An infrared nebula associated with δ Cephei: Evidence of mass loss?

M. Marengo; N. R. Evans; P. Barmby; L. D. Matthews; G. Bono; D. L. Welch; M. Romaniello; D. Huelsman; K. Y.L. Su; G. G. Fazio

doi:10.1088/0004-637X/725/2/2392

An infrared nebula associated with δ Cephei: Evidence of mass loss?

M. Marengo, N. R. Evans, P. Barmby, L. D. Matthews, G. Bono, D. L. Welch, M. Romaniello, D. Huelsman, K. Y.L. Su, G. G. Fazio

Steward Observatory

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

43 Scopus citations

Abstract

We present the discovery of an infrared nebula around the Cepheid prototype δ Cephei and its hot companion HD 213307. Large-scale (∼2.1 × 10⁴ AU) nebulosity is detected at 5.8, 8.0, 24, and 70 μm. Surrounding the two stars, the 5.8 and 8.0 μm emission is largely attributable to polycyclic aromatic hydrocarbon emission swept from the interstellar medium by a wind originating from δ Cephei and/or its companion. Stochastically heated small dust grains are the most likely source of the 24 and 70 μm extended emission. The 70 μm emission, in particular, resembles a bow shock aligned in the direction of the proper motion of δ Cephei. This discovery supports the hypothesis that δ Cephei may be currently losing mass, at a rate in the range of ≈5 × 10^-9 to 6 × 10^-8M⊙ yr^-1.

Original language	English (US)
Pages (from-to)	2392-2400
Number of pages	9
Journal	Astrophysical Journal
Volume	725
Issue number	2
DOIs	https://doi.org/10.1088/0004-637X/725/2/2392
State	Published - Dec 20 2010

Keywords

Infrared: stars
Stars: individual (delta Cephei)
Stars: mass-loss
Stars: variables: Cepheids

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/725/2/2392

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title = "An infrared nebula associated with δ Cephei: Evidence of mass loss?",

abstract = "We present the discovery of an infrared nebula around the Cepheid prototype δ Cephei and its hot companion HD 213307. Large-scale (∼2.1 × 104 AU) nebulosity is detected at 5.8, 8.0, 24, and 70 μm. Surrounding the two stars, the 5.8 and 8.0 μm emission is largely attributable to polycyclic aromatic hydrocarbon emission swept from the interstellar medium by a wind originating from δ Cephei and/or its companion. Stochastically heated small dust grains are the most likely source of the 24 and 70 μm extended emission. The 70 μm emission, in particular, resembles a bow shock aligned in the direction of the proper motion of δ Cephei. This discovery supports the hypothesis that δ Cephei may be currently losing mass, at a rate in the range of ≈5 × 10-9 to 6 × 10-8M⊙ yr-1.",

keywords = "Infrared: stars, Stars: individual (delta Cephei), Stars: mass-loss, Stars: variables: Cepheids",

author = "M. Marengo and Evans, {N. R.} and P. Barmby and Matthews, {L. D.} and G. Bono and Welch, {D. L.} and M. Romaniello and D. Huelsman and Su, {K. Y.L.} and Fazio, {G. G.}",

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doi = "10.1088/0004-637X/725/2/2392",

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T1 - An infrared nebula associated with δ Cephei

T2 - Evidence of mass loss?

AU - Marengo, M.

AU - Evans, N. R.

AU - Barmby, P.

AU - Matthews, L. D.

AU - Bono, G.

AU - Welch, D. L.

AU - Romaniello, M.

AU - Huelsman, D.

AU - Su, K. Y.L.

AU - Fazio, G. G.

PY - 2010/12/20

Y1 - 2010/12/20

N2 - We present the discovery of an infrared nebula around the Cepheid prototype δ Cephei and its hot companion HD 213307. Large-scale (∼2.1 × 104 AU) nebulosity is detected at 5.8, 8.0, 24, and 70 μm. Surrounding the two stars, the 5.8 and 8.0 μm emission is largely attributable to polycyclic aromatic hydrocarbon emission swept from the interstellar medium by a wind originating from δ Cephei and/or its companion. Stochastically heated small dust grains are the most likely source of the 24 and 70 μm extended emission. The 70 μm emission, in particular, resembles a bow shock aligned in the direction of the proper motion of δ Cephei. This discovery supports the hypothesis that δ Cephei may be currently losing mass, at a rate in the range of ≈5 × 10-9 to 6 × 10-8M⊙ yr-1.

AB - We present the discovery of an infrared nebula around the Cepheid prototype δ Cephei and its hot companion HD 213307. Large-scale (∼2.1 × 104 AU) nebulosity is detected at 5.8, 8.0, 24, and 70 μm. Surrounding the two stars, the 5.8 and 8.0 μm emission is largely attributable to polycyclic aromatic hydrocarbon emission swept from the interstellar medium by a wind originating from δ Cephei and/or its companion. Stochastically heated small dust grains are the most likely source of the 24 and 70 μm extended emission. The 70 μm emission, in particular, resembles a bow shock aligned in the direction of the proper motion of δ Cephei. This discovery supports the hypothesis that δ Cephei may be currently losing mass, at a rate in the range of ≈5 × 10-9 to 6 × 10-8M⊙ yr-1.

KW - Infrared: stars

KW - Stars: individual (delta Cephei)

KW - Stars: mass-loss

KW - Stars: variables: Cepheids

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JO - Astrophysical Journal

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ER -

An infrared nebula associated with δ Cephei: Evidence of mass loss?

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