Dust Structure Around White Dwarf WD 1003-44 in 60 & 100 μm Iras Survey


  • Binil Aryal Central Department of Physics, Tribhuvan University, Kirtipur
  • Ronald Weinberger Institute of Astro- and Particle Physics, Innsbruck University, Innsbruck




White dwarf, Interstellar medium, Flux density, Interstellar dust, Mass of the gas


We studied the dust structures in 100 micron infrared image around the white dwarf WD 1003-441. The post Asymptotic Giant Branch (AGB) emission of the white dwarf's precursors' wind and the ambient interstellar matter is studied. For this, distribution of the relative flux density is studied and analyzed in the context of the dust color temperature, mass loading trend and the amount of total mass deposited due the interaction in the interstellar medium. The 100 micron far-infrared image is provided by the Groningen server of Infrared Astronomical Satellite (IRAS) survey. The curved emission structure at 100 micron in the region of interest is probably due to the interaction between the ambient interstellar medium and the He-flashes of the parent planetary nebula of the central white dwarf WD 1003-441. This white dwarf is a PG1159 star with 9-11 detected periods and an associated planetary nebula mass ejection. The total mass of the filamentary arc is found to be ~ 8 x 10-2 solar masses, as predicted. The mass loss rate of the post AGB star goes up to 10-5 solar masses per year. It is concluded that the first He-flash occurred at least ~1000 years ago. The amount of total mass around this white dwarf is about ~ 0.134 solar mass. The maximum and minimum dust color temperature around the white dwarf is found to be 19.0 K (±1.5 K) and 22.0 K (±2.0 K), respectively.

Key-Words: White dwarf; Interstellar medium; Flux density; Interstellar dust; Mass of the gas

The Himalayan Physics

Vol.2, No.2, May, 2011

Page: 5-10

Uploaded Date: 31 July, 2011


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How to Cite

Aryal, B., & Weinberger, R. (2011). Dust Structure Around White Dwarf WD 1003-44 in 60 & 100 μm Iras Survey. Himalayan Physics, 2(2), 5–10. https://doi.org/10.3126/hj.v2i2.5202