<i>Kepler</i>and<i>Hale</i>observations of V523 Lyrae

Mason, E.; Howell, Steve B.

doi:10.1051/0004-6361/201628245

Cited by 5 publications

(4 citation statements)

References 43 publications

(62 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…They reported detecting stunted bursts in about ∼20% of the monitored systems. More recently, Mason & Howell (2016) note that the stunted burst behavior resembles the anomalous Z Cam behavior described by Simonsen (2011) 5 .…”

Section: Discussionmentioning

confidence: 59%

“…Such outburst/dip pairs are occasionally seen in other NL CVs having stunted outbursts, as noted in Honeycutt et al (1998) and Honeycutt (2001). Dips following stunted outbursts have also been documented in Kepler photometry of KIC 9406652 (Gies et al 2013), V523 Lyr (Mason & Howell 2016), and KIC 9202990 (Ramsay et al 2016). Figure 6 is useful to demonstrate the excursions from a mean behavior.…”

Section: Stunted Outburstsmentioning

confidence: 65%

See 1 more Smart Citation

The K2 Light Curves and Stunted Outbursts of AC Cnc

Schlegel

Honeycutt

2019

ApJ

View full text Add to dashboard Cite

We describe two observations of the nova-like cataclysmic variable AC Cnc obtained with Kepler during its revamped second mission (K2). Using the K2 1-minute cadence mode, the data were obtained during Campaigns 5 and 18. Campaign 5 (C05) lasted from ∼2015 Apr 27 to ∼2015 July 10, a total of 74.8 days, and yielded ∼106,000 measurements. Campaign 18 (C18) lasted from ∼2018 May 13 to ∼2018 July 2, a total of 50.7 days, yielding ∼72,000 measurements. The C05 light curve reveals two 'stunted outbursts' having properties consistent with stunted bursts observed from the ground; a stunted burst was underway during the C18 observation when it ended. During a stunted outburst, the primary eclipse is found to increase in depth but the residual brightness at mid-primary-eclipse remains nearly constant. By contrast, the secondary eclipse retains the same depth but the brightness at mid-secondary eclipse increases during outburst, following the orbital variations of the out-of-eclipse light. The eclipse ephemeris is statistically consistent with historical ephemerides and shows only marginal evidence for a period change. On the basis of the K2 data, we can not confirm a previously-reported non-orbital periodicity in AC Cnc.

show abstract

Section: Discussionmentioning

confidence: 59%

Section: Stunted Outburstsmentioning

confidence: 65%

The K2 Light Curves and Stunted Outbursts of AC Cnc

Schlegel

Honeycutt

2019

ApJ

View full text Add to dashboard Cite

show abstract

“…Similar kinds of dip events followed by the outbursts or brightenings were also seen in several CVs. Unlike the deep dips of HO Pup, where it loses 90% of its starlight, other CVs tend to reduce by only about 50% of their outburst brightness (Mason & Howell 2016;Schlegel & Honeycutt 2019). At most, a reduction of 80% of the outburst brightness can be seen in the case of KIC 9406652 (Gies et al 2013).…”

Section: Introductionmentioning

confidence: 94%

HO Puppis: Not a Be Star, but a Newly Confirmed IW And-type Star

Lee

et al. 2021

ApJ

View full text Add to dashboard Cite

HO Puppis (HO Pup) was considered as a Be-star candidate based on its γ Cassiopeiae-type light curve, but lacked spectroscopic confirmation. Using distance measured from Gaia Data Release 2 and the spectral-energydistribution fit on broadband photometry, the Be-star nature of HO Pup is ruled out. Furthermore, based on the 28,700 photometric data points collected from various time-domain surveys and dedicated intensive-monitoring observations, the light curves of HO Pup closely resemble those of IW And-type stars (as pointed out by Kimura et al.), exhibiting characteristics such as a quasi-standstill phase, brightening, and dips. The light curve of HO Pup displays various variability timescales, including brightening cycles ranging from 23 to 61 days, variations with periods between 3.9 days and 50 minutes during the quasi-standstill phase, and a semiregular ∼14 day period for the dip events. We have also collected time-series spectra (with various spectral resolutions), in which Balmer emission lines and other spectral lines expected for an IW And-type star were detected (even though some of these lines were also expected to be present for Be stars). We detect Bowen fluorescence near the brightening phase, and that can be used to discriminate between IW And-type stars and Be stars. Finally, despite only observing for four nights, the polarization variation was detected, indicating that HO Pup has significant intrinsic polarization.

show abstract

“…They are now widely referred to as IW And-type stars following the suggestion by Kato (2019). There was yet another object in the literature [V523 Lyr (Mason and Howell 2016)] which was not included in Kato (2019).…”

Section: Introductionmentioning

confidence: 99%

IW And-type state in IM Eridani

Katô

Wakamatsu

Kojiguchi

et al. 2019

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

IW And stars are a recently recognized group of dwarf novae which are characterized by a repeated sequence of brightening from a standstill-like phase with damping oscillations followed by a deep dip. Kimura et al. (2019) recently proposed a model based on thermal-viscous disk instability in a tilted disk to reproduce the IW And-type characteristics. IM Eri experienced the IW And-type phase in 2018 and we recorded three cycles of the (damping) oscillation phase terminated by brightening. We identified two periods during the IW And-type state: 4-5 d small-amplitude (often damping) oscillations and a 34-43 d long cycle. This behavior is typical for an IW And-type star. The object gradually brightened within the long cycle before the next brightening which terminated the (damping) oscillation phase. This observation agrees with the increasing disk mass during the long cycle predicted by a model of thermal-viscous disk instability in a tilted disk (Kimura et al. 2019). We, however, did not succeed in detecting negative superhumps, which are considered to be the signature of a tilted disk.

show abstract

KeplerandHaleobservations of V523 Lyrae

Cited by 5 publications

References 43 publications

The K2 Light Curves and Stunted Outbursts of AC Cnc

The K2 Light Curves and Stunted Outbursts of AC Cnc

HO Puppis: Not a Be Star, but a Newly Confirmed IW And-type Star

IW And-type state in IM Eridani

Contact Info

Product

Resources

About