Novae in globular clusters

Mariko Kato, Izumi Hachisu, Martin Henze

Research output: Contribution to journalArticlepeer-review

18 Citations (Scopus)


We present the first light-curve analysis of Population II novae that appeared in M31 globular clusters. Our light-curve models, based on the optically thick wind theory, reproduce well both the X-ray turn-on and turnoff times with the white dwarf (WD) mass of about 1.2 M for M31N 2007-06b in Bol 111 and about 1.37 M for M31N 2010-10f in Bol 126. The transient supersoft X-ray source CXO J004345 in Bol 194 is highly likely a nova remnant of 1.2-1.3 M WD. These WD masses are quite consistent with the temperatures deduced from X-ray spectra. We also present the dependence of nova light curves on the metallicity in the range from [Fe/H] = 0.4 to -2.7. Whereas strong optically thick winds are accelerated in Galactic disk novae owing to a large Fe opacity peak, only weak winds occur in Population II novae with low Fe abundance. Thus, nova light curves are systematically slow in low Fe environment. For an extremely low Fe abundance normal nova outbursts may not occur unless the WD is very massive. We encourage V or y filter observation rather than R as well as high cadence X-ray monitorings to open quantitative studies of extragalactic novae.

Original languageEnglish
Article number19
JournalAstrophysical Journal
Issue number1
Publication statusPublished - 2013 Dec 10
Externally publishedYes


  • X-rays: binaries
  • novae, cataclysmic variables
  • stars: Population II
  • stars: individual (M31N 2007-06b, M31N 2010-10f, CXO J004345)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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