Chemical abundances and dust in the halo planetary nebula K648 IN M15: its origin and evolution based on an analysis of multiwavelength data

Journal Article · Wed Apr 01 04:00:00 EDT 2015 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/217/2/22· OSTI ID:22872406

Otsuka, Masaaki ^[1]; Hyung, Siek ^[2]; Tajitsu, Akito ^[3]

---

1. Institute of Astronomy and Astrophysics, Academia Sinica P.O. Box 23-141, Taipei 10617, Taiwan (China)
2. School of Science Education (Astronomy), Chungbuk National University, CheongJu, Chungbuk 361-763 (Korea, Republic of)
3. Subaru Telescope, NAOJ, 650 North A’ohoku Place, Hilo, HI 96720 (United States)

We report on an investigation of the extremely metal-poor and C-rich planetary nebula (PN) K648 in M15 using the UV to far-infrared data obtained using Subaru, the Hubble Space Telescope, the Far Ultraviolet Spectroscopic Explorer, Spitzer, and Herschel. We determined the nebular abundances of 10 elements. The enhancement of F ([F/H] = +0.96) is comparable to that of the halo PN BoBn1. The central stellar abundances of seven elements are determined. The stellar C/O ratio is similar to the nebular C/O ratios from recombination lines and from collisionally excited lines (CELs) within error, and the stellar Ne/O ratio is also close to the nebular CEL Ne/O ratio. We found evidence of carbonaceous dust grains and molecules including Class B 6–9 and 11.3 μm polycyclic aromatic hydrocarbons and the broad 11 μm feature. The profiles of these bands are similar to those of the C-rich halo PNe H4-1 and BoBn1. Based on the theoretical model, we determined the physical conditions of the gas and dust and their masses, i.e., 0.048 and 4.95 × 10{sup −7} M{sub ⊙}, respectively. The observed chemical abundances and gas mass are in good agreement with an asymptotic giant branch nucleosynthesis model prediction for stars with an initial 1.25 M{sub ⊙} plus a 2.0 × 10{sup −3} M{sub ⊙} partial mixing zone (PMZ) and stars with an initial mass of 1.5 M{sub ⊙} without a PMZ. The core mass of the central star is approximately 0.61–0.63 M{sub ⊙}. K648 is therefore likely to have evolved from a progenitor that experienced coalescence or tidal disruption during the early stages of evolution, and became a ∼1.25–1.5 M{sub ⊙} blue straggler.

• OSTI ID: 22872406
• Journal Information: Astrophysical Journal, Supplement Series, Journal Name: Astrophysical Journal, Supplement Series Journal Issue: 2 Vol. 217; ISSN 0067-0049; ISSN APJSA2
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ABUNDANCE
ASYMPTOTIC SOLUTIONS
CARBON
COALESCENCE
COSMIC DUST
ERRORS
FAR ULTRAVIOLET RADIATION
MASS
NEON
NUCLEOSYNTHESIS
OXYGEN
PLANETARY NEBULAE
RECOMBINATION
STARS
TELESCOPES