On the Origin of Planetary Nebula K648 in Globular Cluster M15

Buell, J. F.; Henry, R. B. C.; Baron, Edward; Kwitter, K. B.

doi:10.1086/304273

Cited by 9 publications

(10 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Owing to this discrepancy, we prefer not to use Hen 2-86 as a primary calibrator. Globular cluster PNe: Both Pease 1, also known as K 648 (Buell et al 1997;Alves, Bond & Livio 2000) and the peculiar H-deficient nebula GJJC 1 (Cohen & Gillett 1989;Borkowski & Harrington 1991) are bona fide members of their respective globular clusters, M 15 (NGC 7078) and M 22 (NGC 6656). Pease 1 has been imaged with HST and has good estimates of its angular size (Alves et al 2000) and integrated flux which qualify it to be a primary calibrator.…”

Section: Bmp J1613-5406mentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

173

127

View full text Add to dashboard Cite

Measuring the distances to Galactic planetary nebulae (PNe) has been an intractable problem for many decades. We have now established a robust optical statistical distance indicator, the Hα surface brightness -radius or S Hα -r relation, which addresses this problem. We developed this relation from a critically evaluated sample of primary calibrating PNe. The robust nature of the method results from our revised calibrating distances with significantly reduced systematic uncertainties, and the recent availability of high-quality data, including updated nebular diameters and integrated Hα fluxes. The S Hα -r technique is simple in its application, requiring only an angular size, an integrated Hα flux, and the reddening to the PN. From these quantities, an intrinsic radius is calculated, which when combined with the angular size, yields the distance directly. Furthermore, we have found that optically thick PNe tend to populate the upper bound of the trend, while optically-thin PNe fall along the lower boundary in the S Hα -r plane. This enables sub-trends to be developed which offer even better precision in the determination of distances, as good as 18 per cent in the case of optically-thin, high-excitation PNe. This is significantly better than any previous statistical indicator. We use this technique to create a catalogue of statistical distances for over 1100 Galactic PNe, the largest such compilation in the literature to date. Finally, in an appendix, we investigate both a set of transitional PNe and a range of PN mimics in the S Hα -r plane, to demonstrate its use as a diagnostic tool. Interestingly, stellar ejecta around massive stars plot on a tight locus in S Hα -r space with the potential to act as a separate distance indicator for these objects.

show abstract

Section: Bmp J1613-5406mentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

173

127

View full text Add to dashboard Cite

show abstract

“…The model used here is the same as discussed in Buell et al (1997), where after a dredge‐up occurs the envelope is so polluted with carbon that it is essentially immediately ejected. As discussed by Buell et al (1997), this single dredge‐up heavily pollutes a low‐metallicity envelope, and the metallicity of the envelope jumps to near solar values. This results in an expansion of the star and this resulting expansion causes the star to immediately switch into a superwind phase.…”

Section: Resultsmentioning

confidence: 99%

“…Most of the relevant details of this model are explained in Buell et al (1997), Buell (1997) and Gavilan, Buell & Molla (2005). In this section, I concentrate on modifications of this model.…”

Section: O D E L Smentioning

confidence: 99%

Thermally pulsing asymptotic giant branch star models and globular cluster planetary nebulae - I. The model

Buell

2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Thermally pulsing asymptotic giant branch models of globular cluster stars are calculated using a synthetic model with the goal of reproducing the chemical composition, core masses and other observational parameters of the four known globular cluster planetary nebulae as well as roughly matching the overall cluster properties. The evolution of stars with an enhanced helium abundance (Y) and blue stragglers are modelled. New pre‐thermally pulsing asymptotic giant branch mass losses for red giant branch and early asymptotic giant branch stars are calculated from the Padova stellar evolution models. The new mass losses are calculated to get the relative differences in mass losses due to enhanced helium abundances. The global properties of the globular cluster planetary nebula are reproduced with these models. The metallicity, mass of the central star, overall metallicities, helium abundance and the nebular mass are matched to the observational values. Globular cluster planetary nebulae JaFu 1 and JaFu 2 are reproduced by assuming progenitor stars with masses near the typical main‐sequence turn‐offs of globular clusters and with enhanced helium abundances very similar to the enhancements inferred from fitting isochrones to globular cluster colour–magnitude diagrams. The globular cluster PN GJJC‐1 can be roughly fitted by a progenitor star with very extreme helium enhancement (Y ≈ 0.40) near the turn‐off producing a central star with the same mass as inferred by observations and a very low nebular mass. The abundances and core mass of planetary nebula Ps 1 and its central star (K648) are reproduced by a blue straggler model. However, it turned out to be impossible to reproduce its nebular mass, and it is concluded some kind of binary scenario may be needed to explain K648.

show abstract

“…The effects of pre-TP-AGB evolution are modeled using fits to published models. Most of the relevant details of this model are explained in Buell et al (1997), Buell (1997), and Gavilan, Buell, & Molla (2005). In paper I the most significant update to the model was an updated rule for treating the mass-loss during the red giant branch (RGB) and early-AGB (E-AGB) phases.…”

Section: Modelsmentioning

confidence: 99%

“…The methods to find both log LHe,max and log LHe,min can be found in Buell et al (1997). log LHe,max is the maximum luminosity of the helium shell during a shell flash and log LHe,min is the minimum luminosity required for a dredgeup to occur.…”

Section: Third Dredge-upmentioning

confidence: 99%

What planetary nebulae tell us about helium and CNO elements in Galactic bulge stars

Buell

2012

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Thermally pulsing asymptotic giant branch (TP-AGB) models of bulge stars are calculated using a synthetic model. The goal is to infer typical progenitor masses and compositions by reproducing the typical chemical composition and central star masses of planetary nebulae (PNe) in the Galactic bulge. The AGB tip luminosity and the observation that the observed lack of bright carbon stars in the bulge are matched by the models.Five sets of galactic bulge PNe were analyzed to find typical abundances and central star of planetary nebulae (CSPN) masses. These global parameters were matched by the AGB models. These sets are shown to be consistent with the most massive CSPN having the largest abundances of helium and heavy elements. The CSPN masses of the most helium rich (He/H 0.130 or Y 0.34) PNe are estimated to be between 0.58 and 0.62 M ⊙ . The oxygen abundance in form log (O/H) + 12 of these highest mass CSPN is estimated to be ≈8.85.TP-AGB models with ZAMS masses between 1.2 and 1.8 M ⊙ with Y ZAMS ≈ 0.31− 0.33 and Z ZAMS ≈ 0.19 − 0.22 fit the typical global parameters, mass, and abundances of the highest mass CSPN. The inferred ZAMS helium abundance of the most metal enriched stars implies dY /dZ ∼ 4 for the Galactic bulge. These models produce no bright carbon stars in agreement with observations of the bulge. These models produce an AGB tip luminosity for the bulge in agreement with the observations. These models suggest the youngest main sequence stars in the Galactic bulge have enhanced helium abundance (Y ≈ 0.32) on the main sequence and their ages are between 2 and 4 Gyrs.The chemical evolution of nitrogen in the Galactic bulge inferred from the models is consistent with the cosmic evolution inferred from HII regions and unevolved stars. The inferred ZAMS N/O ratio (log N/O ≈ −0.35) of bulge PNe with the largest CSPN masses are shown to be above the solar ratio. The inferred ZAMS N/O ratios of the entire range of PNe metallicities is consistent with both primary and secondary production of nitrogen contributing to the chemical evolution of nitrogen in the Galactic bulge.The inferred ZAMS value of C/O is less than 1. This indicates the mass of the PNe progenitors are low enough (M 1.8 M ⊙ ) to not produce carbon stars via the third dredge-up.

show abstract

On the Origin of Planetary Nebula K648 in Globular Cluster M15

Cited by 9 publications

References 40 publications

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Thermally pulsing asymptotic giant branch star models and globular cluster planetary nebulae - I. The model

What planetary nebulae tell us about helium and CNO elements in Galactic bulge stars

Contact Info

Product

Resources

About