Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-14T09:10:54.545Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopic Diagnostics of Precessing Discs: The Stream-Disc Impact in XTE J1118+480 (= KV UMA) in Outburst

Published online by Cambridge University Press:  22 February 2018

С. A. Haswell ,
S. B. Foulkes ,
D. J. Rolfe ,
J. R. Murray ,
G. H. Tovmassian ,
S. V. Zharikov ,
P. F. L. Maxted ,
R. North ,
P. A. Charles  and
R. I. Hynes
С. A. Haswell
Affiliation:
Open University, UK
S. B. Foulkes
Affiliation:
Open University, UK
D. J. Rolfe
Affiliation:
Open University, UK U. Leicester, UK
J. R. Murray
Affiliation:
U. Leicester, UK Swinburne University, Australia
G. H. Tovmassian
Affiliation:
Institutо de Astronomia, UNAM, Ensenada, México
S. V. Zharikov
Affiliation:
Institutо de Astronomia, UNAM, Ensenada, México
P. F. L. Maxted
Affiliation:
U. Keele, UK
R. North
Affiliation:
U. Southampton, UK
P. A. Charles
Affiliation:
U. Southampton, UK
R. I. Hynes
Affiliation:
U. Southampton, UK U. Texas at Austin, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present orbital trailed spectrograms of XTE J1118+480 taken at the rise to outburst maximum in 2000. These show an evolving S-wave feature arising from the stream impact on the edge of the eccentric precessing disc. By comparing the observed S-waves with those generated in an SPH simulation, we deduce the disc precession phases corresponding to our observations. Hence we infer changes in the disc precession period around the outburst maximum: taken at face value our spectroscopy suggests a precession period temporarily as short as 20 days.

Resumen

Resumen

Presentamos las trazas de espectrogramas orbitales de XTE J1118+480 tomados en el momento de alcanzar e máximo en 2000. Muestran un rasgo envolvente de onda S creciendo desde el impacto del chorro en el borde de disco excéntrico en precesión. Comparando las ondas S observadas con las generadas en una simulación SPH deducimos las fases del disco en precesión correspondientes a nuestras observaciones. A partir de ahí inferimos cambios en el período de precesión del disco alrededor del máximo de la explosión: nuestra espectroscopía sugiere un período de precesión con una duración tan corta como 20 días.

Keywords

AccretionAccretion Discs — Stars: Individual (XTE J1118+480)
Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 160 - 161
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Foulkes, S.B., Haswell, C.A., Murray, J.R., Rolfe, D.J. 2004, MNRAS, in press; astro-ph/0401xxxx.Google Scholar
Lubow, S. 1992, Ap.J, 401, 317L Google Scholar
Mineshige, S., Hirose, M., & Osaki, Y. 1992. PASJ, 14, L15 Google Scholar
Murray, J.R. 2004, these proceedingsGoogle Scholar
Torres, M. A. P. et al. 2002, ApJ, 569, 423 Google Scholar
Uemura, M. et al. 2002, PASJ, 54, 285 Google Scholar
Zurita, C. et al. 2002, MNRAS, 333, 791 Google Scholar