thermal properties of moving prominence features seen in euv
DESCRIPTION
Thermal Properties of Moving Prominence Features Seen in EUV. Terry Kucera (NASA/GSFC). Enrico Landi (NRL) and Judy Karpen (GSFC). Study Goals. Measure thermal properties of individual moving prominence features and compare them to model outputs, particularly the Dynamic Equilibrium Model. - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/1.jpg)
Thermal Properties of Moving Prominence Features Seen in EUV
Terry Kucera (NASA/GSFC)
Enrico Landi (NRL) and Judy Karpen (GSFC)
![Page 2: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/2.jpg)
Study Goals
• Measure thermal properties of individual moving prominence features and compare them to model outputs, particularly the Dynamic Equilibrium Model
![Page 3: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/3.jpg)
Targets
Apr. 29, 2004 Large prominence between active regions
Apr. 17, 2003 Quiet and Activated Prominence
Apr. 30, 2004 Erupting Prominence
Apr. 30 -May 1, 2004 Quiet and Activated prominence
![Page 4: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/4.jpg)
Data
Ion Wavelength (Å) Temp. (K)
N III 764.34 80,000
N III 763.33 80,000
N IV 765.15 160,000
S V 786.47 160,000
O IV
O V
787.715
760.43,760.21
200,000250,000
O V 761.13 250,000
O V 761.99 250,000
Ne VIII 770.42 630,000
Mg VIII 782.34 790,000
Mg VIII 762.65 790,000
S X
S XI
787.558
783.01
1,000,0001,500,000
SOHO/SUMER2" resolution, 120" slit length90 sec cadence Waveband Sources of
EmissionTemp. (K)
20,000 1216 Å Ly
1600 Å C IV 100,000
C I, Fe II, Si Cont.
4,000-10,000
195 Å H & He continuum absorption,
10,000-30,000
Fe XII 1,500,000
TRACE1" resolution, 60-91 sec cadence
Global Hα Network1.1 resolution, 1 min cadence6563 Å H 10,000
![Page 5: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/5.jpg)
![Page 6: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/6.jpg)
![Page 7: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/7.jpg)
![Page 8: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/8.jpg)
DEM techniqueLandi & Landini 1997Assumes:
Ionization EquilibriumOptically thin plasmaSmooth function (spline)
Also:No material below 104 K or above 108 KCoronal abundances
Does not trust points below LogT=4.4 (ionization fraction problems - charge transfer not well understood)
or Na or Li -like ions (ionization fraction not sufficiently well understood)
We tried where possible to subtract off or compare to a background component
![Page 9: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/9.jpg)
DEM comments
In general these curves tend to look pretty similarThey are different in many details from other prominence DEMs
Transition region temperature lines pretty goodBig gap between O V (LogT 5.4) and Ne VIII ( LogT 5.8)Ne VIII lines the only really strong ones for LogT≥5.8
![Page 10: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/10.jpg)
Typical DEM
![Page 11: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/11.jpg)
Typical DEM background subtracted
![Page 12: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/12.jpg)
Comparison of SUMER and CDS
![Page 13: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/13.jpg)
Dynamic Equilibrium Model
Karpen & Antiochos 2008.
![Page 14: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/14.jpg)
Karpen & Antiochos 2008
![Page 15: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/15.jpg)
Typical DEM background subtracted
![Page 16: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/16.jpg)
![Page 17: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/17.jpg)
![Page 18: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/18.jpg)
![Page 19: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/19.jpg)
Data Results
•Prominence DEMs uniform for T< 250,000 K from on prominence to the next, but with minimum at higher temp than prominence DEMs from other studies.
•For T>250,000 K (i.e., Ne VIII) the amount of emission varied
•DEMs of individual moving features show the same high slope at low T seen in DEMs taken over prominences over longer periods of time, so a model in which this portion of the DEM is replicated by many sources is not adequate.
![Page 20: Thermal Properties of Moving Prominence Features Seen in EUV](https://reader036.vdocument.in/reader036/viewer/2022062519/56814f16550346895dbca896/html5/thumbnails/20.jpg)
Dynamic Equilibrium Model comparison
Previously Karpen & Antiochos (2008) showed that the average of a long run of the model could be successfully compared to DEM spectra taken over long time periods.
Here we see that the DEM of a short run of the model (5 min) exhibits the same shape, so a single moving feature in the model exhibits high amounts a material in the low temperature TR.
High temperature TR curve is consistent with “background subtracted” DEMs.
Differences with individual feature DEMs Temp minima