The progenitor of binary millisecond radio pulsar PSR J1713+0747
Department of PhysicsShangqiu Normal University,
Shangqiu, PR China
2 School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, 100871 Beijing, PR China
3 Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, 210093 Nanjing, PR China
4 Facultad de Ciencias Astronómicas y Geofísicas, UNLP, Paseo del Bosque S/N, La Plata B1900 FWA, Argentina
5 Instituto de Astrofísica de La Plata (CCT La Plata), CONICET-UNLP, Argentina
Accepted: 10 January 2011
Context. PSR J1713+0747 is a binary system comprising millisecond radio pulsar with a spin period of 4.57 ms, and a low-mass white dwarf (WD) companion orbiting the pulsar with a period of 67.8 days. Using the general relativistic Shapiro delay, the masses of the WD and pulsar components were previously found to be 0.28 ± 0.03 M⊙ and 1.3 ± 0.2 M⊙ (68% confidence), respectively.
Aims. Standard binary evolution theory suggests that PSR J1713+0747 evolved from a low-mass X-ray binary (LMXB). Here, we test this hypothesis.
Methods. We used a binary evolution code and a WD evolution code to calculate evolutionary sequences of LMXBs that could result in binary millisecond radio pulsars such as PSR J1713+0747.
Results. During the mass exchange, the mass transfer is nonconservative. Because of the thermal and viscous instabilities developing in the accretion disk, the neutron star accretes only a small part of the incoming material. We find that the progenitor of PSR J1713+0747 can be modelled as an LMXB including a donor star with mass 1.3 − 1.6 M⊙ and an initial orbital period ranging from 2.40 to 4.15 days. If the cooling timescale of the WD is 8 Gyr, its present effective temperature is between 3870 and 4120 K, slightly higher than the observed value. We estimate a surface gravity of Log(g) ≈ 7.38 − 7.40.
Key words: stars: low-mass / pulsars: general / white dwarfs
© ESO, 2011