Direct detection of SDSS J0926+3624 orbital expansion with ARCONS

Szypryt, Paul; Duggan, G.; Mazin, Benjamin A.; Meeker, Seth R.; Strader, M. J.; Eyken, J. C. van; Marsden, Danica; O’Brien, Kieran; Walter, Alex; Ulbricht, Gerhard; Prince, Thomas A.; Stoughton, Chris; Bumble, B.

doi:10.1093/mnras/stu137

Cited by 21 publications

(18 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For such a measurement, we need a star with a fairly precise signature of orbital phase (e.g., eclipsing systems, such as YZ LMi (Szypryt et al 2014) or Gaia14aae (Campbell et al 2015)). We also need to track it for 10 years or more (possibly much more if the orbital period is long).…”

Section: Discussionmentioning

confidence: 99%

Orbital Period Increase in ES Ceti

Miguel

Patterson

Kemp

et al. 2017

ApJ

View full text Add to dashboard Cite

We report a long-term study of the eclipse times in the 10minute helium binary ES Ceti. The binary period increases rapidly, with P P 6.2 10 6=´years. This is consistent with the assumption that gravitational radiation (GR) drives the mass transfer, and it appears to be the first dynamical evidence that GR is indeed the driver of evolution in this class of very old cataclysmic variables-the AM Canum Venaticorum stars.

show abstract

Section: Discussionmentioning

confidence: 99%

Orbital Period Increase in ES Ceti

Miguel

Patterson

Kemp

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…The orbital period change Ṗ orb = (3.07 ± 0.56) × 10 −13 day day −1 at the 5.4 σ level was quite recently found for the first discovered eclipsing AM CVn type binary SDSS J0926+3624 ( P orb = 28.3 min. [746]). This value of Ṗ is consistent with the mass-exchange rate close to 1.8 × 10 −10 M ⊙ yr −1 , expected both in the “double-degenerate” and “helium-star” channels of the evolution of AM CVn stars for the period of SDSS J0926+3624.…”

Section: Evolution Of Interacting Double-degenerate Systemsmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

461

382

View full text Add to dashboard Cite

We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

show abstract

“…The extreme mass ratios of AM CVns mean that the likelihood of observing such systems is low and currently only two eclipsing AM CVn systems are known. SDSSJ0926+3624 was the first eclipsing AM CVn star to be discovered (Anderson et al 2005;Copperwheat et al 2011;Szypryt et al 2014), however its WD is only partially eclipsed. A second partial eclipser (PTF1 J191905.19+481506.2; Levitan et al 2014) was recently discovered, but it only eclipses the edge of the disc and not the WD, and so cannot be used for parameter determination.…”

Section: Introductionmentioning

confidence: 99%

Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

Campbell

Marsh

Fraser

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We report the discovery and characterization of a deeply eclipsing AM CVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third outburst is seen in archival Pan-STARRS-1 (PS1; Schlafly et al.; Tonry et al.; Magnier et al.) and ASAS-SN data. Spectroscopy reveals a hot, hydrogen-deficient spectrum with clear double-peaked emission lines, consistent with an accreting double-degenerate classification. We use follow-up photometry to constrain the orbital parameters of the system. We find an orbital period of 49.71 min, which places Gaia14aae at the long period extremum of the outbursting AM CVn period distribution. Gaia14aae is dominated by the light from its accreting white dwarf (WD). Assuming an orbital inclination of 90 • for the binary system, the contact phases of the WD lead to lower limits of 0.78 and 0.015 M on the masses of the accretor and donor, respectively, and a lower limit on the mass ratio of 0.019. Gaia14aae is only the third eclipsing AM CVn star known, and the first in which the WD is totally eclipsed. Using a helium WD model, we estimate the accretor's effective temperature to be 12 900 ± 200 K. The three outburst events occurred within four months of each other, while no other outburst activity is seen in the previous 8 yr of Catalina Real-time Transient Survey (CRTS; Drake et al.), Pan-STARRS-1 and ASAS-SN data. This suggests that these events might be rebrightenings of the first outburst rather than individual events.

show abstract

Direct detection of SDSS J0926+3624 orbital expansion with ARCONS

Cited by 21 publications

References 15 publications

Orbital Period Increase in ES Ceti

Orbital Period Increase in ES Ceti

The Evolution of Compact Binary Star Systems

Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

Contact Info

Product

Resources

About