Analysis of the optical emission of the young precataclysmic variables HS 1857+5144 and ABELL 65

Shimansky, V. V.; Pozdnyakova, S. A.; Borisov, N. V.; Bikmaev, I.; Vlasyuk, V. V.; Spiridonova, O. I.; Galeev, A.; Melnikov, S. S.

doi:10.1134/s1990341309040051

Cited by 21 publications

(36 citation statements)

References 18 publications

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“…While a ∼1 day period is highly suspicious, one other bCSPN is known to have a period extremely close to ∼1 day (Abell 65, Shimansky et al 2009;Bond & Livio 1990) meaning that such a period should not be ruled out. However, it is ultimately unclear whether the photometric variability in the central star of Hen 2-161 is associated with binarity, but we conclude that it is the most likely cause and 9 Note that Kingsburgh & Barlow (1994) proposed a higher threshold for being Type i which Hen 2-161 does not satisfy (N/O ≥ 0.8).…”

Section: Discussionmentioning

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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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: Discussionmentioning

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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“…Walsh & Walton (1996) also suggested that the CS was a cataclysmic variable (CV) star based on strong Balmer emission lines observed in the spectrum. Improved light curves (Shimansky et al 2009;Louie & Hillwig 2010) along with phase-resolved stellar spectra (Shimansky et al 2009) have since confirmed that the photometric variability is due to a strong irradiation effect, rather than eclipses, and that the irradiation effect is also the source of the strong emission lines observed in the optical spectrum. Those papers also confirmed a period very close to one day.…”

Section: Introductionmentioning

confidence: 99%

“…The complete phase-folded V-, R-, and I-band light curves are shown in Figure 2, where each has also been shifted to the apparent magnitude scale as described above. Shimansky et al (2009) use their spectra and V-band light curve to calculate a model for the binary system confirming that it is indeed an irradiated binary with a hot central star and cool companion. However, we believe that with our light curves in the V, R, and I bands along with some additional information described below, we are able to produce a more accurate model of the system.…”

Section: Orbital Ephemerismentioning

confidence: 99%

“…Because of the large number of parameters, binary system modeling often requires that a number of those parameters be estimated independently and used as fixed values in the modeling in order to reduce the degeneracy of the solution. Shimansky et al (2009) use the size and expansion rate of the PN to arrive at a nebular age and then use the evolutionary tracks of Blöcker (1995) to derive a radius of the central star. The primary difference in our approach to modeling the system occurs at this point.…”

Section: Orbital Ephemerismentioning

confidence: 99%

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Binary Central Stars of Planetary Nebulae Discovered Through Photometric Variability. Iii. The Central Star of Abell 65

Hillwig

Frew

Louie

et al. 2015

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A growing number of close binary stars are being discovered among central stars of planetary nebulae. Recent and ongoing surveys are finding new systems and contributing to our knowledge of the evolution of close binary systems. The push to find more systems was largely based on early discoveries which suggested that 10%-15% of all central stars are close binaries. One goal of this series of papers is confirmation and classification of these systems as close binaries and determination of binary system parameters. Here we provide time-resolved multiwavelength photometry of the central star of Abell 65 as well as further analysis of the nebula and discussion of possible binary-nebula connections. Our results for Abell 65 confirm recent work showing that it has a close, cool binary companion, though several of our model parameters disagree with the recently published values. With our longer time baseline of photometric observations from 1989 to 2009 we also provide a more precise orbital period of 1.0037577 days.

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“…The upper limit X-ray luminosities derived from our observations of the remaining undetected binary CSPNe (A65 and Hen 2-11) for an 8 MK plasma are 1.4 and 8.9×10 29 erg s −1 , respectively (see Table 5). For the secondaries found in A65 (Shimansky et al 2009) and Hen 2-11 (Jones et al 2014), the limit on log L X /L bol,2 is −3.6 and −2.8, respectively. These two limits are similar to what we expect to observe from spun-up companions, thus deeper observations may yet detect saturated (or somewhat less than saturated) X-ray emission from the companions.…”

Section: Detectability and The Undetected Cspnementioning

confidence: 99%

THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

Montez

Kastner

Balick

et al. 2015

ApJ

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We present X-ray spectral analysis of 20 point-like X-ray sources detected in Chandra Planetary Nebula Survey observations of 59 planetary nebulae (PNe) in the solar neighborhood. Most of these 20 detections are associated with luminous central stars within relatively young, compact nebulae. The vast majority of these point-like X-rayemitting sources at PN cores display relatively "hard" ( 0.5 keV) X-ray emission components that are unlikely to be due to photospheric emission from the hot central stars (CSPN). Instead, we demonstrate that these sources are well modeled by optically thin thermal plasmas. From the plasma properties, we identify two classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray luminosities, L X , that appear uncorrelated with the CSPN bolometric luminosity, L bol and (2) lower-temperature plasmas with L X /L bol ∼ 10 −7 . We suggest these two classes correspond to the physical processes of magnetically active binary companions and self-shocking stellar winds, respectively. In many cases this conclusion is supported by corroborative multiwavelength evidence for the wind and binary properties of the PN central stars. By thus honing in on the origins of X-ray emission from PN central stars, we enhance the ability of CSPN X-ray sources to constrain models of PN shaping that invoke wind interactions and binarity.

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Analysis of the optical emission of the young precataclysmic variables HS 1857+5144 and ABELL 65

Cited by 21 publications

References 18 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 Discovered Through Photometric Variability. Iii. The Central Star of Abell 65

THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

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