, and TeV gamma-rays, and shows orbital-phase-dependent variability in these frequencies. The first detection of GeV gamma-rays from the system was made around the 2010 periastron passage. In this Letter, we present an analysis of X-ray and gamma-ray data obtained by the Swift/XRT, NuSTAR/FPM, and Fermi/LAT, through the recent periastron passage which occurred on 2014 May 4. While PSR B1259-63/LS 2883 was not detected by the Large Area Telescope before and during this passage, we show that the GeV flares occurred at a similar orbital phase as in early 2011, thus establishing the repetitive nature of the post-periastron GeV flares. Multiple flares each lasting for a few days have been observed and short-term variability is seen as well. We also found X-ray flux variation contemporaneous with the GeV flare for the first time. Strong evidence of the keV-to-GeV connection came from the broadband high-energy spectra, which we interpret as synchrotron radiation from the shocked pulsar wind.</P>