Investigation of rocket effect in bright-rimmed clouds using Gaia EDR3

Abstract

Bright-rimmed clouds (BRCs) are excellent laboratories to explore the radiation-driven implosion mode of star formation because they show evidence of triggered star formation. In our previous study, BRC 18 has been found to accelerate away from the direction of the ionizing H ii region because of the well known ‘Rocket Effect’. Based on the assumption that both BRC 18 and the candidate young stellar objects (YSOs) are kinematically coupled and using the latest Gaia EDR3 measurements, we found that the relative proper motions of the candidate YSOs exhibit a tendency of moving away from the ionizing source. Using BRC 18 as a prototype, we made our further analysis for 21 more BRCs, a majority of which showed a similar trend. For most of the BRCs, the median angle of the relative proper motion of the candidate YSOs is similar to the angle of on-sky direction from the ionizing source to the central IRAS source of the BRC. Based on Pearson’s and Spearman’s correlation coefficients, we found a strong correlation between these two angles, which is further supported by the Kolmogorov-Smirnov (K−S) test on them. The strong correlation between these two angles supports the ‘Rocket Effect’ in the BRCs on the plane-of-sky.

ATOMS: ALMA three-millimeter observations of massive star-forming regions – XIII. Ongoing triggered star formation within clump-fed scenario found in the massive (∼1500 M⨀) clump

“…Note that the estimated photon rate has large uncertainties because (1) The interstellar absorption is ignored. (2) The initial separation between I18290 and the exciting OB cluster can be smaller than we observe now because of the rocket effect (Saha et al 2022 ) and supernov a e vents. (3) The projection effect leads to an underestimated separation.…”

ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -XIII. Ongoing triggered star formation within clump-fed scenario found in the massive ($\sim1500$ $\rm M_\odot$) clump

“…Note that the estimated photon rate has large uncertainties because (1) The interstellar absorption is ignored. (2) The initial separation between I18290 and the exciting OB cluster can be smaller than we observe now because of the rocket effect (Saha et al 2022) and supernova events. (3) The projection effect leads to an underestimated separation.…”