The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission

V. H. Tyne; S. P. S. Eyres; T. R. Geballe; B. Smalley; H. W. Duerbeck; M. Asplund; A. Evans

doi:10.1046/j.1365-8711.2000.03412.x

The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission

V. H. Tyne, S. P. S. Eyres, T. R. Geballe, B. Smalley, H. W. Duerbeck, M. Asplund, A. Evans

Faculty of Computing, Engineering and Science

Research output: Contribution to journal › Article › peer-review

Abstract

We report further UKIRT spectroscopic observations of Sakurai's object (V4334 Sgr) made in 1999 April/May in the 1–4.75 μm range, and find that the emission is dominated by amorphous carbon at Td~600 K. The estimated maximum grain size is 0.6 μm, and the mass lower limit is 1.7±0.2×10−8 M⊙ to 8.9±0.6×10−7 M⊙ for distances of 1.1–8 kpc. For 3.8 kpc the mass is 2.0±0.1×10−7 M⊙.

We also report strong He i emission at 1.083 μm, in contrast to the strong absorption in this line in 1998. We conclude that the excitation is collisional, and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998.

Original language	English
Pages (from-to)	595-599
Journal	Monthly Notices of the Royal Astronomical Society
Volume	315
Issue number	3
DOIs	https://doi.org/10.1046/j.1365-8711.2000.03412.x
Publication status	Published - 1 Jul 2000

Keywords

stars: AGB and post-AGB
circumstellar matter
stars: individual: Sakurai's Object
stars: individual: V4334 Sgr
infrared: stars

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10.1046/j.1365-8711.2000.03412.xLicence: CC BY-NC-ND

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title = "The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission",

abstract = "We report further UKIRT spectroscopic observations of Sakurai's object (V4334 Sgr) made in 1999 April/May in the 1–4.75 μm range, and find that the emission is dominated by amorphous carbon at Td~600 K. The estimated maximum grain size is 0.6 μm, and the mass lower limit is 1.7±0.2×10−8 M⊙ to 8.9±0.6×10−7 M⊙ for distances of 1.1–8 kpc. For 3.8 kpc the mass is 2.0±0.1×10−7 M⊙.We also report strong He i emission at 1.083 μm, in contrast to the strong absorption in this line in 1998. We conclude that the excitation is collisional, and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998.",

keywords = "stars: AGB and post-AGB, circumstellar matter, stars: individual: Sakurai's Object, stars: individual: V4334 Sgr, infrared: stars",

author = "Tyne, {V. H.} and Eyres, {S. P. S.} and Geballe, {T. R.} and B. Smalley and Duerbeck, {H. W.} and M. Asplund and A. Evans",

year = "2000",

month = jul,

day = "1",

doi = "10.1046/j.1365-8711.2000.03412.x",

language = "English",

volume = "315",

pages = "595--599",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

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TY - JOUR

T1 - The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission

AU - Tyne, V. H.

AU - Eyres, S. P. S.

AU - Geballe, T. R.

AU - Smalley, B.

AU - Duerbeck, H. W.

AU - Asplund, M.

AU - Evans, A.

PY - 2000/7/1

Y1 - 2000/7/1

N2 - We report further UKIRT spectroscopic observations of Sakurai's object (V4334 Sgr) made in 1999 April/May in the 1–4.75 μm range, and find that the emission is dominated by amorphous carbon at Td~600 K. The estimated maximum grain size is 0.6 μm, and the mass lower limit is 1.7±0.2×10−8 M⊙ to 8.9±0.6×10−7 M⊙ for distances of 1.1–8 kpc. For 3.8 kpc the mass is 2.0±0.1×10−7 M⊙.We also report strong He i emission at 1.083 μm, in contrast to the strong absorption in this line in 1998. We conclude that the excitation is collisional, and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998.

AB - We report further UKIRT spectroscopic observations of Sakurai's object (V4334 Sgr) made in 1999 April/May in the 1–4.75 μm range, and find that the emission is dominated by amorphous carbon at Td~600 K. The estimated maximum grain size is 0.6 μm, and the mass lower limit is 1.7±0.2×10−8 M⊙ to 8.9±0.6×10−7 M⊙ for distances of 1.1–8 kpc. For 3.8 kpc the mass is 2.0±0.1×10−7 M⊙.We also report strong He i emission at 1.083 μm, in contrast to the strong absorption in this line in 1998. We conclude that the excitation is collisional, and is probably caused by a wind, consistent with the P Cygni profile observed by Eyres et al. in 1998.

KW - stars: AGB and post-AGB

KW - circumstellar matter

KW - stars: individual: Sakurai's Object

KW - stars: individual: V4334 Sgr

KW - infrared: stars

U2 - 10.1046/j.1365-8711.2000.03412.x

DO - 10.1046/j.1365-8711.2000.03412.x

M3 - Article

VL - 315

SP - 595

EP - 599

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -

The continuing saga of Sakurai's object (V4334 Sgr): dust production and helium line emission

Abstract

Keywords

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