R CrB: Long-period variations of radial velocity and velocity of outflow

The recently discovered variation in the mean radial velocity (RV) of R CrB on a time scale of about 10,000 days may be associated with a long-term pulsation of a star with the amplitude of about 2.5 km s(-1), which results in the known mass loss of the star at the rate of 10(-6) times the mass of the Sun. It is also possible the connection with the 46-year cycle in the sequence of the great R CrB declines. The absence of an obvious connection between the onset of R CrB decline and a certain phase of the 40-day pulsation is suggested to relate to a long time delay between the processes in the noncoherently pulsating photosphere and in the zone of dust condensation. The search for the long-term variability of the RV of R CrB from the data of the recently published large homogeneous database made it possible to identify two types of unique behavior of the RV in the JD 2451500-2454400 interval immediately before the unique Great decline in 2007. At first, the RV showed a superposition of known 40-day pulsations of six pulsations with a period of 238 days, an average velocity of 25 km s(-1) and amplitude of 3 km s(-1). Near JD 2454600, this pulsation was abruptly replaced by the 792-day cycle. The cycle has a radically different half, with an average velocity about of 24.5 km s(-1). The first half can be termed abnormal because of the unique central 40-day pulsation with a very high amplitude of about 14 km s(-1). The second half of cycle is a superposition of the half-wave normal-like prolonged pulsation and pulsations with a period of about 42 days and an amplitude of about 3 km s(-1). At the beginning of the third cycle, the IV Great RCB-type decline started.