X-Ray Emission from Planetary Nebulae Calculated by 1D Spherical Numerical Simulations

Abstract

We calculate the X-ray emission from both constant and time evolving shocked fast winds blown by the central stars of planetary nebulae (PNs) and compare with observations. Using spherically symmetric numerical simulations with radiative cooling, we calculate the flow structure, and the X-ray temperature and luminosity of the hot bubble formed by the shocked fast wind. We find that a constant fast wind gives results that are very close to those obtained from the self-similar solution. We show that in order for a fast shocked wind to explain the observed X-ray properties of PNs, rapid evolution of the wind is essential. More specifically, the mass loss rate of the fast wind should be high early on when the speed is ~300-700 km/s, and then it needs to drop drastically by the time the PN age reaches ~1000 yr. This implies that the central star has a very short pre-PN (post-AGB) phase.

accepted to MNRAS

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Cited by in corpus (14)

• The Chandra X-ray Survey of Planetary Nebulae (ChanPlaNS): Probing Binarity, Magnetic Fields, and Wind Collisions
• Formation and X-ray emission from Hot Bubbles in Planetary Nebulae. I. Hot Bubble formation
• Formation and X-ray Emission from Hot Bubbles in Planetary Nebulae. II. Hot bubble X-ray emission
• Serendipitous Chandra X-ray Detection of a Hot Bubble within the Planetary Nebula NGC 5315
• The X-Ray Spectrum of a Planetary Nebula at High Resolution: Chandra Gratings Spectroscopy of BD+30 3639
• A Model for the Formation of Large Circumbinary Disks Around Post AGB Stars
• X-Ray Emission from Jet-Wind Interaction in Planetary Nebulae
• Serendipitous XMM-Newton Detection of X-ray Emission from the Bipolar Planetary Nebula Hb 5
• Narrow Radiative Recombination Continua: A Signature of Ions Crossing the Contact Discontinuity of Astrophysical Shocks
• Diffuse X-ray Emissions from Dynamic Planetary Nebulae
• Comparing shocks in planetary nebulae with the solar wind termination shock
• Consequences of Magnetic Field Structure for Heat Transport in Magnetohydrodynamics
• The Creation of AGB Fallback Shells
• Supernova remnants, planetary nebulae and superbubbles: prospects for new XMM-Newton observations