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

Multi-periodic pulsations of a stripped red-giant star in an eclipsing binary system

Tools
- Tools
+ Tools

Maxted, Pierre F. L., Serenelli, Aldo M., Miglio, Andrea, Marsh, Tom, Heber, Ulrich, Dhillon, Vik S., Littlefair, Stuart, Copperwheat, C. M., Smalley, Barry, Breedt, E. and Schaffenroth, Veronika (2013) Multi-periodic pulsations of a stripped red-giant star in an eclipsing binary system. Nature, Volume 498 (Number 7455). pp. 463-465. doi:10.1038/nature12192 ISSN 0028-0836.

Research output not available from this repository.

Request-a-Copy directly from author or use local Library Get it For Me service.

Official URL: http://dx.doi.org/10.1038/nature12192

Request Changes to record.

Abstract

Low-mass white-dwarf stars are the remnants of disrupted red-giant stars in binary millisecond pulsars(1) and other exotic binary star systems(2-4). Some low-mass white dwarfs cool rapidly, whereas others stay bright for millions of years because of stable fusion in thick surface hydrogen layers(5). This dichotomy is not well understood, so the potential use of low-mass white dwarfs as independent clocks with which to test the spin-down ages of pulsars(6,7) or as probes of the extreme environments in which low-mass white dwarfs form(8-10) cannot fully be exploited. Here we report precise mass and radius measurements for the precursor to a low-mass white dwarf. We find that only models in which this disrupted red-giant star has a thick hydrogen envelope can match the strong constraints provided by our data. Very cool low-mass white dwarfs must therefore have lost their thick hydrogen envelopes by irradiation from pulsar companions(11,12) or by episodes of unstable hydrogen fusion (shell flashes). We also find that this low-mass white-dwarf precursor is a type of pulsating star not hitherto seen. The observed pulsation frequencies are sensitive to internal processes that determine whether this star will undergo shell flashes.

Item Type: Journal Article
Divisions: Faculty of Science, Engineering and Medicine > Science > Physics
Journal or Publication Title: Nature
Publisher: Nature Publishing
ISSN: 0028-0836
Official Date: 27 June 2013
Dates:
DateEvent
27 June 2013Published
Volume: Volume 498
Number: Number 7455
Page Range: pp. 463-465
DOI: 10.1038/nature12192
Status: Peer Reviewed
Publication Status: Published
Access rights to Published version: Restricted or Subscription Access

Request changes or add full text files to a record

Repository staff actions (login required)

View Item View Item
twitter

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