from spectral lines to emission measures emission measure distributions of different stars
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Emission Measure Distributions: A Tutorial Nancy S. Brickhouse Harvard-Smithsonian Center for Astrophysics. New England Space Science Cambridge, MA March 1, 2006. From Spectral Lines to Emission Measures Emission Measure Distributions of Different Stars Hot Research Questions - PowerPoint PPT PresentationTRANSCRIPT
Emission Measure Distributions: A Tutorial
Nancy S. Brickhouse
Harvard-Smithsonian Center for Astrophysics
• From Spectral Lines to Emission Measures
• Emission Measure Distributions of Different Stars
• Hot Research Questions
Coronal Structure
Coronal Abundances
Coronal heating: flares and nanoflares
New England Space ScienceCambridge, MA March 1, 2006
We use UV, EUV, and X-ray Lines from log T = 4.0 to 8.0
Chandra
From Spectral Lines to Emission Measure
Line Flux = ∑ ε (T) EM(T) / (4 π R2), where
R is the distance,
EM (T) = ∫ Ne NH dV is the emission measure, and
ε (T) depends on a lot of atomic physics, e.g.
ionization and recombination rates collisional excitation rates radiative decay rates
AND we make a number of assumptions, such as negligible optical depth collisional ionization equilibrium
Emission Measure Distributions for Different Stars
I .Understanding Coronal StructureRotation and ActivityEvolution
Sun (G2 V)Yohkoh Image
Capella (G8 III + G1 III);Expanding Loops?
Hot Research Questions
Chandra Gratings
Capella
Electron Density Determination
•Compelling evidence for high density, small emitting region(s)
•Multiple pressures in the system
Lower Pressure; L=.02 R*
High Pressure; L=.003 R*
II. Abundances: Continuum and Line Modeling
HR 1099High Neon AbundanceAn Inverse FIP Effect?
Hot Research Questions
Hot Research QuestionsIII. Coronal heating: flares
> 1 day flare with exponential decay
Eclipse gives the extent of the flare loop
Algol
Hot Research Topics
III. Coronal heating: nanoflares
Discrepancies are not explained by: atomic rate uncertainties calibration uncertainties absorption time variability
IEUV ΩEUV [Te]
—— = ———— exp (-ΔE/kTe)
IX-ray ΩX-ray[Te]
6 MK EMD peak
Breaking the Assumptions of Emission Measure Distribution Analysis
We consider episodic heating (nanoflares) with:
- heat input to the chromosphere
- adiabatic expansion with rapid cooling.
We calculate the time-dependent ionization state
and obtain the resulting line emission.
Chromosphere
B
Te(0) = 12 MKNe(0) = 4 x 1012 cm-3
~cs
Loop Footpoint
Energetic Beam Te(t) = 5 MK
Ne(t) = 1012 cm-3
Δt~ 1 sec
Chromosphere