Possible emission lines from the gaseous β Pictoris disk

A. Lecavelier Des Etangs; L. M. Hobbs; A. Vidal-Madjar; H. Beust; P. D. Feldman; R. Ferlet; A. M. Lagrange; W. Moos; M. McGrath

Possible emission lines from the gaseous β Pictoris disk

A. Lecavelier Des Etangs
, L. M. Hobbs
, A. Vidal-Madjar
, H. Beust
, P. D. Feldman
, R. Ferlet
, A. M. Lagrange
, W. Moos
, M. McGrath

École Polytechnique

Yerkes Observatory
CNRS
LTHE (UMR 5564 CNRS/IRD/Université de Grenoble)
Johns Hopkins University
Space Telescope Science Institute

Résultats de recherche: Contribution à un journal › Article › Revue par des pairs

Résumé

We present the results of exploratory HST observations to detect the emission lines of ions in the β Pictoris disk with the spectrograph slit placed off the star. Possible emission lines from Fe n have been detected at ∼ 10^-14erg cm^-2 s^-1 at 0.5″ from β Pictoris, which would suggest a total Fe II density of ≳ 2 · 10^-2cm^-3 at 10 AU. This detection needs confirmation. If real, it requires a large production rate of gas and dust equivalent to the total disruption of ten bodies 30 kilometers in radius per year.

langue originale	Anglais
Pages (de - à)	691-694
Nombre de pages	4
journal	Astronomy and Astrophysics
Volume	356
Numéro de publication	2
état	Publié - 1 déc. 2000

Contient cette citation

@article{3d96a407b4b244a1846d034ad1aa3177,

title = "Possible emission lines from the gaseous β Pictoris disk",

abstract = "We present the results of exploratory HST observations to detect the emission lines of ions in the β Pictoris disk with the spectrograph slit placed off the star. Possible emission lines from Fe n have been detected at ∼ 10-14erg cm-2 s-1 at 0.5″ from β Pictoris, which would suggest a total Fe II density of ≳ 2 · 10-2cm-3 at 10 AU. This detection needs confirmation. If real, it requires a large production rate of gas and dust equivalent to the total disruption of ten bodies 30 kilometers in radius per year.",

keywords = "Methods: data analysis, Stars: circumstellar matter, Stars: individual: βPic, Stars: planetary systems",

author = "\{Lecavelier Des Etangs\}, A. and Hobbs, \{L. M.\} and A. Vidal-Madjar and H. Beust and Feldman, \{P. D.\} and R. Ferlet and Lagrange, \{A. M.\} and W. Moos and M. McGrath",

year = "2000",

month = dec,

day = "1",

language = "English",

volume = "356",

pages = "691--694",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

number = "2",

}

TY - JOUR

T1 - Possible emission lines from the gaseous β Pictoris disk

AU - Lecavelier Des Etangs, A.

AU - Hobbs, L. M.

AU - Vidal-Madjar, A.

AU - Beust, H.

AU - Feldman, P. D.

AU - Ferlet, R.

AU - Lagrange, A. M.

AU - Moos, W.

AU - McGrath, M.

PY - 2000/12/1

Y1 - 2000/12/1

N2 - We present the results of exploratory HST observations to detect the emission lines of ions in the β Pictoris disk with the spectrograph slit placed off the star. Possible emission lines from Fe n have been detected at ∼ 10-14erg cm-2 s-1 at 0.5″ from β Pictoris, which would suggest a total Fe II density of ≳ 2 · 10-2cm-3 at 10 AU. This detection needs confirmation. If real, it requires a large production rate of gas and dust equivalent to the total disruption of ten bodies 30 kilometers in radius per year.

AB - We present the results of exploratory HST observations to detect the emission lines of ions in the β Pictoris disk with the spectrograph slit placed off the star. Possible emission lines from Fe n have been detected at ∼ 10-14erg cm-2 s-1 at 0.5″ from β Pictoris, which would suggest a total Fe II density of ≳ 2 · 10-2cm-3 at 10 AU. This detection needs confirmation. If real, it requires a large production rate of gas and dust equivalent to the total disruption of ten bodies 30 kilometers in radius per year.

KW - Methods: data analysis

KW - Stars: circumstellar matter

KW - Stars: individual: βPic

KW - Stars: planetary systems

M3 - Article

AN - SCOPUS:0041171522

SN - 0004-6361

VL - 356

SP - 691

EP - 694

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 2

ER -

Possible emission lines from the gaseous β Pictoris disk

Résumé

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