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ERRATUM: "HYDROGEN BURNING ON ACCRETING WHITE DWARFS: STABILITY, RECURRENT NOVAE, AND THE POST-NOVAE SUPERSOFT PHASE" (2013, ApJ, 777, 136)

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Published 2014 February 4 • © 2014. The American Astronomical Society. All rights reserved.
, , Citation William M. Wolf et al 2014 ApJ 782 117 DOI 10.1088/0004-637X/782/2/117

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This is a correction for 2013 ApJ 777 136

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1 Department of Physics, University of California, Santa Barbara, CA 93106, USA

2 Kavli Institute for Theoretical Physics, Santa Barbara, CA 93106, USA

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  1. Received 2014 January 13
  2. Published
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Due to an error at the publisher, in Figures 2 and 13 in the published version of this paper, no markers were rendered, though the corresponding error bars appeared in Figure 13. The correct versions of these figures are shown in Figures 1 and 2. Also, in Section 6, paragraph 8 of the published paper, the phrase M ⩾ M☉ appeared in bold. This was a relic of the refereeing process, as no emphasis was intended.

IOP Publishing sincerely regrets this error.

Figure 1.

Figure 1. Positions of stable burning models of accreting WDs on the HR diagram. The different colors indicate the different WD masses used in the simulations. Lines of constant radii are drawn for R = 0.01 R☉ and 0.1 R☉. The most luminous point for each mass corresponds to the WD accreting at $\dot{M} = \dot{M}_{\mathrm{stable}} \,{+}\, 0.8(\dot{M}_{\mathrm{RG}}\,{-}\,\dot{M}_{\mathrm{stable}})$. At accretion rates close to $\dot{M}_{\mathrm{RG}}$, the radius becomes ill-defined as the envelope slowly expands, so we only report those WDs with well-established radii.

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Figure 2.

Figure 2. Turn-off time against kTeff for observed CNe from the catalog of M31 CNe in (Henze et al. 2011; black dots), the CN in globular cluster Bol 126 in M31 (Henze et al. 2013; orange triangle), V4743 Sgr (Rauch et al. 2010; red diamond), the recurrent nova RS Oph (Osborne et al. 2011; brown star), HV Ceti (Beardmore et al. 2012; gray square), as well as the results of our work. Solid lines represent the super Eddington wind models and the dotted lines represent RLOF models. The range of effective temperatures shown for the computational models are the temperatures during the latter 70% of the stable burning period. Note that the Teff for the MESA simulations are from the Stefan–Boltzmann law given a luminosity and a photospheric radius. Teff's from Henze et al. (2011, 2013) are blackbody approximations taken from X-ray spectra, and Teff's from the galactic novae are from NLTE models of hot WD atmospheres. These temperatures can differ by ≈10% due to radiative transfer effects.

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10.1088/0004-637X/782/2/117