People who have signed up for the workshop


Id:  1
First Name:Hugh
Last Names:Hudson
Affiliation:UCB
Address:SSL, 7 Gauss Way, Berkeley, CA, 94720-, United States
Telephone:510-643-0333
Email:none
Student:no
Paper Title:Oscillations and shocks
Author List:H. Hudson, A. Warmuth
Abstract:We note the strong association of type II bursts with the loop oscillations detected by TRACE.
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000001 (2004-08-02 18:21:43), 0042000002 (2004-08-02 18:21:43), 0042000062 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  2
First Name:Gordon
Last Names:Emslie
Affiliation:Oklahoma State University
Address:Department of Physics, Stillwater, OK, 74078, USA
Telephone:405-744-6368
Email:none
Student:no
Paper Title:Global Energetics Synthesis
Author List:Emslie, G., Vourlidas, A., et al.
Abstract:Leader of Group 8 on Global energetics. Will identify events to study and construct energetics of various components (CME, nonthermal particles, etc.)
Poster:No
Group:8. Global energetics
ApplicationRequestIDs:0042000003 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  3
First Name:Mandy
Last Names:Hagenaar
Affiliation:
Address:, , , , 
Telephone:650-354-5313
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000004 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  4
First Name:Rudolf
Last Names:Komm
Affiliation:National Solar Observatory
Address:950 N. Cherry Ave., Tucson, AZ, 85719, USA
Telephone:520-318-8428
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000005 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  5
First Name:Astrid
Last Names:Veronig
Affiliation:Institute for Geophysics, Astrophysics and Meteorology, University of Graz
Address:Universitatsplatz 5, Graz, , A-8010, Austria
Telephone:++43 316 380 8609
Email:none
Student:no
Paper Title:The Neupert effect: Comparison of data and theory
Author List:Veronig, A., Brown, J.C., Dennis, B.R., Schwartz, R.A.,
Abstract:I have recently worked on testing the Neupert effect using RHESSI and GOES flare observations. A simple model on the flare energy budget was derived (including nonthermal energy in electrons, the thermal energy in the plasma as well as estimates of conductive and radiative cooling losses) and compared with observations. This kind of analysis could be applied to other flares in order to get an idea on the thermal/nonthermal energy fractions. It would be definitely helpful to have also additional information from other instruments on the flare geometry/size and thermal plasma parameters.
Poster:No
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000006 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  6
First Name:Marian
Last Names:Karlicky
Affiliation:Astonomical Institute, Academy of Sciences
Address:Astronomical Institute, Ondrejov, , 251 65, Czech Republic
Telephone:420-323-620356
Email:none
Student:no
Paper Title:Acceleration processes in a collapsing magnetic trap
Author List:Karlicky, M.
Abstract:We study the acceleration processes in a collapsing magnetic trap formed in the cusp structure of the flare model, using a test-particle numerical method. Coulomb collisions and scattering are included. It was found that if the trap collapse is sufficiently fast and the energies of the injected electrons are sufficiently high, electrons can be accelerated in this secondary acceleration process to very high energies. This process gives us a new possibility to explain the formation of loop-top sources observed in hard X-ray and radio emission.
Poster:Yes
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000007 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  7
First Name:Frantisek
Last Names:Farnik
Affiliation:Astronomical Institute, Academy of Sciences
Address:Ondrejov, Ondrejov, , 251 65, Czech Republic
Telephone:+420 323 620329
Email:none
Student:no
Paper Title:Reverse Drift Bursts in Radio Spectra above 1 GHz and their
Author List:Farnik, F. and Karlicky, M.
Abstract:In the study we compare radio emission of 7 flares with their hard X-ray emission. The selected flares belong to a group of flares which exhibit reverse drift bursts and, at the same time, were observed by RHESSI. These parallel observations enable us to search and describe relation between the two emissions.
Poster:Yes
Group:4. Flares without CMEs
ApplicationRequestIDs:0042000008 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  8
First Name:James
Last Names:McTiernan
Affiliation:Space Sciences Lab, Univ. of California
Address:7 Gauss Way, Berkeley, CA, 94720, USA
Telephone:510-643-9246
Email:none
Student:no
Paper Title:DEM models of Flare emission
Author List:McTiernan, J., Caspi, A., Hudson, H.
Abstract:We use data from RHESSI and other spacecraft (GOES, GOES-SXI, EIT, TRACE)to determine the characteristics of thermal emission during solar flares. Previous attempts to do this have been hampered by the assumption that flare thermal emission has a single temprature. We now have a method for calculating the differential emission measure for high temperature flare emission, while accounting for contamination of the spectrum due to the presence of nonthermal emission. This gives a more accurate measure of the amount of energy that is released into high temperature (3 to 20 MK) plasma.
Poster:Yes
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000009 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  9
First Name:Weiqun
Last Names:Gan
Affiliation:Purple Mountain Observatory
Address:West Beijing Road 2, Nanjing, Jiangsu, 210008, China
Telephone:86-25-83332178
Email:none
Student:no
Paper Title:TBD (Group 2 & 5)
Author List:W. Q. Gan
Abstract:I plan to submit two contributions which belong to group 2 and 5, respectively. I will let you know the titles some time later. In order to apply for the visa smoothly, I need an invitation letter from the LOC as early as possible.
Poster:No
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000010 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  10
First Name:Harry
Last Names:Warren
Affiliation:NRL
Address:4555 Overlook Ave, SW, Washington, DC, 20375, USA
Telephone:202-404-1453
Email:none
Student:no
Paper Title:Observation and Modeling of Thermal Flare Plasma
Author List:Warren, H. P.
Abstract:I am interested in the analysis and hydrodynamic modeling of the thermal plasma in large flares.
Poster:No
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000011 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  11
First Name:Thomas
Last Names:Metcalf
Affiliation:LMSAL
Address:3251 Hanover St., Dept. ADBS, Bldg. 252, Palo Alto, CA, 94304, USA
Telephone:650-424-2209
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000012 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  12
First Name:David
Last Names:Rust
Affiliation:JHU/APL
Address:11100 Johns Hopkins Rd., Laurel, MD, 20723, USA
Telephone:240-228-5414
Email:none
Student:no
Paper Title:Helicity Buildups and CMEs
Author List:Rust, D. M., LaBonte, B. J.
Abstract:Analysis of helicity flow through the photosphere into the corona and subsequent flare and CME activity.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000013 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  13
First Name:Petrus
Last Names:Martens
Affiliation:Montana State University
Address:EPS 237, Bozeman, MT, 59717, USA
Telephone:406-994-7049
Email:none
Student:no
Paper Title:Flare X-ray and EUV Emission Simulations
Author List:Trae Winter & Piet Martens
Abstract:We are developing a code to carry out a set of numerical simulations of solar flare non-thermal hard X-ray and thermal EUV and soft X-ray emission pertinent to RHESSI and TRACE flare observations. We are simulating the emissions fenerated by a variety of evolving magnetic field configurations and energy release mechanisms and will show our results at the Workshop.
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000014 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  14
First Name:Angelos
Last Names:Vourlidas
Affiliation:NRL
Address:4555 Overlook Ave, SW, Washington, DC, 20375, United States
Telephone:202-767-2800
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:8. Global energetics
ApplicationRequestIDs:0042000015 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  15
First Name:Nicole
Last Names:Vilmer
Affiliation:LESIA
Address:5 Place Janssen, Meudon, , 92195, France
Telephone:33-1-45077806
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000016 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  16
First Name:Cyril
Last Names:Dauphin
Affiliation:LESIA-Observatoire de Paris Meudon
Address:Observatoire de Paris Meudon LESIA F92190, Meudon, , 92190, France
Telephone:01 45 07 77 79
Email:none
Student:yes
Paper Title:
Author List:
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000017 (2004-08-02 18:21:43), 0042000120 (2004-08-22 21:19:05),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  17
First Name:Terry
Last Names:Forbes
Affiliation:University of New Hampshire
Address:EOS Inst. Morse Hall, 39 College Road, Durham, NH, 03824, USA
Telephone:603-862-3872
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000018 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  18
First Name:Karel
Last Names:Schrijver
Affiliation:LM Advanced Technology Center
Address:ADBS/B252, 3251 Hanover Street, Palo Alto, CA, 94304, USA
Telephone:650-424-2907
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000019 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  19
First Name:Sharad
Last Names:Kane
Affiliation:University of California, Berkeley
Address:4412 Fleetwood Road, Danville, CA, 94506, USA
Telephone:925-648-7317
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000020 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  20
First Name:Aleksey
Last Names:Golovko
Affiliation:Institute of Solar-Terrestrial Physics, Russian Academy of Sciences
Address:Lermontov St., 126, Irkutsk 33, Irkutsk, , 664033, Russia
Telephone:(3952) 427891
Email:none
Student:no
Paper Title:The fractal properties of active regions and their association with solar activity
Author List:I.I.Salakhutdinova, A.A.Golovko
Abstract:In this study we used H-alpha filtergrams of the Baikal observatory operated by ISTP SD RAS. The telescope is coupled with the Halle birefringent filter (0.05 nm bandpass, tunable). The Princeton Instruments 2048x2048 pixel CCD-camera with 16-bit amplitude resolution is used. We investigated the active region NOAA 9077 (July 2000) and complex of active regions NOAA 0050 and NOAA 0039 (July 2002). The method of structural functions was applied to obtain a number of characteristics of the chromospheric emission intensity field in the H-alpha line in the aforementioned active regions. A calculation of the parameters of the structural functions was performed in terms of Kolmogorov's theory of turbulence. The study revealed intervals of linear dependence of the structural functions on the scales of the field under consideration where a cascade redistribution of energy is taking place from larger to smaller scales. It is found that as solar activity progresses, the active region undergoes an intense structuring. This is associated with the development of an abundant multifractal structure. Fractal characteristics of the structural functions in this case undergo stepwise changes that come into play shortly before a next flare from among a cascade of flares preceding the main strong flare. Therein lies a possibility of predicting the flaring process.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000021 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  22
First Name:Richard
Last Names:Canfield
Affiliation:Montana State University
Address:Physics Department, Bozeman, MT, 59717-, USA
Telephone:406-994-5581
Email:none
Student:no
Paper Title:
Author List:
Abstract:My contribution will be to serve as co-leader of working group 1.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000023 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  23
First Name:Paolo
Last Names:Romano
Affiliation:Dipartimento di Fisica e Astronomia - Sezione Astrofisica
Address:Via S. Sofia 78, Catania, , 95125, Italy
Telephone:+390957332329
Email:none
Student:yes
Paper Title:Study of a twisted magnetic flux tube in an eruptive event
Author List:Romano, P., Contarino, L., Zuccarello, F.
Abstract:In the past many observations have shown sigmoidal structures (Canfield et al., 1999) and twisted flux ropes with a helical-like pattern of the magnetic field (Romano et al., 2003a), associated with eruptions of filaments. As demonstrated by Rust and Kumar (1994), a twisted flux rope will writhe and take on the S shape if the amount of twist in it exceeds the limit for the kink instability, which occurs when 2pTwR/L > 0.581, with Tw the number of turns of the magnetic field from end to end and 2R/L the ratio between the width and the length of the filament. There are some controversy about whether peculiar motions of shearing or emersion of twisted flux tubes are responsible of these unstable configurations (see, e.g., Romano et al., 2003b). In this context, we plan to investigate these two mechanisms, able to reach the limit for the kink instability, analysing the eruption of a reverse S shaped filament which preceded the onset of a flare of class X17.2, occurred in active region NOAA 10486 on October 28, 2003. Using H-alpha full-disc images taken at INAF-Catania Astrophysical Observatory we intend to measure the morphological parameters of the filament before its eruption. Using 1 minute cadence MDI full-disc longitudinal magnetograms taken about 24 hours before the event we plan to measure the rate of emergence of magnetic flux and the photospheric horizontal flows in all the active region and in areas corresponding to filament footpoints. We will compute the velocities using the local correlation tracking (LCT) method. Moreover, we will compute the magnetic helicity injected by the horizontal flows (Chae, 2001) in order to investigate a possible correlation between the magnetic helicity accumulated along the filament and its transformation from twist to writhe before the eruptive event. Canfield, R.C., Hudson, H.S., and McKenzie, D.E., Geophys. Res. Lett. , 26, 627, 1999. Chae, J., ApJ, 560, L95, 2001. Romano, P., Contarino, L., and Zuccarello, F. , Sol. Phys., 214, 313, 2003a. Romano, P., Contarino, L., and Zuccarello, F. , Sol. Phys., 218, 137, 2003b. Rust, D.M., and Kumar, A., Sol. Phys., 155, 69, 1994.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000024 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  24
First Name:Kanya
Last Names:Kusano
Affiliation:ADSM, Hiroshima University
Address:Kagamiyama 1-3-1, Higashi-Hiroshima, , 7398526, Japan
Telephone:+81824247016
Email:none
Student:no
Paper Title:Reversal of Magnetic Shear as a Trigger Mechanism of Solar Flares
Author List:K.Kusano, T.Maeshiro, T.Yokoyama, and T.Sakurai
Abstract:Based on the three-dimensional numerical simulations, we propose a new model of solar flare trigger mechanism, that the reversal of magnetic shear near magnetic neutral line may lead to the onset of solar flares. The simulation results clearly demonstrate that the resistive tearing mode instability slowly growing on the shear inversion layer can consequently cause the collapse of magnetic arcade and the sudden release of magnetic energy. Also the formation of sigmoid-like structure in pre-flare phase can be explained by this new model. The prediction of the model was carefully examined using the vector magnetograms observed by Solar Flare Telescope at National Astronomical Observatory in Japan.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000025 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  25
First Name:Michele
Last Names:Piana
Affiliation:Dipartimento di Matematica Universita di Genova
Address:Via Dodecaneso 35, Genova, , 16146, Italy
Telephone:+390103536816
Email:none
Student:no
Paper Title:Inversion methods for the analysis of RHESSI X-ray spectra under thermal conditions
Author List:Piana, M., Massone, A. M.
Abstract:Reconstruction of the differential emission measure under thermal condition by means of regularization methods formulated in appropriate function spaces and by using a generalized sampling theorem.
Poster:No
Group:8. Global energetics
ApplicationRequestIDs:0042000026 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  26
First Name:Anna Maria
Last Names:Massone
Affiliation:INFM, Unita di Ricerca di Genova
Address:Via Dodecaneso 33, Genova, , 16146, Italy
Telephone:+390103536607
Email:none
Student:no
Paper Title:Inversion methods for the analysis of RHESSI X-ray spectra under non-thermal conditions
Author List:Massone, A. M., Piana, M.
Abstract:Reconstruction of the mean electron flux spectra from RHESSI photon data by means of regularization techniques and by accounting for the angular dependence of the cross-section.
Poster:No
Group:8. Global energetics
ApplicationRequestIDs:0042000027 (2004-08-02 18:21:43), 0042000142 (2004-08-30 05:27:45),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  27
First Name:Brian
Last Names:Welsch
Affiliation:Space Sciences Laboratory
Address:7 Gauss way, Berkeley, CA, 94720, USA
Telephone:510-642-9650
Email:none
Student:no
Paper Title:Cancellation, Prominence Formation, and Eruptions
Author List:Welsch, B.T.
Abstract:Martin (1998) observed that the cancellation of photospheric magnetic flux (see, e.g., Chae et al., 2004) is omnipresent during the formation of prominences. In a series of MHD simulations of prominence formation, Welsch et al.(in prep.) found that the magnetic reconnection necessary to form prominences above the photosphere does not proceed efficiently without flux cancellation, which accords with Martin's observations. To illuminate the significance of flux cancellation in the formation of eruptive structures (if any), I report observed flux cancellation rates around the time of eruptions from AR's 8210 and 8038.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000028 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  28
First Name:Yong-Jae
Last Names:Moon
Affiliation:
Address:, , , , 
Telephone:82-42-865-324
Email:none
Student:no
Paper Title:Discussion on how to test the energy build-up process
Author List:Moon, Y.-J., Chae, J., Cho, K.-S.
Abstract:1. Flux change and its projection effect 2. Estimation of magnetic helicity estimation 3. Magnetic helicity budget for homologous events
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000029 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  29
First Name:Joel
Last Names:Allred
Affiliation:University of Washington
Address:Box 351560, Seattle, WA, 98195, USA
Telephone:206-616-1505
Email:none
Student:yes
Paper Title:Radiative Hydrodynamic Models of Solar Flares
Author List:Allred, J. C., Hawley, S. L.
Abstract:I will present on radiative hydrodynamic models of solar flares. The model atmosphere is heated by a beam of non-thermal electrons, and I will use RHESSI HXR spectra to obtain the energy distribution of the injected electron beam for particular flare events. The energy deposition rate will be calculated by numerically solving the Fokker-Planck equation. I will compare calculated white light emission with observations.
Poster:No
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000030 (2004-08-02 18:21:43), 0042000068 (2004-08-02 18:21:43), 0042000069 (2004-08-02 18:21:43), 0042000070 (2004-08-02 18:21:43), 0042000085 (2004-08-02 18:21:43), 0042000128 (2004-08-23 19:54:29), 0042000138 (2004-08-26 07:48:48),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  30
First Name:Stephane
Last Names:Regnier
Affiliation:ESTEC/ESA
Address:, , , , 
Telephone:(+31) (0&
Email:none
Student:no
Paper Title:
Author List:
Abstract:1- Magnetic energy build-up and photospheric motions 2- Eruptive events in AR 8210 3- Magnetic helicities: self, mutual and vacuum helicity
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000031 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  31
First Name:KyungSeok
Last Names:Cho
Affiliation:Korea Astronomy Observatory
Address:61-1, Whaam-dong, Yusong-gu, Daejeon, , 305-34, Korea
Telephone:+82-42-865
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000032 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  32
First Name:Tomohiro
Last Names:Maeshiro
Affiliation:
Address:Hiroshima University, Higashi-Hiroshima 739-8530, , , , Japan
Telephone:+81-82-424
Email:none
Student:yes
Paper Title:Relationship between pre-flare brightening and the shear structure of photospheric magnetic field
Author List:Maeshiro,T., Kusano,K., Yokoyama,T., Sakurai,T.
Abstract:Recently, Kusano et al. (2004, ApJ) proposed a new flare model, which explains the trigger process of solar flares as the nonlinear interaction between two reconnections initiated by the resistive tearing mode instability growing on the magnetic shear inversion layer. Aiming to examine their model, we carefully investigated the spatial correlation between the initial brightening of pre-flare events and the shear structure of magnetic field. We studied the GOES X-ray M3.2 and X2.3 class flares occurred in June 4 and 6, 2000, respectively, in NOAA 9026. TRACE 1600 images and the vector magnetograms observed by Solar Flare Telescope at Mitaka, Japan were used. We calculated the axial magnetic field, which is defined as the non-potential magnetic field component parallel to the vector potential, as an index of the magnetic shear strength, and compared the distribution of that with TRACE 1600 images. As a result, it was revealed that the initial brightening of TRACE 1600 images in the both flare events arose from a point where the magnetic neutral line intersected with the shear inversion line, where the sign of the axial field was steeply reversed. This result suggests the necessity of the magnetic shear reversal for the onset of solar flares, and are consistent with the prediction of the reversed-shear flare model.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000033 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  33
First Name:Lidia
Last Names:Contarino
Affiliation:Catania Astrophysical Observatory
Address:Via S. Sofia 78, Catania, , 95125, Italy
Telephone:+39 095 7332330
Email:none
Student:yes
Paper Title:Cancelling magnetic features and eruptive filaments
Author List:Contarino, L., Romano, P., Zuccarello, F.
Abstract:In the framework of the theories of low-lying magnetic reconnection (Litvinenko and Somov, 1994; Litvinenko and Martin, 1999), Ha brightening patches related to cancelling magnetic features, can be considered as indicators of the site of magnetic reconnection and interpreted as precursors of flares and/or coronal mass ejections. In a previus work , we have studied a filament eruption associated to a two-ribbon flare occurred in NOAA AR 9445 on May 5, 2001. It was evidenced that the filament eruption could be triggered by a low-lying reconnection process and that Ha brightening patchs appearing at the sites of cancelling magnetic features (CMF) could be indicative of the site where a slow energy release occured during the reconnection (Contarino et al. 2002). We plan to analyze CMFs (using high resolution magnetograms taken by MDI/SOHO, Ha and TRACE images) related to the evolution of eruptive filaments and use the model proposed by Litvinenko in order to compare the physical parameters of low-lying reconnection current sheets given in the model with the observed parameters of CMFs. References Litvinenko, Yu.E., Somov, B.V., Sol.Phys., 151, 265, 1994 Litvinenko, Yu.E., Martin, S.F., Sol.Phys., 190, 45, 1999 Contarino L., Romano P., Yurchyshyn V.B., Zuccarello F., Sol.Phys., 216, 173, 2003
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000034 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  34
First Name:Jane
Last Names:Noglik
Affiliation:UCLAN
Address:CFA, Dept. of Physics, Astronomy & Maths, University of Central Lancshire, Preston, Lancashire, PR1 2HE, United Kingdom
Telephone:07970508767
Email:none
Student:yes
Paper Title:Analysis of Post Flareloops for the Implication of a Magnetic Reconnection Rate
Author List:Noglik, J. B., Walsh, R. W., Ireland, J.
Abstract:High time resolution TRACE, EIT/SOHO and Yohkoh observations of a solar flare on 1999 March 18 have been investigated. The postflare loop was situated on the northeast solar limb. Allowing the expanding footpoints and the successive brightening of the arcade loops to be studied in order to find an indication of a possible magnetic reconnection rate.
Poster:Yes
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000035 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  35
First Name:George
Last Names:Fisher
Affiliation:UC Berkeley
Address:7 Gauss W ay, Space Sciences Lab #7450, Berkeley, CA, 94720-, USA
Telephone:510-642-8896
Email:none
Student:no
Paper Title:Modeling the Magnetic Evolution of Flaring and Eruptive Active Regions
Author List:Fisher, G. H., and the Solar MURI Team
Abstract:I will present an overview of the Solar MURI project, with an emphasis on numerical models of the evolution of active regions 8210 and 10486.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000036 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  36
First Name:Manolis K.
Last Names:Georgoulis
Affiliation:The Johns Hopkins University Applied Physics Laboratory
Address:11100 John Hopkins Rd., Laurel, MD, 20723, USA
Telephone:240-228-5508
Email:none
Student:no
Paper Title:A Two-Fold Approach in Estimating the Relative Magnetic Helicity in Solar Active Regions
Author List:Georgoulis, M. K., LaBonte, B. J., Rust, D. M.
Abstract:Using two new techniques, we can calculate both the magnetic helicity variations in the active region solar photosphere and a total magnetic helicity budget in solar active regions. The first technique assumes linear force-free magnetic fields and allows the evaluation of the relative magnetic helicity integral. The second technique finds a unique solution of the ideal MHD induction equation and, moreover, determines a field-aligned velocity field, thus reconstructing fully the velocity field vector in the active region solar photosphere. The latter method is completely disentangled from local correlation tracking (LCT) and, applied to vector magnetograms, allows the calculation of both the injected helicity and the helicity built-up by photospheric flows with an accuracy that cannot be matched by LCT. We apply the two helicity calculation techniques to vector magnetograms of flaring/CME-prolific active regions and to NOAA AR 8210 and we discuss the relation between the two types of results. We find that the two approaches are complementary and provide much needed insight into the energy release process and the triggering of coronal ejecta.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000037 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  37
First Name:Paulett
Last Names:Liewer
Affiliation:JPL
Address:MS 169-506, Pasadena, CA, 91109, United States
Telephone:818-354-6538
Email:none
Student:no
Paper Title:TBD
Author List:
Abstract:
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000038 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  38
First Name:Francesca
Last Names:Zuccarello
Affiliation:Department of Physics and Astronomy - University of Catania
Address:Via S. Sofia 78, Catania, , 95125, Italy
Telephone:+39 095 7332237
Email:none
Student:no
Paper Title:Multiwavelength analysis of flaring active regions during the pre-event phase
Author List:Zuccarello, F., Contarino, L., Romano, P.
Abstract:In previous works we have studied the role played by phenomena like cancelling magnetic features and magnetic helicity transport in eruptive prominences. These works were carried out using both ground based (THEMIS, BBSO, Catania Astrophysical Observatory) and space (TRACE, MDI/SOHO, YOHKOH) data. We have analysed these data using specific software which allowed us to determine the physical parameters relevant to the phenomena from the image analysis, to measure the rate of emergence of magnetic flux, to determine the magnetic helicity injected in corona by horizontal flows and, using the Local Correlation Tracking technique, to determine the horizontal velocity fields (Contarino et al. 2003; Romano et al., 2003a; Romano et al., 2003 b). We plan to utilize these methodologies to study the pre-event phase in active regions indicated in Working Group 1. Contarino L., Romano P., Zuccarello F. Yurchyshyn, V.B., Solar Phys., 216, 173, 2003 Romano P., Contarino L., Zuccarello F., Solar Phys., 214, 323, 2003a Romano P., Contarino L., Zuccarello F., Solar Phys., 218, 137, 2003b
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000039 (2004-08-02 18:21:43), 0042000083 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  39
First Name:Henry (Trae)
Last Names:Winter
Affiliation:Montana State University
Address:Department of Physics, EPS 264, MT, 59717-, USA
Telephone:406-994-7375
Email:none
Student:yes
Paper Title:Simulation of Flare Emission Signatures in RHESSI and TRACE
Author List:Winter, H.D., Martens, P.C.H.
Abstract:We are combining thermal and non-thermal numerical modeling codes in a consistent manner in order to produce theoretical flare emission under a variety of realistic solar conditions. The theoretical flare emission is then folded through the response functions of RHESSI and TRACE in order to provide theoretical data that can be compared to observational results. This will provide a means to test multiple flare models with observed flare behavior.
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000040 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  40
First Name:Dana
Last Names:Longcope
Affiliation:Montana State University
Address:Department of Physics, Bozeman, MT, 59717, USA
Telephone:406-994-7851
Email:none
Student:no
Paper Title:Inferring a photospheric velocity field from a sequence of vector magnetograms: The Minimum Energy Fit
Author List:Longcope, D. W.
Abstract:We introduce a technique for inferring a photospheric velocity from a sequence of vector magnetograms. The technique, called The Minimum Energy Fit, demands that the photospheric flow agree with the observed photospheric field evolution according to the magnetic induction equation. It selects, from all consistent flows, that with the smallest overall flow speed by demanding that it minimize an energy functional. Partial or imperfect velocity information, obtained independently, may be incorporated by demanding a velocity consistent with the induction equation which minimizes the squared difference with flow components otherwise known. The combination of low velocity and consistency with the induction equation are desirable when using the magnetogram data and associated flow as boundary conditions of a numerical simulation. The technique is tested on synthetic magnetograms generated by specified flow fields and shown to yield reasonable agreement. It also yields believable flows from magnetograms of NOAA AR8210 made with the Imaging Vector Magnetogram at the Mees Solar Observatory.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000041 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  41
First Name:Alexei
Last Names:Pevtsov
Affiliation:National Solar Observatory
Address:PO Box 62, Sunspot, NM, 88349, USA
Telephone:505-434-7011
Email:none
Student:no
Paper Title:
Author List:
Abstract:Intended contributions: 1. I plan to discuss the possible relationship between the properties of the active regions at their emergence and the flare/CME activity of the regions. 2. Events and active regions for study. * AR 8210 (May 1998) * AR 10229 and 10228 (Dec 2002) For both regions, CMEs were associated with the eruptions of the transequatorial loops (TLs). In my opinion, it would be interesting to understand how these TLs became unstable. There are EIT/MDI/TRACE/ISOON data for 19 Dec 2002 event. Here is an excerpt from our poster given at the SHINE 2003: Analyses of multi-wavelength data sets on 20002 December 19 at approximately 2150 UT show evidence of a large-scale, transequatorial coronal eruption associated with simultaneous flares in active regions in both hemispheres. The coronal manifestations (based on EIT, LASCO, and TRACE images) include a large coronal dimming, an opening/restructuring of magnetic fields, the formation of a transient coronal hole, and a halo CME. In the chromosphere, ISOON H-alpha images show distant flare precursor brightenings and several sympathetic flares. Originating near the main flare is a rapidly propagating (800 km/s), narrowly channeled disturbances detectable as a sequential brightening of numerous pre-existing points in the H-alpha chromospheric network. This disturbance is not a chromospheric Moreton wave, but it does produce a temporary activation of a transequatorial filament. This filament does not erupt not do any other filaments in the vicinity. MDI magnetograms show that the brightened network points are all of the same polarity (the dominant polarity among the points in the disturbance's path), suggesting that the affected field lines extend into the corona where they are energized in sequence as the eruption tears away.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000042 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  42
First Name:Linhui
Last Names:Sui
Affiliation:CUA/GSFC
Address:NASA/Goddard Space Flight Center, Greenbelt, MD, 20771, USA
Telephone:301-286-1857
Email:none
Student:yes
Paper Title:Evidence for Magnetic Reconnection in Solar Eruptive Events
Author List:Sui, L., Holman, G. D., Dennis, B. R.
Abstract:We will analyze the three flares on April 14-16, 2002 with the observations of RHESSI, TRACE and SOHO. In particular, we will focus on the study of features believed to be related to the magnetic reconnection.
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000043 (2004-08-02 18:21:43), 0042000111 (2004-08-18 06:14:14), 0042000112 (2004-08-18 06:22:48), 0042000114 (2004-08-18 06:25:02), 0042000117 (2004-08-22 21:15:54), 0042000118 (2004-08-22 21:16:14), 0042000119 (2004-08-22 21:17:24), 0042000129 (2004-08-24 12:05:14), 0042000130 (2004-08-24 12:10:11), 0042000131 (2004-08-24 12:30:37), 0042000132 (2004-08-24 12:31:13), 0042000135 (2004-08-25 11:53:59),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  43
First Name:Gordon
Last Names:Holman
Affiliation:NASA's Goddard Space Flight Center
Address:Code 682, Greenbelt, MD, 20771, USA
Telephone:301-286-4636
Email:none
Student:no
Paper Title:RHESSI Evidence for Magnetic Reconnection in a Large-Scale Current Sheet
Author List:Holman, G., Sui, L., & Dennis, B.
Abstract:We will present observations of several solar flares from RHESSI that indicate that energy release occured in a large-scale, vertical current sheet above newly formed, hot flare loops. The implications of these results for magnetic reconnection models will be discussed.
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000044 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  44
First Name:Sarah
Last Names:Gibson
Affiliation:NCAR/HAO
Address:PO Box 3000, Boulder, CO, 80305, United States
Telephone:303-497-1587
Email:none
Student:no
Paper Title:Twist and Flare: The role of helical magnetic structures in the solar corona
Author List:Gibson, S. E. , Fan, Y. , Mandrini, C. , Fisher, G., Demoulin, P.
Abstract:Solar explosive events such as coronal mass ejections (CMEs) and flares are commonly considered to be driven by the free magnetic energy stored in current carrying (twisted or sheared) coronal magnetic fields. Since it is presently not feasible to directly observe coronal magnetic fields, it is reasonable to turn to observations of flux-frozen solar plasma for evidence of such twisted magnetic field. Indeed, apparently twisted structures and rotating motions are not hard to find on the Sun. We must be cautious, however, in interpreting observations which are essentially projections of three-dimensional structures, and which highlight sub-regions of the magnetic field for specific physical reasons (for example, regions that are particularly dense or hot). In order to interpret such observations, it is essential to employ a three-dimensional, physical model that realistically simulates observable properties of the relationship between plasma and field. We will demonstrate how a model of a twisted magnetic flux rope emerging into a coronal magnetic field can be used to explain observed helical solar structures and dynamics. In particular, we will consider the structure, evolution, and relative location and orientation of S-shaped, or sigmoidal active regions and filaments. We will also discuss how the emerging flux rope can explain observed rotational and shearing motions at the solar photosphere. Finally, we will address how the emerging magnetic flux rope injects magnetic helicity into the corona, and how this drives dramatic coronal dynamics.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000045 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  45
First Name:Steven
Last Names:Christe
Affiliation:Space Sciences Laboratory, UC Berkeley
Address:7 Gauss way, Berkeley, CA, 94720-, USA
Telephone:510-642-3668
Email:none
Student:yes
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000046 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  46
First Name:Albert
Last Names:Shih
Affiliation:Space Sciences Laboratory
Address:University of California, Berkeley, Berkeley, CA, 94720, USA
Telephone:510-642-1397
Email:none
Student:yes
Paper Title:
Author List:
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000047 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  47
First Name:Peter
Last Names:Schuck
Affiliation:Naval Research
Address:4555 Overlook Ave., Washington, DC, 22153, USA
Telephone:202-7678366
Email:none
Student:no
Paper Title:detection and analysis of pre-event observables
Author List:P. W. Schuck, J. Chen., I. Schwartz, V. Yurchyshyn
Abstract:
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000048 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  48
First Name:James
Last Names:Chen
Affiliation:Naval Research Laboratory
Address:4555 Overlook Ave., SW, Washington, DC, 20375, USA
Telephone:202-767-3134
Email:none
Student:no
Paper Title:Observables associated with pre-event activities and CME eruptions
Author List:J. Chen and P. Schuck
Abstract:
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000049 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  49
First Name:Rim
Last Names:Turkmani
Affiliation:Imperial College/London
Address:SPAT group, Imperial College, Prince Consort Road, London, , SW7, London
Telephone:+447986380690
Email:none
Student:no
Paper Title:Particle acceleration in coronal loops
Author List:Turkmani, R., Vlahos, L., Cargill, P., Galsgaard, K., Isliker, H.
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000050 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  50
First Name:Brian
Last Names:Dennis
Affiliation:NASA Goddard Space Flight Center
Address:Code 682, Greenbelt, MD, 20771-, United States
Telephone:301-286-7983
Email:none
Student:no
Paper Title:Thermal Plasma Parameters from RHESSI Observations
Author List:Dennis, B. R. and Phillips
Abstract:Results from the analysis of RHESSI spectral observations using the latest Chianti code will be presented for the events under study in Group 6. The full spectral range will be used, including the iron and iron/nickel line complexes. Estimates will be made of the temperature and emission measure from the continuum, and the iron abundance from the line equivalent widths. Images will be reconstructed over narrow energy bands to determine the extent of the thermal emission in order to estiamte a source area and emitting volume. Uncertainties and difficulties remaining in this analysis will be discussed in detail, and comparisons will be made with observations of the thermal plasma at other wavelengths.
Poster:No
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000051 (2004-08-02 18:21:43), 0042000063 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  51
First Name:Kenneth
Last Names:Phillips
Affiliation:NRC/GSFC
Address:Code 682, Goddard Space Flight Center, Greenbelt, MD, 20771, USA
Telephone:301-286-1758
Email:none
Student:no
Paper Title:RHESSI observations of the Fe and Fe/Ni line features
Author List:Phillips, K. J. H., Dennis, B. R.
Abstract:I will discuss observations of the Fe line and Fe/Ni line fluxes during several flares and their agreement with theory. Possible reasons for disagreement will be outlined and discussed with Group 6.
Poster:Yes
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000052 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  52
First Name:Lyndsay
Last Names:Fletcher
Affiliation:University of Glasgow
Address:Department of Physics and Astronomy, University of Glasgow, Glasgow, , G12 8QQ, UK
Telephone:+44 141 330 5311
Email:none
Student:no
Paper Title:TRACE UV Flare footpoints
Author List:Fletcher, L., Pollock, J. A.
Abstract:We have developed a technique for tracking individual 'kernels' in UV/EUV flare ribbons observed by TRACE. This shows the overall separation of the ribbons, as well as small-scale dynamics within the ribbons themselves, such as the convergence of kernels towards one location and the meandering of kernels around granular boundaries. We will discuss the relationship between UV kernel dynamics, hard X-ray source location, and inferred magnetic field structures.
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000053 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  53
First Name:Bala
Last Names:Poduval
Affiliation:Stanford University
Address:445 Via Palou HEPL Annex A, Palo Alto, CA, 94305, USA
Telephone:650-724-9649
Email:none
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000054 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  54
First Name:Yuhong
Last Names:Fan
Affiliation:NCAR/HAO
Address:3450 Mitchell Lane, Boulder, CO, 80301, USA
Telephone:303-497-1575
Email:none
Student:no
Paper Title:Numerical Simulations of 3D Coronal Magnetic Fields Resulting from the Emergence of Twisted Magnetic Flux Tubes
Author List:Fan, Y. and Gibson, S. E.
Abstract:We present MHD simulations in the low-$\beta$ regime of the evolution of the 3D coronal magnetic field as an arched, twisted magnetic flux tube is transported into a pre-existing coronal potential magnetic arcade. It is found that the line-tied emerging flux tube becomes kink unstable when a sufficient amount of twist is transported into the corona. For an emerging flux tube with a left-handed twist (which is the preferred sense of twist for active region flux tubes in the northern hemisphere), the kink motion of the tube and its interaction with the ambient coronal magnetic field lead to the formation of an intense current layer which displays an inverse-S shape, consistent with the X-ray sigmoid morphology preferentially seen in the northern hemisphere. Our simulation results may explain the X-ray sigmoid brightenings that are observed during eruptive flares and confirm the prediction by previous topological studies that magnetic tangential discontinuities (or current sheets) should form along the so called ``bald-patch''separatrix surface, across which the connectivity of the coronal magnetic field with the dense photosphere undergoes a sharp transition. Finally, we will also present simulations in a 3D spherical geometry of a CME-like eruption of the coronal magnetic field due to the kink instability of a twisted magnetic flux rope emerging into the corona.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000055 (2004-08-02 18:21:43), 0042000075 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  55
First Name:Takako
Last Names:Ishii
Affiliation:Kwasan Observatory, Kyoto-U.
Address:Yamashina-ku, Kyoto, , 607-84, Japan
Telephone:+81-75-581
Email:none
Student:no
Paper Title:Pre-flare Brightening and Rotational Motion of Magnetic Neutral Lines in Flare-productive Active Regions
Author List:T.T.Ishii, S.Saito, and H.Kurokawa
Abstract:A flare-productive active region NOAA 9026 (2000 June) provided us with a rare opportunity to study a new important aspect of a twisted magnetic flux rope and its rapidly-untwisting motions to have caused strong flares. Based on the analyses of the evolution of this region, we found pre-flare brightenings in TRACE 1600 A images about two hours prior to an X-class flare. Active region NOAA 10486 is the most flare-productive region during this solar cycle, which has produced seven X-class flares including X28 flare on Nov. 4, 2003. We studied the formation process of delta-type magnetic configuration, and found pre-flare brightenings in TRACE 1600 A images on the sheared neutral lines. We studied the evolution of all the active regions in this solar cycle (cycle 23) that have produced at least one X-class flare and have been observed by SOHO/MDI magnetograms. We are planning to summarize the characteristics of flare-productive regions from the viewpoint of pre-flare brightenings and rotational motions of magnetic neutral lines.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000056 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  56
First Name:Alexander
Last Names:Kosovichev
Affiliation:Stanford University
Address:255 Via Palou, Stanford, CA, 94305, USA
Telephone:650-723-7667
Email:none
Student:no
Paper Title:Subphotospheric Dynamics of Flaring Active Regions
Author List:Kosovichev, A.G., Duvall, T.L., Jr
Abstract:We present results of investigation of subsurface plasma flows and emerging structures for several flaring active regions (including AR 9393 and 10486). The results representing 3-D maps of sound-speed perturbations and flow velocities are obtained from SOHO/MDI full-disk Doppler data by time-distance helioseismology with the horizontal resolution of 3 Mm, vertical resolution of 0.7-4 Mm (in the depth range of 0-40 Mm), and temporal resolution of 8 hours. These maps are compared with the corresponding MDI magnetograms, and also with coronal images to determine the role of subphotospheric dynamics in the development of the active regions and their flaring activity.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000057 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  57
First Name:Ayumi
Last Names:Asai
Affiliation:Kwasan Observatory, Kyoto-U.
Address:Kitakasan Ominecho, Yamashina, Kyoto, , 607-84, Japan
Telephone:+81-75-581
Email:none
Student:yes
Paper Title:Flare Ribbon Expansion and Energy Release Rate
Author List:Asai, A., Yokoyama, T., Shimojo, M., Masuda, S., Kurokawa, H., Shibata, K.
Abstract:We report a detailed examination about the relationship between the evolution of the H-alpha flare ribbons and the released magnetic energy during an X2.3 solar flare which occurred on 2001 April 10. We examined the evolution of flare ribbons by using the H-alpha images obtained with the Sartorius telescope at Kwasan Observatory, Kyoto University. Based on the magnetic reconnection model, we calculated quantitatively the released energy was by using the photospheric magnetic field strengths obtained with SOHO/MDI and separation speeds of the fronts of the H-alpha flare ribbons.
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000058 (2004-08-02 18:21:43), 0042000072 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  58
First Name:Junwei
Last Names:Zhao
Affiliation:Stanford University
Address:HEPL, 455 Via Palou, Stanford, CA, 94305, USA
Telephone:650-725-9549
Email:none
Student:no
Paper Title:subsurface kinetic helicity beneath solar active regions
Author List:Junwei Zhao, & Alexander G. Kosovichev
Abstract:I will present our statistics of subsurface kinetic helicity of more than 100 solar active regions, as well as the global kinetic helicity distribution from local helioseimological techniques.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000059 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  59
First Name:Kuhn
Last Names:Jeff
Affiliation:IFA
Address:2680 Woodlawn Dr., Honolulu, HI, 96822, USA
Telephone:808-956-8968
Email:none
Student:no
Paper Title:Infrared Coronal Magnetometry
Author List:Kuhn, J.R., Lin, H.
Abstract:Discussion of new ground-based IR coronal magnetometry and future measurement prospects.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000060 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  60
First Name:Suzanne
Last Names:Hawley
Affiliation:University of Washington
Address:Astronomy Department, Box 351580, Seattle, WA, 98195, USA
Telephone:206-685-2236
Email:none
Student:no
Paper Title:Radiative Hydrodynamic Models of Solar Flares
Author List:Hawley, S.L., Allred, J.C.
Abstract:We will present results from our current program to model solar flares using observed RHESSI particle acceleration data as energy input, accounting for energy deposition through a Fokker-Planck formulation and incorporating radiative backwarming from UV-Xray radiation.
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000061 (2004-08-02 18:21:43),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  62
First Name:Peter
Last Names:Gallagher
Affiliation:NASA Goddard Space Flight Center
Address:, Greenbelt, MD, 20771, USA
Telephone:(301) 309-127
Email:peter.t.gallagher@gsfc.nasa.gov
Student:no
Paper Title:Active Region Properties Associated with Superstorms
Author List:Gallagher, P. T., McAteer, R. T. J.
Abstract:
Poster:No
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000064 (2004-08-02 18:21:43), 0042000065 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  67
First Name:Jun
Last Names:Lin
Affiliation:Harvard-Smithsonian Center for Astrophysics
Address:60 Garden Street, Cambridge, MA, 02138, USA
Telephone:(617) 495-7425
Email:jlin@cfa.harvard.edu
Student:no
Paper Title:Direct Observations of Magnetic Reconnection Sites of A CME/Flare of
Author List:Lin, J., Ko, Y.-K., Sui, L., et al.
Abstract:The event of November 18, 2003 provides us with an opportunity to observe directly the current sheet and the associated magnetic reconnection process. This event occurred on the east limb of the Sun, a group of bright arcades in EIT 195 distributing at both sides of the equator can be seen clearly prior to the eruption. The EIT 195 movie shows that the arcades located at the central position started to change at around 08:48UT and the following significant variation occurs at 9:00UT with a fast expansion of the arcade. No apparent filament or prominence showed. Two legs of the stretched arcade show apparent motion of approaching one another, which implies a magnetic reconnection process driven by the eruption. Consequently, a bright and sharp cusp structure forms and moves upwards. From 11:24UT, the visible top of the cusp structure started getting round and its height also decreases, manifesting an apparent shrinkage process. A sharp cusp can still be seen in MK4 images. Correspondingly, the front of a fast CME appears in the field of view of LASCO/C2 from 9:26UT, showing typical three-component structure of CMEs with a big bright core. The CME front left the field of view of LASCO/C2 after 10:50UT and following the entangled structure of CME, a long and thin streamer-like feature appears in the field of view of LASCO/C2, and a series bright blobs successively flow away from the Sun along this feature. The average velocity of the CME front within the time interval sweeping the field of view of LASCO/C2 is 1700 km/s and that of the CME core is 1412 km/s. Comparisons with the similar feature investigated by Ko et al (2003) suggest that this long and thin streamer-like feature be the current sheet forming and developing during this CME-flare process. Observations made by UVCS caught the initial stage of this eruption when the magnetic arcade thrust upward pushing the adjacent magnetic field and plasma away. The data from RHESSI show significant hard X-ray emission at both the footpoints and the top of the cusp structure, which further confirms the undergoing magnetic reconnection in the progress of eruption.
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000074 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  check
Paid:  No
 

Id:  68
First Name:Wei
Last Names:Liu
Affiliation:Stanford University
Address:Varian Physics Bldg, 382 Via Pueblo Mall, Stanford, CA, 94305-4060, USA
Telephone:650-736-0200
Email:weiliu@quake.Stanford.EDU
Student:yes
Paper Title:TBD
Author List:
Abstract:
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000076 (2004-08-02 18:21:43), 0042000113 (2004-08-18 06:24:35),
Total Amount:100.00
Payment:  credit
Paid:  No
 

Id:  69
First Name:Daniel
Last Names:Brown
Affiliation:University of St Andrews
Address:School of Mathematics, University of St Andrews, St Andrews, , KY16 9SS, UK
Telephone:(+44) 1334 463753
Email:daniel@mcs.st-andrews.ac.uk
Student:no
Paper Title:The magnetic topology near flare ribbons
Author List:Brown, D.S. and Fletcher, L.
Abstract:We extrapolate the magnetic topology of a flare region from SOHO/MDI magnetograms and investigate the magnetic structure along and near the flare ribbons. We discuss the implications of the topology for the activation and dynamics of the flare ribbons and the connectivity between the ribbons and the rest of the flaring region.
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000078 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  70
First Name:Richard
Last Names:Jones
Affiliation:University of Wales, Aberystwyth
Address:Institute of Mathematical & Physical Sciences University of Wales, Aberystwyth, Penglais, Aberystwyth, , SY23 3BZ, UK
Telephone:+44 (0)1970 621902
Email:raj98@aber.ac.uk
Student:yes
Paper Title:Interplanetary scintillation (IPS) observations of interplanetary coronal mass ejections
Author List:Jones, R.A., Breen, A.R., Fallows, R.A.
Abstract:Coronal Mass Ejections (CMEs) have been observed using white-light instruments for over three decades. The structure appears different when observed by white-light instruments in the corona - where a three-part structure comprising leading edge, void and ejecta is frequently observed and as detected by in-situ plasma and field instruments which suggest a two-part structure of shock and ejecta. Interplanetary scintillation(IPS) observations are uniquely capable of determining solar wind parameters over a distance range extending from within the field of view of white-light instruments out into the interplanetary space. In this presentation we discuss the characteristic signatures which allow us to determine whether a CME is present in the ray-path during an IPS observation, before going on to describe a case study of an interplanetary coronal mass ejection (iCME), in which we combine extreme ultra-violet observations from EIT, white-light images from LASCO and IPS results from the EISCAT facility with in-situ measurements from ACE.
Poster:Yes
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000079 (2004-08-02 18:21:43),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  71
First Name:Vasyl
Last Names:Yurchyshyn
Affiliation:Big Bear Solar Observatory
Address:40386 North Shore Lane, Big Bear City, CA, 92314, USA
Telephone:(909) 866-5791x35
Email:vayur@bbso.njit.edu
Student:no
Paper Title:Coronal and Interplanetary Magnetic Fields in Coronal Ejecta in October-November 2004
Author List:Vasyl Yurchyshyn
Abstract:We will discuss the structure of the magnetic fields in the super events on October 28, 29 and November 18 2003 by combining space- (SOHO, TRACE, RHESSI, ACE) and ground- (BBSO DMG, Halpha) based data. The orientation of the corresponding magnetic clouds at 1AU will be mapped onto the relevant active regions with a correction for the angle between the ecliptic and equatorial planes. This mapping will give us approximate orientation of the flux rope when it was launched, provided that it was created in the solar corona and the orientation is preserved during its propagation through the interplanetary media. We will use these data to infer the magnetic topology of the source regions and magnetic fields involved in eruption.
Poster:No
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000080 (2004-08-02 18:21:43), 0042000081 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  72
First Name:Boris
Last Names:Somov
Affiliation:
Address:Solar Physics Department, Astronomical Institute, Moscow State University, Universitetskii Prospect 13, Moscow, , 119992, Russia
Telephone:7 095 939 16 44
Email:somov@sai.msu.ru
Student:no
Paper Title:Collapsing Magnetic Trap Model for Coronal HXR Sources
Author List:Somov, B., Bogachev, S.
Abstract:I would like to review the physical processes (the Fermi acceleration and betatron acceleration of electrons and ions, Coulomb collisions, HXR emission) in collapsing magnetic traps generated by fast reconnection in super-hot turbulent-current layers in flares. The main attension will be paid to the observational predictions of the model and possibilities to compare these predictions with the RHESSI observations.
Poster:No
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000082 (2004-08-02 18:21:43),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  73
First Name:Dr.Saumitra
Last Names:Mukherjee
Affiliation:Commowealth Fellow, UK
Address:SES, Jawaharlal Nehru University, New Delhi, DILLI, 110067, INDIA
Telephone:0091-11-35908512
Email:dr.saumitramukherjee@usa.net
Student:yes
Paper Title:Active region of Sun influences Environment of the Earth
Author List:Mukherjee, S
Abstract:It has been observed during 28th July 2oo4 to 2nd August 2004 that the Actve region 652 of the Sun has direct influence on the atmosphere of the earth. Kp values when increased than 8 after the earth directed CME, has the potential of temporarily disturbing the condensation of cloud on the geocoordinates affected. Subsequently the low value of Kp for more than 36 hours allows the clouds to condence and precipitate. This discovery is a break through in Sun-earth connection. Besides Kp Eflux and P flux also found to be higher during disturbed weather condition.
Poster:Yes
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000084 (2004-08-02 18:21:43), 0042000125 (2004-08-23 10:49:16),
Total Amount:100.00
Payment:  cash
Paid:  No
 

Id:  77
First Name:Phillip
Last Names:Chamberlin
Affiliation:LASP/U of Colorado
Address:1234 Innovation Dr, Boulder, CO, 80303, USA
Telephone:303-492-4496
Email:phil.chamberlin@lasp.colorado.edu
Student:yes
Paper Title:EUV spectral irradiance changes during a flare
Author List:Chamberlin, P. C., Woods, T. N, Eparvier, F. G.
Abstract:EUV spectral irradiance changes during a flare and thier relations to x-ray changes/emissions
Poster:Yes
Group:6. Imaging Spectroscopy of the Thermal Plasma
ApplicationRequestIDs:0042000090 (2004-08-02 18:57:47), 0042000091 (2004-08-02 18:58:55), 0042000116 (2004-08-19 13:47:04), 0042000127 (2004-08-23 14:33:27), 0042000145 (2004-09-03 12:22:24),
Total Amount:100.00
Payment:  credit
Paid:  Yes
 

Id:  78
First Name:Valentyna
Last Names:Abramenko
Affiliation:Big Bear Solar Observatory of NJIT
Address:40386 North Shore Lane, Big Bear City, CA, 92314, USA
Telephone:1 909 866 5791
Email:avi@bbso.njit.edu
Student:no
Paper Title:Diagnostics of flare activity level from turbulence parameters of photospheric plasma
Author List:Abramenko, V.I.
Abstract: We continue our research on the diagnosis of the level of flare activity in different active regions by means of structure functions (parameters of the turbulence state). In this study we used measurements of the photospheric magnetic and velocity fields obtained before the flare onset. The study shows that the state of turbulence in an active region varies in accordance to the level of its flare productivity. For example, a "quiet" active region has classical Kolmogorov turbulence, while active regions which produce strong flares display significant deviations from classical Kolmogorov turbulence. We discuss the observed phenomenon in terms of complexity of photospheric structures.
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000092 (2004-08-05 10:16:29),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  79
First Name:James
Last Names:McAteer
Affiliation:NRC / GSFC
Address:GSFC, Greenbelt, MD, 20771, 
Telephone:301-286-3709
Email:j.mcateer@grasshopper.gsfc.nasa.gov
Student:no
Paper Title:Quantifying Complexity in Solar Active Regions
Author List:McAteer, R.T.J., & Gallagehr, P.T.
Abstract: We discuss several methods of quantifying magnetic complexity (e.g., mult-fractal, wavelet) how these parameters are related to the occurence rate, strength, and timing of flare and CMEs.
Poster:No
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000093 (2004-08-05 12:01:33),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  80
First Name:Phil
Last Names:Isenberg
Affiliation:University of New Hampshire
Address:SSC/Morse Hall, 39 College Road, Durham, NH, 03924, USA
Telephone:603-862-3870
Email:phil.isenberg@unh.edu
Student:no
Paper Title:A 3D Line-Tied Model of an Erupting Flux Rope
Author List:Isenberg, P. A. and Forbes, T. G.
Abstract:We will present and discuss our new analytical 3D line-tied model of an evolving coronal flux rope which exhibits an ideal loss of equilibrium. The model is based on the equilibrium configuration of Titov and Dmoulin (1999), with a more accurate application of line-tied conditions at the photospheric boundary, allowing for the treatment of eruptive behavior. Such a catastrophic loss of equilibrium can lead to rapid rise of the flux rope, triggering reconnection at the quasi-separatrix surfaces, and the manifestation of various CME properties.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000094 (2004-08-06 08:19:52),
Total Amount:300.00
Payment:  check
Paid:  No
 

Id:  81
First Name:Stephen
Last Names:White
Affiliation:University of Maryland
Address:Department of Astronomy, College Park, MD, 20742, USA
Telephone:3014051547
Email:white@astro.umd.edu
Student:no
Paper Title:TBA
Author List:
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000095 (2004-08-06 08:45:17),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  82
First Name:kathy
Last Names:reeves
Affiliation:University of New Hampshire
Address:39 College Rd, Durham, NH, 03824, United States
Telephone:United States
Email:kreeves@unh.edu
Student:yes
Paper Title:Thermal Energy and Light Curves from a Loss of Equilibrium CME Model
Author List:Reeves, K. K. and Forbes, T. G.
Abstract:We use a loss of equilibrium CME model to investigate the thermal energy release in solar eruptions. For this calculation, we assume that the Poynting flux in the current sheet is completely thermalized. We find that the net thermal energy released in strong field regions is a higher percentage of the total energy than in weak field regions, and that the rate of thermal energy release is faster for CMEs originating in strong field regions. It is possible to have a CME that is relatively high speed (~1000 km/s), but with a low thermal energy if the background field is weak and the density of the ejected mass is low. Based on this thermal energy calculation, we calculate TRACE and SXT flare light curves that can be compared to observations. These results lead us to conclude that this model predicts that there would not necessarily be an observable flare associated with the CME for weak magnetic field regions.
Poster:Yes
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000096 (2004-08-06 09:45:15),
Total Amount:100.00
Payment:  credit
Paid:  No
 

Id:  83
First Name:K. D.
Last Names:Leka
Affiliation:CoRA Div., NorthWest Research Associates
Address:3380 Mitchell Ln., Boulder, CO, 80301, USA
Telephone:303-415-9701x219
Email:leka@cora.nwra.com
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000097 (2004-08-06 10:14:50),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  84
First Name:Graham
Last Names:Barnes
Affiliation:CoRA/NWRA & HAO/NCAR
Address:3380 Mitchell Lane, Boulder, CO, 80301, USA
Telephone:303-415-9701x234
Email:graham@cora.nwra.com
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000098 (2004-08-06 10:32:45),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  85
First Name:Valentina
Last Names:Zharkova
Affiliation:Bradford University
Address:Cybernetics Department, Bradford, , BD7 1DP, UK
Telephone:44 1274 234 030
Email:v.v.zharkova@brad.ac.uk
Student:no
Paper Title:Hydrodynmic responses to proton and electron heating
Author List:Zharkova, V.V., Gordovskyy, M. Voitenko, Y.M. Goossens,M.
Abstract:We apply new heating functions for proton and electron beam for calculations of hydrodynamic responses of a flaing atmosphere for two temperature plasma with thermal conduction.
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000099 (2004-08-06 13:13:15), 0042000100 (2004-08-06 13:13:48),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  86
First Name:Yanwei
Last Names:Jiang
Affiliation:
Address:382 Via Pueblo Mall Physics 4060, Stanford, CA, 94305, USA
Telephone:650-7230211
Email:arjiang@stanford.edu
Student:yes
Paper Title:
Author List:
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000101 (2004-08-06 15:51:56),
Total Amount:100.00
Payment:  credit
Paid:  No
 

Id:  87
First Name:Moore
Last Names:Ron
Affiliation:NASA/MSFC/NSSTC
Address:Marshall Space Flight Center, Space Science Department/SD50, Huntsville, AL, 35812, US
Telephone:(256) 961-7613
Email:ron.moore@ nasa.gov
Student:no
Paper Title:Compact Flares and CMEs
Author List:Moore, R., Sterling, A.
Abstract:From a search of the SOHO/LASCO CME Catalog, we found several flares that were strong but short-lived in GOES X-ray flux (peak flux > C5, duration <~2 hr), and produce no CME. We also found several equaly strong and short-lived flares that did initiate CMEs. All of the flares were located in strong magnetic fields near sunspots and were spatially compact (brightened only a small part of the active region. From the magnetic location and magnetic surroundings determined from MDI magnetograms, it appears that the non-CME flares were confined deep within surronding strong closed magnetic fields, while the CME-producing flares either triggered neighboring sheared fields to erupt into a CME, or were able to erupt out of the active region and directly drive a CME. Compact ejective flares of this last type may produce a large CME by driving the eruption of a large coronal loop such a a trans-equatorial loop. We present an example of such a flare and CME.
Poster:Yes
Group:4. Flares without CMEs
ApplicationRequestIDs:0042000102 (2004-08-11 12:01:18),
Total Amount:300.00
Payment:  check
Paid:  No
 

Id:  88
First Name:Richard
Last Names:Mewaldt
Affiliation:Caltech
Address:220-47 Downs Lab, Pasadena, CA, 91125, USA
Telephone:626-395-6612
Email:RMewaldt@SRL.caltech.edu
Student:no
Paper Title:TBD
Author List:TBD
Abstract:Topic will be: Spectra and composition of solar energetic particles at 1 AU associated with large solar events of October/November 2003. I can also contribute to the Global Energetics working group
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000103 (2004-08-13 15:37:31),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  89
First Name:Mykola
Last Names:Gordovskyy
Affiliation:University of Bradford
Address:, Bradford, , BD7 1DP, United Kingdom
Telephone:+441274234269
Email:m.gordovskyy@bradford.ac.uk
Student:yes
Paper Title:Effect of the return current and magnetic field convergence on heating of flaring atmosphere
Author List:Gordovskyy, M. and Zharkova, V.V.
Abstract:Electron beam precipitation is investigated taking into account return current electric field and magnetic field convergence. Resulting electron spectra and beam energy deposition functions are deduced for different initial energy fluxes, initial spectral indices and different magnetic convergence rates.
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000104 (2004-08-16 10:53:57),
Total Amount:100.00
Payment:  credit
Paid:  No
 

Id:  90
First Name:Edward
Last Names:Schmahl
Affiliation:University of Maryland/NASA's GSFC
Address:Astronomy Dept., College Park, MD, 20742, USA
Telephone:3102865114
Email:schmahl@hessi.gsfc.nasa.gov
Student:no
Paper Title:Pre-flare HXR emission associated with eruptive filaments and CME.
Author List:E.J. Schmahl and Haisheng Ji
Abstract:Pre-flare HXR emission associated with eruptive filaments and CMEs.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000105 (2004-08-17 11:41:08),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  91
First Name:MUKUL
Last Names:KUNDU
Affiliation:UNIVERSITY OF MARYLAND
Address:Dept of Astronomy,Univ of Maryland, College Park, MD, 20742, USA
Telephone:301-405-1524
Email:kundu@astro.umd.edu
Student:no
Paper Title:Not available now
Author List:
Abstract:
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000106 (2004-08-17 14:29:08),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  92
First Name:Tim
Last Names:Bastian
Affiliation:NRAO
Address:520 Edgemont Rd, Charlottesville, VA, 22903, USA
Telephone:434 296 0348
Email:tbastian@nrao.edu
Student:no
Paper Title:Radio Signatures of Flares and CMEs
Author List:Bastian, T. S.
Abstract:
Poster:No
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000107 (2004-08-17 20:32:00), 0042000108 (2004-08-17 20:32:44), 0042000109 (2004-08-17 20:33:23),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  93
First Name:Henry
Last Names:Aurass
Affiliation:Astrophysikalisches Institut Potsdam
Address:An der Sternwarte 16, Potsdam, , D - 14482, Germany
Telephone:(+49)-331-7499-293
Email:haurass@aip.de
Student:no
Paper Title:Radio observation of the outflow termination shock
Author List:Aurass, H.
Abstract:We discuss several arguments and examples for the interpretation of type II burst-like radio features as possible signatures of the fast mode reconnection outflow termination shock.
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000110 (2004-08-18 00:08:09),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  94
First Name:Frank C. Z.
Last Names:Cheng
Affiliation:Princeton University
Address:Princeton Plasma Physics Laboratory, Princeton, NJ, 08543, USA
Telephone:609-243-2648
Email:fcheng@pppl.gov
Student:no
Paper Title:Magnetic reconection in flares and CMEs
Author List:Cheng, C.Z., Choe, G., Qiu, J., etc.
Abstract:
Poster:Yes
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000115 (2004-08-18 14:36:03),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  95
First Name:Helen
Last Names:Mason
Affiliation:University of Cambridge
Address:DAMTP, CMS, Wilberforce Rd, Cambridge, , CB3 0WA, 
Telephone:01223 337898
Email:hm11@damtp.cam.ac.uk
Student:no
Paper Title:Cambridge led Active Regions and Flares CDS Campaigns
Author List:Mason, H.E., Del Zanna , G. et al
Abstract:The Cambridge led Active Region and Flare Campaigns have provided a substantial amount of CDS observations. With these data, we are able to relate the high temperature emission with the footpoint regions. This enables us to study the plasma properties and to relate these to features seen with other instruments (MDI, TRACE, RHESSI and GB observations).
Poster:Yes
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000121 (2004-08-23 04:14:49), 0042000122 (2004-08-23 04:15:13), 0042000123 (2004-08-23 04:16:16),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  96
First Name:George
Last Names:Simnett
Affiliation:University of Birmingham
Address:Edgbaston, Birmingham, , B15 2TT, UK
Telephone:44 121 414 6469
Email:gms@star.sr.bham.ac.uk
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:8. Global energetics
ApplicationRequestIDs:0042000124 (2004-08-23 08:44:34),
Total Amount:300.00
Payment:  credit
Paid:  Yes
 

Id:  97
First Name:Gerald
Last Names:Share
Affiliation:NRL
Address:, Washington, DC, 20375, USA
Telephone:202 767-3027
Email:gerald.share@nrl.navy.mil
Student:no
Paper Title:What the Annihilation Line Tells Us About the Flaring Chromosphere
Author List:Share, G., Murphy, R.
Abstract:{\em RHESSI} has measured the positron-electron annihilation line and continuum in three solar flares: 2002 July 23, 2003 October 28 and 2003 November 2. The 511 keV line was broad ($\sim 4 - 8$ keV) in all three flares, consistent with annihilations in an ambient ionized medium at temperatures $> 10^5$ K. The measured continuum from positronium and from Compton scattering was unobservable with the exception of the first 4 min of the October 28 flare observation; this indicates that the density where most annihilations occurred was $> 10^{14}$ H cm$^{-3}$. The width of the line narrowed in 2 min to $\sim 1$ keV late in the October 28 flare consistent with annihilation in ionized H $ <10^4$ K and $\geq 10^{15}$ cm$^{-3}$. There is evidence for a similar decrease in line width late in the Nov. 2 flare. These observations suggest a highly dynamic flaring atmosphere at chromospheric densities that can reach transition-region temperatures, cool to $<10^4$ K in minutes, and still remains highly ionized. Although the energy contained in high-energy accelerated particles may have been enough to heat the plasma, the rate of deposition is not correlated with the temperature determined by the 511-keV line width; this raises questions about the energy source.
Poster:No
Group:5. Ribbons and footpoints
ApplicationRequestIDs:0042000126 (2004-08-23 10:57:32),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  98
First Name:Ed
Last Names:Cliver
Affiliation:AFRL
Address:AFRL/VSBXS, Hanscom AFB, MA, 01731-3010, USA
Telephone:781-377-3975
Email:edward.cliver@hanscom.af.mil
Student:no
Paper Title:
Author List:
Abstract:
Poster:Yes
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000133 (2004-08-24 15:06:01),
Total Amount:350.00
Payment:  cash
Paid:  No
 

Id:  99
First Name:Alphonse
Last Names:Sterling
Affiliation:NASA/MSFC
Address:NSSTC/SD50/Space Science Dept., 320 Sparkman Drive, Huntsville, Alabama, 35805, USA
Telephone:256-961-7634
Email:alphonse.sterling@nasa.gov
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:4. Flares without CMEs
ApplicationRequestIDs:0042000134 (2004-08-24 15:30:18),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  100
First Name:Bernhard
Last Names:Fleck
Affiliation:ESA/RSSD
Address:c/o NASA/GSFC Mailcode 682.3, Greenbelt, MD, 20771, USA
Telephone:301-286-4098
Email:bfleck@esa.nascom.nasa.gov
Student:no
Paper Title:
Author List:
Abstract:
Poster:No
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000136 (2004-08-25 14:23:11),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  101
First Name:Nariaki
Last Names:Nitta
Affiliation:LMSAL
Address:, , , , 
Telephone:6503545458
Email:nitta@lmsal.com
Student:no
Paper Title:Properties of flares associated with and not associated with CMEs
Author List:Nitta, NV
Abstract:We study a handful of flares not far from the limb that are and are not associated with CMEs. The questions we ask include: Do short-duration flares associated with energetic CMEs have some characteristic features? Are all flares, eruptive and confined, explained by the so-called standard model? We mainly deal with pre-RHESSI flares.
Poster:No
Group:4. Flares without CMEs
ApplicationRequestIDs:0042000137 (2004-08-26 07:47:22), 0042000139 (2004-08-26 07:49:08),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  102
First Name:John
Last Names:Raymond
Affiliation:Harvard CFA
Address:none, none, MA, none, USA
Telephone:none
Email:none
Student:no
Paper Title:
Author List:J. Raymond, Y.-K. Ko, A. Ciaravella
Abstract:UWCS has observed several current sheets below CMEs. We estimate temperatures and densities and discuss the time scales over which these events decay.
Poster:No
Group:2. Magnetic Reconnection & Formation of Current Sheets
ApplicationRequestIDs:0042000140 (2004-08-27 08:14:43),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  103
First Name:Paula
Last Names:Balciunaite
Affiliation:SSL/UCB
Address:, , , , 
Telephone:(510) 642 0562
Email:balciunaite@ssl.berkeley.edu
Student:no
Paper Title:Above the Loop-top Non-Thermal Hard X-ray Source in a Partially Occulted Flare
Author List:Balciunaite, p., Krucker, S., Lin, R.P.
Abstract:July 12th flare
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000141 (2004-08-27 11:31:05),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  104
First Name:Yang
Last Names:Liu
Affiliation:Stanford University
Address:455 Via Palou, Stanford, CA, 94305, USA
Telephone:(650)724-5605
Email:yliu@quake.stanford.edu
Student:no
Paper Title:Determination of CME's speed using the cone-model.
Author List:Yang Liu
Abstract:We have used the cone-model, proposed by Zhao et al (2002), to determine the CME's speed for the full halo CMEs occurred in the period from 1997 to 2000. A discussion on these CMEs will be presented here.
Poster:Yes
Group:3. Interrelationships of Flares/CMEs in "Super" Events
ApplicationRequestIDs:0042000143 (2004-08-30 14:30:57),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  105
First Name:Adriana V. R.
Last Names:Silva
Affiliation:Mackenzie University
Address:R. Consolacao, 896, CRAAM, Sao Paulo, SP, 01302907, Brazil
Telephone:55-11-3236-8726
Email:asilva@craam.mackenzie.br
Student:no
Paper Title:Comparison of hard X-ray and submm emission form the 2002 November 2nd flare
Author List:Silva, A. V. R., Gimenez de Castro, C. G., Gary, D. E., Kaufmann, P.
Abstract:The 2002 November 2nd flare is one of the great flares that occurred during the very productive period of October-November 2002. This flare was simultaneously observed by RHESSI above 800 keV, at microwaves by the OVSA, and by the Solar Submillimetric Telescope at 212 and 405 GHz. Time profiles, source position, and spectra at both hard X-ray and radio wavelengths are analyzed. The radio spectra is typical of gyrosynchrotron emission with a decreasing spectra at submm wavelengths. We discuss the comparison with hard X-ray spectra at high energies, in order to infer particle acceleration mechanisms.
Poster:Yes
Group:7. Particle Acceleration and Transport
ApplicationRequestIDs:0042000144 (2004-09-03 08:44:19),
Total Amount:300.00
Payment:  credit
Paid:  No
 

Id:  106
First Name:Richard
Last Names:Nightingale
Affiliation:Lockheed Martin Advanced Technology Center
Address:Orgn/AD-BS, Bldg/252, 3251 Hanover Street, Palo Alto, CA, 94304-1191, USA
Telephone:650 424 3293
Email:nightingale@lmsal.com
Student:no
Paper Title:TRACE Observations of Many Active Regions with X-flares and Rotating Sunspots in the Current Solar Cycle
Author List:Nightingale, R., Metcalf, T.
Abstract:The TRACE instrument in its 7 UV and EUV wavelength channels has observed approximately 55 X-flares throughout its mission so far in solar cycle 23 from launch in April 1998 through August 2004. About 40 of those X-flares (73%) can be associated with 17 solar active regions that contain rotating sunspots, which have been observed by TRACE in its white light channel. These sunspots, rotating about the center of their umbras, appear to be manifestations of the twist and/or writhe, i.e., the helicity, instilled in the rising active region omega loops as they travel through the convection region below the photosphere. Of the 40 X-flaring active regions observed, 26 (65%) can be further associated with large, fast Coronal Mass Ejections (CMEs) leaving the sun, as recorded by the LASCO instrument on SoHO. Furthermore, 24 of these 26 events appear to be geo-effective because the energetic proton fluxes, observed by instruments on the GOES geosynchronous spacecraft, increased by several orders of magnitude shortly after the solar events occurred. The data and the importance of such a high percentage of rotating sunspots being associated with X-flaring active regions and CMEs will be discussed. This work was supported by NASA under the TRACE contract NAS5-38099.
Poster:Yes
Group:1. Pre-Event Physics
ApplicationRequestIDs:0042000146 (2004-09-03 18:52:41),
Total Amount:300.00
Payment:  credit
Paid:  No