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Abstract:
L1448C(N) is a young protostar in Perseus, driving an outflow and an extremely high-velocity molecular jet. We present multi-epoch observations of SiO J = 8 − 7 and CO J = 3 − 2 lines, and the 345 GHz dust continuum toward L1448C(N) in 2006, 2010, and 2017 with the Submillimeter Array. The knots traced by the SiO line show the averaged proper motion of ~0.〞06 yr−1 and ~0.〞04 yr−1 for the blue- and redshifted jet, respectively. The corresponding transverse velocities are ~78 km s−1 (blueshifted) and ~52 km s−1 (redshifted). Together with the radial velocity, we found the inclination angles of the jets from the plane of the sky to be ~34° for the blueshifted jet and ~46° for the redshifted jet. Given the new inclination angles, the mass-loss rate and mechanical power were refined to be ~1.8 × 10−6 M⊙ and ~1.3 L⊙, respectively. In the epoch of 2017, a new knot was detected at the base of the redshifted jet. We found that the mass-loss rate of the new knot is three times higher than the averaged mass-loss rate of the redshifted jet. Besides, the continuum flux has been enhanced by ~37% between 2010 and 2017. These imply that a variation of the mass-accretion rate by a factor of ~3 has occurred in a short timescale of ~10–20 yr. In addition, a knot in the downstream of the redshifted jet is found to be dimming over the three epochs.
