The outflow properties from a magnetically Keplerian protoplanetary diskin low-mass star-forming regions and the relationships with the molecular cloud core properties

In this paper, we investigate the outflow properties driven by a magnetically Keplerian protoplanetary disk and the relationships between the outflow properties and the molecular cloud core properties. We find that in the inner region of the disk (0.1–20[Formula: see text]AU), the outflow can be launched and the outflow mass-loss rate is high (10[Formula: see text]–10[Formula: see text]/year). The simulation parameters of the molecular cloud core are adopted as [Formula: see text]–[Formula: see text] [Formula: see text]s[Formula: see text], [Formula: see text] = 15–25[Formula: see text]K, [Formula: see text]–3[Formula: see text] and [Formula: see text]–10[Formula: see text]. This high mass-loss rate of outflow (10[Formula: see text]–10[Formula: see text] [Formula: see text]/year) can produce energetic luminous phenomena and can account for outbursts qualitatively. We also calculate the total kinetic power [Formula: see text] of the outflow and the luminosity of the accretion disk, and find that total kinetic power of the outflow is 0.001–3 [Formula: see text], which is roughly consistent with conventional results and observations. The terminal velocity of the outflow is from tens of km/s to a few hundreds of km/s. Moreover, we also try to find some relationships with molecular cloud core parameters (angular velocity [Formula: see text], mass [Formula: see text] and temperature [Formula: see text] and the [Formula: see text] parameter. We find that the two parameters of the molecular cloud core (angular velocity [Formula: see text] and the temperature [Formula: see text] have significant influences on outflow properties. The angular velocity [Formula: see text] has a moderate influence on the mass-loss rate of the outflow [Formula: see text], and the temperature [Formula: see text] has a significant influence on the luminosities (the outflow and the disk). The other two parameters ([Formula: see text] and [Formula: see text] have small influences (or no influences) on outflow properties. The significantly larger total kinetic power [Formula: see text] of the outflow and the luminosity of the accretion disk mean a higher temperature [Formula: see text] of the molecular cloud core, and can reflect a smaller angular momentum of the protostar [Formula: see text] disk system somewhat.