X-RAY SPECTROSCOPY
AND ATOMIC DATA
Current Status

Collaborators

Outline

Introduction

Features of the X-Ray Band:
Highly Ionized Atoms

A New Era in X-Ray Astrophysics:
Chandra and XMM-Newton

The Difference High Spectral Resolution Makes (Capella)

Stellar Coronae:
Hot, Collisional X-Ray Sources

Coronal Steady-State Approximations

Coronal Steady-State Approximations

Stellar Coronae (cont.):
Temperatures and Abundances

Coronal Abundances (cont.)
Fe-L uncertainties most suspect

Galaxy Clusters:
Absence of the Cooling Flows

Dielectronic Recombination (DR): The weak link in the ioniz. balance

When the coronal approximation breaks down

Beyond the Coronal Regime (cont.) Density Diagnostics

Presence of UV Field

Can we trust rates for transition
among excited levels?

Fe-L Quick Summary

There is Life After Fe-L

The world beyond Fe-L (e.g. Ar)

Collisional Plasmas:
Atomic Data Status

Spectroscopic Measurements in
Photoionized Plasma

1s-2p (Ka) Inner-Shell Absorption

1s-2p Inner-Shell Line Comparison

Inner-Shell Line Comparison

Need for Laboratory Experiments
Z Pinch (& Laser Plasma)

Inner-Shell Absorption (cont.)
Fe M-shell 2p-3d UTA

Fe M-shell 2p-3d UTA (cont.)

Type II AGN (cont.)
Measuring Elemental Abundances

Low-T DR of Fe-L

Photoexcitation-Autoionization

Conclusions