Infrared observations of dust formation and coronal emission in nova aquilae 1995

C. G. Mason; R. D. Gehrz; Charles E. Woodward; J. B. Smiloerrz; Matthew A. Greenhouse; T. L. Hayward; J. R. Houck

doi:10.1086/177889

Infrared observations of dust formation and coronal emission in nova aquilae 1995

C. G. Mason, R. D. Gehrz, Charles E. Woodward, J. B. Smiloerrz, Matthew A. Greenhouse, T. L. Hayward, J. R. Houck

Minnesota Institute for Astrophysics

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Abstract

We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼ 1365-1600 km s^-1 (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a M_v-t₂ light decline relationship, we calculate a distance of ∼ 3.6-4.8 kpc.

Original language	English (US)
Pages (from-to)	577-582
Number of pages	6
Journal	Astrophysical Journal
Volume	470
Issue number	1 PART I
DOIs	https://doi.org/10.1086/177889
State	Published - Jan 1 1996

Keywords

Dust, extinction - Infrared
Individual (nova aquilae 1995)
Stars - Novae, cataclysmic variables stars

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@article{dde2d48968f04ef099f405a0afde0487,

title = "Infrared observations of dust formation and coronal emission in nova aquilae 1995",

abstract = "We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼ 1365-1600 km s-1 (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a Mv-t2 light decline relationship, we calculate a distance of ∼ 3.6-4.8 kpc.",

keywords = "Dust, extinction - Infrared, Individual (nova aquilae 1995), Stars - Novae, cataclysmic variables stars",

author = "Mason, {C. G.} and Gehrz, {R. D.} and Woodward, {Charles E.} and Smiloerrz, {J. B.} and Greenhouse, {Matthew A.} and Hayward, {T. L.} and Houck, {J. R.}",

year = "1996",

month = jan,

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doi = "10.1086/177889",

language = "English (US)",

volume = "470",

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journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1 PART I",

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TY - JOUR

T1 - Infrared observations of dust formation and coronal emission in nova aquilae 1995

AU - Mason, C. G.

AU - Gehrz, R. D.

AU - Woodward, Charles E.

AU - Smiloerrz, J. B.

AU - Greenhouse, Matthew A.

AU - Hayward, T. L.

AU - Houck, J. R.

PY - 1996/1/1

Y1 - 1996/1/1

N2 - We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼ 1365-1600 km s-1 (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a Mv-t2 light decline relationship, we calculate a distance of ∼ 3.6-4.8 kpc.

AB - We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼ 1365-1600 km s-1 (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a Mv-t2 light decline relationship, we calculate a distance of ∼ 3.6-4.8 kpc.

KW - Dust, extinction - Infrared

KW - Individual (nova aquilae 1995)

KW - Stars - Novae, cataclysmic variables stars

UR - http://www.scopus.com/inward/record.url?scp=0038946547&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0038946547&partnerID=8YFLogxK

U2 - 10.1086/177889

DO - 10.1086/177889

M3 - Article

AN - SCOPUS:0038946547

SN - 0004-637X

VL - 470

SP - 577

EP - 582

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART I

ER -

Infrared observations of dust formation and coronal emission in nova aquilae 1995

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