Multi-wavelength light curve model of the one year recurrence period nova M31N 2008-12a

Mariko Kato, Hideyuki Saio, Izumi Hachisu

研究成果: Article

20 引用 (Scopus)

抄録

We present a theoretical light curve model of the recurrent nova M31N 2008-12a, the current record holder for the shortest recurrence period (1 year).We combined interior structures calculated using a Henyey-type evolution code with optically thick wind solutions of hydrogen-rich envelopes, which give the proper mass-loss rates, photospheric temperatures, and luminosities. The light curve model is calculated for a 1.38 M⊙ white dwarf (WD) with an accretion rate of 1.6 × 10-7 M⊙ yr-1. This model shows a very high effective temperature (log Tph (K) > 4.97) and a very small wind mass-loss rate (Mwind < 9.3 × 10-6 M⊙ yr-1) even at the maximum expansion of the photosphere. These properties are consistent with the faint optical peak of M31N 2008-12a because the brightness of the free-free emission is proportional to the square of the mass-loss rate. The model well reproduces the short supersoft X-ray turn-on time of 6 days and turn-off time of 18 days after the outburst. The ejecta mass of our model is calculated to be 6.3 × 10 M⊙ 8 , corresponding to 37% of the accreted mass. The growth rate of the WD is 0.63 times the mass accretion rate, making it a progenitor for a SN Ia. Our light curve model predicts a bright supersoft X-ray phase one or two days before the optical peak. We encourage detection of this X-ray flash in future outbursts.

元の言語English
記事番号52
ジャーナルAstrophysical Journal
808
発行部数1
DOI
出版物ステータスPublished - 2015 7 20

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light curve
wavelength
wavelengths
outburst
accretion
x rays
ejecta
photosphere
holders
flash
brightness
envelopes
temperature
luminosity
rate
hydrogen
expansion
loss

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

これを引用

Multi-wavelength light curve model of the one year recurrence period nova M31N 2008-12a. / Kato, Mariko; Saio, Hideyuki; Hachisu, Izumi.

:: Astrophysical Journal, 巻 808, 番号 1, 52, 20.07.2015.

研究成果: Article

Kato, Mariko ; Saio, Hideyuki ; Hachisu, Izumi. / Multi-wavelength light curve model of the one year recurrence period nova M31N 2008-12a. :: Astrophysical Journal. 2015 ; 巻 808, 番号 1.
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abstract = "We present a theoretical light curve model of the recurrent nova M31N 2008-12a, the current record holder for the shortest recurrence period (1 year).We combined interior structures calculated using a Henyey-type evolution code with optically thick wind solutions of hydrogen-rich envelopes, which give the proper mass-loss rates, photospheric temperatures, and luminosities. The light curve model is calculated for a 1.38 M⊙ white dwarf (WD) with an accretion rate of 1.6 × 10-7 M⊙ yr-1. This model shows a very high effective temperature (log Tph (K) > 4.97) and a very small wind mass-loss rate (Mwind < 9.3 × 10-6 M⊙ yr-1) even at the maximum expansion of the photosphere. These properties are consistent with the faint optical peak of M31N 2008-12a because the brightness of the free-free emission is proportional to the square of the mass-loss rate. The model well reproduces the short supersoft X-ray turn-on time of 6 days and turn-off time of 18 days after the outburst. The ejecta mass of our model is calculated to be 6.3 × 10 M⊙ 8 , corresponding to 37{\%} of the accreted mass. The growth rate of the WD is 0.63 times the mass accretion rate, making it a progenitor for a SN Ia. Our light curve model predicts a bright supersoft X-ray phase one or two days before the optical peak. We encourage detection of this X-ray flash in future outbursts.",
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N2 - We present a theoretical light curve model of the recurrent nova M31N 2008-12a, the current record holder for the shortest recurrence period (1 year).We combined interior structures calculated using a Henyey-type evolution code with optically thick wind solutions of hydrogen-rich envelopes, which give the proper mass-loss rates, photospheric temperatures, and luminosities. The light curve model is calculated for a 1.38 M⊙ white dwarf (WD) with an accretion rate of 1.6 × 10-7 M⊙ yr-1. This model shows a very high effective temperature (log Tph (K) > 4.97) and a very small wind mass-loss rate (Mwind < 9.3 × 10-6 M⊙ yr-1) even at the maximum expansion of the photosphere. These properties are consistent with the faint optical peak of M31N 2008-12a because the brightness of the free-free emission is proportional to the square of the mass-loss rate. The model well reproduces the short supersoft X-ray turn-on time of 6 days and turn-off time of 18 days after the outburst. The ejecta mass of our model is calculated to be 6.3 × 10 M⊙ 8 , corresponding to 37% of the accreted mass. The growth rate of the WD is 0.63 times the mass accretion rate, making it a progenitor for a SN Ia. Our light curve model predicts a bright supersoft X-ray phase one or two days before the optical peak. We encourage detection of this X-ray flash in future outbursts.

AB - We present a theoretical light curve model of the recurrent nova M31N 2008-12a, the current record holder for the shortest recurrence period (1 year).We combined interior structures calculated using a Henyey-type evolution code with optically thick wind solutions of hydrogen-rich envelopes, which give the proper mass-loss rates, photospheric temperatures, and luminosities. The light curve model is calculated for a 1.38 M⊙ white dwarf (WD) with an accretion rate of 1.6 × 10-7 M⊙ yr-1. This model shows a very high effective temperature (log Tph (K) > 4.97) and a very small wind mass-loss rate (Mwind < 9.3 × 10-6 M⊙ yr-1) even at the maximum expansion of the photosphere. These properties are consistent with the faint optical peak of M31N 2008-12a because the brightness of the free-free emission is proportional to the square of the mass-loss rate. The model well reproduces the short supersoft X-ray turn-on time of 6 days and turn-off time of 18 days after the outburst. The ejecta mass of our model is calculated to be 6.3 × 10 M⊙ 8 , corresponding to 37% of the accreted mass. The growth rate of the WD is 0.63 times the mass accretion rate, making it a progenitor for a SN Ia. Our light curve model predicts a bright supersoft X-ray phase one or two days before the optical peak. We encourage detection of this X-ray flash in future outbursts.

KW - novae cataclysmic variables

KW - stars: individual (M31N 2008-12a)

KW - supernovae: general

KW - white dwarfs

KW - X-rays: binaries

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