Time-Dependent Rebrightenings in Classical Nova Outbursts: A Late-Time Episodic Fuel Burning?

Pejcha, Ondřej

doi:10.1088/0004-637x/701/2/l119

Cited by 14 publications

(17 citation statements)

References 35 publications

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“…The only two exceptions are that V4745 Sgr has a short interval at the first and a long interval at the end, while DK Lac has a vague upward trend. This is in contrast to the plot of Pejcha (2009) which shows both V4745 Sgr and DK Lac having tight linear correlations with a slope of near unity. As we are operating off the same data, we can only think that the conclusion is very sensitive to the selection of which peaks to include.…”

Section: J Class Light Curvescontrasting

confidence: 89%

“…We can get better statistics by making a distribution for all the nova inter-arrival times lumped together (at the cost of smearing together distributions with different averages), and the plot again appears linear to within the error bars, so, it appears that the timing of the jitters is random within the interval over which they occur. Pejcha (2009) claims that the jitters have intervals between successive peaks that increase greatly with time since the maxima. In particular, his plot of log(∆T j ) versus log(∆T max ) shows a nearly linear trend with a slope near unity, so that ∆T j ∝ ∆T max .…”

Section: J Class Light Curvesmentioning

confidence: 99%

“…This has caused one of us to measure plateau parameters for the known RNe, and to ask what fraction of classical novae show similar plateaus (S2010). Pejcha (2009) has been looking at a mixture of oscillations and flares (jitters) in seven novae trying to find whether the peak spacing is uniform in logarithmic or linear time, so as to test his theoretical model.…”

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confidence: 99%

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Catalog of 93 Nova Light Curves: Classification and Properties

Strope

Schaefer

Henden

2010

The Astronomical Journal

255

427

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We present a catalog of 93 very-well-observed nova light curves. The light curves were constructed from 229,796 individual measured magnitudes, with the median coverage extending to 8.0 mag below peak and 26% of the light curves following the eruption all the way to quiescence. Our time-binned light curves are presented in figures and as complete tabulations. We also calculate and tabulate many properties about the light curves, including peak magnitudes and dates, times to decline by 2, 3, 6, and 9 magnitudes from maximum, the time until the brightness returns to quiescence, the quiescent magnitude, power law indices of the decline rates throughout the eruption, the break times in this decline, plus many more properties specific to each nova class. We present a classification system for nova light curves based on the shape and the time to decline by 3 magnitudes from peak (t 3 ). The designations are S for smooth light curves (38% of the novae), P for plateaus (21%), D for dust dips (18%), C for cusp-shaped secondary maxima (1%), O for quasi-sinusoidal oscillations superposed on an otherwise smooth decline (4%), F for flat-topped light curves (2%), and J for jitters or flares superposed on the decline (16%). Our classification consists of this single letter followed by the t 3 value in parentheses; so for example V1500 Cyg is S(4), GK Per is O(13), DQ Her is D(100), and U Sco is P(3).

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Section: J Class Light Curvescontrasting

confidence: 89%

Section: J Class Light Curvesmentioning

confidence: 99%

mentioning

confidence: 99%

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Catalog of 93 Nova Light Curves: Classification and Properties

Strope

Schaefer

Henden

2010

The Astronomical Journal

255

427

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“…Lower panel: time intervals between the peak of successive jitters v.s. time intervals between each jitter and the time of eruption.There is a trend in the log-log plot, consistent with the hydrogen burning envelope instabilities scenario[106].…”

supporting

confidence: 79%

Time-domain studies of M31

Lee

2016

Astronomical Review

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M31, our closest neighboring galaxy, is a stepping stone to studies of stellar evolution, star formation, galaxy evolution, and cosmology. However, due to the difficulties of performing photometry in such crowded fields and the lack of wide cameras to encompass the entire galaxy, there has not been a complete census of the stellar contents of M31. The advent of wide-field camera provides us a unique opportunity to have a complete view of our neighboring galaxy, enabling an inventory of its variable content. We present a review of recent progresses of wide-field, high cadence surveys of M31, covering different population of variables and transients. We also outline future studies enabled by on-going and up-coming facilities.

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“…9. It has been reported that there is a gradual increase of the time intervals between two successive jitters (Bianchini et al 1992;Csák et al 2005;Pejcha 2009;Tanaka et al 2010), while Strope et al (2010), using the same data set as Pejcha (2009), found no distinctive trend. We thus tried to search for such trend in our nova candidate N27 and performed a fitting with the following equation:…”

Section: J Classmentioning

confidence: 94%

The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M 31 nova catalogue

Lee¹,

Riffeser²,

Seitz³

et al. 2012

A&A

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We present light curves from the novae detected in the long-term, M 31-monitoring WeCAPP project. The goal of WeCAPP is to constrain the compact dark matter fraction of the M 31 halo with microlensing observations. As a by product we detected 91 novae benefiting from the high cadence and highly sensitive difference imaging technique required for pixel-lensing. We thus can now present the largest sample of optical/CCD nova lightcurves towards M 31 to date. We also obtained thorough coverage of the light curve before and after the eruption thanks to the long-term monitoring. We apply a nova taxonomy to our nova candidates and found 29 S-class novae, 10 C-class novae, 2 O-class novae, and 1 J-class nova. We investigated a universal decline law on the S-class novae. In addition, we correlated our catalogue with the literature and found 4 potential recurrent novae. Part of our catalogue has been used to search for optical counterparts of the super soft X-ray sources detected in M 31. Optical surveys like WeCAPP, when coordinated with multi-wavelength observation, will continue to shed light on the underlying physical mechanism of novae in the future.

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Time-Dependent Rebrightenings in Classical Nova Outbursts: A Late-Time Episodic Fuel Burning?

Cited by 14 publications

References 35 publications

Catalog of 93 Nova Light Curves: Classification and Properties

Catalog of 93 Nova Light Curves: Classification and Properties

Time-domain studies of M31

The Wendelstein Calar Alto Pixellensing Project (WeCAPP): the M 31 nova catalogue

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