Post on 24-Feb-2016
description
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
05090519
N103B 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.
Configuration interaction (CI) effect cannot be ignoredyCI = c1 1s2s2 (2S) + c2 1s2p2 (2S) ; c2 ~ 0.3 (Gorczyca+2006)
wK ≠ 0 ! Li-like(Gorczyca+06)
Innershell process- Innershell ionization/excitation- Fluorescence or Auger (Kaastra & Mewe 93)
… SPEX, XSPEC NEI v.1
l
# of electrons
Fe Ka a energy(Mendoza+04)
K&M93
this work
Atomic data for emission above 5 keV
Fe I-XVI XVII-XIV Ni I-XVIII XIX-XVI Cr, Mn
Ar, Aa Palmeri+03aMendoza+04
Gorczyca+03;06Hasogle 08 (thesis)
Palmeri+08a Palmeri+12l (Ka) Palmeri
+03b
l (Kb) (not detected) (not detected)
x-sec (EII) phenomenological formula (Haque+06)
x-sec (EIE) (IRON Project)
Kris
Kris
DR data for Fee.g., Bautista & Badnell 07
Atomic data for emission below 5 keV Ar, Aa, l (Ka) for all ionization states
Palmeri+08b, Kucas+12: Ne, Mg, Si, S, Ar, CaPalmeri+11: AlPalmeri+12: Na, Cl, Ti, Zn, etc.(Z <= 30)
No longer need Kaastra & Mewe’s data
Si XII
Fe LS XIV
Ar XVI
Ca XVIII
Fe
Kepler
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)
Abundance & density are important information.
Recombining plasma
RRC (Fe25+ -> Fe24+)
Fe24+ Ka
W49B (Ozawa+09)
a (recomb rate) : Badnell+06k = nFe25+ / (nFe26+ + nFe25+ + nFe24+ + …)
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.