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.
| Original language | English |
|---|---|
| Article number | 52 |
| Journal | Astrophysical Journal |
| Volume | 808 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 2015 Jul 20 |
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Keywords
- novae cataclysmic variables
- stars: individual (M31N 2008-12a)
- supernovae: general
- white dwarfs
- X-rays: binaries
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
Multi-wavelength light curve model of the one year recurrence period nova M31N 2008-12a. / Kato, Mariko; Saio, Hideyuki; Hachisu, Izumi.
In: Astrophysical Journal, Vol. 808, No. 1, 52, 20.07.2015.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Multi-wavelength light curve model of the one year recurrence period nova M31N 2008-12a
AU - Kato, Mariko
AU - Saio, Hideyuki
AU - Hachisu, Izumi
PY - 2015/7/20
Y1 - 2015/7/20
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
UR - http://www.scopus.com/inward/record.url?scp=84940388439&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84940388439&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/808/1/52
DO - 10.1088/0004-637X/808/1/52
M3 - Article
AN - SCOPUS:84940388439
VL - 808
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 52
ER -