Far ultraviolet spectroscopic explorer observation of the ultramassive white dwarf PG 1658+441

Jean Dupuis; Pierre Chayer; Stéphane Vennes; Nicole F. Allard; Guillaume Hébrard

doi:10.1086/378719

Far ultraviolet spectroscopic explorer observation of the ultramassive white dwarf PG 1658+441

Jean Dupuis^*, Pierre Chayer, Stéphane Vennes, Nicole F. Allard, Guillaume Hébrard

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

18 Citations (Scopus)

Abstract

We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of the ultramassive (M = 1.31 M_⊙), magnetic (B _s = 2.3 MG) white dwarf PG 1658+441. The far-ultraviolet (FUV) spectrum exhibits very broad Lyman lines and quasi-molecular Lyβ satellites, but weak Lyγ satellites may also be present. PG 1658+441 is the hottest white dwarf known to show these satellite features. We fit the Lyman lines with stellar models and obtain atmospheric parameters consistent with a published analysis of the Balmer lines. By averaging results obtained for the different FUSE segments, we determine T_eff = 29,620 ± 500 K and log_g = 9.31 ± 0.07. The models match the data over large portions of the spectrum, but discrepancies remain near the satellite features. Finally, no trace elements have been identified in the FUV spectrum, and we provide abundance upper limits for C, N, Si, and P.

Original language	English
Pages (from-to)	486-491
Number of pages	6
Journal	Astrophysical Journal
Volume	598
Issue number	1 I
DOIs	https://doi.org/10.1086/378719
Publication status	Published - 20 Nov 2003

Access to Document

10.1086/378719

Cite this

@article{980da6b48a774c7e8261c57e2a4cf61a,

title = "Far ultraviolet spectroscopic explorer observation of the ultramassive white dwarf PG 1658+441",

abstract = "We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of the ultramassive (M = 1.31 M⊙), magnetic (B s = 2.3 MG) white dwarf PG 1658+441. The far-ultraviolet (FUV) spectrum exhibits very broad Lyman lines and quasi-molecular Lyβ satellites, but weak Lyγ satellites may also be present. PG 1658+441 is the hottest white dwarf known to show these satellite features. We fit the Lyman lines with stellar models and obtain atmospheric parameters consistent with a published analysis of the Balmer lines. By averaging results obtained for the different FUSE segments, we determine Teff = 29,620 ± 500 K and logg = 9.31 ± 0.07. The models match the data over large portions of the spectrum, but discrepancies remain near the satellite features. Finally, no trace elements have been identified in the FUV spectrum, and we provide abundance upper limits for C, N, Si, and P.",

keywords = "Line: profiles, Stars: abundances, Ultraviolet: stars, White dwarfs",

author = "Jean Dupuis and Pierre Chayer and St{\'e}phane Vennes and Allard, {Nicole F.} and Guillaume H{\'e}brard",

year = "2003",

month = nov,

day = "20",

doi = "10.1086/378719",

language = "English",

volume = "598",

pages = "486--491",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 I",

}

TY - JOUR

T1 - Far ultraviolet spectroscopic explorer observation of the ultramassive white dwarf PG 1658+441

AU - Dupuis, Jean

AU - Chayer, Pierre

AU - Vennes, Stéphane

AU - Allard, Nicole F.

AU - Hébrard, Guillaume

PY - 2003/11/20

Y1 - 2003/11/20

N2 - We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of the ultramassive (M = 1.31 M⊙), magnetic (B s = 2.3 MG) white dwarf PG 1658+441. The far-ultraviolet (FUV) spectrum exhibits very broad Lyman lines and quasi-molecular Lyβ satellites, but weak Lyγ satellites may also be present. PG 1658+441 is the hottest white dwarf known to show these satellite features. We fit the Lyman lines with stellar models and obtain atmospheric parameters consistent with a published analysis of the Balmer lines. By averaging results obtained for the different FUSE segments, we determine Teff = 29,620 ± 500 K and logg = 9.31 ± 0.07. The models match the data over large portions of the spectrum, but discrepancies remain near the satellite features. Finally, no trace elements have been identified in the FUV spectrum, and we provide abundance upper limits for C, N, Si, and P.

AB - We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of the ultramassive (M = 1.31 M⊙), magnetic (B s = 2.3 MG) white dwarf PG 1658+441. The far-ultraviolet (FUV) spectrum exhibits very broad Lyman lines and quasi-molecular Lyβ satellites, but weak Lyγ satellites may also be present. PG 1658+441 is the hottest white dwarf known to show these satellite features. We fit the Lyman lines with stellar models and obtain atmospheric parameters consistent with a published analysis of the Balmer lines. By averaging results obtained for the different FUSE segments, we determine Teff = 29,620 ± 500 K and logg = 9.31 ± 0.07. The models match the data over large portions of the spectrum, but discrepancies remain near the satellite features. Finally, no trace elements have been identified in the FUV spectrum, and we provide abundance upper limits for C, N, Si, and P.

KW - Line: profiles

KW - Stars: abundances

KW - Ultraviolet: stars

KW - White dwarfs

UR - http://www.scopus.com/inward/record.url?scp=0346896398&partnerID=8YFLogxK

U2 - 10.1086/378719

DO - 10.1086/378719

M3 - Article

SN - 0004-637X

VL - 598

SP - 486

EP - 491

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

Far ultraviolet spectroscopic explorer observation of the ultramassive white dwarf PG 1658+441

Abstract

Access to Document

Other files and links

Fingerprint

Cite this