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	Solar proton event - Wikipedia, the free encyclopedia
		A Solar proton event occurs when high-energy protons, ejected from the sun's surface during a solar flare, get caught by the Earth's magnetic field and cause ionization in the ionosphere.
		The effect is similar to auroral events, the difference being that electrons and not protons are involved.
		The events typically occur where the Earth's magnetic field is lowest, at the north pole, south pole, and South Atlantic magnetic anomaly.
	en.wikipedia.org /wiki/Solar_proton_event (137 words)

	Solar Protons
		Solar Proton Events (SPE) and Their Impact on HF Communications
		This region is the southern extension of the South Atlantic Anomaly where the energetic particle intensities are normally large and does not indicate the presence of solar protons.
		The equator boundary of solar proton influx generally follows an L value contour and these contours will assist the viewer in extrapolating the boundary of solar proton influx to all longitudes.
	www.sec.noaa.gov /tiger/SolarProtons.html (716 words)

	The Book of THoTH (Leaves of Wisdom) - Solar radiation
		Solar radiation is commonly measured with a pyranometer or pyrheliometer.
		The solar constant is the amount of incoming solar radiation per unit area, measured on the outer surface of Earth's atmosphere, in a plane perpendicular to the rays.
		Hence, the average incoming solar radiation (known as "insolation") is one fourth the solar constant or ~342 W/m².
	www.book-of-thoth.com /thebook/index.php/Solar_radiation (747 words)

	Technology
		Without the solar proton events, the degradation would have been approximately 10% due to the generally constant cosmic-ray background rates found at the satellite's location at the 'L1' point.
		Solar panel are oversized at launch by 25% to allow for this loss of power at the end of the mission lifetime.
		Their press release for December 9, 2003 announced that the satellite was not affected by the particles and radiation events associated with the late-October 2003 storms.
	www.solarstorms.org /Svulnerability.html (2376 words)

	Help: Solar proton models (Site not responding. Last check: 2007-11-06)
		The prediction period used for the proton models is the total mission length.
		The upper limit depends on the selected model; for the ESP worst case event model, the value 100% is allowed: it corresponds to an upper limit that is consistent with long-term historical evidence.
		Solar proton fluences are shielded by the Earth's magnetic field.
	www.spenvis.oma.be /spenvis/help/models/sep.html (575 words)

	EO Study: A Violent Sun Affects Earth's Ozone
		This shower of protons, known by solar science insiders as the Bastille Day event, was the third largest of its kind in the last 30 years.
		Based on his prior experience with protons and ozone, when the solar storm broke on July 14 and Jackman saw the huge proton fluxes measured by another NOAA satellite, he says that he knew right away this was a unique opportunity to gather data.
		The sudden onset of a high energy proton blast from a solar flare is captured by the Large Angle Spectrometric Coronagraph (LASCO) C3 instrument on board the Solar and Heliospheric Observatory (SOHO) on July 14, 2000.
	earthobservatory.nasa.gov /Study/ProtonOzone (1757 words)

	Help: Solar proton models (Site not responding. Last check: 2007-11-06)
		The proton events considered in the JPL models are defined as the total fluence occurring over series of days during which the proton fluence exceeded a selected threshold.
		Solar proton event data from the last 3 complete solar cycles (20-22) were processed to obtain the event fluences.
		In identifying events, the practice of NOAA was followed, where the beginning and end of an event are identified by a threshold proton flux so that a large event may consist of several successive rises and falls in flux.
	www.spenvis.oma.be /spenvis/help/background/flare/flare.html (6658 words)

	Solar Storms Help Destroy The Ozone Layer: Study
		The sudden onset of a high energy proton blast from a solar flare is captured by the LASCO C3 instrument on board SOHO on July 14, 2000.
		NASA researchers used satellites to examine the impact on the northern hemisphere of solar explosions that sent positively-charged protons streaming to earth between July 14 to 16 2000, in what scientists called the third largest "solar proton event" in 30 years.
		The solar protons also break the atmosphere's water vapor molecules into hydrogen oxides which can destroy up to 70 percent of the ozone in the middle mesosphere, located from 50 to 90 kilometers (30 to 55 miles) of altitude.
	www.spacedaily.com /news/solarstorm-01a.html (517 words)

	spe9711 (Site not responding. Last check: 2007-11-06)
		For the first time such events were captured by the "new generation"of spacecraft, including SOHO and a number of other spacecraft whose results are rapidly available on the WWW.
		The right-hand picture is from an orbit during the solar proton event, showing the increased number of tracks.
		This event is directly correlatable with the gigantic solar flare on 6/11/97 as it occurred near the peak of its activity as seen in the Goes data.
	space-env.esa.int /External/spe9711 (1362 words)

	Solar activity harms the Ozone Layer ?
		A solar flare with an associated coronal mass ejection sent positively charged protons streaming to Earth from July 14 to 16, 2000.
		The bombardment of protons, called a solar proton event, was the third largest in the last 30 years.
		While the solar event's impact on humans was negligible, it helped scientists verify their computer models.
	www.crawford2000.co.uk /ozone.htm (686 words)

	Scientific FrontLine by SFL ORG. News Center / Protons from the Sun: What You Can't See Can Hurt You in Space
		Solar storms can sometimes make big parts of interplanetary space fill up with fast protons called a solar "proton event." Solar proton events are the most dangerous space weather event.
		Whenever there is a big proton event, the astronauts in the International Space Station hurry to a specially protected part of the station for safety.
		Solar storm specialists, who receive data from GOES round the clock at the NOAA Space Environment Center in Boulder, Colorado, immediately send a proton storm warning to the Spitzer Flight Control Engineer on duty at the Jet Propulsion Laboratory (JPL), in Pasadena, California.
	www.sflorg.com /spacenews/sn072606_04.html (1537 words)

	NASA Goddard scientists present new results at Fall AGU meeting
		The ability of dust to absorb solar radiation and heat the atmosphere is one of the main uncertainties in climate modeling and the prediction of climate change.
		A large solar flare with an associated coronal mass ejection occurred in mid-July and caused a very large solar proton event at the earth between July 14-16, 2000.
		The solar proton fluxes were measured by instruments aboard the GOES-10 satellite and used in our proton energy deposition model to help quantify the energy input to the middle atmosphere during this large solar event.
	www.eurekalert.org /pub_releases/2000-12/NSFC-NGsp-1312100.php (490 words)

	Spaceflight Now \| Breaking News \| Stormy space weather takes a toll on Earth's ozone
		A solar flare with an associated coronal mass ejection sent positively-charged protons streaming to Earth from July 14 to 16th, 2000.
		The sudden onset of a high energy proton blast from a solar flare is captured by the LASCO C3 instrument on board the SOHO spacecraft on July 14, 2000.
		Solar storms consist of coronal mass ejections and solar flares.
	www.spaceflightnow.com /news/n0108/10solar (995 words)

	Space Radiation Storm
		This SOHO animation of the July 14th X-class solar flare was recorded by the spacecraft's Extreme-ultraviolet Imaging Telescope at 195 angstroms.
		The wave of solar particles - known as a solar proton event - is already four times more intense than any other event detected since the launches of SOHO in 1995 and ACE in 1997.
		Soon after the solar flare, which occurred at 1024 UT (6:24 a.m EDT), coronagraphs on board the ESA/NASA Solar and Heliospheric Observatory recorded a "full-halo" coronal mass ejection (CME).
	science.nasa.gov /headlines/y2000/ast14jul_2m.htm (1189 words)

	ISTP Sun-Earth Connections Event: September 24- (Site not responding. Last check: 2007-11-06)
		The event was associated with active region number 8088 and a coronal shock wave was observed propagating across the solar disk in EIT.
		The solar flares that have been observed were one Class C and two Class M. The flare scale is based on the intensity of x-rays from the sun.
		The solar proton radiation event as measured in space near the Earth was almost undetectable.
	www-spof.gsfc.nasa.gov /istp/events/sept97 (948 words)

	Space Weather (Site not responding. Last check: 2007-11-06)
		High energy protons penetrate the Earth's magnetic field in the polar regions, crash into atmospheric particles and produce ion and electron pairs that temporarily increase the density in the lowest regions of the ionosphere.
		Solar protons are accelerated to very high velocities in the explosive release of energy associated with a solar flare.
		The flare particles, blown out at the limb of the Sun, arrive more rapidly and in greater numbers (flux is almost 10 times higher) than those that began their journey from the center of the solar disk.
	www.windows.ucar.edu /spaceweather/build_storm2.html (351 words)

	Primer on the Solar Space Environment
		Solar prominences (seen as dark filaments on the disk) are usually quiescent clouds of solar material held above the solar surface by magnetic fields.
		The outer solar atmosphere, the corona, is structured by strong magnetic fields.
		During a geomagnetic storm, portions of the solar wind's energy is transferred to the magnetosphere, causing Earth's magnetic field to change rapidly in direction and intensity and energize the particle populations within it.
	www.sec.noaa.gov /primer/primer.html (3116 words)

	Space Radiation Environmental Effects
		For protons there is a systematic increase in the L value at which the proton flux peaks for lower energy protons (e.g.
		During large solar events or magnetic storms, magnetic field lines are compressed allowing cosmic and solar particles to penetrate lower altitudes and inclinations.
		The solar protons are energetic (10 MeV to 1 GeV).
	www.eas.asu.edu /~holbert/eee460/spacerad.html (2059 words)

	Data Mining in Astrophysics
		Prediction of solar activity with a neural network and its effect on orbit prediction.
		A neural network study of the mapping from solar magnetic fields to the daily average solar wind velocity.
		Geomagnetic storm predictions from solar wind data with the use of dynamic neural networks.
	www.cs.queensu.ca /home/mcconell/DMAstroSolar.html (870 words)

	ISTP Sun-Earth Connections Events: July 2000
		The particles were produced by an intense solar flare and by an accompanying explosion of solar plasma, known as a coronal mass ejection.
		The measured speed averaged through 4 points in both the C2 and the C3 field before saturation from particles was 1775 km/sec at PA 262 (SW limb).
		This speed may not be accurate due to limitations of the level of the Proton event in view.
	www-istp.gsfc.nasa.gov /istp/events/2000july14 (2250 words)

	Federal Aviation Administration - OAM Technical Reports
		A Monte Carlo particle transport code was used to estimate the fluences of secondary particles (protons, neutrons, pions, kaons, photons, electrons, and muons) in selected energy ranges at specific altitudes.
		Effective dose rates from solar-proton-induced ionizing radiation in the earth's atmosphere at high geomagnetic latitudes were calculated for the solar proton event of 20 January 2005.
		The event started at 06:50 Universal Time, and within 5 minutes, dose rates at 60,000, 40,000, and 30,000 ft (relative to mean sea level) reached maximum values of: 140, 55, and 21 microsieverts per hour, respectively.
	www.faa.gov /library/reports/medical/oamtechreports/2000s/2005/0514 (233 words)

	Solar Proton Events, 1976 - present
		The >10 MeV protons peaked at 1860 pfu at 20/0810 UTC.
		Compare the amazing proton events of 1989 October with the proton storm of 1997 November.
		SESC defines the start of a proton event to be the first of 3 consecutive data points with fluxes greater than or equal to 10 pfu.
	umbra.nascom.nasa.gov /SEP/seps.html (387 words)

	Space Weather (Site not responding. Last check: 2007-11-06)
		Less than 2 hours later (~13:30 hrs UT), the protons arrived at Earth, and blasted the SOHO spacecraft instruments producing a false signal like "snow" in the images and disrupting their normally clear view of the sun.
		Xrays are the first warning of a solar disturbance in progress.
		A warning of a solar proton event in progress was issued by the Space Environment Center
	www.windows.ucar.edu /tour/link=/spaceweather/SOHO_proton_event.html (201 words)

	Northern hemisphere atmospheric effects due to the July 2000 solar proton event
		The third largest solar proton event in the past thirty years took place during July 14–16, 2000, and had a significant impact on the earth’s atmosphere.
		The observations constitute a dramatic confirmation of the impact of a large particle event in the control of ozone in the polar middle atmosphere and offer the opportunity to test theories of constituent changes driven by particle precipitation.
		Citation: Jackman, C. McPeters, G. Labow, E. Fleming, C. Praderas, and J. Russell (2001), Northern hemisphere atmospheric effects due to the July 2000 solar proton event, Geophys.
	www.agu.org /pubs/crossref/2001/2001GL013221.shtml (289 words)

	SolarNews July 1992
		The proton event reached a maximum of 4600 pfu at 09/2100 UT at energies greater than 10 MeV, making this event the largest since March 1991.
		The Committee on Solar and Space Physics (CSSP) of the Space Studies Board and the Committee on Solar Terrestrial Research (CSTR) of the Board on Atmospheric Sciences and Climate are embarking on an effort to generate an updated and prioritized set of scientific objectives for the next generation of research in our field.
		Comparative solar system environments: the atmospheres, ionospheres, and magnetospheres of the planets, planetary satellites, comets/asteroids, and the Sun and their interactions with their environments (e.g., with the solar wind or with the very local interstellar medium).
	helios.tuc.noao.edu /SolarNews/1992/07_92.html (2234 words)

	Modeling a large solar proton event in the southern polar atmosphere
		Comparing the change in amplitude of NPM at Halley during the SPE with the GOES satellite proton flux measurements, we observe a good correlation and thus conclude that the variability observed in the VLF data is primarily caused by >50 MeV proton fluxes.
		This suggests that the SPE produced ionization dominates all other precipitation sources at these altitudes during 4 and 5 November 2001.
		Our work strongly suggests that VLF subionospheric propagation is a reliable tool for the study of SPEs and that it is particularly effective when used in conjunction with an atmospheric model such as SIC.
	www.agu.org /pubs/crossref/2005/2004JA010922.shtml (439 words)

	NASA SEE TWG-Ionizing Radiation Environment-Related Publications (Site not responding. Last check: 2007-11-06)
		Abstract: The effects that solar proton events have on microelectronics and solar arrays are important considerations for spacecraft in geostationary and polar orbits and for interplanetary missions.
		This includes the cumulative fluence over the course of a mission, the fluence of a worst-case event during a mission, the frequency distribution of event fluences, and the frequency distribution of large peak fluxes.
		This model is called the Emission of Solar Protons (ESP) model.
	see.msfc.nasa.gov /ire/irepub.htm (1430 words)

	ISTP Sun-Earth Connections Event Solar Observations
		It was difficult to determine the speed of the CME because the relative angle of propagation was probably very close to the equatorial plane.
		At a speed of 450 km/sec, the CME would reach L1 in 3 3/4 days, or around 10 UT on January 10.
		On January 10, the Celias MTOF Proton Monitor (XGSM ~230 Re) observed the in-situ changes in the solar wind parameters.
	umbra.nascom.nasa.gov /istp/cloud_event.html (675 words)

	Spitzer Feature: Protons from the Sun: What You Can't See Can Hurt You in Space (Site not responding. Last check: 2007-11-06)
		Astronomers estimate that there are approximately 1,000,000,000,000,000,000,000,000,000,000,000,000,000,000,000,000,000,000,000 protons living in the Sun.
		They send out immediate warnings to the world whenever dangerous solar events are detected or predicted, and even have a web site at www.sec.noaa.gov.
		This website is maintained by the Spitzer Science Center, located on the campus of the California Institute of Technology and part of NASA's Infrared Processing and Analysis Center.
	www.spitzer.caltech.edu /features/articles/20060726.shtml (1590 words)

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