NEI Modeling What do we have? What do we need? 2012.08.09 AtomDB workshop Hiroya Yamaguchi (CfA) Fe...
-
Upload
jonas-watkins -
Category
Documents
-
view
215 -
download
0
Transcript of NEI Modeling What do we have? What do we need? 2012.08.09 AtomDB workshop Hiroya Yamaguchi (CfA) Fe...
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.
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, AaPalmeri+03aMendoza+04
Gorczyca+03;06Hasogle 08 (thesis)
Palmeri+08a Palmeri+12
l (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.