BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Time Scales of Hard X-ray Emission of Large Proton Flares DTSTART;VALUE=DATE-TIME:20070704T133000Z DTEND;VALUE=DATE-TIME:20070704T134200Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-188@cern.ch DESCRIPTION:Speakers: Dr. STRUMINSKY\, Alexei (Space Research Institute)\n The hard X-ray (>150 keV\, ACS SPI) emission during the X-class solar flar es of \n2006\nDecember 5 and 6 lasted about 5 and 15 min respectively and the time profiles \nshow\nseveral distinct peaks of about 1-2 min. If the time-profiles are plotted relatively\nthe onset of 15.4 GHz radio emission \, then the hard X-ray emission of the \nDecember 6\nevent would be delaye d by 4 minutes in comparison with the December 5 \nevent\, so peaks\nof th e two events are not overlapped. From the first look the flash-phase of \n these\nflares is formed by several acts of energy release\, which differ b y features of the\nsoft (1-8 Å\, GOES) and hard X-ray ranges\, as well as at radio frequencies from \n245\nMHz to 15.4 GHz. Comparison with the har d X-ray time profile of the 2003 \nOctober 28\nevent shows that the emissi on of the December 5 event corresponds to the A \nand B\nphases defined by Kiener et al. (2006)\, but to the C phase in a case of the \nDecember\n6. The dominant hard X-ray emission during the C phase also has been \nobser ved in the\nsolar flare of 2005 September 7 and might be considered as a f eature of \neffective\nproton acceleration. These observations would be di scussed in order to \nunderstand\nprocesses of solar proton acceleration a nd release into the interplanetary \nspace.\n\nhttps://indico.nucleares.un am.mx/event/4/session/11/contribution/188 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/188 END:VEVENT BEGIN:VEVENT SUMMARY:The extended inverse-Compton gamma-ray emission from the Sun seen by EGRET DTSTART;VALUE=DATE-TIME:20070704T134200Z DTEND;VALUE=DATE-TIME:20070704T135400Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-600@cern.ch DESCRIPTION:Speakers: Mrs. ORLANDO\, Elena (MPE Garching)\nWe study the Su n as an extended source of gamma-ray\nemission\, produced by\ninverse-Comp ton scattering of cosmic-ray electrons with the\nsolar radiation. This\ne mission contributes to the diffuse gamma-ray background\neven at large ang ular\ndistances from the Sun. While this emission is expected to\nbe read ily detectable by\nthe upcoming gamma-ray satellite GLAST\, the situation for\navailable EGRET data is\nmore challenging. Analyzing the EGRET data base\, we find\nclear evidence for the\nemission from the Sun and its vici nity\, compatible with our\npredictions. The model\nfor solar gamma-ray pr oduction has been implemented taking\ninto account the the solar\nmodulati on of cosmic-ray electrons\, and observations of this\nprocess are promisi ng to\nstudy the solar modulation of electrons as a function of\ndistance from the Sun.\n\nhttps://indico.nucleares.unam.mx/event/4/session/11/contr ibution/600 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/600 END:VEVENT BEGIN:VEVENT SUMMARY:The High Energy Photons Emission from Solar Flares observed by SZ2 -XD DTSTART;VALUE=DATE-TIME:20070704T135400Z DTEND;VALUE=DATE-TIME:20070704T140600Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-973@cern.ch DESCRIPTION:Speakers: Prof. WANG\, Huanyu (Institute of High Energy Physic s\, China)\nThe spectra and light curve of near a hundred Solar X-ray Flar e events\, which \nwere observed by SZ2/XD in the energy band of 10-800 ke V during 2001\, have \nbeen investigated. The events covered from C to X-c lass flares\, which are \nshown different characters of high energy photon s emission. The results will be \npresented in this paper. The discussions will be made especially for 3 of the \nbrightest X-class solar flares SF0 10402(X20)\,SF010406(X5.6) and SF010415\n(X14.4\, a GLE event).\n\nhttps:/ /indico.nucleares.unam.mx/event/4/session/11/contribution/973 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/973 END:VEVENT BEGIN:VEVENT SUMMARY:Study of the 28 October 2003 solar flare by means of 2.223 MeV gam ma-emisiion from it DTSTART;VALUE=DATE-TIME:20070704T140600Z DTEND;VALUE=DATE-TIME:20070704T141800Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-1071@cern.ch DESCRIPTION:Speakers: Dr. MIROSHNICHENKO\, Leonty (Instituto de Geofísica \, UNAM\, C.U.\, Coyoacán\, 04510\, México\, D.F.\, México\; Pushkov I nstitute IZMIRAN\, Troitsk\, Moscow Region\, 142190\, Russia)\nWe have stu died some characteristics of solar flares and surrounding medium (solar\np lasma) by means of 2.223 MeV line time profile of gamma-emission from neut ron\ncaptures by hydrogen nuclei. It was composed the code with making all owance for the\nmain processes of neutron interactions and deceleration in the solar atmosphere\,\ncharacter of neutron source\, losses of neutrons and density model of the solar\natmosphere. The method allowed us to revea l a density enhancement in the photosphere\nor subphotospheric layers for three gamma-flares. In the case of 16 December 1988\ngamma-flare we also f ound a hardening of charged particles spectrum with the time of\nthe decay of gamma-ray flux. In the present work we apply the same method to\ninves tigate the 28 October 2003 solar flare of X17.2/4B importance with coordin ates\nS16E08 and present the results for this powerful and long-duration f lare. The data on\n2.223 MeV gamma emission from INTEGRAL are used.\n\nhtt ps://indico.nucleares.unam.mx/event/4/session/11/contribution/1071 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/1071 END:VEVENT BEGIN:VEVENT SUMMARY:Ion acceleration and neutral emission mechanisms for 2005 Septembe r 7 flare DTSTART;VALUE=DATE-TIME:20070704T141800Z DTEND;VALUE=DATE-TIME:20070704T143000Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-374@cern.ch DESCRIPTION:Speakers: Dr. WATANABE\, Kyoko (Space Sciences Laboratory\, Un iversity of California\, Berkeley\, 7 Gauss Way\, Berkeley\, CA 94720\, U. S.A.)\nIn association with an X17.0 flare on 2005 September 7\, strong neu tral \nemissions were detected both in space and on the ground. In space\, intense \nemissions of gamma-rays were registered by INTEGRAL and by RHES SI during \nthe decay phase. Gamma-ray lines at 0.511\, 2.2\, 4.4\, and 6. 1 MeV were \nobserved and there was evidence for pion-decay radiation. On the ground\, \nrelativistic neutrons were observed by the neutron monitors at Mt. Chacaltaya \nand Mexico City and by the solar neutron telescopes a t Chacaltaya and Mt. \nSierra Negra. The neutron signal continued for more than 20 minutes with high \nstatistical significance. The long decay of t he signals suggests that ions were \ncontinuously accelerated or trapped i n the emission site. We also find that \ngamma-rays were emitted over a co rresponding extended period. Only when \nwe in cooperate the high-energy g amma-ray emission time history can we \nexplain the long-lasting neutron e mission. We also use the Hua et al. (2002) \nsolar-flare magnetic loop tra nsport and interaction model to find the best model \nto explain the data. \n\nhttps://indico.nucleares.unam.mx/event/4/session/11/contribution/374 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/374 END:VEVENT BEGIN:VEVENT SUMMARY:Emission profile of solar neutrons obtained from the ground-based observations for the 7 September 2005 event DTSTART;VALUE=DATE-TIME:20070704T143000Z DTEND;VALUE=DATE-TIME:20070704T144200Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-912@cern.ch DESCRIPTION:Speakers: Dr. SAKO\, Takashi (Solar-Terrestrial Environment La boratory\, Nagoya University)\nStrong signals of energetic neutrons associ ated with the solar flare of 7 \nSeptember 2005 were detected by using the Solar Neutron Telescopes located at \nMt. Chacaltaya in Bolivia and Mt. S ierra Negra in Mexico\, Neutron Monitors \nlocated at Mt. Chacartaya and M exico City. The observed profiles\nindicate a continuous emission of neut rons. In this paper\, we present the\nresults of combined analysis of the SNT and NM data to obtain emission profile\nand spectrum of the neutrons. Especially the SNT data of the different\nenergy threshold gives an unpr ecedented capability of the analysis.\nWe also discuss an association with the electromagnetic radiations and neutron \nemission models.\n\nhttps:// indico.nucleares.unam.mx/event/4/session/11/contribution/912 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/912 END:VEVENT BEGIN:VEVENT SUMMARY:Search for solar neutrons associated with series of X-class flares during the declining period of solar cycle 23 DTSTART;VALUE=DATE-TIME:20070704T144200Z DTEND;VALUE=DATE-TIME:20070704T145400Z DTSTAMP;VALUE=DATE-TIME:20261008T032207Z UID:indico-contribution-11-0-191@cern.ch DESCRIPTION:Speakers: Dr. MATSUBARA\, Yutaka (Solar-Terrestrial Environmen t Laboratory\, Nagoya University)\nIt was surprising that Gigantic solar f lares exceeding X-class occurred 10 times \nin September\, 2005\, because the activity of the Sun had already been in the \ndeclining period. More s urprisingly\, 4 X-class solar flares occurred in December\, \n2006\, when the activity of the Sun was at the minimum. It is expected that \nsome of these flares were accompanied by the acceleration of ions\, which \nwould be observed as solar neutrons or GLEs on the ground. Solar neutron \nteles copes\, which are dedicated to observe solar neutrons and to measure \nthe ir energies\, have been operating during solar cycle 23. Distributed in a \nworldwide network covering all longitudes they watch the Sun 24 hours a day. \nIn this paper\, we report on results of the search for solar neutro n events \nassociated with these 14 X-class flares\, using data obtained b y this \ninternational network of solar neutron telescopes. There was no c lear evidence \nfor detecting solar neutrons within these periods\, except for the significant \ndetection of solar neutrons on September 7\, 2005. Details of this particular \nevent will be presented by Sako et al. during this Conference.\n\nhttps://indico.nucleares.unam.mx/event/4/session/11/c ontribution/191 LOCATION:Merida\, Mexico Yucatan I (Fiesta Americana) URL:https://indico.nucleares.unam.mx/event/4/session/11/contribution/191 END:VEVENT END:VCALENDAR