Hydrostatic evolutionary sequences for the nuclei of planetary nebulae

Wood, P. R.; Faulkner, D. J.

doi:10.1086/164451

Cited by 221 publications

(129 citation statements)

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“…For the non DA/DB stars, we used other spectral models and fits accordingly: Rauch & Deetjen (2003) non-LTE H+He models for the DAOs and Hügelmeyer et al (2006) models for DO and PG1159 spectra. We used stellar radii taken from evolutionary models of Wood (1995) with thick and thin hydrogen layers for DAO and DO WDs and Bloecker (1995), Schoenberner (1983) and Wood & Faulkner (1986) models for PG1159 stars. DAB (3 stars) and DBA (1 star) WDs were treated in the same way as DA and DB WDs, respectively.…”

Section: The Atmospheric Models and Distancesmentioning

confidence: 99%

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

Krzesiński¹,

Kleinman²,

Nitta³

et al. 2009

A&A

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Aims. We present a hot white dwarf (WD) luminosity function (LF) using data taken from the Sloan Digital Sky Survey (SDSS) Data Release 4. We present and discuss a combined LF, along with separate DA and non-DA as LFs. We explore the completeness of our LFs and interpret a sudden drop in the non-DA LF near 2 M bol as a transition of the non-DA WD atmosphere into the DA one during WD evolution. Our LF extends roughly between −0.5 < M bol < 7 or equivalently, ∼120 000 K > T eff > ∼25 000 K. Our LF should now be useful for estimates of recent star formation and for studies of neutrino and other potential particle emission losses in hot WDs. Methods. To create a sample whose completeness can be characterized fully, we used stars whose spectra were obtained via the SDSS's "hot standard" target selection criteria. The hot standard stars were purposefully targeted to a high level of completeness by the SDSS for calibration purposes. We are fortunate that many of them are hot white dwarfs stars. We further limited the sample to stars with fitted temperatures exceeding 23 500 K and log g > 7.0. We determined stellar distances for our sample based on their absolute SDSS g filter magnitudes, derived from WD stellar atmosphere model fits to the SDSS stellar spectra. Results. We compared our LF with those of other researchers where overlap occurs; however, our LFs are unique in their extension to the most luminous/hottest WDs. The cool end of our LF connects with the hot end of previously determined SDSS WD LFs and agreement here is quite good. It is also good with previous non-SDSS WD LFs. We note distinct differences between the DA and non-DA LFs and discuss the reliability of the DA LF at its hot end. We have extended the range of luminosities covered in the most recent WD LFs. The SDSS sample is understood quite well and its exploration should contribute to a number of new insights into early white dwarf evolution.

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Section: The Atmospheric Models and Distancesmentioning

confidence: 99%

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

Krzesiński¹,

Kleinman²,

Nitta³

et al. 2009

A&A

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“…This, in turn, would modify the evolutionary curves to a signiÐcant degree ; one would predict quite di †erent mass functions It would seem, N(M CS ). however, that observations are most consistent with the hydrogen-burning tracks (Tylenda & StaSchonberner sinska 1989), while (1989 has also pointed to Schonberner inconsistencies in the He-burning analysis of Wood & Faulkner (1986).…”

Section: Introductionmentioning

confidence: 85%

The Validity of Mass Functions for the Central Stars of Planetary Nebulae

Phillips¹

2000

The Astronomical Journal

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It is commonly assumed that the distribution of masses for the central stars of planetary nebulae is strongly peaked about Such a mass function is similar to that deduced for white dwarfs. M CS + 0.6 M _ . We show in the following, however, that certain of the procedures used to evaluate are seriously N(M CS ) Ñawed and assume a nebular mass that is probably inappropriate. At the very least, the uncer-M NEB tainty in casts doubts upon the utility of these procedures, while the deduced functions M NEB N(M CS ) may be in error.

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“…The high effective temperatures require non-LTE modeling of the atmospheres. Such models for H-deficient compositions have only become Evolutionary tracks are from [14] and [1] (dashed lines), [23] and [6] (dot-dashed line) (labels: mass in M⊙). The latter 0.604 M⊙ track is the final CSPN track following a VLTP evolution and therefore has a H-deficient composition.…”

Section: Quantitative Spectral Analysis Of Pg1159 Starsmentioning

confidence: 99%

Element Abundance Determination in Hot Evolved Stars

Werner

2010

Recent Advances in Spectroscopy

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Summary. The hydrogen-deficiency in extremely hot post-AGB stars of spectral class PG1159 is probably caused by a (very) late helium-shell flash or a AGB final thermal pulse that consumes the hydrogen envelope, exposing the usually-hidden intershell region. Thus, the photospheric element abundances of these stars allow us to draw conclusions about details of nuclear burning and mixing processes in the precursor AGB stars. We compare predicted element abundances to those determined by quantitative spectral analyses performed with advanced non-LTE model atmospheres. A good qualitative and quantitative agreement is found for many species (He, C, N, O, Ne, F, Si, Ar) but discrepancies for others (P, S, Fe) point at shortcomings in stellar evolution models for AGB stars. Almost all of the chemical trace elements in these hot stars can only be identified in the UV spectral range. The Far Ultraviolet Spectroscopic Explorer and the Hubble Space Telescope played a crucial role for this research.

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Hydrostatic evolutionary sequences for the nuclei of planetary nebulae

Cited by 221 publications

References 0 publications

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

A hot white dwarf luminosity function from the Sloan Digital Sky Survey

The Validity of Mass Functions for the Central Stars of Planetary Nebulae

Element Abundance Determination in Hot Evolved Stars

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