The ISO-SWS spectrum of P Cygni.

H. J. G. L. M. Lamers; F. Najarro; R. P. Kudritzki; P. W. Morris; R. H. M. Voors; J. I. van Gent; L. B. F. M. Waters; T. de Graauw; D. Beintema; E. A. Valentijn; D. J. Hillier

The ISO-SWS spectrum of P Cygni.

H. J. G. L. M. Lamers, F. Najarro, R. P. Kudritzki, P. W. Morris, R. H. M. Voors, J. I. van Gent, L. B. F. M. Waters, T. de Graauw, D. Beintema, E. A. Valentijn, D. J. Hillier

Astronomy

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Abstract

The free-free IR excess and the IR emission lines of H and He I of the Luminous Blue Variable P Cygni are observed with the ISO-SWS instrument. The observed profiles and the free-free emission are compared with predictions from a non-LTE model atmosphere with a stellar wind. The observations agree very well with a model that has the following properties: T_eff_=18100K, R_*_=76Rsun_, He/H=0.30 by number, ˙(M)=3.0x10^-5^Msun_/yr and vinfinity_=185km/s. We observed forbidden emission lines of [Fe II], [Fe III], [Ni II], [Ne II], [Ne III] and [Si II]. From the study of the [Ne II] and [Ne III] lines we find that the Ne abundance is about three times higher than normal. This may be due to clumping in the CS envelope at r=~10^3^R_*_.

Original language	English
Pages (from-to)	L229-L232
Journal	Astronomy & Astrophysics
Volume	315
Publication status	Published - 1-Nov-1996

Keywords

STARS: EARLY-TYPE
STARS: MASS-LOSS
STARS: ATMOSPHERES
STARS: SUPERGIANTS
STARS: INDIVIDUAL: P CYGNI

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@article{fee2e22452e1432c81e936b91c567d01,

title = "The ISO-SWS spectrum of P Cygni.",

abstract = "The free-free IR excess and the IR emission lines of H and He I of the Luminous Blue Variable P Cygni are observed with the ISO-SWS instrument. The observed profiles and the free-free emission are compared with predictions from a non-LTE model atmosphere with a stellar wind. The observations agree very well with a model that has the following properties: T_eff_=18100K, R_*_=76Rsun_, He/H=0.30 by number, ˙(M)=3.0x10^-5^Msun_/yr and vinfinity_=185km/s. We observed forbidden emission lines of [Fe II], [Fe III], [Ni II], [Ne II], [Ne III] and [Si II]. From the study of the [Ne II] and [Ne III] lines we find that the Ne abundance is about three times higher than normal. This may be due to clumping in the CS envelope at r=~10^3^R_*_.",

keywords = "STARS: EARLY-TYPE, STARS: MASS-LOSS, STARS: ATMOSPHERES, STARS: SUPERGIANTS, STARS: INDIVIDUAL: P CYGNI",

author = "Lamers, {H. J. G. L. M.} and F. Najarro and Kudritzki, {R. P.} and Morris, {P. W.} and Voors, {R. H. M.} and {van Gent}, {J. I.} and Waters, {L. B. F. M.} and {de Graauw}, T. and D. Beintema and Valentijn, {E. A.} and Hillier, {D. J.}",

year = "1996",

month = nov,

day = "1",

language = "English",

volume = "315",

pages = "L229--L232",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = " EDP Sciences",

}

TY - JOUR

T1 - The ISO-SWS spectrum of P Cygni.

AU - Lamers, H. J. G. L. M.

AU - Najarro, F.

AU - Kudritzki, R. P.

AU - Morris, P. W.

AU - Voors, R. H. M.

AU - van Gent, J. I.

AU - Waters, L. B. F. M.

AU - de Graauw, T.

AU - Beintema, D.

AU - Valentijn, E. A.

AU - Hillier, D. J.

PY - 1996/11/1

Y1 - 1996/11/1

N2 - The free-free IR excess and the IR emission lines of H and He I of the Luminous Blue Variable P Cygni are observed with the ISO-SWS instrument. The observed profiles and the free-free emission are compared with predictions from a non-LTE model atmosphere with a stellar wind. The observations agree very well with a model that has the following properties: T_eff_=18100K, R_*_=76Rsun_, He/H=0.30 by number, ˙(M)=3.0x10^-5^Msun_/yr and vinfinity_=185km/s. We observed forbidden emission lines of [Fe II], [Fe III], [Ni II], [Ne II], [Ne III] and [Si II]. From the study of the [Ne II] and [Ne III] lines we find that the Ne abundance is about three times higher than normal. This may be due to clumping in the CS envelope at r=~10^3^R_*_.

AB - The free-free IR excess and the IR emission lines of H and He I of the Luminous Blue Variable P Cygni are observed with the ISO-SWS instrument. The observed profiles and the free-free emission are compared with predictions from a non-LTE model atmosphere with a stellar wind. The observations agree very well with a model that has the following properties: T_eff_=18100K, R_*_=76Rsun_, He/H=0.30 by number, ˙(M)=3.0x10^-5^Msun_/yr and vinfinity_=185km/s. We observed forbidden emission lines of [Fe II], [Fe III], [Ni II], [Ne II], [Ne III] and [Si II]. From the study of the [Ne II] and [Ne III] lines we find that the Ne abundance is about three times higher than normal. This may be due to clumping in the CS envelope at r=~10^3^R_*_.

KW - STARS: EARLY-TYPE

KW - STARS: MASS-LOSS

KW - STARS: ATMOSPHERES

KW - STARS: SUPERGIANTS

KW - STARS: INDIVIDUAL: P CYGNI

M3 - Article

SN - 0004-6361

VL - 315

SP - L229-L232

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

ER -

The ISO-SWS spectrum of P Cygni.

Abstract

Keywords

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