CDS can determine these velocities across a wide range of temperatures. Previous Works ... How is the flares' energy budget divided ? What role do ions play? ...
Locarno, 8 June 2005. Peter Gallagher (UCD) Chromospheric Evaporation ... Locarno, 8 June 2005. Peter Gallagher (UCD) CDS and TRACE: 26 March 2002 Flare. SOHO/CDS ...
Criteria for spectral classification of cool stars using high resolution spectra ... The resulting database contains high-resolution optical spectra for 118 ...
Adiabatic Current Sheet of Sweet-Parker type ... (isothermal) g 5/3 (adiabatic) ... An adiabatic current sheet with anomalous resistivity factor of about 50 and ...
The First Far Eastern Workshop on Helioseismology ... The First Far Eastern Workshop on Helioseismology. South Pole Observation. Jefferies et al 1997 ...
Characteristics of chromospheric Ca II jets. guessed from ... At the photosphere (at the wing), the profile is. almost the same as the quiet-region profile. ...
Hinode discovered ubiquitous Ca jets (anemone jets) in the solar chromosphere ... Chromoshperic anemone jet seems to be accelerated by slow mode shock generated ...
... in Science and Technology (CAST) studentship from Queen's University Belfast and ... of the American Astornomical Society for being awarded an SPD Studentship. ...
Dispersion diagrams of chromospheric MHD waves in a 2D simulation. Chris Dove ... Brigham, E. Oran, The Fast Fourier Transform, Prentice-Hall, 1974 ...
Evidence for chromospheric heating in the late phase of solar flares. David ... Sunspot plage. expanding ribbons. CDS DOPPLERGRAMS. distinctive pattern of ...
... He I 584.33 (log T = 4.5) chromosphere ... transition region to chromosphere without any significant bulk ... context images of the chromosphere and corona ...
In plage, Diffuse but some 'kernels' More SXR emission at footpoints. ... At footpoints in plage. Magnetic field strength (Gauss) Magnetic field inclination ...
Electrons are accelerated during impulsive phase of solar flare ... Chromosphere unable to radiate energy deposited by non-thermal electrons. Velocities 400 km/s ...
Non-normality of dynamo equations means that equations have to ... Stellar Magnetic Activity can be inferred by amount of Chromospheric Ca H and K emission ...
Extreme Environmental Conditions: Despite its remote positioning relative to the Sun, Aditya-L1 faces the daunting task of enduring the incredibly intense temperatures and radiation associated with the Sun’s vicinity.
Title ~36pt Arial Black Title Author: Terri A. Cantrell Last modified by: Bruce W. Lites Created Date: 1/14/2002 6:19:56 PM Document presentation format
Low first-ionization-potential (FIP) contribute to ne and ... Not enough contrast for faculae and plage. Umbra profile has reversal unlike the observed ...
1Astronomick stav AV CR, v.v.i., Ondrejov 2Astronomical Institute, University ... a) Optical observations (Multichannel Subtractive Double Pass spectrograph ...
blue wing absorbed. red wing absorbed. outflow. inflow. Ha blueshift. Ha redshift ... Short wavelength (blue) emission wing. Long wavelength (red) emission wing ...
Simulations taking on a new degree of realism. Beginnings of confrontation of ... Magneto-convection (both strong and weak field cases): detailed comparison of ...
From detailed magneto-convection simulations to modelling the ... Institute of Theoretical Astrophysics, University of Oslo. Monterey February 14 2006 ...
stop near the separatrix between active regions and thus appear as a stationary front ... The EIT wave stopped near the separatrix. Discussion. Model of the EIT wave ...
... (1973): Physical Properties of Solar Plages. Physical properties of solar ... Brian Wood (1996): The Physical Properties and Dynamics of Stellar Transition ...
From the solar photosphere: acoustic and magnetic waves. Produced in situ: ... Lighthill-Stein Theory of Sound Generation (Lighthill 1952; Stein 1967) ...
... Extended Atmospheres Photosphere Chromosphere Transition region Corona Wind Corona Observed during solar eclipses or by coronagraph (electron scattering in ...
A Model of the Chromosphere: Heating, Structures, and Convection P. Song1, and V. M. Vasyli nas1,2 Center for Atmospheric Research and Department of Environmental ...
Micro-Flare and High-Speed Down-Flow ... (3) University of Tokyo, (4) Instituto de Astrof sica ... Tower Telescope (VTT), and made a movie of spectrogram. ...
A Space Weather Doppler Imager Mission Concept. Exploration Science Objectives ... Successful space weather forecasting entails reliable characterization of ...
We hypothesize that, since relaxation-based NLFFF techniques tend to smooth ... Free energy is the energy difference between the actual and potential field energies. ...
Task 1B: measure and map the magnetic free energy ... IX: Business plan: Resources ... X: Business plan: Implementation [Define key milestones, test procedures, ...
Photosphere. Spectroscopic observations. 2) origin of the dv2 -1/2 ... Photosphere. Resolution scale. LOS depth. 23. Are low q/m ions hotter than the others ? ...
Focus on interrelation between a star's rotation rate and its magnetic field strength. ... long term trends e.g. Maunder Minimum from 1645: 70 years of no spots ...
Magneto-convection Movies from Hinode/SOT Granules (weak B) Umbral dots (strong B) Magnetic fields suppress convection. Example of convection simulation ...
magnetic field to produce the aurora borealis. Solar flares can also ... Cause of the Aurora. After a solar flare, it takes 2 to 4 days for the solar wind and ...
Long-term optical studies (flare activity; activity cycles, ... Partecipation to the ESA cornerstone mission GAIA; Partecipation to the future ESA mission PLATO. ...
... fields heat the solar atmosphere. Magnetic outbursts affect ... great Northern Lights. Solar flares, prominences, and coronal mass ejections. Global warming ...
Granulation pattern (Tg) in photosphere. Inverse granulation (Tg) in lower-chromosphere ... can now observationally follow emergence from photosphere to corona...
An Introduction to the Physics of Our Star: The Sun Distance from Earth 1 AU Travel time for Light to Earth About 8 minutes Travel time for solar wind to 1 AU
The method of coronal seismology (Uchida 1970; Roberts et al 1984) based on ... We used the observed properties of the waves for coronal seismology. ...
Tom Bogdan, Johnson, Petty-Powell, Zita, et al., 2002, Waves in magnetic flux ... Matt Johnson, Sara Petty-Powell, E.J. Zita, 2001, Energy Transport by MHD waves ...
Temperature stratification of solar atmosphere. Temperature minimum ... The Solar Optical Telescope (SOT) on Hinode observes photosphere and chromosphere ...