A universal decline law of classical novae. III. GQ Muscae 1983

Izumi Hachisu; Mariko Kato; Angelo Cassatella

doi:10.1086/591415

A universal decline law of classical novae. III. GQ Muscae 1983

Izumi Hachisu, Mariko Kato, Angelo Cassatella

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30 Citations (Scopus)

Abstract

We present a unified model of infrared (IR), optical, ultraviolet (UV ), and X-ray light curves for the 1983 outburst of GQ Muscae (Nova Muscae 1983) and estimate its white dwarf (WD) mass. Based on an optically thick wind model of nova outbursts, we model the optical and IR light curves with free-free emission, and the UV 1455 Å and supersoft X-ray light curves with blackbody emission. The best-fit model that simultaneously reproduces the IR, optical, UV 1455 Å, and supersoft X-ray observations is a 0.7 ± 0.05 M_⊙ WD with an assumed chemical composition of the envelope of X = 0.35-0.55, X_CNO = 0.2-0.35, and Z = 0.02 by mass weight. The mass lost by the wind is estimated to be ΔM_wind ∼ 2 × 10^-5 M_&odot. We provide a new determination of the reddening, E(B - V) = 0.55 ± 0.05, and of the distance, ∼5 kpc. Finally, we discuss the strong UV flash that took place on JD 2,445,499 (151 days after the outburst).

Original language	English
Pages (from-to)	1236-1252
Number of pages	17
Journal	Astrophysical Journal
Volume	687
Issue number	2
DOIs	https://doi.org/10.1086/591415
Publication status	Published - 2008 Nov 10
Externally published	Yes

Keywords

Novae, cataclysmic variables
Stars: individual (GQ Muscae)
Stars: mass loss
Ultraviolet: stars
White dwarfs
X-rays: binaries

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/591415

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title = "A universal decline law of classical novae. III. GQ Muscae 1983",

abstract = "We present a unified model of infrared (IR), optical, ultraviolet (UV ), and X-ray light curves for the 1983 outburst of GQ Muscae (Nova Muscae 1983) and estimate its white dwarf (WD) mass. Based on an optically thick wind model of nova outbursts, we model the optical and IR light curves with free-free emission, and the UV 1455 {\AA} and supersoft X-ray light curves with blackbody emission. The best-fit model that simultaneously reproduces the IR, optical, UV 1455 {\AA}, and supersoft X-ray observations is a 0.7 ± 0.05 M⊙ WD with an assumed chemical composition of the envelope of X = 0.35-0.55, XCNO = 0.2-0.35, and Z = 0.02 by mass weight. The mass lost by the wind is estimated to be ΔMwind ∼ 2 × 10-5 M&odot. We provide a new determination of the reddening, E(B - V) = 0.55 ± 0.05, and of the distance, ∼5 kpc. Finally, we discuss the strong UV flash that took place on JD 2,445,499 (151 days after the outburst).",

keywords = "Novae, cataclysmic variables, Stars: individual (GQ Muscae), Stars: mass loss, Ultraviolet: stars, White dwarfs, X-rays: binaries",

author = "Izumi Hachisu and Mariko Kato and Angelo Cassatella",

year = "2008",

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doi = "10.1086/591415",

language = "English",

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AU - Hachisu, Izumi

AU - Kato, Mariko

AU - Cassatella, Angelo

PY - 2008/11/10

Y1 - 2008/11/10

N2 - We present a unified model of infrared (IR), optical, ultraviolet (UV ), and X-ray light curves for the 1983 outburst of GQ Muscae (Nova Muscae 1983) and estimate its white dwarf (WD) mass. Based on an optically thick wind model of nova outbursts, we model the optical and IR light curves with free-free emission, and the UV 1455 Å and supersoft X-ray light curves with blackbody emission. The best-fit model that simultaneously reproduces the IR, optical, UV 1455 Å, and supersoft X-ray observations is a 0.7 ± 0.05 M⊙ WD with an assumed chemical composition of the envelope of X = 0.35-0.55, XCNO = 0.2-0.35, and Z = 0.02 by mass weight. The mass lost by the wind is estimated to be ΔMwind ∼ 2 × 10-5 M&odot. We provide a new determination of the reddening, E(B - V) = 0.55 ± 0.05, and of the distance, ∼5 kpc. Finally, we discuss the strong UV flash that took place on JD 2,445,499 (151 days after the outburst).

AB - We present a unified model of infrared (IR), optical, ultraviolet (UV ), and X-ray light curves for the 1983 outburst of GQ Muscae (Nova Muscae 1983) and estimate its white dwarf (WD) mass. Based on an optically thick wind model of nova outbursts, we model the optical and IR light curves with free-free emission, and the UV 1455 Å and supersoft X-ray light curves with blackbody emission. The best-fit model that simultaneously reproduces the IR, optical, UV 1455 Å, and supersoft X-ray observations is a 0.7 ± 0.05 M⊙ WD with an assumed chemical composition of the envelope of X = 0.35-0.55, XCNO = 0.2-0.35, and Z = 0.02 by mass weight. The mass lost by the wind is estimated to be ΔMwind ∼ 2 × 10-5 M&odot. We provide a new determination of the reddening, E(B - V) = 0.55 ± 0.05, and of the distance, ∼5 kpc. Finally, we discuss the strong UV flash that took place on JD 2,445,499 (151 days after the outburst).

KW - Novae, cataclysmic variables

KW - Stars: individual (GQ Muscae)

KW - Stars: mass loss

KW - Ultraviolet: stars

KW - White dwarfs

KW - X-rays: binaries

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A universal decline law of classical novae. III. GQ Muscae 1983

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Keywords

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