Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-21T17:36:22.895Z Has data issue: false hasContentIssue false
  • English
  • Français

V4046 Sgr: X-rays from accretion shock

Published online by Cambridge University Press:  07 August 2014

C. Argiroffi ,
A. Maggio ,
T. Montmerle ,
D. Huenemoerder ,
E. Alecian ,
M. Audard ,
J. Bouvier ,
F. Damiani ,
J.-F. Donati  and
S. Gregory
...Show all authors
C. Argiroffi
Affiliation:
Dip. di Fisica e Chimica, Università di Palermo, Palermo, Italy, email: [email protected] INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
A. Maggio
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
T. Montmerle
Affiliation:
Institut d'Astrophysique de Paris, France
D. Huenemoerder
Affiliation:
MIT, Kavli Institute for Astrophysics and Space Research, Cambridge, MA, USA
E. Alecian
Affiliation:
Observatoire de Paris, LESIA, Meudon Principal Cedex, France
M. Audard
Affiliation:
ISDC Data Center for Astrophysics, University of Geneva, Switzerland
J. Bouvier
Affiliation:
UJF-Grenoble 1/CNRS-INSU, Institut de Planetologie et d'Astrophysique de Grenoble, France
F. Damiani
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
J.-F. Donati
Affiliation:
IRAP-UMR 5277, CNRS & Univ. de Toulouse, France
S. Gregory
Affiliation:
School of Physics & Astronomy, University of St Andrews, U.K
M. Güdel
Affiliation:
Department of Astronomy, University of Vienna, Austria
G. Hussain
Affiliation:
ESO, Garching, Germany
J. Kastner
Affiliation:
Center for Imaging Science, Rochester Institute of Technology, NY, USA
G. G. Sacco
Affiliation:
INAF Osservatorio Astrofisico di Arcetri, Italy.
Rights & Permissions [Opens in a new window]

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 results of the X-ray monitoring of V4046 Sgr, a close classical T Tauri star binary, with both components accreting material. The 360 ks long XMM observation allowed us to measure the plasma densities at different temperatures, and to check whether and how the density varies with time. We find that plasma at temperatures of 1–4 MK has high densities, and we observe correlated and simultaneous density variations of plasma, probed by O VII and Ne IX triplets. These results strongly indicate that all the inspected He-like triplets are produced by high-density plasma heated in accretion shocks, and located at the base of accretion flows.

Keywords

AccretionStars: pre-main sequenceX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 46 - 47
Copyright
Copyright © International Astronomical Union 2014 

References

Argiroffi, C., Maggio, A., Montmerle, T., et al. 2012, ApJ, 752, 100CrossRefGoogle Scholar
Brickhouse, N. S., Cranmer, S. R., Dupree, A. K., Luna, G. J. M., & Wolk, S. 2010, ApJ, 710, 1835Google Scholar
Donati, J.-F., Gregory, S. G., Montmerle, T., et al. 2011, MNRAS, 417, 1747CrossRefGoogle Scholar
Kastner, J. H., Huenemoerder, D. P., Schulz, N. S., Canizares, C. R., & Weintraub, D. A. 2002, ApJ, 567, 434Google Scholar
Stempels, H. C. & Gahm, G. F. 2004, A&A, 421, 1159Google Scholar