Table 1
The binary parameters for LMXBs from the ASM sample.
| Source | M1(M⊙) | M2(M⊙) | Porb(days) | q | D(kpc) | Ref. |
|
|
||||||
| OAO1657-415 | 1.4 | 14–18 | 10.4436 | 10–12.9 | 6.4 ± 1.2 | 1 |
| SS433 | ~9 | ~30 | 13.082 | ~3.33 | 5 | 2 |
| Vela X-1 | 2.27 ± 0.17 | 27.9 ± 1.3 | 8.964368 | 12.29 ± 0.35 | 1.9 ± 0.2 | |
| 1.88 ± 0.13 | 23.1 ± 0.2 | 12.29 ± 0.74 | ||||
| GX 301-2 | 1.85 ± 0.6 | 39–53 | 41.5 | 21.74 ± 6.62 | 3−4 | 5 |
| SMC X-1 | 1.06 ± 0.1 | 17.2 ± 0.6 | 3.8923 | 16.23 ± 2.10 | 61 | 6 |
| LMC X-1 | 10.91 ± 1.41 | 31.79 ± 3.48 | 3.90917 | 2.91 ± 0.70 | ~ 50 | 7 |
| 4U 1700-377 | 2.44 ± 0.27 | 58 ± 11 | 3.412 | 23.77 ± 7.14 | 1.8 | 8 |
Notes. M1 and M2 are masses of the primary and secondary companions, respectively. Porb is the orbital period, a is the binary separation, q is the mass ratio M1/M2, and D is the distance of the system. The mass of the pulsar of OAO 1657-415 has not been determined to be a certain value and we assumed it to be 1.4 M⊙ in our calculations. The two sets of parameters for HMXRB corresponds to inclination angles i = 70.1deg and 90deg, respectively.
References. (1) Chakrabarty et al. (1993); (2) Cherepashchuk et al. (2005); (3) Sadakane et al. (1985); (4) Quaintrell et al. (2003); (5) Kaper et al. (2006); (6) van der Meer et al. (2007); (7) Orosz et al. (2009); (8) Clark et al. (2002).
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