A neutron-star merger consists of several stages starting from the late inspiral, where accurate numerical waveforms are needed to calibrate analytical models for waveforms, through merger


which requires sophisticated microphysics in terms of finite-temperature equations of state (EOS) satisfying recent observational constraints


and Mg II lines seem to arise from the same part of the BLR in various quasars (e.g.,


and should both yield similar sizes; whereas the Fe II line is thought to arise from a larger part of the BLR


Therefore, the combination of the two signals modelled as a single BLR emission could broaden our measurement and induce its slight bi-modality.


In the solar wind, the evaluation of turbulence is well described by magnetohydrodynamic (MHD) theory


and the turbulence transport throughout the heliosphere has been studied over the years (e.g.,


As mentioned above, after its discovery in 2010, V2492 underwent a long-lasting period of strong activity with intermittent burst and fading events


and reached its maximum recorded brightness in 2017


This equation, usually referred to as the Landau–Lifshitz (LL) equation, has important consequences: it is of the second order, does not violate the principle of inertia, and the self-force vanishes in the absence of the external (Lorentz) force


Many computational works have so far focused on a few important astrochemical species like H, H2, N, O, CO, and CO2, in which BEs are calculated on periodic/cluster models of crystalline/amorphous structural states using different computational techniques (e.g.,


For some Cepheids (OGL0434, OGL0501, OGL0510, OGL0512, OGL0528, OGL0545, OGL0590, OGL0712, OGL0757, OGL0966, and OGL0992), we also included V-band light curves from the


This model can naturally fit the observational positive relationships between αOX and λO as well as Γ and λO in RQAGNs


In observations, RLAGNs appear to have different properties than RQAGNs, for instance the positive relationships listed above in RQAGNs have not been found in RLAGNs


This crude selection of cluster member candidates is obviously prone to contamination by interlopers. So, we further refine it using the shifting gapper method


which uses velocity and spatial information on the candidates simultaneously. The shifting gapper method spatially distributes the candidates according to their clustercentric distance in radial bins. The mean velocity of the candidates within each bin is calculated, and those candidates with velocities that are too far from the others are rejected. As unrelaxed clusters are more likely to have a broader spatial distribution, this procedure naturally allows candidates at larger distances to be identified as cluster members for these systems. These two steps are, thus, essential to guarantee that our cluster membership algorithm implicitly takes into account the dynamical state of the systems and does not bias the measurement of their total luminosity, while minimizing contamination by interlopers at the same time.


The observed ratios of the infrared fine-structure ionic lines (Ne ii, Ar iii, and S iv;


indicate that at least eight O7.5V stars are necessary to account for the ionization of the region.


With the large number of newly discovered exoplanets expected in the next 10 years by ground-based surveys such as


as well as the ongoing Transiting Exoplanet Survey Satellite (TESS) space survey


a rapid characterization scheme of the interior structure of these planets will become increasingly necessary to further our understanding of planetary populations.


To take the contribution of f–f and f–b radiations into account and estimate the corresponding spectra, we used the chianti package


The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power


Since the light curve inversion produced convex shape models only, then shadowing and self-heating effects inside global-scale concavities (see


Through the work of Švestka & Fritzová-Švestková (1974), Kahler et al. (1978, 1984)


1983b), Cane & Stone (1984), Klecker et al. (1984), Mason et al. (1984, 1986), Meyer (1985), Reames et al. (1985, 1994, 1996), Cane et al. (1986, 1988), Luhn et al. (1987), Reames (1990, 1999), Kahler (1992, 1994), Gosling (1993), and others, involving various comparisons of SEP events with flare electromagnetic emissions and coronal mass ejections (CMEs), as well as considerations of SEP composition, charge states, and the longitude distribution of SEP-associated flares, the two-class picture of SEP acceleration presciently proposed by Wild et al. (1963) became established.


At the supranuclear densities of the outer core, the Fermi energy for protons and neutrons is well above the typical temperature of a mature neutron star, and both the neutrons and protons are expected to condense into Bardeen–Cooper–Schrieffer superfluids, with 3PF2 and 1S0 Cooper pairing, respectively


where Φmad ≈ 50Φmad,1.7 is the saturated magnetic flux