Discovery of close binary central stars in the planetary nebulae NGC 6326 and NGC 6778

Miszalski, B.; Jones, D. Heath; Rodríguez‐Gil, P.; Boffin, H. M. J.; Corradi, R. L. M.; Santander-García, M.

doi:10.1051/0004-6361/201117084

Cited by 64 publications

(89 citation statements)

References 41 publications

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“…1) are extremely similar to those found in NGC 6326, NGC 6778, Hen 2-11, and NGC 5189 (Miszalski et al 2011b;Jones et al 2014a;Manick et al 2015). The geometrically opposed pairs of "knots" seen marking the ends of the major axis of the nebula are relatively typical of high velocity outflows or "jets" which are believed to be typical of central star binarity.…”

Section: Introductionsupporting

confidence: 71%

“…He ii λ4542 Å, He ii λ5412 Å, N v λ4604 Å) as well as emission lines frequently, but not exclusively (see above discussion of these lines in the spectra of Hen 2-155), associated with irradiated, main-sequence companions (see Fig. 13, and Miszalski et al 2011b;Corradi et al 2011). Both absorption and emission features visible in all spectra were inspected for velocity shifts, with respect to nebular emission lines (e.g.…”

Section: Stellar Photometry and Spectroscopymentioning

confidence: 99%

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The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

Jones

Boffin

Rodríguez‐Gil

et al. 2015

A&A

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We present a study of Hen 2-155 and Hen 2-161, two planetary nebulae which bear striking morphological similarities to other planetary nebulae known to host close-binary central stars. Both central stars are revealed to be photometric variables while spectroscopic observations confirm that Hen 2-155 is host to a double-eclipsing, post-common-envelope system with an orbital period of 3 h 33 m making it one of the shortest period binary central stars known. The observations of Hen 2-161 are found to be consistent with a post-common-envelope binary of period ∼1 day. A detailed model of the central star of Hen 2-155 is produced, showing the nebular progenitor to be a hot, post-AGB remnant of approximately 0.62 M , consistent with the age of the nebula, and the secondary star to be an M dwarf whose radius is almost twice the expected zero age main sequence radius for its mass. In spite of the small numbers, all main-sequence companions, of planetary nebulae central stars, to have had their masses and radii constrained by both photometric and spectroscopic observations have also been found to display this "inflation". The cause of the "inflation" is uncertain but is probably related to rapid accretion, immediately before the recent common-envelope phase, to which the star has not yet thermally adjusted. The chemical composition of both nebulae is also analysed, showing both to display elevated abundance discrepancy factors. This strengthens the link between elevated abundance discrepancy factors and close binarity in the nebular progenitor.

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Section: Introductionsupporting

confidence: 71%

Section: Stellar Photometry and Spectroscopymentioning

confidence: 99%

The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

Jones

Boffin

Rodríguez‐Gil

et al. 2015

A&A

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“…The most successful method so far is the detection of orbital modulation in the light curve (e.g. Bond 2000; De Marco et al 2008;Miszalski et al 2009aMiszalski et al ,b, 2011, which led to the discovery of about 40 systems. The modulation can be caused by ellipsoidal deformation, eclipses, or irradiation of the cool component by the hot component (e.g.…”

Section: Introductionmentioning

confidence: 99%

Binary central stars of planetary nebulae with long orbits: the radial velocity orbit of BD+33°2642 (PN G052.7+50.7) and the orbital motion of HD 112313 (PN LoTr5)

Winckel

Jorissen

Exter

et al. 2014

A&A

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Aims. We study the impact of binary interaction processes on the evolution of low-and intermediate-mass stars using long-term monitoring of their radial velocity. Here we report on our results on the central stars of two planetary nebulae (PNe): the well-studied spectrophotometric standard BD+33 • 2642 (central star of PNG 052.7+50.7) and HD 112313 (central star of PN LoTr5), the optical light of which is dominated by a rapidly rotating G star. Methods. The high-resolution spectra were cross-correlated with carefully selected masks of spectral lines. The individual masks were optimised for the spectral signatures of the dominant contributor of the optical light. Results. We report on the first detection of orbital motion in these two objects. For BD+33 • 2642 we sampled 1.5 cycles of the 1105 ± 24 day orbital period. For HD 112313 a full period is not yet covered, despite our 1807 days of monitoring. The radial-velocity amplitude shows that it is unlikely that the orbital plane is co-planar with the one defined by the nebular waist of the bipolar nebula. To our knowledge these are the first detections of orbits in PNe that are in a range from several weeks to a few years. Conclusions. The orbital properties and chemical composition of BD+33 • 2642 are similar to what is found in post-AGB binaries with circumbinary discs. The latter are probably progenitors of these PNe. For LoTr5 the Ba-rich central star and the long orbital period are similar to the Ba star giants, which hence serve as natural progeny. In contrast to the central star in LoTr5, normal Ba stars are slow rotators. The orbits of these systems have a low probability of occurrence according to recent population synthesis calculations.

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“…This improvement was largely driven by the improved multiplex advantage offered by the OGLE microlensing survey (Udalski 2009) which allowed for many discoveries to be made by Miszalski et al (2008Miszalski et al ( , 2009a. Substantial progress has also been helped by improved observing strategies including targeting PNe with suspected post-CE morphologies (Miszalski et al 2011a) and the use of less nebulacontaminated filters to obtain lightcurves (Miszalski et al 2011d). In addition to the OGLE discoveries more close binaries were found by Hillwig et al (2010), Hajduk et al (2010), Corradi et al (2011), Santander-García et al (2011 and Miszalski et al (2011aMiszalski et al ( , 2011cMiszalski et al ( , 2011d.…”

Section: Introductionmentioning

confidence: 99%

“…Substantial progress has also been helped by improved observing strategies including targeting PNe with suspected post-CE morphologies (Miszalski et al 2011a) and the use of less nebulacontaminated filters to obtain lightcurves (Miszalski et al 2011d). In addition to the OGLE discoveries more close binaries were found by Hillwig et al (2010), Hajduk et al (2010), Corradi et al (2011), Santander-García et al (2011 and Miszalski et al (2011aMiszalski et al ( , 2011cMiszalski et al ( , 2011d. Fewer wide binary systems are known and they mostly have chemically peculiar giants or sub-giants (e.g.…”

Section: Introductionmentioning

confidence: 99%

Ongoing surveys for close binary central stars and wider implications

Miszalski¹

2011

Proc. IAU

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Abstract. Binary central stars have long been invoked to explain the vexing shapes of planetary nebulae (PNe) despite there being scant direct evidence to support this hypothesis. Modern large-scale surveys and improved observing strategies have allowed us to significantly boost the number of known close binary central stars and estimate at least 20% of PNe have close binary nuclei that passed through a common-envelope (CE) phase. The larger sample of post-CE nebulae appears to have a high proportion of bipolar nebulae, low-ionisation structures (especially in SN1987A-like rings) and polar outflows or jets. These trends are guiding our target selection in ongoing multi-epoch spectroscopic and photometric surveys for new binaries. Multiple new discoveries are being uncovered that further strengthen the connection between post-CE trends and close binaries. These ongoing surveys also have wider implications for understanding CE evolution, low-ionisation structure and jet formation, spectral classification of central stars, asymptotic giant branch (AGB) nucleosynthesis and dust obscuration events in PNe.

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Discovery of close binary central stars in the planetary nebulae NGC 6326 and NGC 6778

Cited by 64 publications

References 41 publications

The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

The post-common envelope central stars of the planetary nebulae Henize 2-155 and Henize 2-161

Binary central stars of planetary nebulae with long orbits: the radial velocity orbit of BD+33°2642 (PN G052.7+50.7) and the orbital motion of HD 112313 (PN LoTr5)

Ongoing surveys for close binary central stars and wider implications

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