The rapid evolution of the exciting star of the Stingray nebula

Reindl, N.; Rauch, T.; Parthasarathy, M.; Werner, K.; Kruk, J. W.; Hamann, Wolf-Rainer; Sander, A. A. C.; Todt, H.

doi:10.1051/0004-6361/201323189

Cited by 34 publications

(86 citation statements)

References 40 publications

(100 reference statements)

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“…Hügelmeyer et al (2006) already noted that the mean value of their sample of 20 DOs from the SDSS DR4 was somewhat larger (0.69 M ), although some of the difference could be due to the calibration problem reported in Kleinman et al (2009Kleinman et al ( , 2013 Reindl et al 2014). In conclusion, there is no significant difference in the mean masses of the three considered H-deficient spectral classes.…”

Section: Discussionmentioning

confidence: 98%

“…It is interesting to compare the properties of our four new O(He) stars to those of the previously known four ones, that were recently re-analyzed by Reindl et al (2014). The latter have T eff = 110 000-135 000 K, log g = 5.8-6.4, i.e.…”

Section: O(he) Starsmentioning

confidence: 89%

“…Their origin must be different from the PG 1159 stars, because the late He-shell flash scenario always produces objects with much higher C abundances. Possible explanations are discussed at length by Reindl et al (2014) in their analysis of the previously known O(He) stars and must not be repeated in detail here. It suffices to state that their origin is mysterious and that they are representing a second H-deficient evolutionary channel leading to DO white dwarfs.…”

Section: Discussionmentioning

confidence: 99%

“…The new four O(He) stars double the number of such stars known (Reindl et al 2014). As to the DO white dwarfs, only nine were hitherto known having T eff ≥ 90 000 K (Dreizler & Werner 1996;Hügelmeyer et al 2006).…”

Section: Observations and Line Identificationsmentioning

confidence: 93%

“…In contrast to the DOs they have low gravity and in contrast to PG 1159 stars they have at most very weak C iv lines. The four previously know O(He)s were recently re-analyzed (T eff = 110 000 K-135 000 K, log g = 5.8-6.4, C/He < 2 × 10 −4 -0.003 by number; Reindl et al 2014). Their origin is rather unclear, A&A 564, A53 (2014) because late He-shell flash evolutionary models do not predict that surface chemistry.…”

Section: Introductionmentioning

confidence: 99%

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New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Werner¹,

Rauch²,

Kepler

2014

A&A

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We have detected 21 new, very hot hydrogen-deficient (pre-) white dwarfs (spectral types O(He), hot DO, PG1159) in the Data Release 10 of the Sloan Digital Sky Survey. We present the results of non-local thermodynamic equilibrium (non-LTE) model-atmosphere analyses. The seven PG1159 stars have effective temperatures and surface gravities in the ranges T eff = 100 000-140 000 K and log g = 6-7.5. The hottest one is a new member of the rare hybrid-PG1159 subtype, indicating the presence of residual hydrogen. The ten new hot DOs span T eff = 65 000-120 000 K and log g = 7.5-8. Carbon abundances were derived and it is found that the PG1159 star values (C/He = 0.33-0.03 by number) and the DO values (<0.0004-0.01) cover distinct but adjacent ranges. With the discovery of four new O(He) stars (T eff = 80 000-100 000 K, log g = 5-5.5, C/He = 0.002-0.01), we double the number of known members of this rare spectral class. One of them is particularly interesting because it is unusually rich in C, N, O, and Si. Unexpected problems arose with the DOs because many He ii lines of every other star are so deep that they cannot be matched by any model. This is most conspicuous in the case of one object which exhibits the occurrence of ultrahigh-ionization metal features, a hitherto unexplained phenomenon that is known from a disquieting large fraction of hot DOs.

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Section: Discussionmentioning

confidence: 98%

Section: O(he) Starsmentioning

confidence: 89%

Section: Discussionmentioning

confidence: 99%

Section: Observations and Line Identificationsmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

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New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Werner¹,

Rauch²,

Kepler

2014

A&A

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Late Thermal Pulse Models and the Rapid Evolution of V839 Ara

Lawlor

2018

Proc. IAU

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We present evolution calculations from the Asymptotic Giant Branch (AGB) to the Planetary Nebula (PNe) phase for models of mass 1.0 to 2.0 M⊙ over a range of metallicities. The understanding of these objects plays an important role in galactic evolution and composition. Here, we particularly focus on Late Thermal Pulse (LTP) models, which are models that experience an intense helium-shell pulse that occurs just following AGB departure and causes a rapid looping evolution between the AGB and PN phases. The transient phases only last decades and centuries while increasing and decreasing in temperature dramatically. We use our models to make comparisons to V839 Ara (SAO 244567). This star has been observed rapidly heating over more than 50 years. Observations have proven difficult to model because the central star has a small radius, high surface gravity, and low temperature compared to our models.

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The inside-out planetary nebula around a born-again star

et al. 2018

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Planetary nebulae are ionized clouds of gas formed by the hydrogen-rich envelopes of low-and intermediate-mass stars ejected at late evolutionary stages. The strong UV flux from their central stars causes a highly stratified ionization structure, with species of higher ionization potential closer to the star. Here we report on the exceptional case of HuBi 1, a double-shell planetary nebula whose inner shell presents emission from low-ionization species close to the star and emission from high-ionization species farther away. Spectral analysis demonstrates that the inner shell of HuBi 1 is excited by shocks, whereas its outer shell is recombining. The anomalous excitation of these shells can be traced to its low-temperature [WC10] central star whose optical brightness has declined continuously by 10 magnitudes in a period of 46 years. Evolutionary models reveal that this star is the descendent of a low-mass star (≃ 1.1 M ⊙ ) that has experienced a born-again event[1] whose ejecta shock-excite the inner shell. HuBi 1 represents the missing link in the formation of metal-rich central stars of planetary nebulae from low-mass progenitors, offering unique insight regarding the future evolution of the born-again Sakurai's object [2]. Coming from a solar-mass progenitor, HuBi 1 represents a potential end-state for our Sun.Planetary nebulae (PNe) are a short-lived ≈20,000 yr period in the transition of lowand intermediate-mass stars (M initial = 0.8 − 8.0M ⊙ ) from the Asymptotic Giant Branch (AGB) phase towards the white-dwarf (WD) phase. The ionization structure of PNe, 1

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The rapid evolution of the exciting star of the Stingray nebula

Cited by 34 publications

References 40 publications

New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Late Thermal Pulse Models and the Rapid Evolution of V839 Ara

The inside-out planetary nebula around a born-again star

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