A Light Curve Analysis of Recurrent and Very Fast Novae in Our Galaxy, Magellanic Clouds, and M31

Hachisu, Izumi; Kato, Mariko

doi:10.3847/1538-4365/aac833

Cited by 25 publications

(56 citation statements)

References 163 publications

(433 reference statements)

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“…Applying the obtained f s and ∆V to Equation (4), we have the relation of Thus, we obtain (m − M ) V = 11.86 ± 0.1 for LV Vul, being consistent with our previous results of (m−M ) V = 11.85 ± 0.1 (Hachisu & Kato 2018b).…”

Section: Vul 1968#1supporting

confidence: 90%

“…By directly fitting the theoretical light curves of M V with the observed m V , we can also estimate the WD mass M WD and distance modulus in the V band of µ V ≡ (m − M ) V for a target nova. Hachisu & Kato (2018b) confirmed that the time-stretching method is applicable to fast and very fast novae in our Galaxy, LMC, and M31.…”

Section: Introductionsupporting

confidence: 77%

“…We estimate the typical total error of ǫ(∆V − 2.5 log f s ) = (±0.2) + (±0.1). In the case of LV Vul, log f s is rather well determined against YY Dor and LMC N 2009a, that is, the error of ǫ(log f s ) = ±0.02 (see Section 5.1 of Hachisu & Kato 2018b). Therefore, the total error is about ǫ(∆V −2.5 log f s ) = (±0.2)+(±0.05).…”

Section: Vul 1968#1mentioning

confidence: 95%

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The UBV Color Evolution of Classical Novae. III. Time-stretched Color–Magnitude Diagram of Novae in Outburst

Hachisu

Kato²

2019

ApJS

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We propose a modified color-magnitude diagram for novae in outburst, i.e., (B − V ) 0 versus (M V − 2.5 log f s ), where f s is the timescaling factor of a (target) nova against a comparison (template) nova, (B − V ) 0 is the intrinsic B − V color, and M V is the absolute V magnitude. We dub it the timestretched color-magnitude diagram. We carefully reanalyzed 20 novae based on the time-stretching method and revised their extinctionsand timescaling factors f s against the template nova LV Vul. We have found that these 20 nova outburst tracks broadly follow one of the two template tracks, LV Vul/V1668 Cyg or V1500 Cyg/V1974 Cyg group, in the time-stretched color-magnitude diagram. In addition, we estimate the white dwarf masses and (m − M ) V of the novae by directly fitting the absolute V model light curves (M V ) with observational apparent V magnitudes (m V ). A good agreement in the two estimates of (m − M ) V confirms the consistency of the time-stretched color-magnitude diagram. Our distance estimates are in good agreement with the results of Gaia Data Release 2.

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Section: Vul 1968#1supporting

confidence: 90%

Section: Introductionsupporting

confidence: 77%

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The UBV Color Evolution of Classical Novae. III. Time-stretched Color–Magnitude Diagram of Novae in Outburst

Hachisu

Kato²

2019

ApJS

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“…Figure 3(a) shows the light curve of U Sco in the 2010 outburst. We adopt the distance modulus in the V band to be (m − M ) V = 16.3 (Hachisu & Kato 2018b). Around the optical peak, the brightness is dominated by the emission from the ejecta.…”

Section: U Scomentioning

confidence: 99%

ASASSN-16oh: A Nova Outburst with No Mass Ejection—A New Type of Supersoft X-Ray Source in Old Populations

Kato

Saio

Hachisu

2020

ApJ

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ASASSN-16oh is a peculiar transient supersoft X-ray source without a mass ejection signature in the field of the Small Magellanic Cloud. Maccarone et al. (2019) concluded that ASASSN-16oh is the first dwarf nova with supersoft X-ray that originated from an equatorial accretion belt on a white dwarf (WD). Hillman et al. (2019) proposed a thermonuclear runaway model that both the X-rays and V /I photons are emitted from the hot WD. We calculated the same parameter models as Hillman et al.'s and found that they manipulated on/off the mass-accretion, and their best fit V light curves are 6 mag fainter, and decay about 10 times slower, than that of ASASSN-16oh. We propose a nova model induced by a high rate of mass-accretion during a dwarf nova outburst, i.e., the X-rays originate from the surface of the hydrogen-burning WD whereas the V /I photons are from the irradiated disk. Our model explains the main observational properties of ASASSN-16oh. We also obtained thermonuclear runaway models with no mass ejection for a wide range of parameters of the WD mass and massaccretion rates including both natural and forced novae in low-metal environments of Z = 0.001 and Z = 0.0001. They are a new type of periodic supersoft X-ray sources with no mass ejection, and also a bright transient in V /I bands if they have a large disk. We suggest that such objects are candidates of Type Ia supernova progenitors because its mass is increasing at a very high efficiency (∼ 100%).

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“…1) to the collision between the slowly expanding torus with the faster nova wind, which is consistent with the model proposed byLi et al (2017).4. According toHachisu & Kato (2018), the slow decline of the optical flux F ∝ t −1 , observed for some novae during the early stage of their evolution, can be caused by the shock interaction that decelerates the ejecta resulting in a slower decrease of its den-…”

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confidence: 99%

Multiwavelength Modeling of the SED of Nova V339 Del: Stopping the Wind and Long-lasting Super-Eddington Luminosity with Dust Emission

Skopal

2019

ApJ

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During the classical nova outburst, the radiation generated by the nuclear burning of hydrogen in the surface layer of a white dwarf (WD) is reprocessed by the outer material into different forms at softer energies, which distribution in the spectrum depends on the nova age. Using the method of multiwavelength modeling the SED we determined physical parameters of the stellar, nebular and dust component of radiation isolated from the spectrum of the classical nova V339 Del from day 35 to day 636 after its explosion. The transition from the iron-curtain phase to the super-soft source phase (days 35-72), when the optical brightness dropped by 3-4 mag, the absorbing column density fell by its circumstellar component from ∼ 1 × 10 23 to ∼ 1 × 10 21 cm −2 , and the emission measure decreased from ∼ 2 × 10 62 to ∼ 8.5 × 10 60 cm −3 , was caused by stopping-down the mass-loss from the WD. The day 35 model SED indicated an oblate shape of the WD pseudophotosphere and the presence of the dust located in a slow equatorially concentrated outflow. The dust emission peaked around day 59. Its co-existence with the strong super-soft X-ray source in the day 100 model SED constrained the presence of the disk-like outflow, where the dust can spend a long time. Both the models SED revealed a super-Eddington luminosity of the burning WD at a level of 1 − 2 × 10 39 (d/4.5 kpc) 2 erg s −1 , lasting from ∼day 2 to at least day 100.

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A Light Curve Analysis of Recurrent and Very Fast Novae in Our Galaxy, Magellanic Clouds, and M31

Cited by 25 publications

References 163 publications

The UBV Color Evolution of Classical Novae. III. Time-stretched Color–Magnitude Diagram of Novae in Outburst

The UBV Color Evolution of Classical Novae. III. Time-stretched Color–Magnitude Diagram of Novae in Outburst

ASASSN-16oh: A Nova Outburst with No Mass Ejection—A New Type of Supersoft X-Ray Source in Old Populations

Multiwavelength Modeling of the SED of Nova V339 Del: Stopping the Wind and Long-lasting Super-Eddington Luminosity with Dust Emission

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