SH52A-0905 

Charge states of energetic tellurium ions: Equilibrium and non-equilibrium calculations

Kartavykh, Y (julia.jarc@mail.ioffe.ru), Ioffe Physical-Technical Institute, Polytechnicheskaya 21, St. Petersburg, 194021, Russian Federation Droege, W (Wolfgang.Droege@astro.uni-wuerzburg.de), Institut fuer Theoretische Physik und Astrophysik, Universiteat Wuerzburg, Institut fuer Theoretische Physik und Astrophysik, Universiteat Wuerzburg, Wuerzburg, 97074, Germany * Klecker, B (berndt.klecker@mpe.mpg.de), Max-Planck-Institut feur Extraterrestrische Physik, Garching, Max-Planck-Institut feur Extraterrestrische Physik, Garching, Garching, 85741, Germany Kocharov, L (kocharov@utu.fi), Department of Physics, University of Turku, Department of Physics, University of Turku, Turku, 20014, Finland Moebius, E (Eberhard.Moebius@unh.edu), Space Science Center and Department of Physics, University of New Hampshire, Morse Hall, 39 College Road, Durham, NH 03824,

Recently, very high abundances of ultraheavy ions were observed in impulsive SEP events, compared to coronal abundances with enrichment factors of >100 for atomic mass > 100 amu. Because wave/particle interaction processes, as discussed for heavy ion enrichment and acceleration, depend critically on the mass per charge (M/Q) of the ions, an estimate of the ionic charge is very important for model calculations. In any realistic acceleration model one would have to use the ionization and recombination rates of these ions as a function of energy, because charge changing processes in the solar corona are inevitable and energy dependent. As an example of high mass ions, we calculate the equilibrium and non-equilibrium charge states for tellurium ions (Te, nuclear charge 52), and present a method to estimate the cross sections and rates for ionization and recombination of ions with arbitrary nuclear charge Z and atomic mass number A.

SH52A-0906 

An Overview of SAMPEX/MAST Measurements of High Energy Ionic Charge States in Gradual Solar Energetic Particle Events

* Labrador, A W (labrador@srl.caltech.edu), California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125, United States Leske, R A (ral@srl.caltech.edu), California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125, United States Cohen, C M (cohen@srl.caltech.edu), California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125, United States Mewaldt, R A (rmewaldt@srl.caltech.edu), California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125, United States Stone, E C (ecs@srl.caltech.edu), California Institute of Technology, Mail Code 220-47, Pasadena, CA 91125, United States von Rosenvinge, T T (tycho@milkyway.gsfc.nasa.gov), NASA/Goddard Space Flight Center, Code 661, Greenbelt, MD 20771, United States

The MAST experiment aboard SAMPEX employs a geomagnetic rigidity filter technique to yield measurements of mean ionic charge states in large solar energetic particle events. Elements measured include N, O, Ne, Mg, Si, and Fe, with energies of 15-60 MeV/nuc (N, O, Ne), 20-60 MeV/nuc (Mg, Si), and 25-90 MeV/nuc (Fe). These measurements, extending from 1992 to 2006, remain the highest energy direct measurements of mean ionic charge states in SEP events, overlapping ACE and STEREO measurements in energy. The measured charge states are probes of source materials and conditions of particle transport and are useful in multi-spacecraft studies of large SEP events. Iron charge states measured by MAST range from ~+10 to ~+22 in various SEP events, corresponding to plasma temperatures from ~1.5 MK to ~16 MK and indicating the possible presence of flare material in some of these events. In this poster, we will review the current state of the charge states analysis, including development of the analysis technique and extension of the analysis to new events, such as the December 2006 large SEP events and other previously unanalyzed SEP events selected with the help of ACE/SIS fluence data. We will also show Q(Fe) correlation with ACE/SIS Fe/O ratios in the same energy ranges.

SH52A-0907 

Charge States of Ions, Accelerated by a Turbulent Shock Waves

* Sokolov, I (igorsok@umich.edu), University of Michigan, 2455 Hayward Str., Ann Arbor, MI 48109, United States

Diffisive-shock acceleration of ions is discussed. The shock wave dynamics is taken from the simulation of the coronal mass ejection event of April, 21, 2002. A self-consistent model is used for the turbulence generated by upstreaming accelerated protons. The acceleration of ions at different charge states is studied. Because of the ion cyclotron frequency dependence on the charge state, the resonance condition for ions occurs at different wavelength of the turbulence spectrum, for a given ion energy. That is why the acceleration efficiency depends on the ion electric charge.

SH52A-0908 

Ion acceleration and neutral emission mechanisms for 2005 September 7 flare

* Watanabe, K (kwatana@ssl.berkeley.edu), Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720, United States Lin, R P (rlin@ssl.berkeley.edu), Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720, United States Krucker, S (krucker@ssl.berkeley.edu), Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720, United States Murphy, R J (murphy@ssd5.nrl.navy.mil), Naval Research Laboratory, 4555 Overlook Avenue, SW, Code 7600A, Washington, DC 20375, United States Share, G H (share@ssd5.nrl.navy.mil), Department of Astronomy, University of Maryland, College Park, MD 20742, United States Harris, M J (harris@csnsm.in2p3.fr), Max Planck Institut fur extraterrestrische Physik, Postfach 1312, Garching, D-85741, Germany Gros, M (maurice.gros@cea.fr), DSM/DAPNIA/SAp, CEA Saclay, 91191, Gif-sur-Yvette, 91191, France Sako, T (sako@stelab.nagoya-u.ac.jp), Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, 464-8601, Japan Muraki, Y (muraki@center.konan-u.ac.jp), Konan University, Nada-ku, Kobe, 657-0000, Japan

In association with an X17.0 flare on 2005 September 7, strong neutral emissions were detected both in space and on the ground. In space, intense emissions of gamma-rays were registered by INTEGRAL and by RHESSI during the decay phase. Gamma-ray lines at 0.511, 2.2, 4.4, and 6.1 MeV were observed and there was evidence for pion-decay radiation. On the ground, relativistic neutrons were observed by the neutron monitors at Mt. Chacaltaya and Mexico City and by the solar neutron telescopes at Chacaltaya and Mt. Sierra Negra. The neutron signal continued for more than 20 minutes with high statistical significance. The long decay of the signals suggests that ions were continuously accelerated or trapped in the emission site. We also find that gamma-rays were emitted over a corresponding extended period. Only when we in cooperate the high-energy gamma-ray emission time history can we explain the long-lasting neutron emission. We also use the Hua et al. (2002) solar- flare magnetic loop transport and interaction model to find the best model to explain the data.

Author(s) (2007), Title, Eos Trans. AGU, 88(52), Fall Meet. Suppl., Abstract #####-##.