On the absence of nova shells

Schmidtobreick, L.; Shara, Michael M.; Tappert, C.; Bayo, A.; Ederoclite, A.

doi:10.1093/mnras/stv250

Cited by 22 publications

(19 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Including our detection limit, the percentage of novae that show shells and the number of observed systems we estimated a lower limit of 13000 years for the recurrence time of these systems. This is well in agreement to what is expected for such CVs with an average mass-transfer rate of about 5 × 10 −10 M /yr: The white dwarf needs to accrete for at least 20000 years to reach the critical mass for the nova explosion [14]. We also observed 20 novalike stars down to a limit of 10 −17 erg cm −2 s −1 arcsec −2 but without detection [15].…”

Section: The Search For Ancient Novaesupporting

confidence: 90%

The hunt for ancient novae

Schmidtobreick¹,

Tappert²,

Shara³

et al. 2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

View full text Add to dashboard Cite

Section: The Search For Ancient Novaesupporting

confidence: 90%

The hunt for ancient novae

Schmidtobreick¹,

Tappert²,

Shara³

et al. 2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

View full text Add to dashboard Cite

“…The success rate of these searches were 8/17, 4/17 and 13/30 nova shells found around potential candidates, these comprise roughly half of the known nova shells, the other half, for the most part, have been uncovered individually. More recently Schmidtobreick et al (2015) searched for nova shells around nova-like cataclysmic variable systems, without the successful detection of shells around the 15 objects in their study. The non-detection of nova shells around these objects are used to place constraints on the recurrence timescale of the objects Table 2.…”

Section: Introductionmentioning

confidence: 99%

Two new nova shells associated with V4362 Sagittarii and DO Aquilae

Harvey

Redman

Boumis

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

A classical nova is an eruption on the surface of a white dwarf in an accreting binary system. The material ejected from the white dwarf surface generally forms an axisymmetric shell. The shaping mechanisms of nova shells are probes of the processes that take place at energy scales between planetary nebulae and supernova remnants. We report on the discovery of nova shells surrounding the post-nova systems V4362 Sagittarii (1994) and more limited observations of DO Aquilae (1925). Distance measurements of $0.5\substack{+1.4 \\-0.2}$ kpc for V4362 Sgr and 6.7 ± 3.5 kpc for DO Aql are found based on the expansion parallax method. The growth rates are measured to be 0.07″/year for DO Aql and 0.32″/year for V4362 Sgr. A preliminary investigation into the ionisation structure of the nova shell associated with V4362 Sgr is presented. The observed ionisation structure of nova shells depends strongly on their morphology and the orientation of the central component towards the observer. X-ray, IR and UV observations as well as optical integral field unit spectroscopy are required to better understand these interesting objects.

show abstract

“…Yet, a variety of authors have failed at identifying nova shells around CVs (e.g. Schmidtobreick et al [13] or Pagnotta & Zurek [10]). This may be due either to the absence of a nova shell around these objects or to the faintness of the shell.…”

Section: Searching For Old Novaementioning

confidence: 99%