Skip to content Skip to navigation
University of Warwick
  • Study
  • |
  • Research
  • |
  • Business
  • |
  • Alumni
  • |
  • News
  • |
  • About

University of Warwick
Publications service & WRAP

Highlight your research

  • WRAP
    • Home
    • Search WRAP
    • Browse by Warwick Author
    • Browse WRAP by Year
    • Browse WRAP by Subject
    • Browse WRAP by Department
    • Browse WRAP by Funder
    • Browse Theses by Department
  • Publications Service
    • Home
    • Search Publications Service
    • Browse by Warwick Author
    • Browse Publications service by Year
    • Browse Publications service by Subject
    • Browse Publications service by Department
    • Browse Publications service by Funder
  • Help & Advice
University of Warwick

The Library

  • Login
  • Admin

Detection of a white dwarf companion to the white dwarf SDSSJ125733.63+542850.5

Tools
- Tools
+ Tools

Marsh, T. R., Gaensicke, B. T., Steeghs, D., Southworth, J., Koester, Detlev, Harris, V. and Merry, L. (2011) Detection of a white dwarf companion to the white dwarf SDSSJ125733.63+542850.5. The Astrophysical Journal, Vol.736 (No.2). p. 95. doi:10.1088/0004-637X/736/2/95 ISSN 0004-637X.

[img]
Preview
Text
WRAP_STeeghs_White_Dwarf_1002.4677v2.pdf - Accepted Version

Download (936Kb) | Preview
Official URL: http://dx.doi.org/10.1088/0004-637X/736/2/95

Request Changes to record.

Abstract

SDSSJ125733.63+542850.5 (hereafter SDSSJ1257+5428) is a compact white dwarf binary from the Sloan Digital Sky Survey that exhibits high-amplitude radial velocity variations on a period of 4.56 hr. While an initial analysis suggested the presence of a neutron star or black hole binary companion, a follow-up study concluded that the spectrum was better understood as a combination of two white dwarfs. Here we present optical spectroscopy and ultraviolet fluxes which directly reveal the presence of the second white dwarf in the system. SDSSJ1257+5428's spectrum is a composite, dominated by the narrow-lined spectrum from a cool, low-gravity white dwarf (T eff 6300 K, log g = 5-6.6) with broad wings from a hotter, high-mass white dwarf companion (11, 000-14, 000 K; ~1 M ). The high-mass white dwarf has unusual line profiles which lack the narrow central core to Hα that is usually seen in white dwarfs. This is consistent with rapid rotation with vsin i = 500-1750 km s–1, although other broadening mechanisms such as magnetic fields, pulsations, or a helium-rich atmosphere could also be contributory factors. The cool component is a puzzle since no evolutionary model matches its combination of low gravity and temperature. Within the constraints set by our data, SDSSJ1257+5428 could have a total mass greater than the Chandrasekhar limit and thus be a potential Type Ia supernova progenitor. However, SDSSJ1257+5428's unusually low-mass ratio q 0.2 suggests that it is more likely that it will evolve into an accreting double white dwarf (AM CVn star).

Item Type: Journal Article
Subjects: Q Science > QB Astronomy
Divisions: Faculty of Science, Engineering and Medicine > Science > Physics
Library of Congress Subject Headings (LCSH): Double stars, Supernovae, White dwarf stars
Journal or Publication Title: The Astrophysical Journal
Publisher: Institute of Physics Publishing, Inc.
ISSN: 0004-637X
Official Date: August 2011
Dates:
DateEvent
August 2011Published
Volume: Vol.736
Number: No.2
Page Range: p. 95
DOI: 10.1088/0004-637X/736/2/95
Status: Peer Reviewed
Publication Status: Published
Access rights to Published version: Restricted or Subscription Access
Date of first compliant deposit: 18 December 2015
Date of first compliant Open Access: 18 December 2015
Funder: Science and Technology Facilities Council (Great Britain) (STFC)
Related URLs:
  • Other Repository

Data sourced from Thomson Reuters' Web of Knowledge

Request changes or add full text files to a record

Repository staff actions (login required)

View Item View Item

Downloads

Downloads per month over past year

View more statistics

twitter

Email us: wrap@warwick.ac.uk
Contact Details
About Us