A Self-consistent Model for a Full Cycle of Recurrent Novae - Wind Mass-loss Rate and X-Ray Luminosity

Mariko Kato, Hideyuki Saio, Izumi Hachisu

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10 Citations (Scopus)

Abstract

An unexpectedly slow evolution in the pre-optical-maximum phase was suggested in the very short recurrence period of nova M31N 2008-12a. To obtain reasonable nova light curves we have improved our calculation method by consistently combining optically thick wind solutions of hydrogen-rich envelopes with white dwarf (WD) structures calculated by a Henyey-type evolution code. The wind mass-loss rate is properly determined with high accuracy. We have calculated light curve models for 1.2 M o and 1.38 M o WDs with mass accretion rates corresponding to recurrence periods of 10 yr and 1 yr, respectively. The outburst lasts 590/29 days, in which the pre-optical-maximum phase is 82/16 days, for 1.2/1.38 M o, respectively. Optically thick winds start at the end of the X-ray flash and cease at the beginning of the supersoft X-ray phase. We also present supersoft X-ray light curves including a prompt X-ray flash and later supersoft X-ray phase.

Original languageEnglish
Article number153
JournalAstrophysical Journal
Volume838
Issue number2
DOIs
Publication statusPublished - 2017 Apr 1

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Keywords

  • X-rays: binaries
  • novae, cataclysmic variables
  • stars: individual (M31N 2008-12a)
  • white dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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