nei modeling what do we have? what do we need?
Post on 24-Feb-2016
Embed Size (px)
DESCRIPTIONNEI Modeling What do we have? What do we need?. Fe ion population in CIE ( AtomDB v.2.0.2). APED/APEC state-of-the-art dataset for He- & H-like ions of Z
Innershell Ionization & Fluorescence/Auger Yields Need of a new NEI code, required from observations
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 Fe XVII-XVIII (Palmeri+03)
Ne-likeneutralHe-likeRCW86G272SN1006TychoKeplerG34405090519N103BW49BCasA3C397G349G292G350N132D4Innershell 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 electronsFe Ka a energy(Mendoza+04)K&M93this workFor example, let us consider the innershell ionization of Be-like ions, this process leave Li-like ion with this state. Considering only this single configuration, the fluorescence decay from this state is forbidden. In fact, Kaastras table gave a probability of zero for every Li-like ions
However, once we take into account the configuration interaction, wave function is given like this, and fluorescence yield becomes non-zero.
5Atomic data for emission above 5 keVFe I-XVIXVII-XIVNi I-XVIIIXIX-XVICr, MnAr, AaPalmeri+03aMendoza+04Gorczyca+03;06Hasogle 08 (thesis) Palmeri+08aPalmeri+12l (Ka) Palmeri +03bl (Kb)(not detected)(not detected)x-sec (EII)phenomenological formula (Haque+06) x-sec (EIE)(IRON Project)KrisKrisDR data for Fee.g., Bautista & Badnell 07This is another impressive spectrum of this supernova remnant. Very strong lines of these elements are detected clearly, and they are also low ionized.
Fortunately, lower-Z elements such as Si, S, and so on, are ionized to He-like state in most SNRs, except for SN1006 and 0509 in the LMC, as far as I know. So, it seems that the emissivity of these elements are more important.
6Atomic data for emission below 5 keV Ar, Aa, l (Ka) for all ionization statesPalmeri+08b, Kucas+12: Ne, Mg, Si, S, Ar, CaPalmeri+11: AlPalmeri+12: Na, Cl, Ti, Zn, etc.(Z Fe24+)Fe24+ KaW49B (Ozawa+09)
Whats 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.APED is most widely-used atomic database for astrophysical plasma. But because it mainly focuses on equilibrium plasma, there are many limitation in innershell process, which are very important for NEI plasma.
Recombining plasmaRRC (Fe25+ -> Fe24+)Fe24+ KaW49B (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.APED is most widely-used atomic database for astrophysical plasma. But because it mainly focuses on equilibrium plasma, there are many limitation in innershell process, which are very important for NEI plasma.
ne t (cm-3 s)Fe24+Fe25+Fe26+Fe16+kTe = 0.5 keV
temperature (keV)ne t (cm-3 s)CIEIonizingRecombining 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-dimensionalAPED is most widely-used atomic database for astrophysical plasma. But because it mainly focuses on equilibrium plasma, there are many limitation in innershell process, which are very important for NEI plasma.
10SummaryIonizing NEI plasma - APEC is ready. - Fluorescence data are completed for all elements (Z