UV spectroscopy of the hot bare stellar core H1504+65 with the HST Cosmic Origins Spectrograph

@article{Werner2011UVSO,
  title={UV spectroscopy of the hot bare stellar core H1504+65 with the HST Cosmic Origins Spectrograph},
  author={Klaus Werner and Thomas Rauch},
  journal={Astrophysics and Space Science},
  year={2011},
  volume={335},
  pages={121-124}
}
  • K. WernerT. Rauch
  • Published 27 January 2011
  • Physics, Geology
  • Astrophysics and Space Science
We present new ultraviolet spectra of the hottest known, peculiar white dwarf H1504+65, obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope. H1504+65 is the hottest known white dwarf (Teff=200 000 K) and has an atmosphere mainly composed by carbon and oxygen, augmented with high amounts of neon and magnesium. This object is unique and the origin of its surface chemistry is completely unclear. We probably see the naked core of either a C–O white dwarf or even a O–Ne–Mg… 

References

SHOWING 1-10 OF 11 REFERENCES

Chandra and FUSE spectroscopy of the hot bare stellar core H 1504+65 ⋆

H 1504+65 is an extremely hot hydrogen-deficient white dwarf with an effective temperature close to 200 000 K. We present new FUV and soft X-ray spectra obtained with FUSE and Chandra, which confirm

H 1504 + 65 - An extraordinarily hot compact star devoid of hydrogen and helium

The optical identification of the bright soft X-ray source H 1504 + 65, originally discovered by the HEAO I A-2 low energy detectors, is reported. The optical counterpart exhibits a steep, virtually

NLTE analysis of the unique pre-white dwarf H 1504+65.

The unique star H 1504+65 is analysed using new high S/N optical spectra and by line profile fits with line blanketed NLTE model atmospheres. The spectra cover the range from 3300 A to 6800 A and

The Elemental Abundances in Bare Planetary Nebula Central Stars and the Shell Burning in AGB Stars

We review the observed properties of extremely hot, hydrogen‐deficient post–asymptotic giant branch (AGB) stars of spectral type [WC] and PG1159. Their H deficiency is probably caused by a (very)

On the formation of hydrogen-deficient post-AGB stars

We present an evolutionary sequence of a low mass star from the Asymptotic Giant Branch (AGB) through its post-AGB stage, during which its surface chemical composition changes from hydrogen-rich to

On the evolution of those nuclei of planetary nebulae that experiencea final helium shell flash.

We suggest that some of the central stars of planetary nebulae experience a final thermal pulse having achieved a white dwarf configuration and begun their descent along a cooling white dwarf

Ultracompact X-Ray Binaries with Neon-rich Degenerate Donors

There are three low-mass X-ray binaries (4U 0614+091, 2S 0918-549, and 4U 1543-624) for which broad-line emission near 0.7 keV was previously reported. A recent high-resolution observation of 4U

On the Evolution of Stars that Form Electron-degenerate Cores Processed by Carbon Burning. IV. Outward Mixing During the Second Dredge-up Phase and Other Properties of a 10.5 M☉ Model Star*

A 10.5 M☉ model of Population I composition is evolved from the main sequence through the core carbon-burning phase. As in 9 and 10 M☉ models studied in earlier papers of this series, carbon is

On the interpretation and implications of nova abundances: An abundance of riches or an overabundance of enrichments

We reexamine the question of the frequency of occurrence of oxygen-neon-magnesium (ONeMg) degenerate dwarfs in classical nova systems, in light of recent observations which have been interpreted as

Quantitative Spectral Analyses of CSPNs of Early [WC]-Type

Among the Central Stars of Planetary Nebulae (CSPN) there are several stars which show Wolf-Rayet-type spectra resembling those of Pop. I Wolf-Rayet (WR) stars of the carbon sequence (WC). Due to