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CSI 769-001/PHYS 590-001 Solar Atmosphere Fall 2004 Lecture 12 Nov. 17, 2004
Filament/Prominence Eruption
Corona Mass Ejection (CME)
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Filament/Prominence
Meudon (France)
Hα
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Filament/Prominence
BBSO Hα
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Filament/Prominence
•Filament/Prominence: dense clouds of chromospheric-temperature material suspended in the corona
•The filament material is either from cooling of coronal plasma or direct injection of chromospheric material
•A filament can remain in a quiet or quiescent state for days or weeks
•A filament can erupt and rise of the Sun over the course of a few minutes or hours
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Filament in different regions
•Active Region Filament•in active region•small in size•shortly lived in time (e.g., day)
•Quiescent Filament•in quiet Sun region•long in size•relatively long lived (e.g., week)
• Polar Crown Filament•close to polar coronal hole region•very long, e.g., circling the whole Sun at high latitude• very long lived (e.g., month)
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Filament in different regions (cont’d)
•Exp., Polar Crown Filament
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Filament Configuration
BBSO Hα Mt. Wilson Magnetogram
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Filament Configuration
•A filament always sits along the magnetic inversion line (magnetic neutral line) that separates regions of different magnetic polarity
•A filament is supported by coronal magnetic field in a supporting configuration
•Magnetic dip at the top of loop arcade (2-D)•Magnetic flux rope (3-D)
•Helical or twisted magnetic structure is seen within filament
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Filament Configuration
•One of filament models: filament is supported by twisted magnetic flux rope
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Filament Eruption
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Filament Eruption
BBSO Hα on 2003/08/05
BBSO Hα on 2002/11/24
BBSO Hα on 2004/03/24
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Filament Eruption
TRACE 195 Å, 1999/10/20
Filament eruption and loop arcade
TRACE 195 Å, 2002/05/27
A failed filament eruption
TRACE 195 Å, 1998/07/27
Filament internal motion
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Filament Eruption Model
•One model by Martens & Kuin
A unified model ofFilament andFlare
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Filament Channel
•A filament channel refers to the envisioned magnetic structure surrounding a filament. It may be larger than the filament itself.
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CME (Coronal Mass Ejection)• A CME is a large scale coronal structure of plasma (and
associated magnetic field) that is being ejected from the Sun, as seen by a coronagraph
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Coronagraph
• Coronagraph• A telescope equipped with an occulting disk that
blocks out light from the disk of the Sun, in order to observe faint light from the corona
• A coronagraph makes artificial solar eclipse
• CMEs are observed by coronagraphs
• The earliest CME observation was made in early 1970s
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White light seen in Corona
• Textbook P. 135-142
• K (continuum) corona, caused by scattering of photospheric light of rapidly-moving coronal electrion (so called Thomson scattering); the major component of white-light corona
• F (Fraunhofer corona), caused by scattering of photospheric light off dust in interplanetary space between the orbits of Mercury and Earth
• E (Emission corona), caused by emission of radiation by highly-ionized species in the actual corona, so called forbidden emission lines, e.g., at 5302 Å from Fe XIV (coronal green line)
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White light from Corona (cont’d)
• K corona: continuum (what a solar physicist wants)• F corona: continuum plus absorption (do not want)• E corona: emission lines (textbook P. 139, Fig. 5.9)
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White light from Corona (cont’d)
• K corona brightness is less than 10-5 that of disk• The instrument design is to reduce scattering of light
(Textbook P.5, Figure 1.3)
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LASCO Coronagraphs
•C1: 1.1 – 3.0 Rs (E corona) (1996 to 1998, then died)•C2: 2.0 – 6.0 Rs (white light) (1996 up to today)•C3: 4.0 – 30.0 Rs (white light) (1996 up to today)
C1 C2 C3•LASCO uses a set of three overlapping coronagraphs to maximum the total effective field of view. A single coronagraph’s field of view is limited by the instrumental dynamic range.
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Streamer
Several streamers in a typical coronagraph image
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Streamer (cont’d)
•A streamer is a stable large-scale structure in the white-light corona.
•It has an appearance of extending away from the Sun along the radial direction•It is often associated with active regions and filaments/filament channels underneath.•It overlies the magnetic inversion line in the solar photospheric magnetic fields. •When a CME occurs underneath a streamer, the associated streamer will be blown away•When a CME occurs nearby a streamer, the streamer may be disturbed, but not necessarily disrupted.