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Articles de revues sur le sujet « SEP events »

Auteur : Grafiati
Publié le 10 mars 2023

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1

Verkhoglyadova, O. P., G. Li, G. P. Zank, Q. Hu, C. M. S. Cohen, R. A. Mewaldt, G. M. Mason, D. K. Haggerty, T. T. von Rosenvinge et M. D. Looper. « Understanding large SEP events with the PATH code : Modeling of the 13 December 2006 SEP event ». Journal of Geophysical Research : Space Physics 115, A12 (décembre 2010) : n/a. http://dx.doi.org/10.1029/2010ja015615.

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Reinard, A. A., et M. A. Andrews. « Comparison of CME characteristics for SEP and non-SEP related events ». Advances in Space Research 38, no 3 (janvier 2006) : 480–83. http://dx.doi.org/10.1016/j.asr.2005.01.028.

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Kahler, Stephen W., et 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.

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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, et Guoyu Ren. « Sea-Effect Precipitation over the Shandong Peninsula, Northern China ». Journal of Applied Meteorology and Climatology 57, no 6 (juin 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 et B. Klecker. « Isotopic Fractionation in 3He-rich SEP Events ». Journal of Physics : Conference Series 1332 (novembre 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 et C. C. Fu. « Top-side ionosphere response to extreme solar events ». Annales Geophysicae 24, no 5 (3 juillet 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 et D. V. Reames. « Spatial Evolution of 20 MeV Solar Energetic Proton Events ». Astrophysical Journal 942, no 2 (1 janvier 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 et I. Usoskin. « New reconstruction of event-integrated spectra (spectral fluences) for major solar energetic particle events ». Astronomy & ; Astrophysics 647 (mars 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, Anastasios Anastasiadis, Ioannis A. Daglis, Rosa Rodríguez-Gasén, Angels Aran, Blai Sanahuja et Petteri Nieminen. « 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, P. Mäkelä, H. Xie, M. L. Kaiser, R. A. Howard et J. L. Bougeret. « Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era ». Annales Geophysicae 26, no 10 (15 octobre 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.
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Swalwell, Bill, Silvia Dalla et Robert Walsh. « Forecasting Solar Energetic Particle Events and Associated False Alarms ». Proceedings of the International Astronomical Union 13, S335 (juillet 2017) : 324–27. http://dx.doi.org/10.1017/s1743921317011036.

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AbstractBecause of the significant dangers they pose, accurate forecasting of Solar Energetic Particle (SEP) events is vital. Whilst it has long been known that SEP-production is associated with high-energy solar events, forecasting algorithms based upon the observation of these types of solar event suffer from high false alarm rates. Here we analyse the parameters of 4 very high energy solar events which were false alarms, with a view to reaching an understanding as to why SEPs were not detected at Earth. We find that in each case at least two factors were present which have been shown to be detrimental to SEP production.
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Klein, Karl-Ludwig. « Radio Astronomical Tools for the Study of Solar Energetic Particles II.Time-Extended Acceleration at Subrelativistic and Relativistic Energies ». Frontiers in Astronomy and Space Sciences 7 (11 mars 2021). http://dx.doi.org/10.3389/fspas.2020.580445.

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Solar energetic particle (SEP) events are commonly separated in two categories: numerous “impulsive” events of relatively short duration, and a few “gradual” events, where SEP-intensities may stay enhanced over several days at energies up to several tens of MeV. In some gradual events the SEP spectrum extends to relativistic energies (>1 GeV), over shorter durations. The two categories are strongly related to an idea developed in the 1960s based on radio observations: Type III bursts, which were addressed in a companion chapter, outline impulsive acceleration of electrons to subrelativistic energies, while the large and the relativistic SEP events were ascribed to a second acceleration process. At radio wavelengths, typical counterparts were bursts emitted by electrons accelerated at coronal shock waves (type II bursts) and by electron populations in large-scale closed coronal structures (type IV bursts). Both burst types are related to coronal mass ejections (CMEs). Type II bursts from metric to kilometric wavelengths tend to accompany large SEP events, which is widely considered as a confirmation that CME-driven shocks accelerate the SEPs. But type II bursts, especially those related to SEP events, are most often accompanied by type IV bursts, where the electrons are rather accelerated in the wake of the CME. Individual event studies suggest that although the CME shock is the most plausible accelerator of SEPs up to some yet unknown limiting energy, the relativistic SEP events show time structure that rather points to coronal acceleration related to type IV bursts. This chapter addresses the question what type II bursts tell us about coronal shock waves and how type II and type IV radio bursts are related with relativistic proton signatures as seen by particle detectors on the Earth and by their gamma-ray emission in the solar atmosphere, focusing on two relativistic SEP events, on 2005 Jan 20 and 2017 Sep 10. The importance of radio emissions as a complement to the upcoming SEP observations from close to the Sun is underlined.
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Kahler, Stephen. « Second-Class Citizen in the Heliophysics Community ». Frontiers in Astronomy and Space Sciences 9 (13 avril 2022). http://dx.doi.org/10.3389/fspas.2022.892965.

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The study of solar energetic particles (SEPs) is an important area of solar research and space weather. An SEP event extends over large regions of the heliosphere, involves energy ranges varying by decades, and evolves over various time and spatial scales and with ion composition, but with SEP observations limited to in situ detections on a few spacecraft for any given event, we are unable to observe these properties synoptically. Solar studies in general are the beneficiaries of imaging and remote sensing observations over practically all wavelengths and timescales from ground and space based detectors that drive increasingly highly sophisticated models. I see this divide as creating a two-class system for researchers, with us SEP researchers as second class members. Following a brief review of my experience with solar imagery and failed ideas on remote imaging of SEP events, I review two remarkable developments that give hope for some new SEP imaging technique. Finally, I discuss two poorly understood questions of impulsive and gradual SEP events that I think can be feasibly approached with current modeling techniques.
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« Healthcare fallout following events of Sep 11 2001 ». PharmacoEconomics & ; Outcomes News 353, no 1 (mars 2002) : 12. http://dx.doi.org/10.1007/bf03278806.

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« Calendar of Events : J. Sep. Science 4/2002 ». Journal of Separation Science 25, no 4 (1 mars 2002) : 265–66. http://dx.doi.org/10.1002/1615-9314(20020301)25:4<265 ::aid-jssc265>3.0.co;2-8.

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« Calendar of Events : J. Sep. Science 7/2002 ». Journal of Separation Science 25, no 7 (1 mai 2002) : 469–70. http://dx.doi.org/10.1002/1615-9314(20020501)25:7<469 ::aid-jssc469>3.0.co;2-c.

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« Calendar of Events : J. Sep. Science 8/2002 ». Journal of Separation Science 25, no 8 (1 juin 2002) : 549–50. http://dx.doi.org/10.1002/1615-9314(20020601)25:8<549 ::aid-jssc549>3.0.co;2-c.

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« Calendar of Events : J. Sep. Science 9/2002 ». Journal of Separation Science 25, no 9 (1 juin 2002) : 629–30. http://dx.doi.org/10.1002/1615-9314(20020601)25:9<629 ::aid-jssc629>3.0.co;2-f.

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« Calendar of Events : J. Sep. Science 12/2002 ». Journal of Separation Science 25, no 12 (1 août 2002) : 780–82. http://dx.doi.org/10.1002/1615-9314(20020801)25:12<780 ::aid-jssc780>3.0.co;2-k.

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« Calendar of Events : J. Sep. Science 13/2002 ». Journal of Separation Science 25, no 13 (1 septembre 2002) : 856–58. http://dx.doi.org/10.1002/1615-9314(20020901)25:13<856 ::aid-jssc856>3.0.co;2-2.

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« Calendar of Events : J. Sep. Science 14/2002 ». Journal of Separation Science 25, no 14 (1 octobre 2002) : 925–26. http://dx.doi.org/10.1002/1615-9314(20021001)25:14<925 ::aid-jssc925>3.0.co;2-j.

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« Calendar of Events : J. Sep. Science 18/2002 ». Journal of Separation Science 25, no 18 (1 décembre 2002) : 1365–66. http://dx.doi.org/10.1002/jssc.200290009.

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« Calendar of Events : J. Sep. Science 5/2003 ». Journal of Separation Science 26, no 5 (1 avril 2003) : 443–44. http://dx.doi.org/10.1002/jssc.200390059.

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« Calendar of Events : J. Sep. Science 8/2003 ». Journal of Separation Science 26, no 8 (1 juin 2003) : 743–44. http://dx.doi.org/10.1002/jssc.200390092.

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« Calendar of Events : J. Sep. Science 11/2003 ». Journal of Separation Science 26, no 11 (1 juillet 2003) : 1075–76. http://dx.doi.org/10.1002/jssc.200390103.

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« Calendar of Events : J. Sep. Science 14/2003 ». Journal of Separation Science 26, no 14 (26 septembre 2003) : 1295–96. http://dx.doi.org/10.1002/jssc.200390109.

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« Calendar of Events : J. Sep. Science 17/2003 ». Journal of Separation Science 26, no 17 (1 novembre 2003) : 1599–600. http://dx.doi.org/10.1002/jssc.200390116.

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« Calendar of Events : J. Sep. Science 18/2003 ». Journal of Separation Science 26, no 18 (1 décembre 2003) : 1717–18. http://dx.doi.org/10.1002/jssc.200390119.

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« Calendar of Events : J. Sep. Science 3/2004 ». Journal of Separation Science 27, no 3 (février 2004) : 255–56. http://dx.doi.org/10.1002/jssc.200490008.

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« Calendar of Events : J. Sep. Science 4/2004 ». Journal of Separation Science 27, no 4 (mars 2004) : 347–48. http://dx.doi.org/10.1002/jssc.200490013.

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« Calendar of Events : J. Sep. Science 9/2004 ». Journal of Separation Science 27, no 9 (juin 2004) : 735–36. http://dx.doi.org/10.1002/jssc.200490032.

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« Calendar of Events : J. Sep. Science 12/2004 ». Journal of Separation Science 27, no 12 (août 2004) : 1051–52. http://dx.doi.org/10.1002/jssc.200490042.

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« Calendar of Events : J. Sep. Science 13/2004 ». Journal of Separation Science 27, no 13 (septembre 2004) : 1139–40. http://dx.doi.org/10.1002/jssc.200490049.

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« Calendar of Events : J. Sep. Science 14/2004 ». Journal of Separation Science 27, no 14 (octobre 2004) : 1235–36. http://dx.doi.org/10.1002/jssc.200490053.

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« Calendar of Events : J. Sep. Science 1/2005 ». Journal of Separation Science 28, no 1 (janvier 2005) : 111–12. http://dx.doi.org/10.1002/jssc.200590002.

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« Calendar of Events : J. Sep. Science 2/2005 ». Journal of Separation Science 28, no 2 (février 2005) : 207–8. http://dx.doi.org/10.1002/jssc.200590009.

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« Calendar of Events : J. Sep. Science 3/2005 ». Journal of Separation Science 28, no 3 (février 2005) : 303–4. http://dx.doi.org/10.1002/jssc.200590013.

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« Calendar of Events : J. Sep. Science 4/2005 ». Journal of Separation Science 28, no 4 (mars 2005) : 399–400. http://dx.doi.org/10.1002/jssc.200590018.

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« Calendar of Events : J. Sep. Science 5/2005 ». Journal of Separation Science 28, no 5 (mars 2005) : 492–93. http://dx.doi.org/10.1002/jssc.200590020.

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« Calendar of Events : J. Sep. Science 6/2005 ». Journal of Separation Science 28, no 6 (avril 2005) : 591–92. http://dx.doi.org/10.1002/jssc.200590024.

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« Calendar of Events : J. Sep. Science 7/2005 ». Journal of Separation Science 28, no 7 (mai 2005) : 679–80. http://dx.doi.org/10.1002/jssc.200590027.

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« Calendar of Events : J. Sep. Science 8/2005 ». Journal of Separation Science 28, no 8 (mai 2005) : 780–81. http://dx.doi.org/10.1002/jssc.200590030.

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« Calendar of Events : J. Sep. Science 11/2005 ». Journal of Separation Science 28, no 11 (juillet 2005) : 1251–52. http://dx.doi.org/10.1002/jssc.200590039.

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« Calendar of Events : J. Sep. Science 12/2005 ». Journal of Separation Science 28, no 12 (août 2005) : 1419–20. http://dx.doi.org/10.1002/jssc.200590044.

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« Calendar of Events : J. Sep. Science 13/2005 ». Journal of Separation Science 28, no 13 (août 2005) : 1604–5. http://dx.doi.org/10.1002/jssc.200590049.

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« Calendar of Events : J. Sep. Science 14/2005 ». Journal of Separation Science 28, no 14 (septembre 2005) : 1836–37. http://dx.doi.org/10.1002/jssc.200590056.

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« Calendar of Events : J. Sep. Science 15/2005 ». Journal of Separation Science 28, no 15 (octobre 2005) : 2036–37. http://dx.doi.org/10.1002/jssc.200590061.

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« Calendar of Events : J. Sep. Science 16/2005 ». Journal of Separation Science 28, no 16 (octobre 2005) : 2233–34. http://dx.doi.org/10.1002/jssc.200590066.

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« Calendar of Events : J. Sep. Science 17/2005 ». Journal of Separation Science 28, no 17 (novembre 2005) : 2431–32. http://dx.doi.org/10.1002/jssc.200590072.

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« Calendar of Events : J. Sep. Science 18/2005 ». Journal of Separation Science 28, no 18 (décembre 2005) : 2557–58. http://dx.doi.org/10.1002/jssc.200590078.

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