The evolution of planetary nebulae

Schönberner, D.; Jacob, R.; Steffen, M.

doi:10.1051/0004-6361:20053108

Cited by 74 publications

(107 citation statements)

References 35 publications

(62 reference statements)

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“…If we take a limiting radius of 0.2 pc for a bright PN (10 arcsec diameter at the distance of the bulge, which is twice the limit of our survey), this corresponds to an expansion age of 10 000 yr for an expansion velocity of 20 km s −1 ) or 5000 yr for 40 km s −1 . The higher value is found in models (Schönberner et al 2005); our data shows about equal numbers of lower and higher velocities, correcting for the outer edge, which expands 1.4 times faster than the mass-averaged velocity derived from the spectra. A PN becomes observable once the central star reaches a temperature of 20 kK and fades when either the nebula becomes optically thin to ionizing radiation or the star begins to fade.…”

Section: Pn Visibilitysupporting

confidence: 40%

“…For A 43, we find 8.5 kyr and for VV 47 13 kyr, using the data of Friederich et al (2011) and Weinberger (1989), respectively. For the last object, we adopt the higher expansion velocity derived from [N ii] rather than lower value from [O iii], as assumed earlier by Schönberner & Napiwotzki (1990) because [N ii] emission better probes the outer shell regions (e.g., Schönberner et al 2005). We do not have a mass-averaged velocity for either object, and the kinematical ages are less certain than for the modelled nebulae.…”

Section: Asteroseismological Massesmentioning

confidence: 99%

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Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Gęsicki

Zijlstra

Hajduk

et al. 2014

A&A

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Aims. We study the star-formation history of the Galactic bulge, as derived from the age distribution of the central stars of planetary nebulae that belong to this stellar population. Methods. The high resolution imaging and spectroscopic observations of 31 compact planetary nebulae are used to derive their central star masses. We use the Blöcker post asymptotic giant branch (post-AGB) evolutionary models, which are accelerated by a factor of three in this case to better fit the white dwarf mass distribution and asteroseismological masses. Initial-final mass relations (IFMR) are derived using white dwarfs in clusters. These are applied to determine original stellar masses and ages. The age distribution is corrected for observational bias as a function of stellar mass. We predict that there are about 2000 planetary nebulae in the bulge. Results. The planetary nebula population points at a young bulge population with an extended star-formation history. The Blöcker tracks with the cluster IFMR result in ages, which are unexpectedly young. We find that the Blöcker post-AGB tracks need to be accelerated by a factor of three to fit the local white dwarf masses. This acceleration extends the age distribution. We adjust the IFMR as a free parameter to map the central star ages on the full age range of bulge stellar populations. This fit requires a steeper IFMR than the cluster relation. We find a star-formation rate in the Galactic bulge, which is approximately constant between 3 and 10 Gyr ago. The result indicates that planetary nebulae are mainly associated with the younger and more metal-rich bulge populations. Conclusions. The constant rate of star-formation between 3 and 10 Gyr agrees with suggestions that the metal-rich component of the bulge is formed during an extended process, such as a bar interaction.

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Section: Pn Visibilitysupporting

confidence: 40%

Section: Asteroseismological Massesmentioning

confidence: 99%

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Gęsicki

Zijlstra

Hajduk

et al. 2014

A&A

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“…A discussion with many results is given by Terzian (1997) and the effect of the ionization front is discussed by Mellema (2004). In addition, Schönberner et al(2005) have made and applied kinematic models of several PNe to obtain expansion distances. There is general agreement for the four PNe common to the results of both Mellema (2004) and Schönberner et al(2005), which indicate some of the expansion distances given by Terzian (1997) should be increased.…”

Section: Pn Distancesmentioning

confidence: 99%

“…In addition, Schönberner et al(2005) have made and applied kinematic models of several PNe to obtain expansion distances. There is general agreement for the four PNe common to the results of both Mellema (2004) and Schönberner et al(2005), which indicate some of the expansion distances given by Terzian (1997) should be increased. The increases depend on the individual models and are thus uncertain.…”

Section: Pn Distancesmentioning

confidence: 99%

Planetary nebulae abundances and stellar evolution II

Pottasch

Bernard─Salas

2010

A&A

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Context. In recent years mid-and far infrared spectra of planetary nebulae have been analysed and lead to more accurate abundances. It may be expected that these better abundances lead to a better understanding of the evolution of these objects. Aims. The observed abundances in planetary nebulae are compared to those predicted by the models of Karakas (2003, Thesis, Monash Univ. Melbourne) in order to predict the progenitor masses of the various PNe used. The morphology of the PNe is included in the comparison. Since the central stars play an important role in the evolution, it is expected that this comparison will yield additional information about them. Methods. First the nitrogen/oxygen ratio is discussed with relation to the helium/hydrogen ratio. The progenitor mass for each PNe can be found by a comparison with the models of Karakas. Then the present luminosity of the central stars is determined in two ways: first by computing the central star effective temperature and radius, and second by computing the nebular luminosity from the hydrogen and helium lines. This luminosity is also a function of the initial mass so that these two values of initial mass can be compared. Results. Six of the seven bipolar nebulae can be identified as descendants of high mass stars (4−6 M ) while the seventh is ambiguous. Most of the elliptical PNe have central stars which descend from low initial mass stars, although there are a few caveats which are discussed. There is no observational evidence for a higher mass for central stars which have a high carbon/oxygen ratio. The evidence provided by the abundance comparison with the models of Karakas is consistent with the HR diagram to which it is compared. In the course of this discussion it is shown how "optically thin" nebulae can be separated from those which are "optically thick".

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“…There are also a few objects with distances obtained by expansion parallaxes observed by GLIMPSE. However this method also has its limitations, especially concerning the derivation of the nebular expansion velocity (Mellema 2004), and the distances determined by this method may be underestimated by a factor 1.3 ∼ 3 (Schoenberner et al 2005). …”

Section: Estimation Of Errorsmentioning

confidence: 99%

A revised distance scale of planetary nebulae

Ortiz¹

2013

A&A

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Context. The advent of large-scale, high-sensitivity surveys of the Galaxy (2MASS, WISE, Spitzer, etc.) has allowed detection of a large number of planetary nebulae (PNe), some of them at large distances. Aims. I propose a new distance scale of planetary nebulae, based on two main quantities: the flux density (or magnitude) at 8 μm and the nebular apparent size. Methods. I used these quantities to calculate the specific intensity of the radiation I 8 μm , which decreases as the nebula evolves. The PNe situated in the Large Magellanic Cloud (LMC) with 8 μm photometry obtained by Spitzer and diameter obtained from HST observations were used as calibrators. Results. After calibration, I recalculated distances of PNe in the LMC, and they show a one-sigma spread of 10 kpc (20%). Eventually, I applied the method to a sample of 47 Galactic PNe observed during the Spitzer survey. These results showed agreement within 0.2 dex with the distances determined with another method of calibrating with PNe in the LMC. Conclusions. The main advantage of the present distance scale is that it is nearly "extinction free", which makes it especially suited to PNe severely affected by interstellar extinction, such as the Galactic disc and bulge. On the other hand, the method requires an unbiased determination of the nebular size, which might be quite uncertain for PNe with extended faint features, such as haloes and ansae.

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The evolution of planetary nebulae

Cited by 74 publications

References 35 publications

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Planetary nebulae abundances and stellar evolution II

A revised distance scale of planetary nebulae

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