Vol 44, No 3 (2018)

We present the results of our analysis of super-Eddington flares recorded fromthe X-ray pulsar LMCX-4 by theNuSTAR observatory in the energy range 3–79 keV. The pulsar spectrumis well described by the thermal Comptonization model (COMPTT) both in quiescence and during flares, when the peak luminosity reaches L_x ~ (2−4) × 10³⁹ erg s⁻¹. An important feature that has been investigated for the first time in this paper is that an increase in luminosity during flares by more than an order of magnitude is observed at energies below 25–30 keV, while at higher energies (30–70 keV) the spectrum shape and the source flux remain virtually unchanged. The increase in luminosity is accompanied by changes in the source pulse profile—in the energy range 3–40 keV it becomes approximately triangular and the pulsed fraction increaseswith rising energy, reaching 60–70%in the energy range 25–40 keV.We discuss possible changes in the geometry of the accretion column consistent with similar changes in the spectra and pulse profiles.

We have studied the simultaneous and separate solutions of the basic kinematic equations obtained using the stellar velocities calculated on the basis of data from the Gaia TGAS and RAVE5 catalogues. By comparing the values of Ω'₀ found by separately analyzing only the line-of-sight velocities of stars and only their proper motions, we have determined the distance scale correction factor p to be close to unity, 0.97 ± 0.04. Based on the proper motions of stars from the Gaia TGAS catalogue with relative trigonometric parallax errors less than 10% (they are at a mean distance of 226 pc), we have found the components of the group velocity vector for the sample stars relative to the Sun (U, V,W)_⊙ = (9.28, 20.35, 7.36) ± (0.05, 0.07, 0.05) km s⁻¹, the angular velocity of Galactic rotation Ω⁰ = 27.24 ± 0.30 km s−1 kpc−1, and its first derivative Ω'₀ = −3.77 ± 0.06 km s⁻¹ kpc⁻²; here, the circular rotation velocity of the Sun around the Galactic center is V₀ = 218 ± 6 km s⁻¹ kpc (for the adopted distance R₀ = 8.0 ± 0.2 kpc), while the Oort constants are A = 15.07 ± 0.25 km s⁻¹ kpc⁻¹ and B = −12.17 ± 0.39 km s⁻¹ kpc⁻¹, p = 0.98 ± 0.08. The kinematics of Gaia TGAS stars with parallax errors more than 10% has been studied by invoking the distances from a paper by Astraatmadja and Bailer-Jones that were corrected for the Lutz–Kelker bias. We show that the second derivative of the angular velocity of Galactic rotation Ω'₀ = 0.864 ± 0.021 km s⁻¹ kpc⁻³ is well determined from stars at a mean distance of 537 pc. On the whole, we have found that the distances of stars from the Gaia TGAS catalogue calculated using their trigonometric parallaxes do not require any additional correction factor.

To investigate the differential rotation of sunspot groups using the Greenwich data, we propose an approach based on a statistical analysis of the histograms of particular longitudinal velocities in different latitude intervals. The general statistical velocity distributions for all such intervals are shown to be described by two rather than one normal distribution, so that two fundamental rotation modes exist simultaneously: fast and slow. The differentiality of rotation for the modes is the same: the coefficient at sin² in Faye’s law is 2.87–2.88 deg/day, while the equatorial rotation rates differ significantly, 0.27 deg/day. On the other hand, an analysis of the longitudinal velocities for the previously revealed two differing populations of sunspot groups has shown that small short-lived groups (SSGs) are associated with the fast rotation mode, while large long-lived groups (LLGs) are associated with both fast and slow modes. The results obtained not only suggest a real physical difference between the two populations of sunspots but also give new empirical data for the development of a dynamo theory, in particular, for the theory of a spatially distributed dynamo.