Plasma diagnostics for planetary nebulae and H II regions using N II and O II

I. McNabb (1), X. Fang (1), X.-W. Liu (1,2), P.J. Storey (3)

(1) Kavli Institute of Astronomy and Astrophysics at Peking University. (2) Department of Astronomy at Peking University. (3) Department of Physics and Astronomy at University College London

We carry out plasma diagnostic analysis for a number of planetary nebulae (PNe) and H II regions. We use N II and O II optical recombination lines (ORLs) with new effective recombination coefficients calculated under the intermediate coupling scheme, for a range of electron temperatures (Te) and densities (Ne) and fitted against the most reliable measurements. Comparing Te derived from ORLs, collisionally excited lines (CELs), the hydrogen Balmer Jump, and/or He I if available, we find the relation Te (ORLs) < Te (He I) < Te (H I BJ) < Te (CELs), confirming the physical conditions in the two-abundance model postulated by Liu et al. (2000), i.e. the nebula contains another cold, metal-rich and probably H-deficient component.

–> See poster

Advertisements
This entry was posted in Atomic data production and tagged , , , , . Bookmark the permalink.

One Response to Plasma diagnostics for planetary nebulae and H II regions using N II and O II

  1. Jorge garcía-Rojas says:

    The conclusions of this work are generalized to PNe and HII regions, but there is only a point in the sample being and HII region (the Orion nebula) and its behavior is just the opposite than those of PNe, as showed also in Garcia-Rojas & Esteban (2007)

Leave a Reply

Fill in your details below or click an icon to log in:

WordPress.com Logo

You are commenting using your WordPress.com account. Log Out / Change )

Twitter picture

You are commenting using your Twitter account. Log Out / Change )

Facebook photo

You are commenting using your Facebook account. Log Out / Change )

Google+ photo

You are commenting using your Google+ account. Log Out / Change )

Connecting to %s