prominence-corona transition region
DESCRIPTION
Prominence-Corona Transition Region. T. Kucera, NASA/GSFC ISSI Prominence Cavity Team Jan. 2009. Outline. Basic structure of the TR What it looks like in the EUV Prominence Motions - Models and Observations ISSI Prominence Group Topics. What is the PCTR?. - PowerPoint PPT PresentationTRANSCRIPT
Prominence-Corona Transition Region
T. Kucera,
NASA/GSFC
ISSI Prominence Cavity Team
Jan. 2009
Outline
• Basic structure of the TR• What it looks like in the EUV • Prominence Motions - Models and Observations• ISSI Prominence Group Topics
What is the PCTR?
B
Material between the bulk of the prominence material at T<104 Kand the corona at T>106 K.
What is the PCTR?
Corona
PCTR
PCTR
Prominence
Corona
What is the PCTR?
What is the PCTR?
What is the PCTR?
Other TR Temperature Radiation
What does it actually look like?
Prominences at 304 Å
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304 Å STEREO/SECCHI/EUVI
304 Å SOHO/EIT
Contributions:He II collisionally excited (50,000-90,000 K)He II scattered (~104 K) (See Labrosse et al.)
Lyman absorption (~104 K)Si XI (~106 K)
SOHO/CDS Chiuderi-Drago & Landi 2002
Coronal Emission?
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prominence associated jetTRACE Chae 2003
Erupting prominence, EIT 195 ÅCiaravella et al. 2000
Not always. These transient bright features at 171 and 195 Å probably around 250,000 K.
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TRACE 171(?) A
Differential Emission Measures
Cirigliano et al. 2004 SOHO/SUMER and CDS
DEMs assume•Ionization equilibrium•Optically thin plasma
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Karpen et al. 2008
Prominence Motions
Prominences are dynamic!
Quiescent prominences in H show steady flows, including counter-streaming, up to 20 km/s, and sometimes show faster motions.
Prominences observed in EUV and UV often show faster motions (30-70 km/s)
Prominence Motions
Study prominence motions at different temperatures to understand their properties and how they are related.
Goal: to test theories of prominence formation(which tie into theories of magnetic structure).
Rising Magnetic Field
Priest, van Ballegooijen, Mackay, 1996
Reconnection driven flows
Wang, 1999
Chromospheric Heating/Siphon Flow Models
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Karpen et al.
Studies of Motions in Prominences - Results
Many motions in the EUV seem to be pretty fastSome seem to have detectable H components.
Are there EUV components to slower H motions? Its hard to tell, but this may be a resolution problem.
In general DEMs of motions look rather like DEMs of prominences of a whole.
One difference is the extent to which you can see >300,000 K material in the structure.
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TRACE Ly and 1600 Å bands, May 26, 2000
SVST H Integrated Intensity and Doppler, May 26, 2000
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Activated Prominence and Cool LoopApr. 17, 2003
Kucera & Landi 2006
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Prominence between active regionsApr. 29, 2004
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Quiet and Activated Prominence Apr. 30 -May 1, 2004
DEMs of Moving Prominence Features
Different from others Promience DEMs because
•Made using as small a piece of a moving feature as possible (in time and space)
•When possible “background” has been estimated or subtracted
Calculated with using method of Landi & Landini 1997
Sample DEMs of Prominence Motions
Loop Differential Emission Measures
Kucera & Landi 2006
Many motions in the EUV seem to be pretty fastSome seem to have detectable H components.
Are there EUV components to slower H motions? Its hard to tell, but this may be a resolution problem.
In general DEMs of moving features look rather like DEMs of prominences of a whole.
One difference is the extent to which you can see >300,000 K material in the structure.
Plans & the Future
•Can Dynamic Equilibrium Model simulate the short times scale DEMs?
•SDO might be able to help understanding of the “high temperature” TR. Does this have any connection to very high temperature emission associated w/ prominences (“Chewy Nougat”)?
ISSI Prominence Group - Some topics
•Prominence Radiative Transfer Observations & Modeling- Lyman Absorption, He lines•PCTR related observations and diagnostics•Flows•Oscillations•Prominence magnetic field, its formations and relationship to the cavity field (Aad)