NEI Modeling What do we have? What do we need?

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.