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

The nature of the X-ray transient MAXI J0556−332

Tools
- Tools
+ Tools

Cornelisse, R., D'Avanzo, P., Campana, S., Casares, J., Charles, P. A., Israel, G. L., Muñoz-Darias, T., O'Brien, K., Steeghs, D., Stella, L. and Torres, M. A. P. (2012) The nature of the X-ray transient MAXI J0556−332. Monthly Notices of the Royal Astronomical Society, Vol.420 (No.4). pp. 3538-3544. doi:10.1111/j.1365-2966.2011.20274.x

[img]
Preview
Text
WRAP_Steeghs_Maxi_1111.6946v1.pdf - Accepted Version

Download (366Kb) | Preview
Official URL: http://dx.doi.org/10.1111/j.1365-2966.2011.20274.x

Request Changes to record.

Abstract

Phase-resolved spectroscopy of the newly discovered X-ray transient MAXIJ0556-332 has revealed the presence of narrow emission lines in the Bowen region that most likely arise on the surface of the mass donor star in this low-mass X-ray binary. A period search of the radial velocities of these lines provides two candidate orbital periods (16.43 ± 0.12 and 9.754 ± 0.048h), which differ from any potential X-ray periods reported. Assuming that MAXIJ0556-332 is a relatively high-inclination system that harbours a precessing accretion disc in order to explain its X-ray properties, it is only possible to obtain a consistent set of system parameters for the longer period. These assumptions imply a mass ratio of q≃ 0.45, a radial velocity semi-amplitude of the secondary of K 2≃ 190kms -1 and a compact object mass of the order of the canonical neutron star mass, making a black hole nature for MAXIJ0556-332 unlikely. We also report the presence of strong Niii emission lines in the spectrum, thereby inferring a high N/O abundance. Finally, we note that the strength of all emission lines shows a continuing decay over the ≃1 month of our observations.

Item Type: Journal Article
Subjects: Q Science > QB Astronomy
Divisions: Faculty of Science > Physics
Library of Congress Subject Headings (LCSH): X-ray bursts, Double stars
Journal or Publication Title: Monthly Notices of the Royal Astronomical Society
Publisher: Wiley
ISSN: 0035-8711
Official Date: March 2012
Dates:
DateEvent
March 2012Published
Date of first compliant deposit: 20 December 2015
Volume: Vol.420
Number: No.4
Page Range: pp. 3538-3544
DOI: 10.1111/j.1365-2966.2011.20274.x
Status: Peer Reviewed
Publication Status: Published
Access rights to Published version: Restricted or Subscription Access
Funder: Spain. Ministerio de Educación y Ciencia (MEC), European Commission (EC), Spain. Ministerio de Ciencia e Innovación (MICINN), Seventh Framework Programme (European Commission) (FP7), Science and Technology Facilities Council (Great Britain) (STFC)
Grant number: RYC-2007-01046 (MEC), PERG04-GA- 2008-239142 (EC), AYA 2010-18080 (MICINN), CSD 2006-00070 (MICINN), ITN 215212 (FP7)

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