Table 2
Parameters of the observables of X-ray pulsars sample used in this study, (Pspin).
| Source | LX | B | Porb | Pspin(*) | Accretion type | Pulse profile type(*) | |
|---|---|---|---|---|---|---|---|
| [erg s−1] | [1012 G] | [d] | (XMM-Newton) [s] | (NuSTAR) [s] | |||
| SMCX-1(a) | (1−50) × 1037 | 4.56 ± 0.20 | 3.89 | 0.7002 ± 0.0007 | 0.70025 ± 0.00013 | Accretion disk | 2 |
| 4U 1901+03 (b) |  |
0.4 ± 0.1 | 22.5 | 2.7608 ± 0.0008 | BeXRB | 2 | |
 |
– | – | 2.7616 ± 0.0008 | – | 1 | ||
 |
– | – | 2.7622 ± 0.0008 | – | 2 | ||
 |
– | – | 2.7629 ± 0.0008 | – | 1 | ||
| V 0332+53 (c) | (1.24 − 1.74) × 1038 | 2.44 ± 0.05 | 33.9 | 4.3759 ± 0.0015 | BeXRB | 2 | |
| (5.7−9.5) × 1037 | – | – | 4.3759 ± 0.0017 | – | 0 | ||
| Cen X-3 (d) | (5.3−14) × 1036 | – | – | 4.3767 ± 0.0016 | – | 2 | |
| (1−5) × 1037 | 2.9–3.2 | 2.09 | 4.802 ± 0.005 | 4.797 ± 0.003 | Accretion disk | 1 | |
| LMC X-4 (e) | (2−5) × 1038 | 10–30 | 1.41 | 13.48 ± 0.05 | 13.49 ± 0.03 | Accretion disk | 0 |
| GRO J2058+42(f) | (4.0−4.4) × 1037 | 1.1 – 1.6 | 53.9 ± 1.2/110 ± 3 | 194±3 | BeXRB | 2 | |
| VelaX-1 (g) | (1−10) × 1036 | 2.60 ± 0.01 | 8.96 | 283 ± 4 | 283 ± 6 | Wind-fed | 2 |
| 1E1145.1–6141 (h) | (1−10) × 1036 | 14.4 | 297 ± 6 | 297 ± 8 | Wind-fed | 1 | |
| IGR J17252–3616 (i) | (6−16) × 1035 | 0.71 ± 0.03 | 9.74 | 412±15 | Wind-fed | 0 | |
| GX301–2 (j) | (8−20) × 1036 | 3.89 ± 0.43 | 41.5 | 680 ± 30 | 690 ± 20 | Wind-fed | 2 |
| IGR J16393–4643 (k) | (5−20) × 1036 | 2.5 ± 0.1 | 4.24 | 900 ± 20 | Wind-fed | 0 | |
Notes. Column (1): name of the observed source, Col. (2): x-ray luminosity, Col. (3): magnetic field strength, Cols. (4) and (5): spin period obtained from XMM-Newton and NuSTAR observations respectively, Col. (6): type of accretion mechanism, and Col. (7): pulse profile type according to the classification obtained in this study. The sources are ordered by their spin periods. (*) The Pspin values were obtained with the epoch folding statistic and their uncertainties as a FWHM/2 of the fitted Lorentzian distribution for each observation. The pulse profile types were obtained by qualitative classification in the groups described in this section.
References. (a)Ephemeris from Falanga et al. (2015); Brumback et al. (2020); other values from Pike et al. (2019); Pradhan et al. (2020). (b)Ephemeris from Sootome et al. (2011); luminosities from Coley et al. (priv. comm.); magnetic field from Reig & Milonaki (2016). (c)Ephemeris from Doroshenko et al. (2016); other values from Vybornov et al. (2018). (d)Ephemeris from M.H.Finger (HEAD 2010 poster); other values from Shtykovsky et al. (2017). (e)Ephemeris from Levine et al. (2000); other values from Shtykovsky et al. (2017). (f)Ephemeris not determined; other values from Mukerjee et al. (2020); Corbet et al. (1997); Wilson et al. (1998). (g)Ephemeris from Kreykenbohm et al. (2008); other values from Sidoli et al. (2015); Kretschmar et al. (2019b). (h)Ephemeris from Ray & Chakrabarty (2002); other values from Ferrigno et al. (2007). (i)Ephemeris from Manousakis & Walter (2010); other values from Manousakis et al. (2012); Zurita Heras et al. (2006).(j)Ephemeris from Doroshenko et al. (2010); other values from Nishimura (2014). (k)Ephemeris not determined; other values from Bodaghee et al. (2016); Islam et al. (2015).
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