X-ray Emission from PNe Martín A. Guerrero You-Hua Chu Robert A. Gruendl Univ. of Illinois APN III, Mt Rainier, 7/30/03

X-ray Expectations In a simple, adiabatic shock, it is possible to generate X-ray emitting plasma: T X ~ 1.5  10 7 K (v/1000 km/s) 2 PN central stars have fast stellar winds with terminal velocities up to 4,000 km/s ==> T X ~ 10 8 K PNe show fast collimated outflows with velocities >1,000 km/s (e.g. Hen ) ==> T X ~ 10 7 K Coronal activity from AGB stars or binary companions

ROSAT Observations of PNe ROSAT made useful observations of >60 PNe (Guerrero, Chu, & Gruendl 2000) Only three PNe were marginally resolved A Chu et al BD +30º Leahy et al NGC Kreysing et al Two additional PNe showed a hard X-ray component NGC Leahy et al NGC Guerrero et al Chandra spatial resolution times sharper XMM collecting area times larger Spectral resolution times better

Chandra and XMM Observations of PNe 3(4?) detections of point sources at the central star NGC 6543, NGC Guerrero et al Mz 3 -- Kastner et al Hen (?) -- this talk Chandra and XMM observations of 14 PNe 6 detections of diffuse X-ray emission BD Kastner et al NGC Chu et al NGC Kastner et al NGC Guerrero et al Mz 3 -- Kastner et al Hen Sahai, this meeting 4 non-detections of diffuse X-ray emission Hen 2-90, M 1-16, NGC 246, NGC 7293

NGC Chu et al. 2001; Guerrero et al B = X-ray, R= H-alpha, G = [N II] PNe with Diffuse X-ray Emission

NGC Guerrero et al PNe with Diffuse X-ray Emission

BD Kastner, Soker, Vrtilek, & Dgani 2000 NGC 7027 Kastner, Vrtilek, & Soker 2001

PNe with Diffuse X-ray Emission Mz 3 -- Kastner et al. 2003

PNe with Diffuse X-ray Emission Hen , Sahai (this meeting)

PNe with Diffuse X-ray Emission

X-ray Spectra of Hot Gas in PNe NGC 7009 T=1.7  10 6 K Hen T=2.4  10 6 K=>400 km s -1 NGC 6543 T=1.8  10 6 K BD T=3.0  10 6 K NGC 7027 T=3  10 6 K Mz 3 T=3-6  10 6 K

Morphology L X (erg/s) T (10 6 K) N (cm -3 ) NGC ~3  NGC 6543 limb-bright. 1.0  NGC 7027 bipolar? ~ ~3 150 BD  Mz 3 bipolar-jet? 3  Hen ~ Chandra and XMM-Newton Analysis of PNe

PNe without Diffuse X-ray Emission … PNe with modest velocity collimated outflows: Hen 2-90, M 1-16 Evolved PNe: NGC 246, NGC 7293 … but NGC 7293 central star!

… and also a Symbiotic Star with Bipolar Nebula Hen 2-104

PNe with X-ray-emitting Central Stars Chandra revealed hard X-ray point sources at the central stars of NGC 7293 and NGC 6543 (Guerrero et al. 2001) NGC 7293 central star shows variability in X-rays, as well as in the H-alpha line (Gruendl et al. 2001) Coronal activity from an unseen companion star (Guerrero et al. 2001; Soker & Kastner 2002) NGC 6543: a companion star or shocks in its fast stellar wind More recently, Mz 3 (Kastner et al. 2003), and maybe Hen

X-rays from PNe in a Nutshell (so far) Sharp shell morphology Young PNe (X-rays don’t last long) Central stars Fast collimated outflows (I mean, real fast) Something is going on along the major axis 4 more PNe have been observed by Chandra and 12 more will be observed by Chandra and XMM

Circumstellar Bubble Basic Model

O +5,N +4 X-ray Adiabatic shock Adopted from Weaver et al. (1977) for a 10 6 yr old O7 star Isothermal shock

Normalized radius  T 2001 Pittard, Dyson, & Hartquist 2001 Pittard, Hartquist, & Dyson Mass-loading and Ablation in Bubble Interiors Normalized radius

X-ray Spectra of Hot Gas in PNe

NGC 6888 S 308 Morphology limb-brightened? limb-brightened? L X (erg/s) 1.6  ~ 4  T (10 6 K) ~ 2 1.5, 28 (2.4 : 1) ASCA T 1.5, 8 Wrigge et al Wrigge 1999 ROSAT and ASCA Analysis of WR Bubbles

S 308 R - H  G - [O III] B - X-rays

R - H  G - [O III] B - X-rays Chandra Image of NGC 6888

R - H  G - [O III] B - X-rays S 308 and NGC 6888, two of a kind?

X-ray Spectra of Hot Gas in WR Bubbles Enhanced N/O - stellar wind or nebular? No hard component is needed. Previous claims are due to unresolved point sources.

M 17 Rosette Nebula L X (erg/s) 4   T (10 6 K) 1.5, 7 0.7, 9.3 ( 1:8.5 ) ( 1:3) N (cm -3 ) M (M  ) ~ The low L X reveals the effects of a strong magnetic field. Chandra Analysis of Superbubbles

X-ray Observations of Bubbles Detection of shocked fast stellar winds - 5 PNe, 2 WR bubbles, 2 HII regions Properties of the hot gas: T e [10 6 K ] N e [cm -3 ] L X [erg/s] PN 2-3   WR 1-2   HII (1-10)  10 6 low 10 33