NEI Modeling What do we have? What do we need? 2012.08.09 AtomDB workshop Hiroya Yamaguchi (CfA) ion population in CIE (AtomDB v.2.0.2) Temperature (keV) Fe 24+ Fe 25+ Fe 26+ Fe 16+ APED/APEC state-of-the-art dataset for He- & H-like ions of Z<=30 (+ DR lines of Fe) X-ray-emitting plasma: T = 10 6-8 K (0.1-10 keV) most of atoms are ionized to b He- or H-like states in CIE
11
Embed
NEI Modeling What do we have? What do we need? 2012.08.09 AtomDB workshop Hiroya Yamaguchi (CfA) Fe ion population in CIE (AtomDB v.2.0.2) Temperature.
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
NEI ModelingWhat do we have? What do we need?
2012.08.09 AtomDB workshopHiroya Yamaguchi (CfA)
Fe ion population in CIE (AtomDB v.2.0.2)
Temperature (keV)
Fe24+
Fe25+
Fe26+Fe16+
APED/APEC state-of-the-art dataset for He- & H-like ions of Z<=30 (+ DR lines of Fe)
X-ray-emitting plasma: T = 106-8 K (0.1-10 keV)most of atoms are ionized to be He- or H-like states in CIE
Supernova Remnants = NEI !!
E0102-72
H-dominant (solar abundance) matterheavy elements are neutral
metal-rich, almost neutral
Shock-heated electrons ionize heavy elements.
t = ne t = 1012 (cm-3 s) t = 30000 (ne /1cm-3)-1 yr
Supernova Remnants = NEI !!
ne t (cm-3 s)
Fe ion population in NEI (AtomDB v.2.0.2)
Fe24+
Fe25+
Fe26+Fe16+
kTe = 20 keV
typical SNRs
- Inner-shell process is essentially important for SNRs!- APEC can calculate ion population, but doesn’t output emission.
SNRs’ spectra of Fe K-shell band
9
3C397 (Type II)
Kepler (Type Ia)
Cr MnFe
Ni
Fe Kb
6.44 keV -> Fe XVII-XVIII (Palmeri+03)
Ne-likeneutral He-like
RCW86
G272
SN1006
Tycho
Kepler G344
0509
0519N103B W49B
CasA
3C397 G349
G292G350
N132D
Innershell ionization of Be-like ionsLi-like : 1s2s2 (2S) -> wK = 0 (for single-configuration wave function) in fact, K&M(1993) gave zero values for every Li-like ions.
Lighter elements are usually ionized to be He-like state.
but a few exception…0509-67.5: Kb from low-ionized Si (Warren & Hughes 04)Tycho: low-ionized Ca (Hwang+98)
Also needed:Si thru Ca (Ne-like – Li-like)and L-shell data for Fe, Ca, Ni, …
Recombining plasma
RRC (Fe25+ -> Fe24+)
Fe24+ Ka
W49B (Ozawa+09)
What’s the origin? - collision with dense stellar wind matter and following adiabatic cooling? (HY+09)- thermal conduction into cloudy matter? (Zhou+11)
We only know nFe25+ /nFe24+ from the RRC/line ratio…(~ 0.06 in W49B)
Fe ion population in CIE (Mazzotta+98)
Temperature (keV)
Fe24+
Fe25+
Fe26+Fe16+
then, used k = 0.04 to estimate Fe abundance and density.
We (wrongly) assumed that ion pop in arbitrary recomb plasma is consistent to that in CIE plasma with a certain electron temperature.
Recombining plasma
ne t (cm-3 s)
Fe24+
Fe25+
Fe26+Fe16+
kTe = 0.5 keV
temperature (keV)
ne t (cm-3 s)
CIE
IonizingRecombining plasma model in XSPEC must be useful.We do already have atomic data!
Some difficulty… Ionizing: kTe, net, abundances, normalization Recombining: + initial ion population -> 3-dimensional
Summary
Ionizing NEI plasma - APEC is ready. - Fluorescence data are completed for all elements (Z <=30)! except for Kb lines from lowly-ionized atoms (Kaastra & Mewe’s is no longer needed.) - EII/EIE rates for Fe & Ni are calculated by Kris & collaborators! - EII/EIE rates for Cr & Mn would be mostly important now. - and other abundant elements, Si, S, Ca…
Recombining plasma - APEC & APED are both (almost) ready. - one more parameter (init ion pop.) is needed.