PPT-Global Structure of the Solar Corona

Roberto J Pérez UPRM Charles Kankelborg MSU Sarah Jaeggli MSU Abstract The AIA instrument on the Solar Dynamics Observatory obtains images of the sun in seven different extreme ultraviolet wavebands Each filter produces images with distinctive appearance that is apparent to experienced observers Subjective descriptions abound in the literature and in conference presentations as do qualitative explanations of the physical reasons for these differences We seek a quantitative description of the image properties with the aim of understanding what the general image properties indicate about the temperature structure of the corona Our preliminary results obtained at multiple heliocentric angles above and below the limb show that some channels consistently present a high or low intensity contrast which we attribute to the differing temperature density and filling factor of the structures imaged We also investigate the power spectra characteristic of each waveband . Robust Low Atomicity Peer-To-Peer . Systems. Rizal . Mohd. . Nor. Mikhail . Nesterenko. Christian Scheideler. Overlay Networks and Stabilization. self-stabilization . guarantees that. starting from . Steven R. Spangler, University of Iowa. Division of Plasma Physics, American Physical Society. To gain a perspective on gaseous media in space, first consider a more familiar gaseous medium….the Earth’s atmosphere. Louise Harra. lkh. @mssl.ucl.ac.uk. UCL Department of Space and Climate Physics. Mullard Space Science Laboratory. Extended solar minimum. Hinode X-ray corona. 2007 Oct. – 2009 Apr.. The solar wind is weaker… . Solar Observatory . Location . The University of Hawaii . About. 3,054 meters (approximately 10,000 feet) above sea level.. It is used for many different purposes other than a solar observatory. However the . 24.3. The Sun .  . Because the sun is made of gas, no sharp boundaries exist between its various layers. Keeping this in mind, we can divide the sun into four parts: the solar interior; the visible surface, or photosphere; and two atmospheric layers, the chromosphere and corona.. Chashei. I.V., . Shishov. V.I., . Tyul’bashev. S.A., . Oreshko. V.V., . Subaev. . S.A.. . Radio telescope BSA LPI (Big Scanning Array of . Lebedev. Physical Institute) . Frequency 111 MHz. Bandwidth 2.5 MHz, sampling rate 0.1 s . 16.1 Physical Properties of the Sun. 16.2 The Solar Interior. . SOHO. : Eavesdropping on the Sun. 16.3 The Sun’s Atmosphere. 16.4 Solar Magnetism. 16.5 The Active Sun. Solar. –. Terrestrial Relations. The core of the sun is . approx. . 15,000,000 . degrees . Kelvin. . . The sun gives out heat by turning Hydrogen into Helium (it loses about . 4,000,000 . Hydrogen . tons . per second doing this). All the energy is created in the core of the sun, this energy is transferred to the surface by radiation. However we receive the heat in the form of Radiation.. Emily E. Richards (NRC-NRL). Tracy Clarke (NRL). Simona . Giacintucci. (NRL). Qian Wang (UMD, College Park). Maxim . Markevitch. (NASA Goddard). Cool X-ray Coronae in Cluster Galaxies. 2001:. discovery of thermal X-ray coronae in two Coma cluster galaxies (. James A. . Klimchuk. . NASA Goddard Space Flight Center . Hinode. / SOT. Disclaimer:. This discussion concerns spicules as observationally distinct features.. Spicules may by just one manifestation of a larger sequence of events that generates waves and creates electric currents that could potentially give rise to substantial coronal heating.. In paper I (Huang et al. 2012, ApJ, 755), we showed that solar minimum, quiet-Sun coronal loops exhibited new structures we dubbed ``down-loops” - loops in which the temperature decreases with height SOHO SOHO, the Solar and Heliospheric Observatory, is a project of international Together with two other ESA missions, Cluster and Ulysses, SOHO is studying the Sun-Earth interaction from different Ken Phillips. Scientific Associate, Natural History Museum, and Honorary . Prof.. , QUB. 1. Solar Corona: Physical Properties. Solar corona has very . high temperatures:. . 10. 6. K – 2. ×10. 6. -. What Fermi Adds to the Picture. Brian R. Dennis. GSFC, Solar Physics Lab., Code 671. High Energy Solar . Flares. Eruptive Events. Tutorial on Solar Eruptive Events. Analysis of GBM spectral data.