Sun
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In order to get a better understanding of coronal mass ejection (CME) events that occur on the Sun, C2H2 researchers create numerical simulations to model real CMEs observed by satellites. Reproducing observed results through simulations helps explain and constrain the underlying physics, boundary conditions, and processes behind a CME’s creation and evolution. To illustrate how numerical simulations are carried out, we describe a case in which a series of CMEs was modeled by C2H2 researchers. X-class flare from AR 9236
C2H2 - Simulations of Specific Events
Regular contributor M.A. Vukcevic has kindly given permission to reproduce some ongoing research which will be of interest to people learning about earthquakes and their precursor indicators. Vukcevic states: “the tb’s talkshop does not take any responsibility either for statements or data presented.
M.A. Vukcevic: Earthquakes and Geomagnetic Storms « tallbloke's talkshop
The "Solar Flare" is an explosive release of energy (both electromagnetic and charged particles) within a relatively small (but greater than earth-sized) region of the solar atmosphere. Solar flares happen 150 million kilometres (93 million miles) away from Earth but can damage satellites and interfere with terrestrial communications and power supplies. Solar Wind The thermal energy of ionized coronal gas is so great that Sun's gravitational field cannot retain the gas in a confined static atmosphere. Instead, there is a continuous, near-radial, outflow of charged particles into interplanetary space, called solar wind.
What the #$*! is all this about - Earth in Danger
We present here work carried out over the last decade focused on understanding the large scale coronal evolution and signatures associated with coronal mass ejection (CME) generation. In particular we present a (1) summary of the use of x-ray arcades as CME proxies, (2) the resultant discovery of certain "active locations" for CMEs in the declining phase of the solar cycle, and (3) the suggestion that besides the 2D photospheric shearing due to differential rotation we should consider 3D shearing due to different rotational dynamics for the photosphere and the corona. Coronal Streamers, Coronal Arcades and CMEs The Solar Maximum Mission (SMM) observations [Hundhausen, 1993] suggested that there was an association between the white light streamers which are the main source of CMEs (as seen in coronagraphs) and the dynamic coronal arcades seen in x-rays following at least some CMEs.
Coronal Topology and CMEs
A solar prominence is a cloud of gas ejected from the solar surface, supported by a loop of magnetic field. Although very hot, prominences are slightly colder than the surface. A prominence can last about a month, and eventually released, through a coronal mass ejection of hot gas throughout the solar system.
Solar prominences - Astronoo
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