author={Izumi Hachisu and Mariko Kato},
  journal={The Astrophysical Journal Supplement Series},
  • I. HachisuM. Kato
  • Published 3 February 2016
  • Physics
  • The Astrophysical Journal Supplement Series
We have examined the outburst tracks of 40 novae in the color–magnitude diagram (intrinsic B − V color versus absolute V magnitude). After reaching the optical maximum, each nova generally evolves toward blue from the upper right to the lower left and then turns back toward the right. The 40 tracks are categorized into one of six templates: very fast nova V1500 Cyg; fast novae V1668 Cyg, V1974 Cyg, and LV Vul; moderately fast nova FH Ser; and very slow nova PU Vul. These templates are located… 

The UBV Color Evolution of Classical Novae. IV. Time-stretched (U − B)0–(M B − 2.5 log f s) and (V − I)0–(M I − 2.5 log f s) Color–Magnitude Diagrams of Novae in Outbursts

Light curves and color evolutions of two classical novae can be largely overlapped if we properly squeeze or stretch the timescale of a target nova against that of a template nova by . Then, the

A Light-curve Analysis of 32 Recent Galactic Novae: Distances and White Dwarf Masses

We obtained the absolute magnitudes, distances, and white dwarf (WD) masses of 32 recent galactic novae based on the time-stretching method for nova light curves. A large part of the light/color

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

We analyzed optical, UV, and X-ray light curves of 14 recurrent and very fast novae in our Galaxy, Magellanic Clouds, and M31, and obtained their distances and white dwarf (WD) masses. Among the 14

A Light-curve Analysis of Gamma-Ray Nova V959 Mon: Distance and White Dwarf Mass

V959 Mon is a nova detected in gamma-rays. It was discovered optically about 50 days after the gamma-ray detection owing to its proximity to the Sun. The nova’s speed class is unknown because of the

A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate

The nova rate in the Milky Way remains largely uncertain, despite its vital importance in constraining models of Galactic chemical evolution as well as understanding progenitor channels for Type Ia

Discovery of a Rapid, Luminous Nova in NGC 300 by the KMTNet Supernova Program

We present the discovery of a rapidly evolving transient by the Korean Microlensing Telescope Network Supernova Program (KSP). KSP is a novel high-cadence supernova survey that offers deep (∼21.5 mag

A light curve model of V2491 Cyg: Classical nova outburst on a cool and massive white dwarf

The classical nova V2491 Cyg was once suggested to be a recurrent nova. We have broadly reproduced the light curve of V2491 Cyg by a nova outburst model on a cold 1.36 M⊙ white dwarf (WD), which

0 1 5 ) 0 5 6 Classical nova V 339 Del ( Nova Del 2013 )-a short review

Multifrequency observations of the classical CO nova V339 Del, detected in all frequencies from γ-rays to radio, are reviewed. Nova V339 Del was discovered on 2013 August 14.584 UT. The times of

Supersoft X-ray phases of recurrent novae as an indicator of their white dwarf masses

We have examined the optical/X-ray light curves of seven well-observed recurrent novae, V745 Sco, M31N 2008-12a, LMC N 1968, U Sco, RS Oph, LMC N 2009a, T Pyx, and one recurrent nova candidate LMC N

Structure and evolution of classical Nova Shells

This thesis focuses on shells ejected during classical nova events. Novae are due to thermonuclear runaway on the surface of a white dwarf in a binary system. The work herein concentrates on nova



The extragalactic distance scale

Significant progress has been made during the last 10 years toward resolving the debate over the expansion rate of the Universe. The current value of the Hubble parameter, H0, is now arguably known

The Cataclysmic Variable Stars

Preface 1. Historical development 2. Structure of non-magnetic systems 3. Dwarf novae 4. Nova-like variables and nova remnants 5. Novae in eruption 6. Polars 7. Intermediate polars 8. DQ Herculis

The Physics of Cataclysmic Variables and Related Objects

This conference continues a long line of meetings on the general topic of cataclysmic variables (CVs) that started with the first North American Workshop in 1981. The conference held on on

Binaries - Key to Comprehension of the Universe

Proceedings of the conference Binaries - Key to comprehension of the Universe, held in Brno, Czech Republic in June 8-12, 2009

Publications of the Dominion Astrophysical Observatory

  • 1970

RS Ophiuchi (2006) and the recurrent nova phenomenon : proceedings of a workshop held at Keele University, Keele, United kingdom

On 12 February 2006, the recurrent nova RS Ophiuchi erupted for the first time since 1985, its 6th (at least!) known eruption. This event triggered an intensive multi-wavelength observational

2008b, RS Ophiuchi

  • 2008

The Astronomer’s Telegram

  • 2008

s (B − V ) 0 data are consistently overlapping those of Page et al. as shown in Figure 75(b). The

  • 2014