A Universal Decline Law of Classical Novae. III. GQ Muscae 1983

@article{Hachisu2008AUD,
  title={A Universal Decline Law of Classical Novae. III. GQ Muscae 1983},
  author={Izumi Hachisu and Mariko Kato and Angelo Cassatella},
  journal={The Astrophysical Journal},
  year={2008},
  volume={687},
  pages={1236-1252}
}
We present a unified model of infrared (IR), optical, ultraviolet (UV), and X-ray light curves for the 1983 outburst of GQ Muscae (Nova Muscae 1983) and estimate its white dwarf (WD) mass. Based on an optically thick wind model of nova outbursts, we model the optical and IR light curves with free-free emission, and the UV 1455 A and supersoft X-ray light curves with blackbody emission. The best-fit model that simultaneously reproduces the IR, optical, UV 1455 A, and supersoft X-ray observations… Expand
A UNIVERSAL DECLINE LAW OF CLASSICAL NOVAE. IV. V838 HER (1991): A VERY MASSIVE WHITE DWARF
We present a unified model of optical and ultraviolet (UV) light curves for one of the fastest classical novae, V838 Herculis (Nova Herculis 1991), and estimate its white dwarf (WD) mass. Based on anExpand
Novae in globular clusters
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 theExpand
Optical and supersoft x-ray light-curve models of classical nova v2491 cygni: A new clue to the secondary maximum
V2491 Cygni (Nova Cygni 2008 No. 2) was detected as a transient supersoft X-ray source with the Swift XRT as early as 40 days after the outburst, suggesting a very massive white dwarf (WD) close toExpand
A Light-Curve Model of the Symbiotic Nova PU Vul (1979) -- A Very Quiet Explosion with Long-Lasted Flat Peak
We present a light curve model of the symbiotic nova PU Vul (Nova Vulpeculae 1979) that shows a long-lasted flat peak with no spectral indication of wind mass-loss before decline. Our quasi-evolutionExpand
A Light Curve Analysis of Gamma-ray Nova V959 Mon -- Distance and White Dwarf Mass
V959 Mon is one of the gamma-ray detected novae. It was optically discovered about 50 days after the gamma-ray detection due to proximity to the Sun. The nova speed class is unknown because of lackExpand
Spectral behavior of Nova GQ Mus in the ultraviolet
We present ultraviolet spectroscopic study of nova GQ Mus observed with the International Ultraviolet Explorer (IUE) during the period 1983–1985. Different spectra showing the changes in line fluxesExpand
A Self-consistent Model for a Full Cycle of Recurrent Novae—Wind Mass-loss Rate and X-Ray Luminosity
An unexpectedly slow evolution in the pre-optical-maximum phase was suggested in the very short recurrence period nova M31N 2008-12a. To obtain reasonable nova light curves we have improved ourExpand
A Light Curve Analysis of Classical Novae: Free-free Emission vs. Photospheric Emission
We analyzed light curves of seven relatively slower novae, PW Vul, V705 Cas, GQ Mus, RR Pic, V5558 Sgr, HR Del, and V723 Cas, based on an optically thick wind theory of nova outbursts. For fastExpand
Light Curve Analysis of Neon Novae
We analyzed light curves of five neon novae, QU Vul, V351 Pup, V382 Vel, V693 CrA, and V1974 Cyg, and determined their white dwarf (WD) masses and distance moduli on the basis of theoretical lightExpand
EVOLUTION OF THE SYMBIOTIC NOVA PU VUL-OUTBURSTING WHITE DWARF, NEBULAE, AND PULSATING RED GIANT COMPANION
We present a composite light-curve model of the symbiotic nova PU Vul (Nova Vulpeculae 1979) that shows a long-lasting flat optical peak followed by a slow decline. Our model light curve consists ofExpand
...
1
2
3
...

References

SHOWING 1-10 OF 59 REFERENCES
A Universal Decline Law of Classical Novae. II. GK Persei 1901 and Novae in 2005
Optical and infrared light curves of classical novae are approximately homologous among various white dwarf (WD) masses and chemical compositions when free-free emission from optically thin ejecta isExpand
A Universal Decline Law of Classical Novae
We calculate many different nova light curves for a variety of white dwarf masses and chemical compositions, with the assumption that free-free emission from optically thin ejecta dominates theExpand
Optically Thick Winds from Degenerate Dwarfs. I. Classical Novae of Populations I and II
Twenty-six sequences of optically thick wind solutions have been calculated that mimic time-dependent evolution of classical novae of Populations I and II. The peak of the new opacity around log T =Expand
Optically thick wind solutions for an extremely rapid light curve of recurrent novae
Wind mass-loss solutions and theoretical light curves for rapid outbursts of recurrent novae are presented for a wide range of parameters of white-dwarf masses of 1.2, 1.3, 1.35, and 1.377 M® withExpand
The soft X-ray turnoff of Nova Muscae 1983
Nova GQ Muscae 1983 was detected by ROSAT as a luminous 'supersoft' X-ray source in 1992, nearly a decade after outburst. Further, this is the only classical postnova known to have maintainedExpand
Detection of supersoft X-ray emission from GQ Muscae nine years after a nova outburst
GQ MUS (Nova Muscae 1983) was the first classical nova from which X-rays were detected during outburst1'2. Those Exosat observations were consistent with thermonuclear burning on the surface of aExpand
A Theoretical Light-Curve Model for the 1999 Outburst of U Scorpii.
TLDR
A theoretical light curve for the 1999 outburst of U Scorpii is presented in order to obtain various physical parameters of the recurrent nova, which are exactly the same as those predicted in a new progenitor model of Type Ia supernovae. Expand
The temporal evolution of the near-infrared light curves of V1974 cygni (Nova Cygni 1992)
We report 1.25-18.5 μm infrared (IR) photometric measurements acquired during an 850 day period following outburst of the ONeMg "neon nova" V1974 Cygni (Nova Cygni 1992). The decline rates of theExpand
Spectroscopic observations of Nova Cygni 1975: The coronal line region revisited
A synopsis of the McDonald Observatory spectrophotometric observations of Nova Cyg 1975 (V1500 Cyg) is presented. We present these data in a form in which they can be readily accessed in the future,Expand
The X-Ray Spectral Evolution of Classical Nova V1974 Cygni 1992: A Reanalysis of the ROSAT Data
We present a spectral analysis of the archival X-ray data of classical Nova V1974 Cygni 1992 (Nova Cygni 1992) obtained by the ROSAT Position Sensitive Proportional Counter (PSPC). The X-ray spectrumExpand
...
1
2
3
4
5
...