A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

Hachisu, Izumi; Kato, Mariko

doi:10.1086/517600

Cited by 49 publications

(28 citation statements)

References 54 publications

(53 reference statements)

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“…We attribute this drop in luminosity to the end of nuclear burning. Hachisu & Kato (2007) assumed that hydrogen burning ended on day 75, and from model fitting determined that the mass of the white dwarf was 1.35 M . However, given that burning duration is inversely proportional to white dwarf mass, we conclude from our data that the white dwarf mass may be even higher than this estimate.…”

Section: Discussionmentioning

confidence: 99%

“…The most recent determination of the orbital period of the binary is 456 days ( Fekel et al 2000). The secondary is believed to underfill its Roche lobe, and so accretion proceeds through a wind and not through Roche lobe overflow ( RLO), as in cataclysmic variables and classical novae (e.g., Dobrzycka et al 1996;Hachisu & Kato 2001). The distance to the system has been discussed extensively in the literature, and disagreements remain.…”

Section: Introductionmentioning

confidence: 99%

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X‐Ray Spectroscopy of the 2006 Outburst of RS Ophiuchi

Nelson¹,

Orio

Cassinelli³

et al. 2008

ApJ

151

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We present X-ray grating spectra of the recurrent nova RS Ophiuchi during its 2006 outburst, obtained with XMMNewton and Chandra. For the first month after optical maximum, the X-ray spectrum was hard and dominated by emission lines of H-like and He-like ions. The X-ray luminosity was 2:4 ; 10 36 ergs s À1 in the 0.33Y10 keV range. The spectra indicate a collisionally dominated plasma with a broad range of temperatures and an energy-dependent velocity structure. During an observation obtained in week 4, a soft X-ray flare occurred in which a new system of soft, higher velocity emission lines appeared in the spectrum. Then, during weeks 6Y10, the supersoft continuum of the hot white dwarf atmosphere was the dominant emission component. The X-ray luminosity reached at least 9 ; 10 37 ergs s À1 in the 0.2Y1 keV range, while the intrinsic nebular absorption decreased by a factor of 5 since the first observation. Preliminary model fitting indicates a white dwarf temperature of $800,000 K, and a mass of at least 1.2 M . Therefore, RS Oph may be an important Type Ia supernova progenitor. We show that the data are consistent with mass loss ending before day 54 of the outburst, and nuclear burning ending around day 69. A rapid decay in X-ray luminosity followed after week 10. The X-ray luminosity 5, 7, and 8 months after optical maximum dropped by more than 2 orders of magnitude. The spectra do not appear to be consistent with emission from an accretion disk.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

X‐Ray Spectroscopy of the 2006 Outburst of RS Ophiuchi

Nelson¹,

Orio

Cassinelli³

et al. 2008

ApJ

151

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show abstract

“…We adopt the optically thick winds (e.g., Kato 1983Kato , 1985Kato & Hachisu 1994) as the main mechanism of mass-loss during the nova outburst. The optically thick winds have been applied to a number of novae and have successfully reproduced light curves and characteristic properties (e.g., Hachisu & Kato 2006, 2007Hachisu et al 2008;Kato et al 2009;. The interior structures of WDs are calculated with a Henyey code (Section 2.1).…”

Section: Methodsmentioning

confidence: 99%

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

Kato

Saio

Hachisu

2017

ApJ

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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 e and 1.38 M e 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 e , 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.

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“…Using this approach Hachisu & Kato (2007) determined for GK Per a WD mass of M/M = 1.15 ± 0.05. However, this result depends on the assumed hydrogen mass fraction (X = 0.54) in the expanded Nova Persei 1901 envelope.…”

Section: Gk Permentioning

confidence: 99%

GK Persei and EX Hydrae: Intermediate polars with small magnetospheres

Suleimanov

Doroshenko

Ducci

et al. 2016

A&A

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Observed hard X-ray spectra of intermediate polars are determined mainly by the accretion flow velocity at the white dwarf surface, which is normally close to the free-fall velocity. This allows us to estimate the white dwarf masses as the white dwarf mass-radius relation M − R and the expected free-fall velocities at the surface are well known. This method is widely used. However, derived white dwarf masses M can be systematically underestimated because the accretion flow is stopped at, and re-accelerates from, the magnetospheric boundary R m and, therefore, its velocity at the surface is lower than free fall. To avoid this problem, we computed a two-parameter set of model hard X-ray spectra, which allows us to constrain a degenerate M − R m dependence. Previous works showed that power spectra of accreting X-ray pulsars and intermediate polars exhibit breaks at frequencies corresponding to Keplerian frequencies at the magnetospheric boundary. Therefore, the break frequency ν b in an intermediate polar power spectrum gives another relation in the M − R m plane. The intersection of the two dependences allows us, therefore, to determine the white dwarf mass and magnetospheric radius simultaneously. To verify the method, we analysed the archival Suzaku observation of EX Hya, obtaining M/M = 0.73 ± 0.06 and R m /R = 2.6 ± 0.4, which is consistent with the values determined by other authors. Subsequently, we applied the same method to a recent NuSTAR observation of another intermediate polar GK Per performed during an outburst and found M/M = 0.86 ± 0.02 and R m /R = 2.8 ± 0.2. The long duration observations of GK Per in quiescence performed by Swift/BAT and INTEGRAL observatories indicate increase of magnetosphere radius R m at lower accretion rates.

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A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005

Cited by 49 publications

References 54 publications

X‐Ray Spectroscopy of the 2006 Outburst of RS Ophiuchi

X‐Ray Spectroscopy of the 2006 Outburst of RS Ophiuchi

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

GK Persei and EX Hydrae: Intermediate polars with small magnetospheres

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