2015
DOI: 10.1093/mnras/stv249
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Identifying close binary central stars of PN with Kepler

Abstract: Six planetary nebulae (PN) are known in the Kepler space telescope field of view, three newly identified. Of the 5 central stars of PN with useful Kepler data, one, J 193110888+4324577, is a short-period, post common envelope binary exhibiting relativistic beaming effects. A second, the central star of the newly identified PN Pa 5, has a rare O(He) spectral type and a periodic variability consistent with an evolved companion, where the orbital axis is almost aligned with the line of sight. The third PN, NGC 68… Show more

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Cited by 69 publications
(58 citation statements)
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“…De Marco et al (2015) analyze the Kepler light curve of the central star of planetary nebula Kn 61, which exhibits brightening events every 2-12 days, each lasting 1-2 days with amplitudes of 8%-14%. These events are similar to the outbursts on KIC 4552982, at least in that they are also unlike previously studied behavior.…”
Section: Discussion Of Outburstsmentioning
confidence: 99%
“…De Marco et al (2015) analyze the Kepler light curve of the central star of planetary nebula Kn 61, which exhibits brightening events every 2-12 days, each lasting 1-2 days with amplitudes of 8%-14%. These events are similar to the outbursts on KIC 4552982, at least in that they are also unlike previously studied behavior.…”
Section: Discussion Of Outburstsmentioning
confidence: 99%
“…The element abundances are summarized in Table 4 and displayed in Fig. 7, together with results for RCB and EHe stars (from Jeffery et al 2011, and references Currently, ten objects were assigned to the group of O(He) stars (Reindl et al 2014;Werner et al 2014;De Marco et al 2015). They cover a parameter range of T eff = 80 000−195 000 K and log g = 5.0−6.7.…”
Section: Summary and Discussionmentioning
confidence: 99%
“…Many of those systems were discovered through photometric variability, and while most are likely to be real binaries, additional confirmation is necessary for some of them (e.g., Kn 61; De Marco et al 2015). Along with studies confirming the binarity of several of these systems (e.g., Shimanskii et al 2008;Hillwig et al 2015Hillwig et al , 2016, discoveries of additional close binary CSPNe are helping us to better understand the nature of these systems.…”
Section: Introductionmentioning
confidence: 99%