Variable Stars - X-ray sources
Hills Observatory: 1 January 2013 to 6 May 2018
Optically Variable Close Binary Sources of Strong, Variable X-ray Radiation (X-ray Sources) X     Close binary systems that are sources of strong, variable X-ray emission and        which do not belong to or are not yet attributed to any of the first five types of        variable stars. One of the components of the system is a hot compact object        (white dwarf, neutron star, or possibly a black hole). X-ray emission originates        from the infall of matter onto the compact object or onto an accretion disk        surrounding the compact object. In turn, the X-ray emission is incident upon the        atmosphere of the cooler companion of the compact object and is reradiated in        the form of optical high-temperature radiation (reflection effect), thus making        that area of the cooler companion's surface an earlier spectral type.  These        effects lead to quite a peculiar complex character of optical variability in such        systems. These objects may be subdivided into the following types:        XB   X-ray bursters. Close binary systems showing X-ray and optical bursts, their        duration being from several seconds to ten minutes, with amplitudes of about        0.1 mag in V (V 801 Ara, V 926 Sco); XF    Fluctuating X-ray systems showing rapid variations of X-ray (Cygnus X-1 =        V1357 Cyg) and optical (V821 Ara) radiation on time scales of dozens of        milliseconds; XI    X-ray irregulars. Close binary systems consisting of a hot compact object        surrounded by an accretion disk and a dA - dM-type dwarf.  These display        irregular light changes on time scales of minutes and hours, and amplitudes        of about 1 mag in V. Superposition of a periodic variation because of orbital        motion is possible (V818 Sco); XJ    X-ray binaries characterized by the presence of relativistic jets evident at X-ray        and radio wavelengths, as well as in the optical spectrum in the form of emission        components showing periodic displacements with relativistic velocities (V1343        Aql); XND X-ray, novalike (transient) systems containing, along with a hot compact object,        a dwarf or subgiant of G-M spectral type. These systems occasionally rapidly        increase in brightness by 4-9 mag in V, in the visible simultaneously with the        X-ray range, with no envelope ejected. The duration of the outburst may be        up to several months (V616 Mon);        XNG X-ray, novalike (transient) systems with an early-type supergiant or giant        primary component and a hot compact object as a companion.  Following the        main component's outburst, the material ejected by it falls onto the compact        object and causes, with a significant delay, the appearance of X rays. The        amplitudes are about 1-2 mag in V (V725 Tau);        XP   X-ray pulsar systems. The primary component is usually an ellipsoidal early-type        supergiant. The reflection effect is very small and light variability is mainly        caused by the ellipsoidal primary component's rotation. Periods of light changes        are between 1 and 10 days; the period of the pulsar in the system is from        1 s to 100 min. Light amplitudes usually do not exceed several tenths of a        magnitude (Vela X-1 = GP Vel); XPR X-ray pulsar systems featuring the presence of the reflection effect.  They consist        of a dB-dF-type primary and an X-ray pulsar, which may also be an optical pulsar.        The mean light of the system is brightest when the primary component is        irradiated by X rays; it is faintest during a low state of the X-ray source. The total        light amplitude may reach 2-3 mag in V (HZ Her); XPRM X-ray systems consisting of a late-type dwarf (dK-dM) and a pulsar with a        strong magnetic field. Matter accretion on the compact object's magnetic poles is        accompanied by the appearance of variable linear and circular polarization; hence        these systems are sometimes known as "polars". The amplitudes of the light        changes are usually about 1 mag in V but, provided that the primary component        is irradiated by X rays, the mean brightness of a system may increase by 3 mag        in V. The total light amplitude may reach 4-5 mag in V (AM Her, AN UMa).               If the beam of X-ray emission originating at the magnetic poles of the rotating        hot compact object does not pass through the observer's position and the system        is not observed as a pulsar, the letter "P" in the above symbols for X-ray- system        types is not used. If an X-ray system is also an eclipsing or an ellipsoidal        variable, the X-ray symbol is preceded by "E" or "ELL" joined with the X-ray        symbol by a "+" sign (e.g., E+X, ELL+X).