Littérature scientifique sur le sujet « SEP events »
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Articles de revues sur le sujet "SEP events"
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Verkhoglyadova, O. P., G. Li, G. P. Zank, et al. "Understanding large SEP events with the PATH code: Modeling of the 13 December 2006 SEP event." Journal of Geophysical Research: Space Physics 115, A12 (2010): n/a. http://dx.doi.org/10.1029/2010ja015615.
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Reinard, A. A., and M. A. Andrews. "Comparison of CME characteristics for SEP and non-SEP related events." Advances in Space Research 38, no. 3 (2006): 480–83. http://dx.doi.org/10.1016/j.asr.2005.01.028.
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Kahler, Stephen W., and Alan G. Ling. "Forecasting Solar Energetic Particle (SEP) events with Flare X-ray peak ratios." Journal of Space Weather and Space Climate 8 (2018): A47. http://dx.doi.org/10.1051/swsc/2018033.
Texte intégralRésumé :
Solar flare X-ray peak fluxes and fluences in the 0.1–0.8 nm band are often used in models to forecast solar energetic particle (SEP) events. Garcia (2004) [Forecasting methods for occurrence and magnitude of proton storms with solar soft X rays, Space Weather, 2, S02002, 2004] used ratios of the 0.05–0.4 and 0.1–0.8 nm bands of the X-ray instrument on the GOES spacecraft to plot inferred peak flare temperatures versus peak 0.1–0.8 nm fluxes for flares from 1988 to 2002. Flares associated with E > 10 MeV SEP events of >10 proton flux units (pfu) had statistically lower peak temperatures than those without SEP events and therefore offered a possible empirical forecasting tool for SEP events. We review the soft and hard X-ray flare spectral variations as SEP event forecast tools and repeat Garcia’s work for the period 1998–2016, comparing both the peak ratios and the ratios of the preceding 0.05–0.4 nm peak fluxes to the later 0.1–0.8 nm peak fluxes of flares >M3 to the occurrence of associated SEP events. We divide the events into eastern and western hemisphere sources and compare both small (1.2–10 pfu) and large (≥300 pfu) SEP events with those of >10 pfu. In the western hemisphere X-ray peak ratios are statistically lower for >10 pfu SEP events than for non-SEP events and are even lower for the large (>300 pfu) events. The small SEP events, however, are not distinguished from the non-SEP events. We discuss the possible connections between the flare X-ray peak ratios and associated coronal mass ejections that are presumed to be the sources of the SEPs.
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Bao, Baoleerqimuge, and Guoyu Ren. "Sea-Effect Precipitation over the Shandong Peninsula, Northern China." Journal of Applied Meteorology and Climatology 57, no. 6 (2018): 1291–308. http://dx.doi.org/10.1175/jamc-d-17-0200.1.
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AbstractSea-effect precipitation (SEP) over the Shandong Peninsula is a unique climatological phenomenon in mainland China, and it exerts a considerable impact on the southern shore of the Bohai Sea. From observed data from 123 stations for the period 1962–2012, the characteristics of cold-season (November–February) SEP in this area were analyzed. Results showed that SEP occurred throughout the late autumn and winter. In all, 1173 SEP days were identified during the 51 years, of which snow days accounted for 73.7% and rain and snow–rain days accounted for 16.1% and 10.1%, respectively. December had the largest number of SEP snow days, followed by January and November. November was the most productive month in terms of SEP rain and snow–rain days. Intense SEP snowfall mainly affected the inland hill area of the peninsula, whereas light SEP snowfall reached farther inland. SEP rainfall shared a similar pattern with snowfall. The SEP frequency showed a significant interannual variability and a nonsignificant upward trend over the period analyzed. SEP was most likely to occur when the temperature difference between sea surface and 850 hPa over the Bohai Sea was above 10°C, indicating a dominant influence of low-level cold-air advection over the sea on the generation and development of the weather phenomenon. A significant negative correlation was also found between the area of sea ice in the Bohai Sea and intense SEP snowfall, indicating that sea ice extent had an important effect on SEP variability over the peninsula. In the case of extremely intense SEP events, a deeper East Asian trough at the 500-hPa level developed over the southwest of the study area and temperature and geopotential height contours were orthogonal to each other, indicating strong geostrophic cold-air advection over the Bohai Sea and the Shandong Peninsula. The extremely intense SEP events were also characterized by anomalous low temperature and high relative humidity in the lower troposphere, which contributed to greater gravitational instability in the study area.
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Wiedenbeck, M. E., G. M. Mason, and B. Klecker. "Isotopic Fractionation in 3He-rich SEP Events." Journal of Physics: Conference Series 1332 (November 2019): 012017. http://dx.doi.org/10.1088/1742-6596/1332/1/012017.
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Dmitriev, A. V., H. C. Yeh, J. K. Chao, I. S. Veselovsky, S. Y. Su, and C. C. Fu. "Top-side ionosphere response to extreme solar events." Annales Geophysicae 24, no. 5 (2006): 1469–77. http://dx.doi.org/10.5194/angeo-24-1469-2006.
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Abstract. Strong X-flares and solar energetic particle (SEP) fluxes are considered as sources of topside ionospheric disturbances observed by the ROCSAT-1/IPEI instrument during the Bastille Day event on 14 July 2000 and the Halloween event on 28 October–4 November 2003. It was found that within a prestorm period in the dayside ionosphere at altitudes of ~600 km the ion density increased up to ~80% in response to flare-associated enhancements of the solar X-ray emission. Ionospheric response to the SEP events was revealed both at sunlit and nightside hemispheres, where the ion density increased up to ~40% and 100%, respectively. We did not find any prominent response of the ion temperature to the X-ray and SEP enhancements. The largest X-ray and SEP impacts were found for the X17 solar flare on 28 October 2003, which was characterized by the most intense fluxes of solar EUV (Tsurutani et al., 2005) and relativistic solar particles (Veselovsky et al., 2004). Solar events on 14 July 2000 and 29 October 2003 demonstrate weaker impacts with respect to their X-ray and SEP intensities. The weakest ionospheric response is observed for the limb X28 solar flare on 4 November 2003. The topside ionosphere response to the extreme solar events is interpreted in terms of the short-duration impact of the solar electromagnetic radiation and the long-lasting impact of the SEP.
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Kahler, S. W., A. G. Ling, and D. V. Reames. "Spatial Evolution of 20 MeV Solar Energetic Proton Events." Astrophysical Journal 942, no. 2 (2023): 68. http://dx.doi.org/10.3847/1538-4357/aca7c0.
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Abstract The longitudinal extents of solar energetic (E > 10 MeV) particle (SEP) events in the heliosphere are a characteristic important for understanding SEP acceleration and transport as well as their space weather effects. SEP detectors on the STEREO A and B spacecraft launched in 2008, combined with those on Earth-orbiting spacecraft, have enabled recent studies of this characteristic for many events. Each SEP event distribution has been characterized by a single central longitude, width, and amplitude derived from Gaussian fits to peak intensities or fluences at each spacecraft. To capture dynamic changes of those parameters through SEP events, we apply Gaussian fits in solar-based Carrington longitude coordinates with 1 hr resolution to four selected large 20 MeV proton events. The limitations of single-Gaussian fits for very extended events is discussed. In all four examples the widths are increasing throughout the event, as expected, while the projected Gaussian centers at SEP onset start from 30° to 100° east of the associated flare, move westward, then remain stationary well east of the flare for several days before moving west as the event amplitudes decrease. Late decay phases can be characterized by eastward movements away from the flare longitudes. We introduce schematic Buffett plots to show successive snapshots of event longitudes and amplitudes.
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Koldobskiy, S., O. Raukunen, R. Vainio, G. A. Kovaltsov, and I. Usoskin. "New reconstruction of event-integrated spectra (spectral fluences) for major solar energetic particle events." Astronomy & Astrophysics 647 (March 2021): A132. http://dx.doi.org/10.1051/0004-6361/202040058.
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Aims. Fluences of solar energetic particles (SEPs) are not easy to evaluate, especially for high-energy events (i.e. ground-level enhancements, GLEs). Earlier estimates of event-integrated SEP fluences for GLEs were based on partly outdated assumptions and data, and they required revisions. Here, we present the results of a full revision of the spectral fluences for most major SEP events (GLEs) for the period from 1956 to 2017 using updated low-energy flux estimates along with greatly revisited high-energy flux data and applying the newly invented reconstruction method including an improved neutron-monitor yield function. Methods. Low- and high-energy parts of the SEP fluence were estimated using a revised space-borne/ionospheric data and ground-based neutron monitors, respectively. The measured data were fitted by the modified Band function spectral shape. The best-fit parameters and their uncertainties were assessed using a direct Monte Carlo method. Results. A full reconstruction of the event-integrated spectral fluences was performed in the energy range above 30 MeV, parametrised and tabulated for easy use along with estimates of the 68% confidence intervals. Conclusions. This forms a solid basis for more precise studies of the physics of solar eruptive events and the transport of energetic particles in the interplanetary medium, as well as the related applications.
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Georgoulis, Manolis K., Athanasios Papaioannou, Ingmar Sandberg, et al. "Analysis and interpretation of inner-heliospheric SEP events with the ESA Standard Radiation Environment Monitor (SREM) onboard the INTEGRAL and Rosetta Missions." Journal of Space Weather and Space Climate 8 (2018): A40. http://dx.doi.org/10.1051/swsc/2018027.
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Using two heliospheric vantage points, we study 22 solar energetic particle (SEP) events, 14 of which were detected at both locations. SEP proton events were detected during the declining phase of solar cycle 23 (November 2003–December 2006) by means of two nearly identical Standard Radiation Environment Monitor (SREM) units in energies ranging between 12.6 MeV and 166.3 MeV. In this work we combine SREM data with diverse solar and interplanetary measurements, aiming to backtrace solar eruptions from their impact in geospace (i.e., from L1 Lagrangian point to Earth’s magnetosphere) to their parent eruptions at the Sun’s low atmosphere. Our SREM SEP data support and complement a consistent inner-heliospheric description of solar eruptions (solar flares and coronal mass ejections [CMEs]) and their magnetospheric impact. In addition, they provide useful information on the understanding of the origin, acceleration, and propagation of SEP events at multi-spacecraft settings. All SEP events in our sample originate from major eruptions consisting of major (>M-class) solar flares and fast (>1800 km/s, on average), overwhelmingly (>78%) halo, CMEs. All but one SEP event studied are unambiguously associated with shock-fronted CMEs, suggesting a CME-driven shock acceleration mechanism. Moreover, a significant correlation is found between the SEP event peak and the onset of the storm sudden commencement, that might help improve prediction of magnetospheric disturbances. In general, SEP events correlate better with interplanetary (i.e., in-situ; L1-based) than with solar eruption features. Our findings support (a) the routine use of cost-effective SREM units, or future improvements thereof, for the detection of SEP events and (b) their implementation in multi-spacecraft settings as a means to improve both the physical understanding of SEP events and their forecasting.
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Gopalswamy, N., S. Yashiro, S. Akiyama, et al. "Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era." Annales Geophysicae 26, no. 10 (2008): 3033–47. http://dx.doi.org/10.5194/angeo-26-3033-2008.
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Abstract. Using the extensive and uniform data on coronal mass ejections (CMEs), solar energetic particle (SEP) events, and type II radio bursts during the SOHO era, we discuss how the CME properties such as speed, width and solar-source longitude decide whether CMEs are associated with type II radio bursts and SEP events. We discuss why some radio-quiet CMEs are associated with small SEP events while some radio-loud CMEs are not associated with SEP events. We conclude that either some fast and wide CMEs do not drive shocks or they drive weak shocks that do not produce significant levels of particle acceleration. We also infer that the Alfvén speed in the corona and near-Sun interplanetary medium ranges from <200 km/s to ~1600 km/s. Radio-quiet fast and wide CMEs are also poor SEP producers and the association rate of type II bursts and SEP events steadily increases with CME speed and width (i.e. energy). If we consider western hemispheric CMEs, the SEP association rate increases linearly from ~30% for 800 km/s CMEs to 100% for ≥1800 km/s. Essentially all type II bursts in the decametre-hectometric (DH) wavelength range are associated with SEP events once the source location on the Sun is taken into account. This is a significant result for space weather applications, because if a CME originating from the western hemisphere is accompanied by a DH type II burst, there is a high probability that it will produce an SEP event.
Thèses sur le sujet "SEP events"
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Rodríguez, Gasén Rosa. "Modelling SEP events: latitudinal and longitudinal dependence of the injection rate of shock-accelerated protons and their flux profiles." Doctoral thesis, Universitat de Barcelona, 2011. http://hdl.handle.net/10803/31855.
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Gradual SEP events is one of the greatest hazards in space environment, particularly for the launch and operation of spacecraft and for manned exploration. Predictions of their occurrence and intensity are essential to ensure the proper operation of technical and scientific instruments. However, nowadays there is a large gap between observations and models these events that can lead to predictions. This work focuses on the modelling of SEP events, particularly, on the influence of the observer's relative position and of the shock strength, on the simulated SEP flux profiles.
Part I of the thesis, deals with 3D MHD simulations of interplanetary shocks. We have studied the potential relevance of the latitude of the observer on the evolution of the strength of the shock and its influence on the injection rate of shock-accelerated particles; thus, on the resulting flux profiles. It is the first time that such dependence on the latitude is quantified from the modelling of SEP events, because most of the codes used so far to simulate interplanetary shocks are not 3D codes or they have been applied to near-ecliptic events.
To study the influence of the latitude of the observer and the strength of the shock in the SEP flux profiles, we have simulated the propagation of two shocks (slow and fast) up to several observers placed at different positions with respect to the nose of the shock. We have calculated the evolution of the plasma and magnetic field variables at the cobpoint, and we have derived the injection rate of shock-accelerated particles and the resulting proton flux profiles to be measured by each observer. We have discussed how observers located at different positions in space measure different SEP profiles, showing that variations on the latitude may result in intensity changes of up to one order of magnitude.
In Part II, we have used a new shock-and-particle model to simulate the 1 March 1979 SEP event that was observed by three different spacecraft. These spacecraft were positioned at similar radial distances but at significantly different angular positions, with respect to the associated solar source location. This particular scenario allows us to test the capability of the model to study the relevance of longitudinal variations in the shape of the intensity flux profiles, and to derive the injection rate of shock-accelerated particles. Despite the interest of multi-spacecraft events and due to the restrictions that they impose, this is just the second multi-spacecraft scenario for which their shock-particle characteristics have been modelled.
For the first time, a simulation of a propagation of an interplanetary shock has simultaneously reproduced the time shock arrival and the relevant plasma jumps across the shock at three spacecraft. We have fitted the proton intensities at the three spacecraft for different energy channels, and we have derived the particle transport conditions in space. We have quantified the efficiency of the shock at injecting particles in its way toward each observer, and we have discussed the influence of the observer's relative position on the injection rate of shock-accelerated particles. We have concluded that in this specific event the evolution of the injection rate can not be completely explained in terms of the normalized velocity jump.
The work performed during this thesis shows that the injection rate of shock-accelerated particles and their resulting flux profiles depend both on the latitude and on the longitude of the observer. This implies that more SEP events have to be modelled in order to quantify this conclusion on firm ground.<br>Els esdeveniments graduals de partícules solars energètiques (SEP) són un risc important per als astronautes i l’ instrumentació espacial. És per això que són necessàries eines de predicció de la intensitat i l'ocurrència de les tempestes de partícules solars per a garantitzar l'operativitat del material tècnic i científic embarcat. Existeix un gran buit, però, entre les prediccions del models actuals (per a ús en meteorologia espacial), i les observacions d'esdeveniments SEP. El treball realitzat durant aquesta tesi doctoral es centra en diversos aspectes de la simulació d'esdeveniments SEP. En particular, analitzem la influència de la posició relativa de l'observador i de la força del xoc en els perfils de flux derivats del nostre model combinat xoc-i-partícula. A partir de simulacions 3D, obtenim que el ritme d'injecció de partícules accelerades pel xoc depèn de la longitud de l'observador i demostrem, per primera vegada, que també depèn de la seva latitud. I es mostra que, conseqüentment, els perfils de flux detectats poden variar en un ordre de magnitud depenent de la connexió magnètica de l'observador amb el front del xoc. A més a més, presentem una simulació 2D d'un esdeveniment solar vist per tres sondes interplanetàries, pel qual s'ha ajustat, per primera vegada, l'arribada del xoc i els perfils de intensitat dels protons de diferents canals d'energia observats per cadascuna de les sondes. Així mateix, hem ajustat els salts en velocitat i camp magnètic a l'arribada del xoc, hem derivat les condicions de transport de les partícules i hem quantificat l'eficiència del xoc com a injector de partícules. La conclusió final del treball és que els futurs models de predicció d'esdeveniments SEP per a meteorologia espacial han de tenir en compte la geometria global de l'escenari solar-interplanetari.
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Landowski, Matthew. "DESIGN AND MODELING OF RADIATION HARDENED LATERAL POWER MOSFETS." Master's thesis, University of Central Florida, 2009. http://digital.library.ucf.edu/cdm/ref/collection/ETD/id/2823.
Texte intégralRésumé :
Galactic-cosmic-rays (GCR) exist in space from unknown origins. A cosmic ray is a very high energy electron, proton, or heavy ion. As a GCR transverses a power semiconductor device, electron-hole-pairs (ehps) are generated along the ion track. Effects from this are referred to as single-event-effects (SEEs). A subset of a SEE is single-event burnout (SEB) which occurs when the parasitic bipolar junction transistor is triggered leading to thermal runaway. The failure mechanism is a complicated mix of photo-generated current, avalanche generated current, and activation of the inherent parasitic bipolar transistor. Current space-borne power systems lack the utility and advantages of terrestrial power systems. Vertical-double-diffused MOSFETs (VDMOS) is by far the most common power semiconductor device and are very susceptible to SEEs by their vertical structure. Modern space power switches typically require system designers to de-rate the power semiconductor switching device to account for this. Consequently, the power system suffers from increased size, cost, and decreased performance. Their switching speed is limited due to their vertical structure and cannot be used for MHz frequency applications limiting the use of modern digital electronics for space missions. Thus, the Power Semiconductor Research Laboratory at the University of Central Florida in conjunction with Sandia National Laboratories is developing a rad-hard by design lateral-double-diffused MOSFET (LDMOS). The study provides a novel in-depth physical analysis of the mechanisms that cause the LDMOS to burnout during an SEE and provides guidelines for making the LDMOS rad-hard to SEB. Total dose radiation, another important radiation effect, can cause threshold voltage shifts but is beyond the scope of this study. The devices presented have been fabricated with a known total dose radiation hard CMOS process. Single-event burnout data from simulations and experiments are presented in the study to prove the viability of using the LDMOS to replace the VDMOS for space power systems. The LDMOS is capable of higher switching speeds due to a reduced drain-gate feedback capacitance (Miller Capacitor). Since the device is lateral it is compatible with complimentary-metal-oxide-semiconductor (CMOS) processes, lowering developing time and fabrication costs. High switching frequencies permit the use of high density point-of-load conversion and provide a fast dynamic response.<br>M.S.E.E.<br>School of Electrical Engineering and Computer Science<br>Engineering and Computer Science<br>Electrical Engineering MSEE
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Zhang, Fan. "Changing seasonality of convective events in the Labrador Sea." Thesis, Georgia Institute of Technology, 2014. http://hdl.handle.net/1853/51896.
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The representation of deep convection in ocean models is a fundamental challenge for climate science. Here a regional simulation of the Labrador Sea circulation and convective activity obtained with the Regional Oceanic Modeling System (ROMS) over the period 1980-2009 is used to characterize the response of convection to atmospheric forcing and the variability in its seasonal cycle. This integration compares well with the sparse in time and space hydrographic surveys and ARGO data (Luo et al. 2012). It is found that convection in the convective region of the Labrador Sea has experienced variability in three key aspects over the 30 years considered. First, the magnitude of convection varies greatly at decadal scales. This aspect is supported by the in-situ observations. Second, the initiation and peak of convection (i.e. initiation and maximum) shift by two to three weeks between strong and weak convective years. Third, the duration of convection varies by approximately one month between strong and weak years. The last two changes are associated to the variability of winter and spring time heat fluxes in the Labrador Sea, while the first results from changes in both atmospheric heat fluxes and oceanic conditions through the inflow of warm Irminger Water from the boundary current system to the basin interior. Changes in heat fluxes over the Labrador Sea convective region are strongly linked to large scale modes of variability, the North Atlantic Oscillation and Arctic Oscillation. Correlations between the mode indices and the local heat fluxes in the convective area are largest in winter during strong, deep events and in spring whenever convection is shallow.
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Krebs-Kanzow, Uta [Verfasser]. "Air-sea interactions during glacial Heinrich events / Uta Krebs." Kiel : Universitätsbibliothek Kiel, 2008. http://d-nb.info/1019732083/34.
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Hallgren, Linnéa. "Comparison of intensified turbulence events in the Baltic Sea." Thesis, Uppsala universitet, Institutionen för geovetenskaper, 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-443584.
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Turbulence is important since it affects the exchange of momentum, heat, and trace gases between the atmosphere and the ocean. However, measuring oceanic turbulence is not straightforward and that is why parameterizations that describe turbulence events are important. In this thesis turbulence data from the Baltic Sea is investigated and compared to already existing parameterizations. The thesis considers turbulence in the ocean surface boundary layer (OSBL) and how atmospheric parameters act as driving mechanisms. Turbulence creates mixing that enables the dispersion of various particles and a more efficient gas transfer at the air-sea interface. This thesis aimed to investigate the connection between the drivers of oceanic turbulence, wind, waves, and buoyancy fluxes and how they contribute to the formation of enhanced turbulence events. To investigate this, turbulence data from the Baltic Sea from June to August 2020, collected by an ADCP (Acoustic Doppler Current Profiler), was used to find connections to meteorological data during the same time period. Since turbulence is difficult to measure, three already existing parameterizations were compared to the observed turbulence to investigate their performance. The results showed that conditions with higher wind speeds with corresponding waves gave a better correlation between surface turbulence and wind and waves. The parameterization that included wind and waves gave results closest to the observed turbulence at the surfaces, compared to when only wind shear was included. It was also detected that the parameterized turbulence was in almost all cases under-predicted in comparison to the observed turbulence. To clarify why this is the case, a more detailed analysis would be needed to find what parameters are missing for better predictions of the surface turbulence.
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MERONI, AGOSTINO NIYONKURU. "Interactions between the ocean and extreme meteorological events." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2018. http://hdl.handle.net/10281/199143.
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Le interazioni oceano-atmosfera sono di primaria importanza sia in ambito climatico che meteorologico. Sono importanti sia su scale temporali orarie, come nell'intensificazione di cicloni tropicali, che su scale interannuali o interdecadali, come nel modo di variabilità climatica ENSO. Questa tesi si focalizza sui transferimenti di energia e quantità di moto all'interfaccia aria-mare in processi su scale temporali brevi caratterizzati da condizioni estreme. Sono presi in considerazione sia la risposta dinamica dell'oceano ad una forzante atmosferica estrema che l'effetto dello stato del mare sullo sviluppo di un evento meteorologico estremo. I sistemi studiati sono il campo di onde interne oceaniche nella scia di un ciclone tropicale e il ruolo dello stato termico dell'oceano superficiale nello sviluppo di piogge intense. In particolare, gli scambi di energia tra onde interne oceaniche nella scia di un ciclone tropicale idealizzato sono studiati con un approccio teorico supportato da appropriate simulazioni numeriche alle equazioni primitive. Si vuole capire come i cicloni tropicali possano contribuire al mescolamento oceanico interno in luoghi lontani dalla loro scia. Infatti, nonostante siano intermittenti nel tempo e nello spazio, sono caratterizzati da venti molto intensi, che eccitano onde interne oceaniche. Esse contribuiscono al mescolamento lontano dal luogo in cui sono state generate, attraverso la loro rottura. Dato che la propagazione di energia è legata alle loro caratteristiche spettrali, una descrizione dettagliata di come l'energia è divisa tra modi verticali e frequenze aiuta a quantificare l'estensione e la velocità di tale propagazione. Una nuova descrizione analitica degli scambi energetici che portano alla formazione del picco doppio-inerziale viene introdotta sulla base della teoria sviluppata. Rispetto a lavori precedenti, si considera una stratificazione oceanica realistica e viene sottolineata una possibile cascata energetica dalla larga scala della forzante atmosferica alla piccola scala del mescolamento. L'altra categoria di eventi estremi considerata è quella del sistemi convettivi a mesoscala (MCS). Essi sono fenomeni comuni lungo le coste del Mediterraneo e rilasciano abbondanti volumi di pioggia in poche ore e su aree dell'ordine di 100 km2. Si sa che un mare mediamente più caldo in prossimità di un MCS produce più pioggia, ma prima di questa tesi non c'erano informazioni circa l'influenza che un pattern spaziale di temperatura marina superficiale (SST) a scala chilometrica potesse avere sull'evento precipitativo. Opportune simulazioni atmosferiche, eseguite con un modello numerico non-idrostatico alle equazioni primitive, fanno luce sui meccanismi attraverso cui le strutture alla sotto-mesoscala di SST possono influenzare la struttura del vento superficiale e, di conseguenza, possono influenzare l'evoluzione della pioggia intensa. Si trova che, attraverso un maggiore mescolamento verticale di quantità di moto su aree di SST più calda, la presenza di fronti di temperatura nel mare può significativamente influenzare la convergenza superficiale, che è spesso l'elemento scatenante della convezione nei MCS, su scale temporali orarie. Questo potrebbe anche far spostare le linee di pioggia. Viene introdotta, poi, la possibilità di un fenomeno di retroazione oceanico legato al profilo verticale di temperatura. Con simulazioni accoppiate oceano-atmosfera, si trova che, in condizioni particolari, i venti intensi in cui il MCS è inglobato possono mischiare l'oceano superficiale a tal punto che la stabilità atmosferica è aumentata e la convezione è soppressa. Tali condizioni, tipiche della tarda estate, sono caratterizzate da uno strato mescolato sottile e una forte stratificazione. Questo potrebbe essere il motivo per cui i MCS sono generalmente osservati più avanti nell'anno, quando lo strato mescolato è più profondo e tale effetto oceanico di mitigazione è assente.<br>Ocean-atmosphere interactions are of paramount importance in both climatic and meteorological contexts. They are known to play important roles from hourly time scales, such as in the intensification of tropical cyclones, to interannual and even longer time scales, such as in El Niño Southern Oscillation mode of variability of the climate system. The focus of this thesis has been on the energy and momentum transfers at the air-sea interface in short time scales processes characterized by extreme conditions. Both the oceanic dynamical response to an extreme atmospheric forcing and the effects of the sea state on the development of a meteorological extreme event are considered. The systems under study are the ocean internal wave field in the wake of a tropical cyclone and the role of the upper ocean thermal state on the development of heavy rainfalls.
In particular, the energy exchanges among oceanic internal waves in the wake of an idealized tropical cyclone are studied with a theoretical approach supported by relevant primitve equation numerical simulations. The goal of this analysis is to understand how tropical cyclones might contribute to the internal ocean mixing in locations far from their track. In fact, despite their intermittency in space and time, they are characterized by very intense winds, which are known to excite oceanic internal waves. These are thought to contribute to ocean mixing far from their generation site through their breaking. Since the energy propagation is linked to the spectral features of the waves, a detailed description of the energy partitioning in different vertical modes and frequencies helps to better constrain the extent and the velocity of such energy propagation. A new detailed analytical description of the exchanges leading to the formation of the first superinertial peak is introduced on the basis of the theory developed. Compared to previous works, a realistic oceanic stratification is included and a path for the energy cascade from the large scales of the atmospheric forcing to the small scales of the mixing is highlighted.
The second category of extreme events considered are the heavy-rain-producing mesoscale convective systems (MCSs). They are common phenomena along the coasts of the Mediterranean sea and they release large amounts of rain in few hours and over relatively small areas, O(100 km2). It is known that an average warmer sea in the vicinity of their location produces a larger volume of rain, but before this thesis work no information was available on the influence that a spatial pattern of sea surface temperature (SST), with structures on the kilometric scale, might have on the precipitation event. Appropriate atmospheric numerical simulations, run with a non-hydrostatic primitive equation model, shed light on the mechanisms through which submesoscale SST oceanic features can influence the surface wind structure and, in turns, can affect the evolution of the heavy rainfall. It is found that through enhanced vertical momentum mixing in the atmosphere over warmer SST areas, the presence of temperature fronts in the sea can significantly affect the surface wind convergence, which is often the trigger for deep convection in MCSs, over hourly time scales. This might also lead to significant displacement of the rain bands.
The possibility of an ocean dynamical feedback related to the vertical temperature profile is then introduced. By means of atmosphere-ocean coupled numerical simulations, it is found that in particular conditions the intense winds in which the MCS is embedded can mix the upper ocean strongly enough to enhance the stability of the atmospheric boundary layer and suppress deep convection. Such conditions, characterized by a shallow mixed layer and strong stratification, are typical of the late summer. This could be the reason why MCSs are generally observed later during the year, when the mixed layer is deeper and this oceanic mitigating effect is absent.
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Truyen, David. "Etude par simulation composant 3D des effets singuliers SEU et SET induits par ions lourds sur le noeud technologique CMOS bulk 180 nm." Montpellier 2, 2007. http://www.theses.fr/2007MON20139.
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Hagelin, Susanna. "Effects of Upwelling Events on the Atmosphere." Thesis, Uppsala universitet, Luft-, vatten och landskapslära, 2006. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-303882.
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During an upwelling event the cold bottom-water is brought to the sea surface. This cools the atmosphere from below and the stratification becomes more stable. When the atmosphere is more stable the turbulence is reduced and, as a consequence, so are the turbulent fluxes. This study is investigating four periods of upwelling from the Östergarnsholm-site, in the Baltic Sea east of Gotland, during the summer of 2005. The air measurements are taken at a tower at the southernmost tip of Östergarnsholm while the measurements in the water are from a buoy moored 1 km south-southeast of the tower. During all the upwelling events the wind is south-westerly, along the coast of Gotland. This means that the buoy is not within the flux footprint area and is perhaps not always representative of what happens there. All the periods show a stabilization of the atmosphere as the SST (Sea Surface Temperature) decreases. The heat fluxes, especially the latent heat flux, decreases as the SST decreases. The amount of CO2 in the atmosphere, in the summer, is usually higher than the amount in the surface water of the seas because the oceans are a net sink of CO2. The air-sea flux of CO2 is to a large extent controlled by this difference. Therefore the flux of CO2 is usually directed to the sea. The deep-water contains more CO2 than the surface water because the phytoplankton near the surface removes CO2 through photosynthesis. The deep-water is also colder and can solve more CO2. During an upwelling event this CO2-rich water is brought to the surface. As an upwelling event progresses the difference in CO2-concentration between the air and the sea is reduced, sometimes reversed, and the flux decreases. This is what happens in three of the investigated periods in this study. During the fourth period a counter gradient flux is observed.<br>När en uppvällning inträffar förs kallt djupvatten upp till havsytan. Det kalla vattnet kyler atmosfären nedifrån, något som leder till mer stabil skiktning. När atmosfären blir mer stabilt skiktad dämpas turbulensen och det medför att de turbulenta flödena också avtar. I den här studien analyseras fyra perioder med uppvällning. Mätningarna kommer från Östergarnsholm, öster om Gotland, under sommaren 2005. Mätningarna i luften är tagna från en mast vid Östergarnsholms södra udde. Mätningarna i vattnet kommer från en boj som är förankrad 1 km sydsydöst om masten. Vid samtliga uppvällnings-perioder i den här studien är vinden sydvästlig (längs Gotlandskusten). Det betyder att bojen inte befinner sig inom flödenas footprint-area och dess mätningar är kanske inte hela tiden representativa för vad som händer i footprint-arean. Samtliga undersökta perioder visar på en stabilisering av atmosfären då havsytans temperatur avtar. Värmeflödena, i synnerhet det latenta värmeflödet, avtar i samband med att temperaturen i havsytan sjunker. Halten av CO2 i atmosfären är vanligtvis högre än halten i havens ytvatten (under sommaren) eftersom de är en nettosänka för CO2 globalt sett. CO2-flödet mellan havsytan och atmosfären styr till en stor del av denna skillnaden i CO2-halt. Det innebär att CO2-flödet är riktat neråt, mot havet. Havens djupvatten innehåller mer CO2 därför att växtplankton nära ytan reducerar CO2-halten genom fotosyntesen. Djupvattnet är också kallare och kan därför lösa mer CO2. Under en uppvällning förs detta CO2-rika vatten upp till ytan. När en uppvällning fortskrider minskar skillnaden i CO2-halt mellan hav och atmosfär (ibland kan CO2-halten i ytvattnet även komma att överstiga atmosfärens halt) och flödet avtar. Tre av perioderna i den här studien visar på ett avtagande flöde. Den fjärde perioden uppvisar ett flöde motriktat CO2-gradienten.
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Benfenati, Francesco Maria. "Statistical analysis of oceanographic extreme events." Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2020. http://amslaurea.unibo.it/19885/.
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Condizioni ambientali estreme del mare possono avere un forte impatto sulla navigazione e/o sul successo di operazioni di salvataggio. Le tecniche statistiche sono cruciali per quantificare la presenza di eventi estremi e monitorarne
variazioni di frequenza e intensità. Gli eventi estremi "vivono" nella coda di una funzione distribuzione di probabilità (PDF), per questo è importante studiare la PDF in punti lontani diverse deviazioni standard dalla media.
L’altezza significativa dell’onda (SWH) è il parametro solitamente usato per valutare l’intensità degli stati del mare. L’analisi degli estremi nella coda di una distribuzione richiede lunghe serie temporali per stime ragionevoli della loro intesità e e frequenza. Dati osservativi (i.e. dati storici da boe), sono
spesso assenti e vengono invece utilizzate ricostruzioni numeriche delle onde, con il vantaggio che l’analisi di eventi estremi diventa possibile su una vasta area.
Questa tesi vuole condurre un’analisi preliminare delle variazioni spaziali dei valori estremi della SWH nel Mediterraneo. Vengono usati dati orari dal modello del Med-MFC (dal portale del CMEMS), una ricostruzione numerica di onde per il Mediterraneo, che sfrutta il modello "WAM Cycle 4.5.4",
coprendo il periodo 2006-2018, con risoluzione spaziale 0.042° (~ 4km).
In particolare, consideriamo dati di 11 anni (dal 2007 al 2017), concentrandoci sulle regioni del Mar Ionio e del Mar Iberico.
La PDF della SWH è seguita piuttosto bene dall’andamento di una curva Weibull a 2 parametri sia durante l’inverno (Gennaio) che durante l’estate (Luglio), con difetti per quanto riguarda il picco e la coda della distribuzione. A confronto, la curva a 3 parametri Weibull Esponenziata sembra essere più appropriata, anche se non è stato trovato un metodo per dimostrare che sia
un fit migliore. Alla fine, viene proposto un metodo di stima del rischio basato sul periodo giornaliero di ritorno delle onde più alte di un certo valore di soglia, ritenute pericolose.
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King, Adrian. "Terminal Palaeocene events in the North Sea and Faeroe-Shetland Basin." Thesis, University of Southampton, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.274437.
Texte intégralLivres sur le sujet "SEP events"
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Implementing and configuring SAP event management (EM). Galileo Press, 2010.
Trouver le texte intégral
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Unforgettable Atlantic Canada: The 100 must-see destinations and events. Nimbus Pub., 2010.
Trouver le texte intégralChapitres de livres sur le sujet "SEP events"
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Reames, Donald V. "Impulsive SEP Events." In Solar Energetic Particles. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-50871-9_4.
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Reames, Donald V. "Gradual SEP Events." In Solar Energetic Particles. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-50871-9_5.
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Reames, Donald V. "Gradual SEP Events." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_5.
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AbstractGradual solar energetic-particle (SEP) events are “big proton events” and are usually much more “gradual” in their decay than in their onset. As their intensities increase, particles streaming away from the shock amplify Alfvén waves that scatter subsequent particles, increasing their acceleration, eventually limiting ion flow at the “streaming limit.” Waves generated by higher-speed protons running ahead can also throttle the flow of lower-energy ions, flattening spectra and altering abundances in the biggest SEP events. Thus, we find that the A/Q-dependence of scattering causes element-abundance patterns varying in space and time, which define source-plasma temperatures T, since the pattern of Q values of the ions depends upon temperature. Differences in T explain much of the variation of element abundances in gradual SEP events. In nearly 70% of gradual events, SEPs are shock-accelerated from ambient coronal plasma of ~0.8–1.6 MK, while 24% of the events involve material with T ≈ 2–4 MK re-accelerated from residual impulsive-suprathermal ions with pre-enhanced abundances. This source-plasma temperature can occasionally vary with solar longitude across the face of a shock. Non-thermal variations in ion abundances in gradual SEP events reaccelerated from the 2–4 MK impulsive source plasma are reduced, relative to those in the original impulsive SEPs, probably because the accelerating shock waves sample a pool of ions from multiple jet sources. Late in gradual events, SEPs become magnetically trapped in a reservoir behind the CME where spectra are uniform in space and decrease adiabatically in time as the magnetic bottle containing them slowly expands. Finally, we find variations of the He/O abundance ratio in the source plasma of different events.
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Reames, Donald V. "Impulsive SEP Events (and Flares)." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_4.
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Abstract3He-rich, Fe-rich, and enriched in elements with Z > 50, the abundances of solar energetic particles (SEPs) from the small impulsive SEP events stand out as luminaries in our study. The 3He is enhanced by resonant wave-particle interactions. Element abundances increase 1000-fold as the ~3.6 power of the mass-to-charge ratio A/Q from He to heavy elements like Au or Pb, enhanced during acceleration in islands of magnetic reconnection in solar jets, and probably also in flares. This power-law of enhancement vs. A/Q implies Q determined by a source temperature of 2.5–3.2 MK, typical of jets from solar active regions where these impulsive SEPs occur. However, a few small events are unusual; several have suppressed 4He, and rarely, a few very small events with steep spectra have elements N or S greatly enhanced, perhaps by the same resonant-wave mechanism that enhances 3He. Which mechanism will dominate? The impulsive SEP events we see are associated with narrow CMEs, from solar jets where magnetic reconnection on open field lines gives energetic particles and CMEs direct access to space. Gamma-ray lines tell us that the same acceleration physics may occur in flares.
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Reames, Donald V. "A Turbulent History." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_2.
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AbstractLarge solar energetic-particle (SEP) events are clearly associated in time with eruptive phenomena on the Sun, but how? When large SEP events were first observed, flares were the only visible candidate, and diffusion theory was stretched to explain how the particles could spread through space, as widely as observed. The observation of coronal mass ejections (CMEs), and the wide, fast shock waves they can drive, provided better candidates later. Then small events were found with 1000-fold enhancements in 3He/4He that required a different kind of source—should we reconsider flares, or their open-field cousins, solar jets? The 3He-rich events were soon associated with the electron beams that produce type III radio bursts. It seems the radio astronomers knew of both SEP sources all along. Sometimes the distinction between the sources is blurred when shocks reaccelerate residual 3He-rich impulsive suprathermal ions. Eventually, however, we would even begin to measure the source-plasma temperature that helps to better distinguish the SEP sources.
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Klein, Karl-Ludwig, Kostas Tziotziou, Pietro Zucca, et al. "X-Ray, Radio and SEP Observations of Relativistic Gamma-Ray Events." In Astrophysics and Space Science Library. Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-60051-2_8.
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Reames, Donald V. "Distinguishing the Sources." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_3.
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AbstractOur discussion of history has covered many of the observations that have led to the ideas of acceleration by shock waves or by magnetic reconnection in gradual and impulsive solar energetic particle (SEP) events, respectively. We now present other compelling observations, including onset timing, SEP-shock correlations, injection time profiles, high-energy spectral knees, e/p ratios, and intensity dropouts caused by a compact source, that have helped clarify these acceleration mechanisms and sources. However, some of the newest evidence now comes from source-plasma temperatures. In this and the next two chapters, we will find that impulsive events come from solar active regions at ≈ 3 MK, controlling ionization states Q, hence A/Q, and, in most gradual events, shocks accelerate ambient coronal material from ≤1.6 MK. When SEPs are trapped on closed loops they supply the energy for flares. In addition to helping to define their own origin, SEPs also probe the structure of the interplanetary magnetic field.
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Reames, Donald V. "Introducing the Sun and SEPs." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_1.
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AbstractThe structure of the Sun, with its energy generation and heating, creates convection and differential rotation of the outer solar plasma. This convection and rotation of the ionized plasma generates the solar magnetic field. This field and its variation spawn all of the solar activity: solar active regions, flares, jets, and coronal mass ejections (CMEs). Solar activity provides the origin and environment for both the impulsive and gradual solar energetic particle (SEP) events. This chapter introduces the background environment and basic properties of SEP events, time durations, abundances, and solar cycle variations.
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Reames, Donald V. "Summary and Conclusions." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_10.
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AbstractIn this chapter we summarize our current understanding of SEPs, of properties of the sites of their origin and of the physical processes that accelerate or modify them. These processes can leave an indelible mark on the abundances of elements, isotopes, ionization states, anisotropies, energy spectra and time profiles of the SEPs. Transport of the ions to us along magnetic fields can impose new variations in large events or even enhance the visibility of the source parameters as the SEPs expand into the heliosphere. We lack physical models that can follow the complexity of SEP abundance variations.
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Reames, Donald V. "High Energies and Radiation Effects." In Solar Energetic Particles. Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-66402-2_6.
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AbstractIn this chapter we characterize the high-energy spectra of protons that can penetrate shielding and determine the radiation dose to humans and equipment in space. High-energy spectral breaks or “knees”, seen in all large SEP events, determine the contribution of highly penetrating protons. The streaming limit, discussed earlier, places an upper bound on particle fluences early in events and the radial variation of intensities is important for near-solar and deep-space missions. The streaming limit is a strong function of radial distance from the Sun. We also consider requirements for a radiation storm shelter for deep space, a mission to Mars, suitability of exoplanets for life, and radiation-induced chemistry of the upper atmosphere of Earth.
Actes de conférences sur le sujet "SEP events"
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Miyake, Fusa. "Cosmogenic Evidence for Past SEP Events." In 36th International Cosmic Ray Conference. Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.0011.
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Cohen, Christina, J. G. Luhmann, R. A. Mewaldt, et al. "Searching for Extreme SEP Events with STEREO." In 35th International Cosmic Ray Conference. Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0134.
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Li, G., X. Ao, O. Verkhoglyadova, G. P. Zank, and L. Ding. "Diffusive shock acceleration in large SEP events." In PHYSICS OF THE HELIOSPHERE: A 10 YEAR RETROSPECTIVE: Proceedings of the 10th Annual International Astrophysics Conference. AIP, 2012. http://dx.doi.org/10.1063/1.4723606.
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Li, G., G. Zank, O. Verkhoglyadova, and L. Ding. "Diffusive shock acceleration and large SEP events." In SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4811000.
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Dalla, S. "Characterization of SEP events at high heliographic latitudes." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618680.
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Dalla, S. "Multi-spacecraft observations of decay phases of SEP events." In SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1618681.
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Bućík, R., U. Mall, A. Korth, G. M. Mason, and R. Gómez-Herrero. "[sup 3]He-rich SEP events observed by STEREO-A." In SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4811007.
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Li, G., G. Zank, O. Verkhoglyadova, X. Ao, and L. Ding. "What controls the maximum particle energy in large SEP events." In SPACE WEATHER: THE SPACE RADIATION ENVIRONMENT: 11th Annual International Astrophysics Conference. AIP, 2012. http://dx.doi.org/10.1063/1.4768753.
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Didkovsky, Leonid, Darrell Judge, Seth Wieman, et al. "SEP Temporal Fluctuations Related to Extreme Solar Flare Events Detected by SOHO/CELIAS/SEM." In 45th AIAA Aerospace Sciences Meeting and Exhibit. American Institute of Aeronautics and Astronautics, 2007. http://dx.doi.org/10.2514/6.2007-496.
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Slocum, P. L. "Measurements of heavy elements in [sup 3]He-rich SEP events." In Acceleration and transport of energetic particles observed in the heliosphere (ACE-2000 symposium). AIP, 2000. http://dx.doi.org/10.1063/1.1324289.
Texte intégralRapports d'organisations sur le sujet "SEP events"
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Niemi, A. An Extension to Session Initiation Protocol (SIP) Events for Conditional Event Notification. Edited by D. Willis. RFC Editor, 2010. http://dx.doi.org/10.17487/rfc5839.
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Roach, A. B. SIP-Specific Event Notification. RFC Editor, 2012. http://dx.doi.org/10.17487/rfc6665.
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Jones, M., W. Denniss, and M. Ansari. Security Event Token (SET). Edited by P. Hunt. RFC Editor, 2018. http://dx.doi.org/10.17487/rfc8417.
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B., A. Session Initiation Protocol (SIP)-Specific Event Notification. RFC Editor, 2002. http://dx.doi.org/10.17487/rfc3265.
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Ackerley, N., A. L. Bird, M. Kolaj, H. Kao, and M. Lamontagne. Procedures for seismic event type discrimination at the Canadian Hazards Information Service. Natural Resources Canada/CMSS/Information Management, 2022. http://dx.doi.org/10.4095/329613.
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Within a catalogue of seismic events, it is necessary to distinguish natural tectonic earthquakes from seismic events due to human activity or other natural processes. This becomes very important when the data are incorporated into models of seismic hazard, since natural and anthropogenic events follow different recurrence and scaling laws. This document outlines a two-step procedure whereby first, a most likely event type is identified, and second, confirmation or refutation is sought. The procedure is intended to be compatible with current and past practices at the Canadian Hazards Information Service and the Geological Survey of Canada in assigning event types in the National Earthquake Database (NEDB). Furthermore, this document presents a new nomenclature and coding system for event types and their certainty, one that is compatible with QuakeML. Detailed classification criteria are given for all common event types; for rare event types, only definitions and examples are given.
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Polk, J. Extending the Session Initiation Protocol (SIP) Reason Header for Preemption Events. RFC Editor, 2006. http://dx.doi.org/10.17487/rfc4411.
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Blais-Stevens, A. Historical landslide events along the Sea to Sky corridor, British Columbia. Natural Resources Canada/ESS/Scientific and Technical Publishing Services, 2007. http://dx.doi.org/10.4095/224585.
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Rosenberg, J. A Session Initiation Protocol (SIP) Event Package for Registrations. RFC Editor, 2004. http://dx.doi.org/10.17487/rfc3680.
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Niemi, A., ed. Session Initiation Protocol (SIP) Extension for Event State Publication. RFC Editor, 2004. http://dx.doi.org/10.17487/rfc3903.
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Camarillo, G. The Session Initiation Protocol (SIP) Pending Additions Event Package. RFC Editor, 2008. http://dx.doi.org/10.17487/rfc5362.
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