Unusual “Stunted” Outbursts in Old Novae and Nova-like Cataclysmic Variables

Honeycutt, R. K.; Robertson, J. W.; Turner, G. W.

doi:10.1086/300381

Cited by 72 publications

(90 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This result is consistent with the previous authors (e.g. Oppenheimer et al 1998;Honeycutt et al 1998). Moreover, the trend in Fig.…”

Section: Normal Outbursts and K−p Relationsupporting

confidence: 94%

“…These events are best characterized as the small amplitude outbursts, which have properties very similar to the stunted outbursts seen in some NLs (e.g. Honeycutt et al 1995Honeycutt et al , 1998Honeycutt et al , 2001Honeycutt et al , 2014Warner 1995;Hoard et al 2000;Ramsay et al 2016). Table 2 summarizes the properties of stunted outbursts in AY Psc.…”

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 94%

“…However, to date, the origin of stunted outbursts is still uncertain. Some possible mechanisms are proposed to account for the stunted outbursts, including a disk truncated by the magnetic field of the white dwarf or a very hot white dwarf, dwarf nova-type outbursts being related to the standard disc instability and the mass transfer modulations (Honeycutt et al 1998(Honeycutt et al , 2001(Honeycutt et al , 2014Ramsay et al 2016). …”

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 99%

“…For AY Psc, a truncated disk mechanism can rule out because the inside-out outbursts (Type B) in a truncated disk are infrequent (Honeycutt et al 1998). During standstill,Ṁ 2 from the secondary star exceedsṀ crit , the disk stays in the steady state, without DN outbursts.…”

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 99%

See 3 more Smart Citations

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

Han

Qian

Voloshina

et al. 2017

Res. Astron. Astrophys.

View full text Add to dashboard Cite

New eclipse timings of the Z Cam-type dwarf nova AY Psc were measured and the orbital ephemeris was revised. Based on the long-term AAVSO data, moreover, the outburst behaviors were also explored. Our analysis suggests that the normal outbursts are quasiperiodic, with an amplitude of ∼ 2.5(±0.1) mag and a period of ∼ 18.3(±0.7) days. The amplitude vs. recurrence-time relation of AY Psc is discussed, and we concluded that this relation may represents general properties of dwarf nova (DN) outbursts. The observed standstill ends with an outburst, which is inconsistent with the general picture of Z Cam-type stars.This unusual behavior was considered to be related to the mass-transfer outbursts. Moreover, the average luminosity is brighter during standstills than during outburst cycles. The changes in brightness marks the variations inṀ 2 due to the disc of AY Psc is nearly steady state.Ṁ 2 value was limited to the range from 6.35 × 10 −9 to 1.18 × 10 −8 M ⊙ yr −1 . More detailed examination shows that there are a few small outbursts presence during standstills. These events with amplitudes of ∼ 0.5 − 0.9 mag are very similar to the stunted outbursts reported in some NLs. We discussed several possible mechanisms and suggested that the most reasonable mechanism for these stunted outbursts is a changing mass-transfer rate.

show abstract

“…This result is consistent with the previous authors (e.g. Oppenheimer et al 1998;Honeycutt et al 1998). Moreover, the trend in Fig.…”

Section: Normal Outbursts and K−p Relationsupporting

confidence: 94%

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 94%

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 99%

Section: Stunted Outbursts In Ay Pscmentioning

confidence: 99%

See 2 more Smart Citations

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

Han

Qian

Voloshina

et al. 2017

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…Thorstensen & Taylor (2000) found a long (P orb = 1. d 48) spectroscopic orbital period for X Ser. Brightness variations with different amplitudes and characteristic times are typical of this old nova A119, page 10 of 24 during quiescence (Duerbeck & Seitter 1990;Howell et al 1990;Honeycutt et al 1998). Spectral observations during the X Ser outburst are missing.…”

Section: Cn Velmentioning

confidence: 99%

SALT observations of southern post-novae

Tomov

Swierczynski

Mikołajewski

et al. 2015

A&A

View full text Add to dashboard Cite

Aims. We report on recent optical observations of the stellar and the nebular remnants of 22 southern post-novae. Methods. In this study, for each of our targets, we obtained and analysed long-slit spectra in the spectral range 3500-6600 Å and inResults. The changes in the emission lines' equivalent widths with the time since the outburst agree with earlier published results of other authors. We estimated an average value α = 2.37 for the exponent of the power law fitted to the post-novae continua. Our observations clearly show the two-component structure of the V842 Cen expanding nebulae, owing to the different velocities of the ejected matter. We discovered an expanding shell around V382 Vel with an outer diameter of about 12 .

show abstract

UU Aqr from high to low state

Vrielmann

Baptista

2002

Astron. Nachr.

View full text Add to dashboard Cite

In this paper we present Physical Parameter Eclipse Mapping (PPEM) of UBVRI eclipse light curves of UU Aqr from high to low states. We used a simple, pure hydrogen LTE model to derive the temperature and surface density distribution in the accretion disc. The reconstructed effective temperatures in the disc range between 9000 K and 15000 K in the inner part of the disc and below 7000 K in the outer parts. In the higher states it shows a more or less prominent bright spot with Teff between about 7000 K and 8000 K. The inner part of the disc (R < 0.3R) isL1 optically thick at all times, while the outer parts of the disc up to the disc edge (0.51 ± 0.04RL1 in the high state and 0.40 ± 0.03RL1 in the low state) deviate from a simple black body spectrum indicating that either the outer disc is optically thin or it shows a temperature inversion in the vertical direction. While during high state the disc is variable, it appears rather stable in low state. The variation during high state affects the size of the optically thick part of the disc, the white dwarf or boundary layer temperature and the uneclipsed component (originating in a disc chromosphere and/or cool disc wind), while the actual size of the disc remains constant. The difference between high and low state is expressed as a change in disc size that also affects the size of the optically thick part of the disc and the presence of the bright spot. Using the PPEM method we retrieve a distance for UU Aqr of 207±10 pc, compatible with previous estimates.

show abstract

Unusual “Stunted” Outbursts in Old Novae and Nova-like Cataclysmic Variables

Cited by 72 publications

References 43 publications

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

SALT observations of southern post-novae

UU Aqr from high to low state

Contact Info

Product

Resources

About