Spectroscopy of planetary nebulae in M 33

Magrini, L.; Perinotto, M.; Corradi, R. L. M.; Mampaso, A.

doi:10.1051/0004-6361:20030031

Cited by 64 publications

(139 citation statements)

References 35 publications

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“…The most important difference between the new and the old simulation is that the old one uses a central star mass distribution extending down to masses as low as 0.55 M . The luminosity drop suffered by H-burning central stars is in fact much less dramatic for lower mass central stars, (2002) and Magrini et al (2000), are compared with PN evolutionary tracks from SJSS07. Z GD means the metallicity of our Galactic disk.…”

Section: Resultsmentioning

confidence: 98%

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Méndez

Teodorescu

Schönberner

et al. 2008

ApJ

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We describe a procedure for the numerical simulation of the planetary nebulae luminosity function ( PNLF), improving on previous work. Earlier PNLF simulations were based on an imitation of the observed distribution of the intensities of [O iii] k5007 relative to H , generated predominantly using random numbers. We are now able to replace this by a distribution derived from the predictions of hydrodynamical PN models (Schönberner et al. 2007), which are made to evolve as the central star moves across the HR diagram, using proper initial and boundary conditions. In this way we move one step closer to a physically consistent procedure for the generation of a PNLF. As an example of these new simulations, we have been able to reproduce the observed PNLF in the Small Magellanic Cloud.

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Section: Resultsmentioning

confidence: 98%

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Méndez

Teodorescu

Schönberner

et al. 2008

ApJ

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“…28 compares the data of two Local Group galaxies, M 31 (Ciardullo et al 2002) and M 33 (Magrini et al 2000), with our model predictions. The observations occupy a wedge-like region in this diagram and are, according to Herrmann et al (2008) The lower boundary is nearly perfectly matched by all of our models during their early, optically-thick evolution towards maximum 5007 Å emission, virtually independently of their parameters and chemical composition.…”

Section: L(5007)/l(hα + [N Ii]) With the Brightness In [O Iii] M(5007)mentioning

confidence: 91%

“…Models which remain optically thick (i.e. the ones with the 0.696 M (Ciardullo et al 2002) and the disk of M 33 (Magrini et al 2000), as a function of M (5007), compared with the predictions of various hydrodynamical sequences with different metallicities. Evolution proceeds always from faint magnitudes and low line ratios up to maximum 5007 Å emission and then back again, but at higher line ratios.…”

Section: L(5007)/l(hα + [N Ii]) With the Brightness In [O Iii] M(5007)mentioning

confidence: 99%

The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

A&A

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Aims. By means of hydrodynamical models we do the first investigations of how the properties of planetary nebulae are affected by their metal content and what can be learned from spatially unresolved spectrograms of planetary nebulae in distant stellar systems. Methods. We computed a new series of 1D radiation-hydrodynamics planetary nebulae model sequences with central stars of 0.595 M surrounded by initial envelope structures that differ only by their metal content. At selected phases along the evolutionary path, the hydrodynamic terms were switched off, allowing the models to relax for fixed radial structure and radiation field into their equilibrium state with respect to energy and ionisation. The analyses of the line spectra emitted from both the dynamical and static models enabled us to systematically study the influence of hydrodynamics as a function of metallicity and evolution. We also recomputed selected sequences already used in previous publications, but now with different metal abundances. These sequences were used to study the expansion properties of planetary nebulae close to the bright cut-off of the planetary nebula luminosity function. Results. Our simulations show that the metal content strongly influences the expansion of planetary nebulae: the lower the metal content, the weaker the pressure of the stellar wind bubble, but the faster the expansion of the outer shell because of the higher electron temperature. This is in variance with the predictions of the interacting-stellar-winds model (or its variants) according to which only the central-star wind is thought to be responsible for driving the expansion of a planetary nebula. Metal-poor objects around slowly evolving central stars become very dilute and are prone to depart from thermal equilibrium because then adiabatic expansion contributes to gas cooling. We find indications that photoheating and line cooling are not fully balanced in the evolved planetary nebulae of the Galactic halo. Expansion rates based on widths of volume-integrated line profiles computed from our radiation-hydrodynamics models compare very well with observations of distant stellar system. Objects close to the bright cut-off of the planetary nebula luminosity function consist of rather massive central stars (>0.6 M ) with optically thick (or nearly thick) nebular shells. The halfwidth-half-maximum velocity during this bright phase is virtually independent of metallicity, as observed, but somewhat depends on the final AGB-wind parameters. Conclusions. The observed expansion properties of planetary nebulae in distant stellar systems with different metallicities are explained very well by our 1D radiation-hydrodynamics models. This result demonstrates convincingly that the formation and acceleration of a planetary nebula occurs mainly because of ionisation and heating of the circumstellar matter by the stellar radiation field, and that the pressure exerted by the shocked stellar wind is less important. Determinations of nebular abundances by means of photoionisa...

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“…Emission-line objects were identified using a standard on-band/off-band technique (Magrini et al 2000). Briefly, the stellar continuum of Sextans B (Strömgren y images, properly scaled) was subtracted from the narrow-band images in order to highlight emission-line objects.…”

Section: Data Reduction and Analysismentioning

confidence: 99%

The Local Group Census: Planetary nebulae in Sextans B

Magrini

Corradi

Walton

et al. 2002

A&A

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Abstract. Five planetary nebulae (PNe) have been discovered in the nearby dwarf irregular galaxy. Emission line images were obtained using the Wide Field Camera of the 2.5 m Isaac Newton Telescope (INT) at La Palma (Spain). The candidate PNe were identified by their point-like appearance and relatively strong [O iii] emission-line fluxes. They are located within a galactocentric distance of 2.8 arcmin, corresponding to 1.1 kpc at the distance of Sextans B. Luminosities are in the range 1800-5600 L . Sextans B is one of the smallest dwarf irregular galaxies with a PN population. The number of PNe detected suggest an enhanced star formation rate between 1 and 5 Gyr ago.

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Spectroscopy of planetary nebulae in M 33

Cited by 64 publications

References 35 publications

Toward Better Simulations of Planetary Nebulae Luminosity Functions

Toward Better Simulations of Planetary Nebulae Luminosity Functions

The evolution of planetary nebulae

The Local Group Census: Planetary nebulae in Sextans B

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