IUE and ISO observations of the bipolar proto-planetary nebula Hen 401 (IRAS 10178-5958)
| Autor: | D. de Martino, Yoshikazu Nakada, Lsf de Cordoba, P Garcia-Lario, G. Gauba, [No Value] Pottasch, Takahiro Fujii, Mudumba Parthasarathy |
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| Přispěvatelé: | Astronomy |
| Jazyk: | angličtina |
| Rok vydání: | 2001 |
| Předmět: |
Infrared
MODELS Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics medicine.disease_cause CO OBSERVATIONS EMISSION BANDS PROTOPLANETARY NEBULAE PREPLANETARY NEBULAE medicine Astrophysics::Solar and Stellar Astrophysics OUTFLOW Emission spectrum planetary nebulae : individual : Hen 401 ultraviolet : stars Astrophysics::Galaxy Astrophysics Physics Nebula SPECTRUM POST-AGB STAR Near-infrared spectroscopy Astronomy Astronomy and Astrophysics Circumstellar envelope Planetary nebula stars : evolution EXTINCTION stars : emission-line Space and Planetary Science Spectral energy distribution Astrophysics::Earth and Planetary Astrophysics OBJECTS Ultraviolet stars : AGB and post-AGB |
| Zdroj: | Astronomy & astrophysics, 376(3), 941-949. EDP Sciences |
| ISSN: | 1432-0746 0004-6361 |
| Popis: | We present ultraviolet (IUE) and infrared (ISO) observations of the bipolar proto-planetary nebula Hen 401 which, combined with previously available optical and near infrared data, are used to reconstruct the overall spectral energy distribution from 1150 Angstrom to 100 mum. The ISO spectrum is dominated by strong PAH emission superimposed on a very cold continuum which is interpreted as thermal emission originating in the C-rich cool dust (similar to 106 K) present in the circumstellar envelope, the remnant of the previous AGB phase. In addition, a second, hotter component detected in the near infrared is attributed to thermal emission from hot dust (similar to 640 K), suggesting that mass loss and dust grain formation is still on-going during the current post-AGB phase. The ultraviolet (IUE) spectrum shows a stellar continuum in the wavelength interval 2400 Angstrom to 3200 Angstrom which corresponds to a moderately reddened B8-type central star. Unexpectedly, the UV flux in the wavelength interval 1150 Angstrom to 1900 Angstrom is very weak or absent with no evidence of a hotter binary companion which could explain the detection of the nebular emission lines observed in the available ground-based optical spectra of Hen 401. HST WFPC2 high resolution images also show no indication of a hot companion to the B8-type central star observed both in the optical and in the UV. The evolutionary implications of a possible single nature for the central star of Hen 401 are discussed. |
| Databáze: | OpenAIRE |
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