Spectroscopic monitoring of the transition phase in nova V4745 Sgr

Csák, B.; Kiss, L. L.; Retter, A.; Jacob, A. P.; Kaspi, S.

doi:10.1051/0004-6361:20035751

Cited by 29 publications

(40 citation statements)

References 33 publications

(37 reference statements)

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“…This means that the intervals between consecutive maxima get gradually longer, as was noted for this nova by Csák et al (2005). V2540 Oph and DK Lac apparently exhibit the same behavior.…”

Section: Long-term Behavior Of the Flaressupporting

confidence: 74%

“…They spectroscopically monitored the transition phase of V4745 Sgr and found that during the rebrightenings the continuum emission rose and that the spectral lines showed P-Cyg profiles, which suggests a temporary increase in massloss rate. On the basis of these observations, Csák et al (2005) suggested that the rebrightenings are envelope-hydrogenburning instabilities. They also observed a gradual increase of the time intervals between rebrightenings, which was also noted previously in GK Per and DK Lac by Bianchini et al (1992).…”

Section: Introductionmentioning

confidence: 99%

“…The underlying physical reason for the transition phase is not yet clear; for a recent review of the proposed models, see Csák et al (2005). They spectroscopically monitored the transition phase of V4745 Sgr and found that during the rebrightenings the continuum emission rose and that the spectral lines showed P-Cyg profiles, which suggests a temporary increase in massloss rate.…”

Section: Introductionmentioning

confidence: 99%

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

Pejcha

2009

ApJ

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A significant fraction of novae exhibit a series of rebrightenings on the decline branch of their light curves. We use visual observations to study this phase in several well-observed novae. We find that these rebrightenings are isolated flare-like events on otherwise smooth light curves and we show that in most novae in our sample the time intervals between consecutive flares gradually increase as a geometric series; rebrightenings are equally spaced in logarithmic time. We also find a correlation between the rate of increase in the time between rebrightenings with the speed class of the nova in the sense that slower novae tend to increase the time intervals faster. We attribute these rebrightenings to instabilities in the envelope hydrogen burning and we mention other cases of such timing patterns in astronomy and natural sciences in general.

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“…This means that the intervals between consecutive maxima get gradually longer, as was noted for this nova by Csák et al (2005). V2540 Oph and DK Lac apparently exhibit the same behavior.…”

Section: Long-term Behavior Of the Flaressupporting

confidence: 74%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Pejcha

2009

ApJ

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“…The fact that the accretion disk is recovered around the same time the transition phase occurs supports a connection between the two phenomena. Csák et al (2005) found that spectra obtained during the maxima of the oscillations in the transition phase of V4745 Sgr are similar to spectra taken just after its nova eruption in 2003. Therefore, they proposed to explain the oscillations by several episodes of mass ejection, which they called ''mini nova-outbursts.''…”

Section: The Transition Phase In Novaementioning

confidence: 60%

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang

Retter

Liu³

et al. 2006

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We present the results of 11 nights of CCD unfiltered photometry of V4743 Sgr (Nova Sgr 2002 No. 3) from 2003 and 2005. We find two periods of 0.2799 days (%6.7 hr) and 0.01642 days (%24 minutes) in the 2005 data. The long period is also present in the 2003 data, but only weak evidence of the shorter period is found in this year. The 24 minute period is somewhat longer than the 22 minute period that was detected from X-ray observations. We suggest that the 6.7 hr periodicity represents the orbital period of the underlying binary system and that the 24 minute period is the beat periodicity between the orbital period and the X-ray period, which is presumably the spin period of the white dwarf. Thus, V4743 Sgr should be classified as an intermediate polar (DQ Her star). About 6 months after the nova outburst, the optical light curve of V4743 Sgr seemed to show quasi-periodic oscillations, which are typical of the transient phase in classical novae. Therefore, our results support the previous suggestion that the transition phase in novae may be related to intermediate polars.

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“…it was not an hybrid nova, and its emission lines were twice as wide as in V5588 Sgr. In addition, while the spectra of V5588 Sgr did not change during SdM other than for the appearance of the weak broad pedestal, the emission lines of V4745 Sgr during SdM switched back to strong P-Cyg absorption profiles as for the primary maximum (Csák et al 2005, Tanaka et al 2011.…”

Section: Discussionmentioning

confidence: 92%

The hybrid, coronal lines nova V5588 Sgr (2011 N.2) and its six repeating secondary maxima

Munari¹,

Henden²,

Banerjee³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The outburst of Nova Sgr 2011 N.2 (=V5588 Sgr) was followed with optical and near-IR photometric and spectroscopic observations for 3.5 years, beginning shortly before the maximum. V5588 Sgr is located close to Galactic center, suffering from E B−V =1.56 (±0.1) extinction. The primary maximum was reached at V =12.37 on UT 2011 April 2.5 (±0.2), and the underlying smooth decline was moderately fast with t V 2 =38 and t V 3 =77 days. On top of an otherwise normal decline, six self-similar, fast evolving and bright secondary maxima (SdM) appeared in succession. Only very few other novae have presented so clear secondary maxima. Both the primary maximum and all SdM occurred at later times with increasing wavelengths, by amounts in agreement with expectations from fireball expansions. The radiative energy released during SdM declined following an exponential pattern, while the breadth of individual SdM and the time interval between them widened. Emission lines remained sharp (FWHM∼1000 km/s) throughout the whole nova evolution, with the exception of a broad pedestal with a trapezoidal shape (∆vel=3600 km/sec at the top and 4500 km/sec at the bottom) which was only seen during the advanced decline from SdM maxima and was absent in between SdM. V5588 Sgr at maximum light displayed a typical FeII-class spectrum which did not evolve into a nebular stage. About 10 days into the decline from primary maximum, a typical high-ionization He/N-class spectrum appeared and remained visible simultaneously with the FeII-class spectrum, qualifying V5588 Sgr as a rare hybrid nova. While the FeII-class spectrum faded into oblivion, the He/N-class spectrum developed strong [FeX] coronal lines.

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Spectroscopic monitoring of the transition phase in nova V4745 Sgr

Cited by 29 publications

References 33 publications

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

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

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

The hybrid, coronal lines nova V5588 Sgr (2011 N.2) and its six repeating secondary maxima

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