Issue |
A&A
Volume 527, March 2011
|
|
---|---|---|
Article Number | A128 | |
Number of page(s) | 6 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/201014833 | |
Published online | 10 February 2011 |
Research Note
The progenitor of binary millisecond radio pulsar PSR J1713+0747
1
Department of PhysicsShangqiu Normal University,
476000
Shangqiu, PR China
e-mail: chenwc@nju.edu.cn
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
e-mail: panei@fcaglp.unlp.edu.ar
5
Instituto de Astrofísica de La Plata (CCT La Plata),
CONICET-UNLP,
Argentina
Received:
21
April
2010
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
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