Rotational Broadening and Doppler Tomography of the Quiescent X-Ray Nova Centaurus X-4

2; 2); 3); 5) ((1) Univ. of La Laguna; Cork; I. G. Martinez-Pais (1; Ireland; (4) Department of Astrophysics; J. Casares (2); M. A. P. Torres (1; Oxford

arxiv: astro-ph/0203406 · v1 · submitted 2002-03-22 · 🌌 astro-ph

Rotational Broadening and Doppler Tomography of the Quiescent X-Ray Nova Centaurus X-4

M. A. P. Torres (1 , 2 , 3) , J. Casares (2) , I. G. Martinez-Pais (1 , 2) , P. A. Charles (4 , 5) ((1) Univ. of La Laguna

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Spain; (2) IAC Spain; (3) Univ. College Cork Ireland; (4) Department of Astrophysics Oxford UK; (5) Univ. of Southampton UK)

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keywords starsecondarybinarybroadeningcentaurusdoppleremissionhalpha

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We present high and intermediate resolution spectroscopy of the X-ray nova Centaurus X-4 during its quiescent phase. Our analysis of the absorption features supports a K3-K5V spectral classification for the companion star, which contributes approximately 75 % of the total flux at Halpha. Using the high resolution spectra we have measured the secondary star's rotational broadening to be V_rot*sin(i) = 43 +/- 6 km/s and determined a binary mass ratio of q=0.17 +/- 0.06. Combining our results for K_2 and q with the published limits for the binary inclination, we constrain the mass of the compact object and the secondary star to the ranges 0.49 < M_1 < 2.49 Msun and 0.04 < M_2 < 0.58 Msun. A Doppler image of the Halpha line shows emission coming from the secondary star, but no hotspot is present. We discuss the possible origins of this emission.

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Rotational Broadening and Doppler Tomography of the Quiescent X-Ray Nova Centaurus X-4

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