Detection of Two-armed Spiral Shocks on the Accretion Disk of the Eclipsing Fast Nova V1494 Aquilae

Hachisu, Izumi; Kato, Mariko; Katô, Takeo

doi:10.1086/421295

Cited by 18 publications

(15 citation statements)

References 23 publications

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“…(1) Crampton et al (1987); (2 Kahabka (1996); (9) Tomov et al (1998) Ribeiro et al (2013b); (17) Munari et al (2013); (18) Bos et al (2001); (19) Barsukova & Goranskii (2003); (20) Hachisu et al (2004); (21) Iijima & Esenoglu (2003); (22) Ribeiro et al (2011);(23) Helton et al (2008); (24) Dobrotka et al (2008); (25) Sala et al (2008); (26) Lyke & Campbell (2009); (27) Goranskij et al (2007); (28) Shore et al (2003); (29) Della Valle et al (2002); (30) Dobrzycka & Kenyon (1994); (31) Ribeiro et al (2009);(32) Bode (1987); (33) Barry et al (2008); (34) Schaefer (1990); (35) Thoroughgood et al (2001); (36) Schaefer (2010); (37) Chesneau et al (2011);(38) Uthas et al (2010); (39) Sokoloski et al (2013); …”

Section: Referencesmentioning

confidence: 99%

Obscuration effects in super-soft-source X-ray spectra

Ness

Osborne

Henze

et al. 2013

A&A

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Context. Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ∼3−7 × 10 5 K and luminosities of 10 35−38 erg s −1 . Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. Aims. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. Methods. We collected all grating spectra of conventional SSS like Cal 83 and Cal 87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature.

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Section: Referencesmentioning

confidence: 99%

Obscuration effects in super-soft-source X-ray spectra

Ness

Osborne

Henze

et al. 2013

A&A

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“…We adopt ν = 2. Spiral structures of surface of the accretion disk are assumed in the same manner as that adopted by Hachisu et al (2004), which is defined by…”

Section: Light Curve Model Of Early Superhumpsmentioning

confidence: 99%

Photometric Observation and Numerical Simulation of Early Superhumps in BC Ursae Majoris during the 2003 Superoutburst

Maehara

Hachisu

Nakajima³

2007

Publications of the Astronomical Society of Japan

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We carried out time-resolved photometric observations of an SU UMa type dwarf nova, BC UMa, during its superoutburst in February 2003. We detect early superhumps ( or outburst orbital humps) during the first two days of the outburst. The period of early superhumps is 0.06258(13) d and the amplitude is 0.04 mag. After the early superhump phase, common superhumps with an amplitude of 0.3 mag and a period of 0.064466(16) d developed. The change rate of superhump periods (Ṗ sh /P sh ) was positive through the superoutburst. The superhump period excess (ε ≡ P sh /P orb − 1) is 3% and we derive a mass ratio of 0.13. This is twice as large as that of WZ Sge, suggesting that the mechanism of early superhumps in BC UMa is not the 2:1 resonance which was proposed in WZ Sge.We have modelled early superhump light curves including irradiation effects of the accretion disk and secondary star by the white dwarf and accretion disk. The observed early superhumps can be reproduced when two-armed spirals appear on the accretion disk.We have found the long term data taken from AAVSO, VSOLJ and VSNET shows BC UMa has normal outbursts with a maximum magnitude of m V ∼ 13 and two types of superoutbursts: one has a short duration (around 10 days) and faint maximum magnitude (m V ∼ 12.5), the other has a long duration (around 20 days) and bright maximum (m V ∼ 11 − 11.5). BC UMa is the first example of dwarf novae showing the two types of superoutbursts. The supercycle of BC UMa is between 600 days and 1000 days. This is shorter than WZ Sge type dwarf novae and longer than normal SU UMa type stars. This phenomenon suggests that BC UMa is an intermediate dwarf nova between WZ Sge and SU UMa.

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“…The model apart from the standard components (WD, secondary star, accretion stream and bright spot) takes into account positions of the bright structures in the Doppler maps, according to the description of the spiral density waves in Hachisu et al (2004). From our models, we find that the shape and the amplitude of the double hump light curve can be realistically re-produced as can be seen from Fig.…”

Section: Nature Of the Accretion Disk In Bounce-back Systemsmentioning

confidence: 83%

Accretion Disks of Bounce-Back CVs

Tovmassian

Zharikov

2012

Proc. IAU

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Abstract. We explore conditions and structure of accretion disks in the short-period Cataclysmic Variables, which have evolved beyond the period minimum. We show that the accretion disk in a system with extreme mass ratio grows in the size reaching 2:1 resonance radius and are relatively cool. They also become largely optically thin in the continuum, contributing to the total flux less than the stellar components of the system. In contrast, the viscosity and the temperature in spiral arms formed at the outer edge of the disk are higher and their contribution in continuum plays an increasingly important role. We model such disks and generate light curves which successfully simulate the observed double-humped light curves in the quiescence.

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Detection of Two-armed Spiral Shocks on the Accretion Disk of the Eclipsing Fast Nova V1494 Aquilae

Cited by 18 publications

References 23 publications

Obscuration effects in super-soft-source X-ray spectra

Obscuration effects in super-soft-source X-ray spectra

Photometric Observation and Numerical Simulation of Early Superhumps in BC Ursae Majoris during the 2003 Superoutburst

Accretion Disks of Bounce-Back CVs

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