Fig. 3 from The X‐Ray Position and Optical Counterpart of the Accretion‐powered Millisecond Pulsar XTE J1814−338

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The X‐Ray Position and Optical Counterpart of the Accretion‐powered Millisecond Pulsar XTE J1814−338

Authors: Miriam I. Krauss, Zhongxiang Wang, Allyn Dullighan, Adrienne M. Juett, David L. Kaplan, Deepto Chakrabarty, Marten H. van Kerkwijk, Danny Steeghs, Peter G. Jonker, and Craig B. Markwardt

Krauss et al. 2005 The Astrophysical Journal 627 910.

Provider: AAS Journals

Caption: Fig. 3.

Mass‐radius relationship for a Roche lobe–filling companion of XTE J1814−338 (solid curve) and low‐mass main‐sequence stars (dashed curve), with corresponding inclination angles indicated. The dashed curve is based on the analytic mass‐radius function presented in Tout et al. (1996). The intersection of the curves suggests a companion mass of ≈0.5 M_⊙.

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